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astro-ph0303454

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we have found that the non - linear bulk viscosity terms cause no dramatic changes in the evolution of a young neutron star . they can decrease the maximum amplitude achieved by the r - modes , but can not completely saturate the modes . the reheating makes the rapid spin - down phase take place at higher temperatures , possibly simplifiying the models by avoiding the formation of a solid crust and a superfluid core . the most important consequence of reheating is that , with strong bulk viscosity at sufficiently low temperatures , it can balance neutrino cooling , keeping the star close to the instability boundary , and turning it into a persistent source of gravitational radiation for hundreds of years . the possible importance of the nonlinear terms in the bulk viscosity was realized , independently of us , by p. arras , and that of reheating through bulk viscosity by y. levin . our work on this topic was initiated during a. r.s participation in the program on `` spin and magnetism in young neutron stars '' at the itp in santa barbara , organized by l. bildsten . a. r. thanks many of the participants of that program , but specially g. ushomirsky and s. morsink , for teaching him about r - modes and the cfs instability . we are also grateful to l. lindblom for information about his work , and the organizers of the marsala workshop for their efforts , which made an excellent conference happen . most of the work presented here was funded by fondecyt grant 1020840 . andersson , n. 1998 , apj , 502 , 708 andersson , n. , jones , d. i. , & kokkotas , k. d. 2002 , mnras , 337 , 1224 arras , p. , flanagan , e. e. , morsink , s. m. , schenk , a. k. , teukolsky , s. a. , & wasserman , i. 2002 , preprint astro - ph/0202345 chandrasekhar , s. 1970 , phys . lett . , 24 , 611 friedman , j. l. , & morsink , s. m. 1998 , apj , 502 , 714 friedman , j. l. , & schutz , b. f. 1978a , apj , 221 , 937 friedman , j. l. , & schutz , b. f. 1978b , apj , 222 , 281 jones , p. b. 2001 , phys . d , 64 , 084003 levin , y. , & ushomirsky , g. 2001a , mnras , 322 , 515 levin , y. , & ushomirsky , g. 2001b , mnras , 324 , 917 lindblom , l. , & owen , b. j. 2002 , phys . d , 65 , 063006 lindblom , l. , owen , b. j. , & morsink , s. m. 1998 , phys . lett . , 80 , 4843 madsen , j. 1992 , phys . d , 46 , 3290 owen , b. j. , lindblom , l. , cutler , c. , schutz , b. f. , vecchio , a. , & andersson , n. 1998 , phys . rev . d , 58 , 084020 reisenegger , a. 1995 , apj , 442 , 749

we discuss the effect of nonlinear bulk viscosity and the associated reheating on the evolution of newly born , rapidly rotating neutron stars with r - modes destabilized through the chandrasekhar - friedman - schutz ( cfs ) mechanism . the reheating effect makes spin - down occur at a higher temperature than would otherwise be the case , in this way possibly avoiding complications associated with a solid crust or a core superfluid . on the other hand , stars with a substantial hyperon bulk viscosity and a moderate magnetic field saturate their mode amplitude at a low value , which makes them gravitational radiators for hundreds of years , while they lose angular momentum through gravitational waves and magnetic braking . # 1 # 2 _ astron . astrophys . _ * # 1 * , # 2 # 1 # 2 _ astron . astrophys . lett . _ * # 1 * , l#2 # 1 # 2 _ astron . astrophys . rev . _ * # 1 * , # 2 # 1 # 2 _ astron . astrophys . suppl . ser . _ * # 1 * , # 2 # 1 # 2 _ astron . j. _ * # 1 * , # 2 # 1 # 2 _ ann . rev . astron . astrophys . _ * # 1 * , # 2 # 1 # 2 _ astrophys . j. _ * # 1 * , # 2 # 1 # 2 _ astrophys . j. lett . _ * # 1 * , l#2 # 1 # 2 _ astrophys . j. suppl . _ * # 1 * , # 2 # 1 # 2 _ astrophys . space sci . _ * # 1 * , # 2 # 1 # 2 _ adv . space res . _ * # 1 * , # 2 # 1 # 2 _ bull . astron . inst . czechosl . _ * # 1 * , # 2 # 1 # 2 _ j. quant . spectrosc . r. astr . soc . _ * # 1 * , # 2 # 1 # 2 _ mem . r. astr . soc . _ * # 1 * , # 2 # 1 # 2 _ phys . lett . rev . _ * # 1 * , # 2 # 1 # 2 _ publ . astron . soc . japan _ * # 1 * , # 2 # 1 # 2 _ publ . astr . soc . pacific _ * # 1 * , # 2 # 1 # 2 _ nature _ * # 1 * , # 2 # 1 # 2 _ mem . soc . astron . nach . _ * # 1 * , # 2 epsf.sty

we discuss the effect of nonlinear bulk viscosity and the associated reheating on the evolution of newly born , rapidly rotating neutron stars with r - modes destabilized through the chandrasekhar - friedman - schutz ( cfs ) mechanism . bulk viscosity in these stars is due to the adjustment of the relative abundances of different particle species as the density of a fluid element is perturbed . it becomes nonlinear when the chemical potential difference @xmath0 , measuring the chemical imbalance in the fluid element , becomes larger than the temperature @xmath1 , which is generally much smaller than the fermi energy . from this scale on , the bulk viscosity increases much faster with @xmath0 than predicted by the usual , linear approximation . this provides a potential saturation mechanism for stellar oscillation modes at a small to moderate amplitude . in addition , bulk viscosity dissipates energy , which can lead to neutrino emission , reheating of the star , or both . this is the first study to explicitly consider these effects in the evolution of the r - mode instability . for stars with little or no hyperon bulk viscosity , these effects are not strong enough to prevent the r - modes from growing to amplitudes @xmath2 or higher , so other saturation mechanisms will probably set in earlier . the reheating effect makes spin - down occur at a higher temperature than would otherwise be the case , in this way possibly avoiding complications associated with a solid crust or a core superfluid . on the other hand , stars with a substantial hyperon bulk viscosity and a moderate magnetic field saturate their mode amplitude at a low value , which makes them gravitational radiators for hundreds of years , while they lose angular momentum through gravitational waves and magnetic braking . # 1 # 2 _ astron . astrophys . _ * # 1 * , # 2 # 1 # 2 _ astron . astrophys . lett . _ * # 1 * , l#2 # 1 # 2 _ astron . astrophys . rev . _ * # 1 * , # 2 # 1 # 2 _ astron . astrophys . suppl . ser . _ * # 1 * , # 2 # 1 # 2 _ astron . j. _ * # 1 * , # 2 # 1 # 2 _ ann . rev . astron . astrophys . _ * # 1 * , # 2 # 1 # 2 _ astrophys . j. _ * # 1 * , # 2 # 1 # 2 _ astrophys . j. lett . _ * # 1 * , l#2 # 1 # 2 _ astrophys . j. suppl . _ * # 1 * , # 2 # 1 # 2 _ astrophys . space sci . _ * # 1 * , # 2 # 1 # 2 _ adv . space res . _ * # 1 * , # 2 # 1 # 2 _ bull . astron . inst . czechosl . _ * # 1 * , # 2 # 1 # 2 _ j. quant . spectrosc . . transfer _ * # 1 * , # 2 # 1 # 2 _ mon . not . r. astr . soc . _ * # 1 * , # 2 # 1 # 2 _ mem . r. astr . soc . _ * # 1 * , # 2 # 1 # 2 _ phys . lett . rev . _ * # 1 * , # 2 # 1 # 2 _ publ . astron . soc . japan _ * # 1 * , # 2 # 1 # 2 _ publ . astr . soc . pacific _ * # 1 * , # 2 # 1 # 2 _ nature _ * # 1 * , # 2 # 1 # 2 _ mem . soc . astron . it . _ * # 1 * , # 2 # 1 # 2 _ the messenger _ * # 1 * , # 2 # 1 # 2 _ astron . nach . _ * # 1 * , # 2 epsf.sty

hep-ph9805295

i

experimentally , the vast majority of data sensitive to parton densities have been taken without fixing the polarization of the initial beams or the target . the densities extracted in this way are usually refered to as the ` unpolarized ' parton distributions @xmath0 ( @xmath1 ) . within roughly the last decade , also more and more data have become available that are sensitive to the ` longitudinally ' polarized ( ` helicity weighted ' ) parton densities of the nucleon . the tool to obtain such information has ( almost exclusively ) been deep inelastic scattering ( dis ) of longitudinally polarized leptons and nucleons . the spin asymmetry measured in such reactions is related to the probability for finding a certain parton type with positive helicity in a nucleon of positive helicity _ minus _ the probability for finding it with negative helicity . these densities , denoted as @xmath2 ( @xmath1 ) , contain information different from that contained in the more familiar unpolarized ones . for a _ transversely _ polarized spin@xmath3 hadron one can define a further quark density @xcite in very much the same way as the longitudinally polarized quark distributions , by taking differences of probabilities for finding quarks with transverse spin aligned and anti aligned with the transverse hadron spin . these densities are called ` transversity ' densities and are denoted by @xmath4 . it turns out that unlike the situation for unpolarized and longitudinally polarized densities there is _ no _ gluonic analogue of quark transversity @xcite . this is due to angular momentum conservation : transversity densities are related to helicity flip amplitudes . a gluonic helicity flip amplitude would require the hadron to absorb two units of helicity , which no spin@xmath3 target can do . the transversity distributions are completely unmeasured so far since they can not be directly accessed in dis . it seems certain , however , that measurements of the @xmath5 will be attempted at the future polarized proton - proton collider rhic at brookhaven @xcite . the most suitable candidate for such measurements is believed to be drell yan dimuon production @xcite . the @xmath5 complete the twist2 sector of parton densities of spin@xmath3 hadrons . nevertheless , we have not yet depleted the full set of parton densities that can be defined if spin is taken into account . there finally is a further spin dependent _ gluon _ distribution that to some extent can be regarded as the gluonic counterpart of quark transversity . unlike the ` helicity ' density @xmath6 that describes _ circular _ polarization of the gluon , it is encountered if the gluon is _ linearly _ polarized @xcite . the density is denoted by @xmath7 and exists only in a linearly polarized hadron ( or photon @xcite ) , which therefore has to have spin @xmath8 . there is no quark distribution in this case @xcite . even though a measurement of @xmath9 does not seem very realistic at the moment , it possesses some interesting theoretical aspects which justify its analysis . table 1 summarizes the parton densities we have defined . .list of twist2 quark and gluon densities including spin dependence . we have suppressed the ubiquitous argument @xmath10 of the densities . note that ` @xmath11 ' always runs over quarks as well as over antiquarks . labels @xmath12 denote helicities , @xmath13 transverse polarizations , and @xmath14 ( @xmath15 ) stands for linear polarization along the @xmath16 ( @xmath17 ) axis , where the particle is moving along the @xmath18direction . subscripts refer to partons and superscripts to the parent hadron . [ cols="^,^,^",options="header " , ] it is important to realize that each set of parton densities in tab . 1 ( i.e. , each of the rows of tab . 1 ) is subject to its own set of evolution equations . for instance , the evolution of the longitudinally polarized densities proceeds independently from that of the unpolarized partons , and so forth . in this way , we are led to introducing separate sets of evolution kernels ( splitting functions ) for each type of polarization . the @xmath19evolution of the unpolarized densities has been worked out up to nlo accuracy of qcd already a long time ago @xcite , and it has become standard since about ten years to analyse the unpolarized data within the nlo framework . the lo evolution of the @xmath2 , the @xmath20 , and of @xmath21 has also been known for a long time @xcite , whereas the derivation of the nlo evolution kernels for longitudinally polarized partons has been a more recent development @xcite . very recently , the nlo splitting functions for transversity were derived within three independent calculations @xcite . in this paper , we will discuss the nlo evolution of the @xmath5 , and its implications for an inequality between the @xmath22 , @xmath23 and @xmath5 derived by soffer @xcite . we will also for the first time present the nlo evolution kernel for @xmath9 .

we discuss the nlo evolution of quark transversity densities and of the parton distribution function for linearly polarized gluons in a linearly polarized hadron . a supersymmetric relation between the nlo evolution kernels for transversity and for linear polarization we also study the implications of nlo evolution for soffer s inequality and the prospects of measuring transversity densities in polarized drell

we discuss the nlo evolution of quark transversity densities and of the parton distribution function for linearly polarized gluons in a linearly polarized hadron . a supersymmetric relation between the nlo evolution kernels for transversity and for linear polarization is found . we also study the implications of nlo evolution for soffer s inequality and the prospects of measuring transversity densities in polarized drell yan at rhic . cern - th/98 - 151 + + + theory division , cern , ch-1211 geneva 23 , switzerland

1405.5341

i

this article deals with some algorithmic questions related to linear differential operators in positive characteristic @xmath0 . more precisely , we address the problem of the efficient computation of the characteristic polynomial of the @xmath0-curvature of such a differential operator @xmath1 . roughly speaking , the @xmath0-curvature of @xmath1 is a matrix that measures to what extent the solution space of @xmath1 has dimension close to its order . the theory was initiated in the 1970s by katz , dwork and honda @xcite in connection with one of grothendieck s conjectures which states that an irreducible linear differential operator with coefficients in @xmath5 admits a basis of algebraic solutions over @xmath5 if and only if its reductions modulo @xmath0 admit a zero @xmath0-curvature for almost all primes @xmath0 . let @xmath6 be _ any _ field of characteristic @xmath0 , and let @xmath7 be the algebra of differential operators with coefficients in @xmath8 , with the commutation rule @xmath9 . the @xmath0-curvature of a differential operator @xmath1 of order @xmath10 in @xmath11 , hereafter denoted @xmath12 , is the @xmath13 matrix with coefficients in @xmath8 , whose @xmath14 entry is the coefficient of @xmath15 in the remainder of the euclidean ( right ) division of @xmath16 by @xmath1 , for @xmath17 . we focus on the computation in good complexity , notably with respect to the parameter @xmath0 , of the characteristic polynomial @xmath2 of the @xmath0-curvature @xmath18 . an important sub - task is to decide efficiently whether @xmath18 is nilpotent . by a celebrated theorem of the chudnovskys @xcite , least order differential operators satisfied by @xmath19-series possess reductions modulo @xmath0 with nilpotent @xmath0-curvatures for almost all primes @xmath0 . studying the complexity of the computation of @xmath2 is an interesting problem in its own right . this computation is for instance one of the basic steps in algorithms for factoring linear differential operators in characteristic @xmath0 @xcite . additional motivations for studying this question come from concrete applications , in combinatorics @xcite and in statistical physics @xcite , where the @xmath0-curvature serves as an _ a posteriori _ certification filter for differential operators obtained by guessing techniques from power series expansions . in such applications , the prime number @xmath0 may be quite large ( thousands , or tens of thousands ) , since its value is lower bounded by the precision of the power series needed by guessing , which is typically large for operators of large size . this explains our choice of considering @xmath0 as the most important complexity parameter . * previous work . * since @xmath7 is noncommutative , binary powering can not be used to compute @xmath20 . katz @xcite gave the first algorithm for @xmath12 , based on the recurrence @xmath21 where @xmath22 is the companion matrix associated to @xmath1 . this algorithm , as well as its variants @xcite and ( * ? ? ? * prop . 3.2 ) have complexity quadratic in @xmath0 . the first subquadratic algorithm was designed in @xcite . it has complexity @xmath4 and it is based on the observation that the @xmath0-curvature @xmath18 is obtained by applying the matrix operator @xmath23 to @xmath24 , and on a baby steps / giant steps algorithm for applying differential operators to polynomials . several partial results concerning the @xmath0-curvature were obtained in @xcite : computation of @xmath18 in @xmath25 for _ first order _ operators and in quasi - linear time @xmath26 for _ certain second order _ operators ; algorithms of complexity @xmath27 for deciding nilpotency of @xmath12 for _ second order _ operators , and @xmath26 for the nullity of @xmath12 for _ arbitrary operators_. * our contribution . * prior to this work , the computation of the characteristic polynomial of the @xmath0-curvature required the computation of the @xmath0-curvature itself as a preliminary step . we manage to compute @xmath2 without @xmath18 by exploiting in a completely explicit and elementary way the fact that the weyl algebra @xmath28\langle \partial \rangle$ ] is a central separable ( azumaya ) algebra over its centre @xmath29 $ ] , and thus endowed with a _ reduced norm map _ @xcite . our crucial observation is that the characteristic polynomials of the @xmath0-curvature of elements in @xmath11 are closely related to other polynomials associated to operators lying in the skew ring @xmath30 on which the multiplication is determined by the rule @xmath31 . more precisely , given such an operator @xmath1 , we define its @xmath0-curvature @xmath32 and compare its characteristic polynomial to that of @xmath12 when @xmath1 makes sense in both rings @xmath11 and @xmath33 ( theorem [ theo : comparison ] ) . in addition , the computation of the characteristic polynomial of @xmath32 reduces to that of a matrix factorial of length @xmath0 , which can be performed in @xmath3 operations in @xmath6 via the baby steps / giant steps approach in @xcite . this allows us to compute @xmath2 in complexity quasi - linear in @xmath34 . * structure of the paper . * in section [ sec : rings ] , we introduce all rings of differential operators that we need and recall their basic properties . section [ sec : pcurv ] is devoted to the theoretical study of the @xmath0-curvature of there differential operators and culminates in the proof of theorem [ theo : comparison ] . in section [ sec : algo ] , we move to applications to algorithmics : after some preliminaries , we describe our main algorithm for computing @xmath2 in complexity @xmath3 . we conclude with the implementation of our algorithm and some benchmarks and applications . * acknowledgements . * we would like to thank the referees for their insightful remarks . this work was supported by nserc , the crc program and the msr - inria joint centre .

we discuss theoretical and algorithmic questions related to the @xmath0-curvature of differential operators in characteristic @xmath0 . given such an operator @xmath1 , and denoting by @xmath2 the characteristic polynomial of its @xmath0-curvature , we first prove a new , alternative , description of @xmath2 . this description turns out to be particularly well suited to the fast computation of @xmath2 when @xmath0 is large : based on it , we design a new algorithm for computing @xmath2 , whose cost with respect to @xmath0 is @xmath3 operations in the ground field . this is remarkable since , prior to this work , the fastest algorithms for this task , and even for the subtask of deciding nilpotency of the @xmath0-curvature , had merely slightly subquadratic complexity @xmath4 . # 1 # 1 # 1#1 [ section ] [ theo]lemma [ theo]proposition [ theo]corollary [ theo]question [ theo]example [ theo]remark [ theo]definition * categories and subject descriptors : * + i.1.2 [ * computing methodologies * ] : symbolic and algebraic manipulation _ algebraic algorithms _ * general terms : * algorithms , theory * keywords : * algorithms , complexity , differential equations , @xmath0-curvature .

we discuss theoretical and algorithmic questions related to the @xmath0-curvature of differential operators in characteristic @xmath0 . given such an operator @xmath1 , and denoting by @xmath2 the characteristic polynomial of its @xmath0-curvature , we first prove a new , alternative , description of @xmath2 . this description turns out to be particularly well suited to the fast computation of @xmath2 when @xmath0 is large : based on it , we design a new algorithm for computing @xmath2 , whose cost with respect to @xmath0 is @xmath3 operations in the ground field . this is remarkable since , prior to this work , the fastest algorithms for this task , and even for the subtask of deciding nilpotency of the @xmath0-curvature , had merely slightly subquadratic complexity @xmath4 . # 1 # 1 # 1#1 [ section ] [ theo]lemma [ theo]proposition [ theo]corollary [ theo]question [ theo]example [ theo]remark [ theo]definition * categories and subject descriptors : * + i.1.2 [ * computing methodologies * ] : symbolic and algebraic manipulation _ algebraic algorithms _ * general terms : * algorithms , theory * keywords : * algorithms , complexity , differential equations , @xmath0-curvature .

0803.3075

r

the five wfcam tiles used in this paper cover the western portion of perseus , which includes ngc1333 , l1455 , l1448 , and barnard 1 ( b1 ) . wfcam h@xmath0 images of regions where outflows were detected are shown in figs [ h2b1][h2ngc1333s ] . the positions of protostars and ysos identified in the spitzer c2d survey are overplotted in each figure . circles indicate sources that were given the `` yso '' designation in the c2d catalogue , while triangles mark sources classified as `` red '' , `` red2 '' , `` pah - em '' , or `` star+dust '' . @xcite have compared the c2d data with scuba observations at 850@xmath1 m . they present a catalogue of 49 `` embedded '' ysos ; all are mips detections that are either red in [ 3.6]-[4.5 ] and [ 8.0]-[24 ] colours or are located within 15 of scuba peaks . they also include a few concentrated scuba cores with no mips counterparts . we label these sources as `` yso '' with the numbers from jrgensen et al.s catalogue ( their table 3 ) and list those sources located in the perseus - west region in table [ outflows ] . the locations of herbig - haro ( hh ) objects found by @xcite in their wide - field optical imaging , as well as hh objects that were previously known , are also marked on our figures . note that these positions are often rather vague , representing the location of what is usually an extended object or diffuse feature . in the online appendix we present ukirt - wfcam / spitzer - irac colour - composite images of each region , and discuss the outflows marked in figs . [ h2b1][h2ngc1333s ] in some detail , noting in particular the association of h@xmath0 emission - line features with hh objects , molecular co outflows , dense cloud cores and the embedded source identified through spitzer photometry . h@xmath0 knot parameters ( flow position angles , flow lengths , associated hh objects , etc . ) are listed in table [ jets ] , where we also give the embedded yso that is likely to be driving each flow . many of these knots or groups of knots are known hh objects or parts of outflows imaged in less extensive surveys . we therefore also list the names of associated hh objects and previous h@xmath0 outflow names in table [ jets ] . overall , the combined wfcam h@xmath0 imaging , spitzer imaging and photometry , and co outflow observations provide a clear and rather complete picture of dynamic activity in perseus - west . our wfcam observations demonstrate that even shallow h@xmath0 imaging is an effective tool for finding outflows from the youngest ysos . of the 26 molecular outflows in our wfcam tiles , 24 of them ( 92% ) are driven by sources identified as embedded ysos by @xcite ; only 9% of the 85 h@xmath0 features have no obvious co flow counterpart or jrgensen ysos . the two outflow sources not identified by jrgensen et al . as embedded yso , lkh@xmath4327 and l1448-irs1 , were probably missed because of saturation in the spitzer bands . neither source coincides with a scuba core @xcite , so these bright sources have probably already cleared their cores . of the 38 jrgensen ysos in our field , 24 ( 63% ) drive outflows . clearly , the criteria used by @xcite ( mips / irac colours [ 3.6]-[4.5]@xmath31 and [ 8.0]-[24]@xmath34.5 and/or associated scuba cores ) is not only very good at identifying ysos , but also at identifying ysos that drive molecular outflows . shock - excited outflow features can of course be detected at both optical and infrared wavelengths , by virtue of their forbidden emission lines ( [ oi ] , [ sii ] , [ oiii ] , etc . ) , hydrogen recombination lines ( h@xmath4 ) , or in the near - ir and mid - ir molecular hydrogen ro - vibrational lines . however , the longer - wavelength transitions will be more effective in regions of high extinction . also , these lines derive from very different gas components : the optical lines typically trace hot , dense , partially - ionised , high - velocity gas ( t@xmath1010,000k ; flow velocities approaching 100 - 200 km s@xmath11 ) while the h@xmath0 lines trace low - excitation , shocked molecular gas at much lower velocities ( t@xmath10500 - 2,000k ; v@xmath1010 - 50 km s@xmath11 ) . it is therefore perhaps not surprising that , of the 158 hh objects from @xcite in our field , only 72 ( 46% ) of them were detectable in h@xmath0 2.122@xmath1 m emission . similarly , only 37 ( 44% ) of the 85 labelled h@xmath0 features are associated with an hh object . many of the hh objects are faint in the optical , so in a few cases the lack of a detection in near - ir h@xmath0 emission may be due to the modest sensitivity of the wfcam survey . however , many of the hh objects are located around the periphery of each star - forming cloud ( see for example the comparison of hh and h@xmath0 positions in fig . [ h2ngc1333 ] ) , where the molecular gas density may be too low to facilitate h@xmath0 excitation . clearly , a colour - composite image comprised of optical ( [ sii ] or h@xmath4 ) , near - ir 2.12@xmath1 m and mid - ir 4.5@xmath1 m imaging would be ideal for illustrating the high - excitation atomic / ionised ( hh ) , hot molecular ( ro - vibrational h@xmath0 ) , and warm molecular ( pure - rotational h@xmath0 ) flow components simultaneously , as well as the colours of white / blue foreground stars through to the reddest protostars . such a comparison is obviously now possible with ground - based optical imaging , wfcam survey data , and spitzer observations , for a number of well - known star forming regions . = 16.5 cm = 16.5 cm of the 26 h@xmath0 outflows identified in column 2 in table [ outflows ] , 20 ( 77% ) exceed an arcminute in mean length ; three are parsec - scale flows , with a mean lobe length exceeding 11.5 ( the outflows driven by ysos 2 , 5 , and 20c ) . longer flows might be expected from more evolved sources , and indeed yso 20c and yso 5 do have flat spectral indices . however , yso 2 has a steeply rising sed ( @xmath12 ) . this high value of @xmath4 may in part be due to excess emission from lines in some of the spitzer bands ( discussed below ) . however , when we plot flow length against spitzer spectral index we find no correlation between these two parameters . this suggests that even the most deeply embedded h@xmath0 jet source are old enough to produce parsec - scale flows . it seems likely that jet length , when derived from h@xmath0 observations , is more sensitive to the environment ( specifically the presence of ambient molecular gas that may be shock - excited into emission ) than the `` age '' of the jet central engine . can we say anything about flow opening angles from our sample of jets in perseus - west ? high - resolution co maps of outflows seem to indicate that class 0 sources produce more collimated flows than their more evolved class i counterparts ( e.g. * ? ? ? * ; * ? ? ? h@xmath0 emission features ( bow shocks ) often envelope the outer edges of co flow lobes , so one might expect to see a similar trend in h@xmath0 data . however , shock - excited h@xmath0 emission has a very short cooling time ( of the order of a few years ) , so h@xmath0 features are often short - lived and confined to a small percentage of the flow surface area . moreover , close to the central source h@xmath0 emission features tend to be associated with the central , on - axis jet rather than the swept - out cavity walls . defining flow opening angles from h@xmath0 images is therefore rather difficult . even so , in table [ outflows ] we list the mean opening angle , @xmath13 , for well - defined flows with multiple , bright h@xmath0 emission features . @xmath13 is measured from cones in each flow lobe that are centred on the outflow source and which include all h@xmath0 line - emission features . a plot of @xmath13 against source spectral index @xmath4 ( not shown ) reveals no correlation between these two parameters . at best , we can only say that most of the flows in perseus - west appear to be well collimated , as is expected for jets from young , embedded ( high-@xmath4 ) sources . the opening angles listed have a mean of 12.5@xmath6 and a standard deviation of only 4.1@xmath6 . the associated sources have a relatively broad range in @xmath4 : -0.87 to 3.79 . many of the h@xmath0 jets in perseus appear to be curved or possibly even precessing . if both lobes curve in the same direction ( h@xmath0 features 24 in the b1 ridge and 76/77 in l1448 are good examples ) the flow curvature may be due to the motion of the source through the ambient medium . in such cases the source would need a proper motion that is a sizable fraction ( at least a few percent ) of the jet velocity . source tangential velocities of the order of 1 - 10 km s@xmath11 would be required . alternatively , the _ apparent _ curvature may simply be due to excitation of h@xmath0 along only one side of an oval cavity , perhaps because of enhanced ambient gas densities or an ambient density gradient across the width of the flow lobe . precession or jet `` meandering '' has been identified in a number of flows ( e.g. * ? ? ? * ; * ? ? ? * ; * ? ? ? precession may result from the misalignment of binary orbital and circum - binary disk axes @xcite , although the disk should be forced into alignment with the orbital plane in roughly one precession period , which should be about 20-times longer than the binary orbital period @xcite . given this time limitation , jet precession is expected from only the most embedded and therefore potentially very youngest sources . notably , ysos 11 , 14 and 38 , the three precessing jet candidates in perseus - west , all have high values of @xmath4 . the h@xmath0 flows from ysos 11 , 14 and 38 appear to have precessed through roughly half a turn . the dynamical age of each flow should thus be a fair estimate of the precession period , to within a factor of @xmath102 @xcite . for a canonical jet velocity of 100 km s@xmath11(consistent with jet proper motions , e.g. * ? ? ? * ) , from the flow lengths listed in table [ outflows ] , flow ages of 7300 yrs , 1400 yrs and 2600 yrs are estimated . hence , a very crude range for the precession period of these remarkable flows is 2800 - 14,600 yrs . [ histograms ] demonstrates how the outflow sources differ from the bulk of the c2d - catalogue ysos in perseus . the outflow sources , plotted with black filled bars , are generally much redder and have a steeper near - ir / mid - ir sed than the general yso population . the flow sources identified in this paper have a mean spectral index ( @xmath4 ) of 1.39@xmath141.14 ; the c2d ysos , which are predominantly class ii t tauri stars , have a mean @xmath4 of -0.32@xmath140.89 . ( in the c2d catalogue , in regions with @xmath15 where sources are mostly background main sequence stars , the average value of @xmath4 is -2.8 : evans et al . 2005 . ) the outflow sources also occupy a relatively distinct region in colour - colour space ( fig . [ ccandcmag ] ) . they possess a high [ 4.5]-[24 ] irac / mips colour , as predicted for young sources with massive accretion disks @xcite . however , they also exhibit positive [ 3.6]-[4.5 ] colours , unlike the bulk of the c2d ysos , where the near - zero [ 3.6]-[4.5 ] colours are due to the intrinsic shape of the yso sed . in fig . [ ccandcmag ] , 80% of the outflow sources that have measured 3.6@xmath1 m and 4.5@xmath1 m magnitudes have a [ 3.6]-[4.5 ] colour greater than 1 . this is compared to only 11% of the total c2d catalogue of ysos in perseus . of the ysos with a [ 3.6]-[4.5 ] colour greater than 1.0 , 18% have outflows ; only 0.4% of ysos with [ 3.6]-[4.5]@xmath161.0 drive outflows . all factors point to the association of outflows traced in h@xmath0 with the youngest class 0/i protostars . in fig . [ alphacolor ] we plot @xmath4 against [ 3.6]-[4.5 ] colour for the entire perseus c2d catalogue . sources with values of @xmath4 derived from just the two spitzer bands plotted on the x - axis ( i.e. those detected in only bands 1 and 2 ) lie along a narrow , diagonal strip . sources detected in multiple spitzer and/or 2mass bands exhibit some scatter about this strip , since @xmath4 is derived from photometry points that are modified by various absorption features ( ice , silicate dust , etc . ) and emission lines ( h@xmath0 , [ feii ] , [ neii ] , etc . ) , as well as the intrinsic shape of the yso sed ( i.e. that of an embedded source with a disk and probably also a disk - hole ) . the spitzer ysos tend towards higher values of @xmath4 and redder [ 3.6]-[4.5 ] colours , though they are largely indistinguishable from the other sources ( field stars , background galaxies , etc . ) in this plot . however , the outflow sources stand out as having excess emission at 4.5@xmath1 m and thus red [ 3.6]-[4.5 ] colours . this is partly due to the inclusion of emission lines associated with infall and outflow in their integrated 4.5@xmath1mfluxes . the 4.5@xmath1 m spitzer band covers the h@xmath0 pure - rotational 0 - 0s(9 ) , s(10 ) and s(11 ) lines at 4.69 , 4.41 and 4.18@xmath1 m , as well as the co v=1 - 0 band between 4.45 - 4.95@xmath1 m and the hi br@xmath4 line at 4.052@xmath1 m , both of which may be excited in accretion flows . some of the sources identified in the c2d catalogue as ysos , based on their spitzer colours and/or spectral index , will in fact be molecular hydrogen emission - line knots . shock models developed by @xcite predict [ 3.6]-[4.5 ] colours in excess of @xmath100.5 , as well as positive values for @xmath4 ( when derived from all four irac bands ) . these predictions are supported by recent spitzer observations of hh 46/47 , where the jet and bow shocks are detected in all four irac channels @xcite note that there are pure - rotation h@xmath0 emission lines in all of the irac bands . in fig . [ alphacolor ] we plot the [ 3.6]-[4.5 ] colours and corresponding spectral indices for six shock models . the arrows indicate the effect of 5 magnitudes of k - band extinction ( reddening moves the points to the upper - right in the figure ) . the arrow labelled `` planar '' represents a slab of molecular gas at a temperature of 2000 k with a density of @xmath17 @xmath18 . arrows labelled c80 , c50 , c40 and c20 are c - type bow shocks : all have the same shape and post - shock density ( @xmath17 @xmath18 ) , differing only in shock velocity ( 80 km s@xmath11 , 50 km s@xmath11 , 40 km s@xmath11 and 20 km s@xmath11 respectively ) . decreasing shock velocity pushes the c - bow data points toward the upper - right in fig . [ alphacolor ] . higher values of @xmath4 and redder [ 3.6]-[4.5 ] colours are produced by a relative increase in emission from the lower - energy pure - rotational h@xmath0 lines ( 0 - 0s(4 ) and s(5 ) in irac band 4 and 0 - 0s(6 ) and s(7 ) in band 3 ) over the higher energy 0 - 0 lines ( s(9)-s(11 ) in band 2 and s(13 ) and above in band 1 ) and ro - vibrational lines ( 1 - 0o(5 ) and o(7 ) in band 1 ) at shorter wavelengths . the fastest c - type bow , c80 , has a dissociative cap and is much like the j - type bow shock . it is therefore not too surprising that it coincides almost precisely with the 50 km s@xmath11 j - type bow model arrow , j50 , in fig . [ alphacolor ] . the shock model data points overlap quite significantly with the outflow sources in fig . [ alphacolor ] . the c2d `` ysos '' that are most likely to be h@xmath0 knots , features 7 , 12 , 13 , 16 , 38 , 49 and 72 ( the green circles in fig . [ alphacolor ] ) have relatively low values of @xmath4 and therefore appear to be associated with either fast c - type or j - type bow shocks . the low spectral indices measured for the observed knots could be caused by co bandhead emission in irac band 2 or the inclusion of 24@xmath1 m data when calculating @xmath4 for the observed knots . we do not include this data point in the model points , since there are no h@xmath0 lines in the mips 24@xmath1 m bandpass . however , weak forbidden emission from [ feii ] at 24.51@xmath1 m and 25.98@xmath1 m ( like that seen in hh 46/47 ; * ? ? ? * ) could result in the `` weak '' detection of an outflow feature in this band in the c2d catalogue , and hence a lower value of @xmath4 based on a fit to irac and mips data . co emission is unlikely to contribute to observed outflow photometry data since very high densities , in excess of 10@xmath19 @xmath18 , are required to produce appreciable flux from this molecule . however , under such circumstances ( seen perhaps in high - mass star forming regions ) co could account for as much as 10% of the observed emission in irac band 2 . = 8.4 cm the number of outflows identified here matches ( to within 20% ) the number of protostellar cores in l1448 , l1455 and b1 @xcite , though it is lower by a factor of 2 in ngc1333 . in this densely - populated region this discrepancy is partly due to h@xmath0 features being identified as part of a single flow , when in fact they are associated with multiple flows . even so , the association of protostellar cores with molecular ( h@xmath0/co ) outflows is clear . it is also worth noting that the more massive clouds produce more outflows in perseus - west . in b1 , ngc1333 , l1448 and l1455 we identify ( at least ) 8 , 11 , 4 and 5 outflows , respectively . from near - ir extinction mapping of perseus , maps which cover an @xmath20 range of about 3 - 7 , @xcite identify large scale structures which they refer to as `` supercores '' . they stress that the bulk of the cloud material is contained in these extensive , moderate - density regions , rather than in the high - extinction cores not traced by the extinction map . kirk et al . measure masses of 441m@xmath21 , 973m@xmath21 , 174m@xmath21 and 240m@xmath21 for the b1 , ngc1333 , l1448 and l1455 supercores , respectively . thus , in perseus - west there is one molecular outflow for every 44 - 88m@xmath21 of ambient material . roughly 50 generations of accretion / outflow activity would be needed to convert all of this molecular material into solar - mass stars . in some regions many of the jets appear to be roughly parallel , though this common angle is not obviously related to the large - scale cloud structure . l1448 is perhaps the best example , where the position angles of the four outflows identified in fig . [ h2l1448 ] are between 147@xmath6 and 155@xmath6 . @xcite fit 2-dimensional gaussians to their supercores and , from their fig . 5 , we measure a supercore position angle of 120@xmath6 for l1448 . in l1448 , the outflows thus appear to flow along the length of the supercore . however , the two parallel flows in the b1-ridge region ( fig . [ h2b1r ] ; pas of 124@xmath6 and 130@xmath6 ) are almost perpendicular to the elongated b1-ridge supercore ( pa @xmath10 50@xmath6 ) . the flows in b1 , ngc1333 and l1455 are more randomly orientated , although at least four of the larger flows in ngc1333 are aligned roughly north - south , parallel with the associated supercore ( pa @xmath10 10@xmath6 ) . even so , we conclude that in general the outflows are randomly orientated and that the large - scale could structure , as traced by the extinction mapping of @xcite , has no obvious influence on flow orientations . molecular outflows from young stars inject turbulent energy and momentum into the surrounding medium . over time these flows probably provide turbulent support against cloud collapse and may even hinder the star formation process . in low - mass star forming regions usually only a dozen or so outflows are observed at any one time ( ngc1333 is a good example ) . here we investigate whether these outflows provide sufficient kinetic energy to account for the observed turbulence in the ambient medium . as was noted by @xcite , one can estimate the turbulent momentum and energy in a star - forming region from the cloud mass , @xmath22 , and velocity dispersion , @xmath23 , measured from ( sub)millimetre molecular lines : * for perseus - west we again use cloud masses from @xcite . the masses of their supercores ( estimated from 2mass extinction mapping for @xmath243 ) are listed in sect . 4.4 . although a sizable fraction of the overall cloud mass is likely to be in diffuse , lower-@xmath25 regions , outflows are unlikely to impart much of their momentum into these extended regions . also , masses derived from an extinction map are preferred over masses estimated from molecular line observations , since the latter may suffer from depletion and/or opacity effects . and like submillimetre dust continuum maps , optically thin molecular lines will only trace the denser core regions ( @xmath245 ) . * a turbulent velocity is difficult to generalise for each region . the widths of molecular lines will result from turbulent and thermal motions in the molecular gas , as well as macroscopic motions if many independent cores are viewed along the same line of sight . in nearby , low - mass star forming regions the latter should not be a major problem . however , due to opacity and depletion effects , different molecular lines will trace different components of the ambient gas . @xcite find that in perseus n@xmath0h@xmath26 ( 1 - 0 ) lines are broadened almost exclusively by thermal motions in dense cores ; c@xmath27o ( 2 - 1 ) is more sensitive to lower density material in the envelopes of dense cores ( the c@xmath27o transition has a critical density of 10@xmath28 @xmath18 and freezes out onto dust grains at densities above 10@xmath29 @xmath18 ) . c@xmath27o is therefore a better tracer of the non - thermal motions in the interstellar and intercore environment pervaded by molecular outflows . across perseus c@xmath27o profile widths vary by only a few tenths of a km s@xmath11 . from kirk et al . ( 2007 ) we therefore adopt a mean value of 0.6 km s@xmath11 for @xmath23 for all regions considered . in table [ turb ] we list the turbulent momentum @xmath30 and turbulent energy @xmath31 in each of the clouds observed in perseus . the momentum and energy of an outflow from a young star is hard to measure from infrared observations . therefore , to estimate the combined momentum and energy , @xmath32 and @xmath33 , of the outflows from the embedded ysos in each supercore in perseus , we use the canonical values for the momentum flux for class 0 and class i low mass protostellar outflows measured by @xcite , and multiply these by the accretion lifetime of the embedded phase @xcite . the momentum and energy flux of an outflow is thought to decrease with time , in line with decreasing accretion rates ( e.g. * ? ? ? we therefore ignore the class ii / iii outflow phase . if the momentum flux for the class 0 and i phases is @xmath34 m@xmath21 km s@xmath11 yr@xmath11 and @xmath35 m@xmath21 km s@xmath11 yr@xmath11 respectively , then for durations of @xmath36 and @xmath17 years , over its lifetime an outflow from a low - mass protostar should inject @xmath101.0 m@xmath21 km s@xmath11 of momentum into its surroundings . the outflow kinetic energy scales with the velocity ; since most of the molecular material in outflows is probably entrained in the relatively slow - moving wings of bow shocks , then for a molecular flow velocity of @xmath1020 km s@xmath11(e.g . * ? ? ? * ; * ? ? ? * ) , the kinetic energy supplied by a typical flow would be @xmath37 j . in table [ turb ] we thus multiply these canonical values by the number of observed h@xmath0 flows in each region to get @xmath32 and @xmath33 . although the combined energy of the outflows , @xmath33 , matches our estimates for the turbulent energy in each cloud , @xmath38 , the combined momentum , @xmath32 , falls short of @xmath39 by at least an order of magnitude in each region in table [ turb ] . it has been argued that a large fraction of the jet momentum may be carried by a collimated , high - velocity jet @xcite . however , the transport of this momentum component to the surrounding cloud may be relatively inefficient , as the heavy jet punches its way through the ambient medium . the existence of parsec - scale jets and the high proper motions of even the most distant jet knots suggest that jets are relatively unhindered by their surroundings . our assumption , that only the massive though low - velocity molecular flow component contributes to the turbulent motions in the ambient medium , is therefore probably still valid . instead , the turbulent momentum in the surrounding cloud may be built up via many generations of outflows . the lifetime of a giant molecular cloud is 1 - 2 orders of magnitude longer than the duration of the class 0/i phase , and class 0 , i and class ii ysos clearly co - exist in many star - forming regions ( e.g. * ? ? ? * ; * ? ? ? * ; * ? ? ? * ; * ? ? ? hence , over the lifetime of a gmc , many generations of outflows may contribute to the observed turbulent momentum in the surrounding cloud .

three are parsec - scale flows , with a mean flow lobe length exceeding 11.5 . 37 ( 44% ) of the detected h@xmath0 features are associated with a known herbig - haro object , while 72 ( 46% ) of catalogued hh objects are detected in h@xmath0 emission . embedded spitzer sources are identified for all but two of the 26 molecular outflows . these candidate outflow sources all have high near - to - mid - ir spectral indices ( mean value of @xmath2 ) as well as red irac 3.6@xmath1m-4.5@xmath1 m and irac / mips 4.5@xmath1m- 24.0@xmath1 m colours : 80% have [ 3.6]-[4.5]@xmath31.0 and [ 4.5]-[24]@xmath31.5 . these criteria high @xmath4 and red [ 4.5]-[24 ] and [ 3.6]-[4.5 ] colours are powerful discriminants when searching for molecular outflow sources . [ firstpage ] stars : formation infrared : stars ism : jets and outflows ism : kinematics and dynamics ism : individual : perseus

we discuss wide - field near - ir imaging of the ngc1333 , l1448 , l1455 and b1 star forming regions in perseus . the observations have been extracted from a much larger narrow - band imaging survey of the taurus - auriga - perseus complex . these h@xmath0 2.122@xmath1 m observations are complemented by broad - band k imaging , mid - ir imaging and photometry from the spitzer space telescope , and published submillimetre co j=3 - 2 maps of high - velocity molecular outflows . we detect and label 85 h@xmath0 features and associate these with 26 molecular outflows . three are parsec - scale flows , with a mean flow lobe length exceeding 11.5 . 37 ( 44% ) of the detected h@xmath0 features are associated with a known herbig - haro object , while 72 ( 46% ) of catalogued hh objects are detected in h@xmath0 emission . embedded spitzer sources are identified for all but two of the 26 molecular outflows . these candidate outflow sources all have high near - to - mid - ir spectral indices ( mean value of @xmath2 ) as well as red irac 3.6@xmath1m-4.5@xmath1 m and irac / mips 4.5@xmath1m- 24.0@xmath1 m colours : 80% have [ 3.6]-[4.5]@xmath31.0 and [ 4.5]-[24]@xmath31.5 . these criteria high @xmath4 and red [ 4.5]-[24 ] and [ 3.6]-[4.5 ] colours are powerful discriminants when searching for molecular outflow sources . however , we find no correlation between @xmath4 and flow length or opening angle , and the outflows appear randomly orientated in each region . the more massive clouds are associated with a greater number of outflows , which suggests that the star formation efficiency is roughly the same in each region . [ firstpage ] stars : formation infrared : stars ism : jets and outflows ism : kinematics and dynamics ism : individual : perseus

0803.3075

c

we examine near- and mid - ir images of a @xmath104 square degree region in perseus - west and compare these to published catalogues of hh objects and moderately - extensive co 3 - 2 maps . we find that in most cases molecular shock features are morphologically the same at 2.12@xmath1 m and 4.5@xmath1 m , although the more embedded portions of some flows are revealed only in the longer - wavelength data . h@xmath0 features are closely associated with high - velocity co lobes , in support of bow shock entrainment scenarios . however , they often do not coincide with their optical hh counterparts , because of extinction effects or the discordant excitation requirements of each tracer . we use irac and mips photometry to identify and characterise the outflow sources . in comparison to the full sample of ysos in the c2d catalogue , the molecular outflow sources possess extreme values of near - to - mid - ir spectral index , @xmath4 , and highly reddened [ 3.6]-[4.5 ] and [ 4.5]-[24 ] colours , as is befitting their extreme youth . we find no correlation between h@xmath0 flow length and @xmath4 , nor between flow opening angle ( as traced in h@xmath0 ) and @xmath4 . in general , the outflows are randomly orientated . however , we do find a correlation between the number of outflows and the number of protostellar cores in three of the four regions studies ; in terms of total cloud mass , there is one molecular outflow for every 44 - 88m@xmath21 of ambient material . the outflows may also be an important source of turbulent energy in the interstellar medium .

we discuss wide - field near - ir imaging of the ngc1333 , l1448 , l1455 and b1 star forming regions in perseus . however , we find no correlation between @xmath4 and flow length or opening angle , and the outflows appear randomly orientated in each region .

we discuss wide - field near - ir imaging of the ngc1333 , l1448 , l1455 and b1 star forming regions in perseus . the observations have been extracted from a much larger narrow - band imaging survey of the taurus - auriga - perseus complex . these h@xmath0 2.122@xmath1 m observations are complemented by broad - band k imaging , mid - ir imaging and photometry from the spitzer space telescope , and published submillimetre co j=3 - 2 maps of high - velocity molecular outflows . we detect and label 85 h@xmath0 features and associate these with 26 molecular outflows . three are parsec - scale flows , with a mean flow lobe length exceeding 11.5 . 37 ( 44% ) of the detected h@xmath0 features are associated with a known herbig - haro object , while 72 ( 46% ) of catalogued hh objects are detected in h@xmath0 emission . embedded spitzer sources are identified for all but two of the 26 molecular outflows . these candidate outflow sources all have high near - to - mid - ir spectral indices ( mean value of @xmath2 ) as well as red irac 3.6@xmath1m-4.5@xmath1 m and irac / mips 4.5@xmath1m- 24.0@xmath1 m colours : 80% have [ 3.6]-[4.5]@xmath31.0 and [ 4.5]-[24]@xmath31.5 . these criteria high @xmath4 and red [ 4.5]-[24 ] and [ 3.6]-[4.5 ] colours are powerful discriminants when searching for molecular outflow sources . however , we find no correlation between @xmath4 and flow length or opening angle , and the outflows appear randomly orientated in each region . the more massive clouds are associated with a greater number of outflows , which suggests that the star formation efficiency is roughly the same in each region . [ firstpage ] stars : formation infrared : stars ism : jets and outflows ism : kinematics and dynamics ism : individual : perseus

1610.05091

c

we have proposed a new setting for the stabilization of localized vortex beams in self - focusing kerr media . the inclusion of the nonlinear dissipative term accounting for the mpa ( multiphoton absorption ) makes the nonlinear bessel vortex beams stable . as described earlier for the zero - vorticity situation @xcite , for airy beams @xcite , and , recently , for nonlinear bessel vortex beams @xcite , the concomitant mpa - induced power loss is balanced by the radial flux from their intrinsic reservoir . stability regions for the nonlinear bessel vortex beams have been predicted by the linear - stability analysis and corroborated by direct simulations . stable states with multiple vorticities have been found too . differently from preceding works , these stable vortices do not require materials with tailored " nonlinearities . they may be common dielectrics , such as air , water or standard optical glasses , all featuring the ubiquitous kerr nonlinearity and mpa ( multiphoton absorption ) at sufficiently high intensities ( tens of tw/@xmath55 in gases , or a fraction of tw/@xmath55 in condensed matter ) . this is probably the reason why , on the contrary to previous proposals , the practical implementation of bvbs ( bessel vortex beams ) precedes the demonstration of their stability . axicon - generated bvbs with finite power were observed in @xcite to propagate steadily within the bessel zone . the proof of the stability has important consequences for these experiments and subsequent applications . the stability implies , for example , that the steady regime can be extended indefinitely long by simply enlarging the bessel zone . the stability analysis and diagnostic numerical simulations also allow us to interpret the two other propagation regimes observed in these experiments . we have concluded that the nonlinear dynamics is always governed by a specific nonlinear bvb , which we have fully specified . the quasi - stationary regime in the bessel zone is observed when this nonlinear bvb is found to be stable in our linear - stability analysis , or is effectively stable over the finite length of the bessel zone . the rotary and speckle - like regimes are observed when this nonlinear bvb is found to be unstable , and the instability can develop , depending on its growth rate and the length of the bessel zone . the azimuthal - symmetry - breaking dynamics in the bessel zone is just a manifestation of the evolution of the unstable bvb . as an extension of this analysis , it may be of interest to study the interaction between spatially separated stable vortices in the same model , as well as the stability of the tubular vortices against spatiotemporal ( longitudinal ) perturbations . 99 yu . s. kivshar and d. e. pelinovsky , self - focusing and transverse instabilities of solitary waves , " phys . rep . * 331 * , 117 ( 2000 ) ; 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h. saito and m. ueda , split instability of a vortex in an attractive bose - einstein condensate , " phys . 89 * , 190402 ( 2002 ) ; t. j. alexander and l. berg , ground states and vortices of matter - wave condensates and optical guided waves , " phys . e * 65 * , 026611 ( 2002 ) ; l. d. carr and c. w. clark , vortices in attractive bose - einstein condensates in two dimensions , " phys lett . * 97 * , 010403 ( 2006 ) . d. mihalache , d. mazilu , b. a. malomed , and f. lederer , vortex stability in nearly - two - dimensional bose - einstein condensates with attraction , , " phys . a * 73 * , 043615 ( 2006 ) ; b. a. malomed , f. lederer , d. mazilu , and d. mihalache , on stability of vortices in three - dimensional self - attractive bose - einstein condensates , " phys . a * 361 * , 336(2007 ) . c. rotschild , o. cohen , o. manela , and m. segev , solitons in nonlinear media with an infinite range of nonlocality : first observation of coherent elliptic solitons and of vortex - ring solitons , " phys . * 95 * , 213904 ( 2005 ) . h. sakaguchi , b. li , and b. a. malomed , creation of two - dimensional composite solitons in spin - orbit - coupled self - attractive bose - einstein condensates in free space , " phys . e * 89 * , 032920 ( 2014 ) . zhang , z .- w . zhou , b. a. malomed , and h. pu , stable solitons in three dimensional free space without the ground state : self - trapped bose - einstein condensates with spin - orbit coupling , " phys . lett . * 115 * , 253902 ( 2015 ) . b. a. malomed , l .- c . crasovan , and d. mihalache , stability of vortex solitons in the cubic - quintic model , " physica d * 161 * , 187 ( 2002 ) ; d. mihalache , d. mazilu , f. lederer , y. v. kartashov , l .- c . crasovan , l. torner , and b. a. malomed , stable vortex tori in the three - dimensional cubic - quintic ginzburg - landau equation , " phys lett . * 97 * , 073904 ( 2006 ) . i. s. aranson and l. kramer , the world of the complex ginzburg - landau equation , " rev . phys . * 74 * , 99 ( 2002 ) ; n. akhmediev , j. m. soto - crespo , and p. grelu , spatiotemporal optical solitons in nonlinear dissipative media : from stationary light bullets to pulsating complexes , " chaos * 17 * , 037112 ( 2007 ) ; e. knobloch , spatial localization in dissipative systems , " annu . rev . condens . matter phys . * 6 * , 325 ( 2015 ) . m. a. porras , a. parola , d. faccio , a. dubietis , and p. di trapani , nonlinear unbalanced bessel beams : stationary conical waves supported by nonlinear losses , " phys . lett . * 93 * , 153902 ( 2004 ) . a. couairon , e. gaizauskas , d. faccio , a. dubietis , and p. di trapani , nonlinear x - wave formation by femtosecond filamentation in kerr media , " phys . e * 73 * , 016608 ( 2006 ) ; p. polesana , m. franco , a. couairon , d. faccio , and p. di trapani , filamentation in kerr media from pulsed bessel beams , " phys . rev . a * 77 * , 043814 ( 2008 ) . s. skupin , r. nuter , and l. berg , optical femtosecond filaments in condensed media , " phys . rev . a * 74 * , 043813 ( 2006 ) ; a. pasquazi , s. stivala , g. assanto , j. gonzalo , and j. solis , transverse nonlinear optics in heavy - metal - oxide glass , " _ ibid_. * 77 * , 043808 ( 2008 ) ; s. d. jenkins , f. prati , l. a. lugiato , l. columbo , and m. brambilla , cavity light bullets in a dispersive kerr medium , " _ ibid_. * 80 * , 033832 ( 2009 ) . p. polesana , p. faccio , d. di trapani , a. dubietis , a. piskarskas , a. couairon , and m. porras , high localization , focal depth and contrast by means of nonlinear bessel beams , " opt . express * 13 * , 6160 ( 2005 ) ; p. polesana , a. dubietis , m. a. porras , e. kucinskas , d. faccio , a. couairon , and p. di trapani , near - field dynamics of ultrashort pulsed bessel beams in media with kerr nonlinearity , " phys . rev . e * 73 * , 056612 ( 2006 ) . p. polesana , a. couairon , d. faccio , a. parola , m. a. porras , a. dubietis , a. piskarskas , and p. di trapani , observation of conical waves in focusing , dispersive , and dissipative kerr media , " phys . lett . * 99 * , 223902 ( 2007 ) . c. xie , v. jukna , c. milin , r. giust , i. ouadghiri - idrissi , t. itina , j. m. dudley , a. couairon , and f. courvoisier , tubular filamentation for laser material processing , " scientific reports * 5 * , 8914 ( 2015 ) .

we elaborate a new solution for the problem of stable propagation of transversely localized vortex beams in homogeneous optical media with self - focusing kerr nonlinearity . stationary nonlinear bessel - vortex states are stabilized against azimuthal breakup and collapse by multiphoton absorption , while the respective power loss is offset by the radial influx of the power from an intrinsic reservoir . a linear stability analysis and direct numerical simulations beams with multiple vorticities have their stability regions too . these beams can then form robust tubular filaments in transparent dielectrics as common as air , water and optical glasses at sufficiently high intensities .

we elaborate a new solution for the problem of stable propagation of transversely localized vortex beams in homogeneous optical media with self - focusing kerr nonlinearity . stationary nonlinear bessel - vortex states are stabilized against azimuthal breakup and collapse by multiphoton absorption , while the respective power loss is offset by the radial influx of the power from an intrinsic reservoir . a linear stability analysis and direct numerical simulations reveal a region of stability of these vortices . beams with multiple vorticities have their stability regions too . these beams can then form robust tubular filaments in transparent dielectrics as common as air , water and optical glasses at sufficiently high intensities . we also show that the tubular , rotating and speckle - like filamentation regimes , previously observed in experiments with axicon - generated bessel beams , can be explained as manifestations of the stability or instability of a specific nonlinear bessel - vortex state , which is fully identified .

1511.05489

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the few - body hamiltonian that we are concerned with is that of three identical bosons confined to two dimensions in a vector potential appropriate to a constant effective magnetic field perpendicular to the plane of motion:@xmath8 where @xmath9 is the single particle hamiltonian for a particle moving in the vector potential @xmath10 , and @xmath11 is the inter - particle separation distance between particles @xmath4 and @xmath5 . here @xmath12 is the vector potential experienced by the @xmath4th particle , and @xmath13 is an overall scaling factor . if the particles in question are charged particles , the scale factor would be simply given by @xmath14 in gaussian units . in eq . [ eq : totham ] , @xmath15 is a pairwise isotropic interaction between two bosons that will be described more fully below . since @xmath10 creates an effective constant magnetic field , here we choose to describe this field in the symmetric gauge : @xmath16 note that we have chosen the magnetic field to be pointing in the @xmath17 direction . inserting the vector potential into eq . [ eq : totham ] gives a total hamiltonian in an illuminating form:@xmath18 where @xmath19 is the total angular momentum of the system . here , we have written the hamiltonian in terms of the cyclotron frequency @xmath20 . the cyclotron frequency also yields a length scale @xmath21 called the magnetic length . the utility of the symmetric gauge is now obvious : the effect of the magnetic field is simply that of an isotropic trap in the system along with an overall shift downward determined by the total angular momentum of the system . to separate out the center of mass , we transform into a set of mass - scaled jacobi coordinates @xcite:@xmath22 where @xmath23 is the 2-body reduced mass , @xmath24 is the reduced mass of a two body system with third particle and @xmath25 is the three - body reduced mass which we choose to be @xmath26 . here the superscript @xmath27 indicates which jacobi coordinates have been chosen using the odd - man out notation where @xmath28 is a cyclic permutation of the particle numbers e.g. if @xmath29 then @xmath30 and @xmath31 . after the transformation the total hamiltonian can be written as@xmath32 here @xmath33 is the angular momentum operator of the center of mass , @xmath34 is the internal angular momentum operator , and @xmath35 is the total mass of the three - body system . in eq . [ eq : hint1 ] , @xmath36 refers to a derivative with respect to the @xmath4th jacobi coordinate . it is important to point out that the internal hamiltonian has the same form , independent of which jacobi coordinate system has been chosen from eq . [ eq : jaccoords ] and thus the superscript @xmath37 has been suppressed . since the center of mass motion is completely separated , we can proceed to examine the internal hamiltonian , @xmath38 . because the interactions are isotropic , the total internal 2d angular momentum of the system is a good quantum number . if we restrict the system to only states with total internal angular momentum @xmath2 , the schrdinger equation that results from eq . [ eq : hint1 ] is that of three particles confined to an isotropic oscillator with oscillator frequency @xmath39 , i.e.@xmath40 \psi_{m}\left ( \vec{\rho}_{1}^{\left ( k\right ) } , \vec{\rho}_{2}^{\left ( k\right ) } \right ) \nonumber\end{aligned}\ ] ] where the first sum on the right hand side runs over the jacobi vectors . here @xmath41 is a three - body eigenfunction with total internal angular momentum @xmath2 . to solve eq . [ eq : se1 ] we employ hyperspherical coordinates and the adiabatic hyperspherical representation , wherein the 4-dimensional schrdinger equation is expressed in terms of the hyperradius @xmath42 and a set of three hyperangles @xmath43 collectively denoted by @xmath44 where @xmath45 and @xmath46 are the standard polar angles for jacobi vectors @xmath47 and @xmath48 respectively , and @xmath13 is an angle that correlates the lengths of the two jacobi vectors , i.e.@xmath49 in hyperspherical coordinates , the internal hamiltonian of eq . [ eq : hint1 ] can be written as@xmath50 here @xmath51 is the grand angular momentum operator , the properties and description of which can be found in a number of references ( see refs . @xcite for example ) . before we solve the fully interacting system , it is instructive to consider the structure of the solutions to the non - interacting system of three particles in an external field . the quantized motion of a particle in an external field described in the symmetric gauge results in a set of infinitely degenerate levels called landau levels , with energy spacing between degenerate manifolds of @xmath52 . it is interesting to note that in setting the interactions in eq . [ eq : hinths ] to zero , the hamiltonian becomes separable in hyperspherical coordinates , reproducing exactly the landau level picture , but with a slightly different interpretation of the level structure ( discussed below ) . the grand angular momentum operator is diagonalized using hyperspherical harmonics @xcite with eigenvalues given by@xmath53 where @xmath54 is the grand angular momentum quantum number and @xmath55 and @xmath56 are the 2d angular momenta associated with the jacobi vectors @xmath47 and @xmath48 respectively . hyperspherical harmonics also diagonalize the total angular momentum of the system as @xmath57 where @xmath58 is the total 2d angular momentum of the system , the allowed values of @xmath54 are given by@xmath59 where @xmath60 is a non - negative integer . note that @xmath54 has a minimum value given by @xmath61 when @xmath62 . inserting the separability ansatz @xmath63 into the schrdinger equation resulting from eq . [ eq : hinths ] ( with the interactions set to zero ) results in a 1d hyperradial schrdinger equation of a harmonic oscillator with frequency @xmath39 that has been shifted down in energy by @xmath64 , i.e.@xmath65 f\left ( r\right ) .\nonumber\end{aligned}\ ] ] note that the @xmath66 factor in the separability ansatz is included to remove first derivatives in the hyperradius . this schrdinger equation can be solved simply @xcite with eigenenergies and eigenfunctions given by@xmath67 , v=0,1,2, ... \label{eq : nienergy}\\ f\left ( r\right ) & = a_{\nu\lambda}\dfrac{e^{-r^{2}/(2\sqrt{2}l)_{c}}}{r^{3/2}}\left ( \dfrac{r}{\sqrt{2}l_{c}}\right ) ^{\lambda+3/2}l_{\nu } ^{\lambda+1}\left ( \dfrac{r^{2}}{2l_{c}^{2}}\right ) , \label{eq : niwf}\ ] ] where @xmath68 is the magnetic length , @xmath69 is a lageurre polynomial and @xmath70 is a normalization constant@xmath71 inserting the restriction on values of @xmath54 from eq . [ eq : lambdarestrict ] into eq . [ eq : nienergy ] the landau level picture emerges:@xmath72 restricting ourselves to positive values of angular momentum it is clear that for fixed @xmath73 and @xmath60 any nonnegative value of total angular momentum @xmath2 produces the same energy , and thus an infinitely degenerate manifold of states . the structure of the energy levels seen in eq . [ eq : llenergies ] is the same as the energy levels seen in the standard landau level picture . here , however , the interpretation of excitation between landau levels is somewhat different . there are two different ways to move from one level to another , either through a hyperradial excitation by incrementing @xmath73 , or through a hyperangular excitation by incrementing @xmath60 . next , we proceed to diagonalize the full interacting hamiltonian of eq . [ eq : hinths ] within the adiabatic hyperspherical method . the heart of the approach is in treating the hyperradius @xmath74 as an adiabatic parameter , and diagonaizing the hamiltonian at fixed @xmath74 in the remaining hyperangular degrees of freedom . in this method , the total wavefunction is expanded as @xmath75 here , the adiabatic channel functions , @xmath76 satisfy the fixed @xmath74 schrdinger equation@xmath77 \phi_{nm}\left ( \omega\right ) = u_{nm}\left ( r\right ) \phi_{nm}\left ( \omega\right ) , \label{eq : adiabaticse}\ ] ] where @xmath78 is the adiabatic potential associated with @xmath79 . note that this is exactly the adiabatic schrdinger equation that is solved in finding the adiabatic potentials for three bosons in the _ absence _ of any external field . thus @xmath78 are simply the adiabatic potentials for three interacting bosons confined to 2d , a system that has been studied extensively @xcite and is of current interest in its own right . inserting eq . [ eq : hinths ] and projecting onto the @xmath60th channel function results is a coupled system of one - dimensional schrdinger equations in @xmath80 @xmath81 f_{nm}\left ( r\right ) -\dfrac{\hbar^{2}}{2\mu}\sum_{m\neq n}\left ( \mathbf{q}_{nm}\left ( r\right ) + 2\mathbf{p}_{nm}\left ( r\right ) \dfrac{d}{dr}\right ) f_{mm}\left ( r\right ) , \label{eq : coupledse}\\u_{nm}\left ( r\right ) = & u_{nm}\left ( r\right ) + \dfrac{\hbar^{2}}{2\mu } \dfrac{3/4}{r^{2}}-\dfrac{\hbar^{2}}{2\mu}\mathbf{q}_{nn}\left ( r\right ) + \dfrac{1}{8}\mu\omega_{c}^{2}r^{2}-\dfrac{\hbar\omega_{c}}{2}m.\label{eq : effectivepot}\ ] ] here the effective hyperradial potentials are given by @xmath82 and the non - adiabatic corrections embodied in the @xmath83 and @xmath84 matrices are a result of hyperradial derivatives of the channel functions , i.e.@xmath85 where the double bracket @xmath86 indicates that the matrix elements are taken over the hyperangular degrees of freedom only . , ( b ) @xmath87 , and ( c ) @xmath0 are shown as a function of @xmath88 on a log scale . dotted lines indicate the hyperangular eigenvalues of hyperspherical harmonics of non - interacting systems expected in the large and small @xmath89 limits.,title="fig:",width=288 ] , ( b ) @xmath87 , and ( c ) @xmath0 are shown as a function of @xmath88 on a log scale . dotted lines indicate the hyperangular eigenvalues of hyperspherical harmonics of non - interacting systems expected in the large and small @xmath89 limits.,title="fig:",width=288 ] , ( b ) @xmath87 , and ( c ) @xmath0 are shown as a function of @xmath88 on a log scale . dotted lines indicate the hyperangular eigenvalues of hyperspherical harmonics of non - interacting systems expected in the large and small @xmath89 limits.,title="fig:",width=288 ] up to this point the treatment described above has been quite general , and is applicable to any two - body , cylindrically symmetric interaction . in fact , by extending the jacobi coordinates to larger numbers of particles , this treatment can be extended to any @xmath6-body system . the adiabatic schrdinger equation ( [ eq : adiabaticse ] ) has been solved for three - body systems with several different interaction potentials and can be approached by a number of different techniques @xcite . in this work we focus on the zero - range pseudo - potential @xcite,@xmath90 } \dfrac{\partial } { \partial \label{eq : pseudopot}\ ] ] where @xmath91 is the 2d , s - wave ( @xmath92 ) scattering length . the effect of this pseudo - potential is to enforce the two - body boundary condition @xmath93 , \label{eq : bc}\\ \tan\delta & = \dfrac{\pi}{2\left ( \ln\dfrac{ka}{2}+\gamma\right ) } .\nonumber\end{aligned}\ ] ] where @xmath94 is a constant , @xmath95 is the 2d s - wave scattering phase shift , @xmath96 is the two - body wavenumber , and @xmath97 is the euler constant . it is important to note that this pseudo - potential only affects wavefunctions with an s - wave component of the angular momentum between pairs of particles ; all higher partial waves are treated as non - interacting . this pseudo - potential can be used when the true inter - particle interaction falls off sufficiently fast at large @xmath98 to be considered short - range the scattering length is much larger than both the range , @xmath99 , and the effective range , @xmath100 , of the interaction , i.e. @xmath101 and @xmath102 . at the two - body level this pseudo - potential interaction produces a large halo dimer state with binding energy @xmath103 @xcite . it is also worth noting that in the limit of large or small scattering length , @xmath104 _ or _ @xmath105 , where @xmath96 is the relative two - body momentum , the pseudo - potential approaches the non - interacting limit . in the present study , we employ the hyperangular green s function approach of ref . the full derivation using this method is somewhat tedious , but straightforward , and we will not detail it here . the heart of the method is in turning the adiabatic schrdinger equation into a lippmann - schwinger ( ls ) equation by employing the free - space hyperangular green s function . within this ls equation , it is easy to apply the boundary condition of eq . [ eq : bc ] when two particles are in contact with each other , and propagate the particles freely between such contact points . the result of this derivation gives the adiabatic potentials as @xmath106 where we refer to @xmath107 as the hyperangular eigenvalues which are roots of the transcendental equation @xmath108 where @xmath109 is the gamma function , @xmath110 is the digamma function and @xmath111 is a hypergeometric function . in the case where @xmath112 , this reduces to the results found in refs . @xcite . examples of the hyperradial eigenvalues @xmath113 for @xmath114 and @xmath115 are shown in fig . [ fig : hyperangvals ] as a function of @xmath88 . in each case the lowest hyperangular eigenvalue goes to @xmath116 quadratically in @xmath74 in the large @xmath74 limit . this corresponds to a particle - dimer hyperangular channel function consisting of a free particle far away from a bound dimer . with the exception of the lowest potential in the large @xmath74 limit , all hyperangular eigenvalues logarithmically approach an integer , corresponding to a non - interacting value , in both the large and small @xmath74 limits . the hyperangular eigenvalues transition from one non - interacting limit to another in the region where @xmath117 . we can understand this behavior by considering the pseudo - potential in eq . [ eq : pseudopot ] . in the limit of large hyperradius , @xmath118 , the average inter - particle separation is much greater than the scattering length , @xmath119 the logarithmic behavior of the scattering length in the pseudo potential indicates that this is a weakly repulsive limit . in the limit of very small hyperradius , @xmath120 , the average inter - particle separation is much smaller than the scattering length , @xmath121 , again , because of the logarithmic nature of the pseudo - potential , this becomes the weakly attractive limit . the matrix elements of the non - adiabatic correction matrix , @xmath83 ( eq ( [ eq : pmat]))are given in ref . @xcite in terms of the hyperangular eigenvalues by@xmath122 where the primes indicate a derivative with respect to @xmath74 . the diagonal correction , @xmath123 , to the potentials in eq . [ eq : effectivepot ] is given by @xmath124 in the infinite channel limit , the off - diagonal elements of @xmath84 can be found using the identity@xmath125 _ { mn } \label{eq : qoffdiag}\ ] ] where @xmath126 _ { mn}$ ] is the @xmath127 element of the square of the p - matrix and @xmath128 indicates a derivative with respect to the hyperradius . while eq . [ eq : qoffdiag ] is only exact in the infinite channel limit , for the purposes of this work , we will use it in a finite channel number expansion to approximate direct , off - diagonal , non - adiabatic contributions .

we examine a system of three - bosons confined to two dimensions in the presence of a perpendicular magnetic field within the framework of the adiabatic hyperspherical method . for the case of zero - range , regularized pseudo - potential interactions , we find that the system is nearly separable in hyperspherical coordinates and that , away from a set of narrow avoided crossings , the full energy eigenspectrum as a function of the 2d s - wave scattering length is well described by ignoring coupling between adiabatic hyperradial potentials . in the case of weak attractive or repulsive interactions ,

we examine a system of three - bosons confined to two dimensions in the presence of a perpendicular magnetic field within the framework of the adiabatic hyperspherical method . for the case of zero - range , regularized pseudo - potential interactions , we find that the system is nearly separable in hyperspherical coordinates and that , away from a set of narrow avoided crossings , the full energy eigenspectrum as a function of the 2d s - wave scattering length is well described by ignoring coupling between adiabatic hyperradial potentials . in the case of weak attractive or repulsive interactions , we find the lowest three - body energy states exhibit even / odd parity oscillations as a function of total internal 2d angular momentum and that for weak repulsive interactions , the universal lowest energy interacting state has an internal angular momentum of @xmath0 . with the inclusion of repulsive higher angular momentum we surmise that the origin of a set of `` magic number '' states ( states with anomalously low energy ) might emerge as the result of a combination of even / odd parity oscillations and the pattern of degeneracy in the non - interacting lowest landau level states .

1511.05489

i

the three - boson problem in 2d in the presence of a transverse magnetic field is suprisingly well described using the adiabatic hyperspherical method . the full energy spectrum presents very narrow avoided crossings between the adiabatic energies , and away from these crossings the couplings between channels can be largely ignored to a good approximation . this indicates that the system is nearly separable in the hyperspherical picture . the adiabatic hyperspherical picture provides a useful interpretation of transitions in which excitations between levels can be achieved through either a hyperangular excitation in which the internal configuration of the three - boson system is changed or through a hyperradial vibrational excitation in which the internal structure of the system remains the same . the adiabatic hyperangular eigenvalues , @xmath107 , are exactly the same as those found for three interacting bosons in free - space . the inclusion of the magnetic field results in the addition of an effective isotropic trap , and an angular momentum dependent shift . when interacting via the s - wave pseudopotential , three - body states transition from the weakly repulsive regime ( @xmath155 ) to the weakly attractive regime ( @xmath141 ) as a function of the 2d scattering length . states that interact via the s - wave interaction display an even / odd parity oscillation as a function of the total internal angular momentum @xmath2 . for small scattering length , this parity oscillation combined with the fact that there is no @xmath87 lowest landau level means that the lowest interacting three - boson state has total internal angular momentum @xmath0 . at higher values of angular momentum the lowest landau level becomes degenerate and a set of non - interacting states emerge in which the inter - particle angular momentum has no @xmath92 component . interestingly , if the same pattern of even / odd parity oscillations persits when higher partial wave interactions are included , in combination with the pattern of degeneracy for the lowest landau level , this might be the source of the magic number behavior seen in three - particle systems interacting via long - range coulomb interactions , and is the subject of ongoing work .

we find the lowest three - body energy states exhibit even / odd parity oscillations as a function of total internal 2d angular momentum and that for weak repulsive interactions , the universal lowest energy interacting state has an internal angular momentum of @xmath0 . with the inclusion of repulsive higher angular momentum

we examine a system of three - bosons confined to two dimensions in the presence of a perpendicular magnetic field within the framework of the adiabatic hyperspherical method . for the case of zero - range , regularized pseudo - potential interactions , we find that the system is nearly separable in hyperspherical coordinates and that , away from a set of narrow avoided crossings , the full energy eigenspectrum as a function of the 2d s - wave scattering length is well described by ignoring coupling between adiabatic hyperradial potentials . in the case of weak attractive or repulsive interactions , we find the lowest three - body energy states exhibit even / odd parity oscillations as a function of total internal 2d angular momentum and that for weak repulsive interactions , the universal lowest energy interacting state has an internal angular momentum of @xmath0 . with the inclusion of repulsive higher angular momentum we surmise that the origin of a set of `` magic number '' states ( states with anomalously low energy ) might emerge as the result of a combination of even / odd parity oscillations and the pattern of degeneracy in the non - interacting lowest landau level states .

0902.2597

i

the reionization and metal enrichment of the universe are thought to begin with the formation of first metal - free ( pop iii ) stars @xcite . hence , the formation rate of pop iii stars is crucial for the subsequent structure formation in the universe . the pop iii objects are expected to collapse at @xmath3 , forming a minihalo with a mass of @xmath4 and an extent of @xmath5pc @xcite . in the course of bottom - up structure formation , such pop iii minihaloes merge to form first galaxies at @xmath6 , having the virial temperature @xmath7k and the mass @xmath8 . even in the evolution of first galaxies , pop iii stars can play a significant role , since an appreciable number of stars may form from metal - free component in interstellar gas @xcite . the formation of very first stars has been investigated intensively in the last decade . many studies have come to a similar conclusion that such stars form in a top - heavy mass function with the peak of @xmath9 ( e.g. , * ? ? ? * ; * ? ? ? * ; * ? ? ? * ; * ? ? ? recently , @xcite have shown that the variations of cosmological density fluctuations allow the mass of pop iii stars to be down to @xmath10 . on the other hand , the secondary pop iii star formation has been investigated recently . the formation of secondary stars is subject to various feedback effects by first stars . one of them is the supernova ( sn ) feedback through mechanical and chemical effects . the negative feedback by sne is the evaporation of neighboring clouds , since the sn shock heats up the gas in clouds . on the hand , sne can bring positive feedback through the compression by shock and the cooling by ejected heavy elements . the secondary star formation can be promoted by such positive feedback effects @xcite . another important feedback effect is brought by the ultraviolet ( uv ) radiation from first stars , since they are very luminous at ultraviolet band . first stars photoionize and photoheat the surrounding media , and also photodissociate h@xmath11 molecules , which are the main coolant of primordial gas . the radiative feedback from first stars is the primary feedback until first stars end the life - time of @xmath12yr with sne . the photodissociation of h@xmath11 molecules leads to a negative radiative feedback effect , which has been studied by many authors so far . @xcite investigated the effect of h@xmath11-dissociating radiation from a single pop iii star residing in a virialized halo . they found that if the halo is uniform , h@xmath11 molecules in the halo are totally dissociated , so that the gas can not collapse to form stars . @xcite considered more realistic clumpy halos . they found that if the gas density is sufficiently high , photodissociation process proceeds slower than the collapse of the cloud . hence , the cloud can form stars . this result is confirmed by the recent 3d radiation hydrodynamic simulation by @xcite including the effects of hydrodynamics as well as the radiation transfer of h@xmath11-dissociating radiation . the feedback effects by diffuse h@xmath11-dissociating radiation can be important after the local feedback in minihaloes @xcite . these works basically focused on the photodissociation effects . we also have to take into account the effects of ionizing photons . ionizing radiation heats up the gas through the photoionization processes . the temperature of photoheated gas is kept to be around @xmath13k , owing to the balance between the radiative cooling and photoheating . if the gravitational potential of star forming halos are not so deep as to retain the photoheated gas , the heated gas evaporates from the halos ( e.g. , * ? ? * ; * ? ? ? * ; * ? ? ? * ; * ? ? ? * ; * ? ? ? * ) . however , the case in which ionizing radiation is coupled with h@xmath11-dissociating radiation is complex . when an ionization front ( i - front ) propagates in a collapsing core , the enhanced fraction of electrons catalyzes h@xmath11 formation @xcite . in particular , the mild ionization ahead of the i - front generates an h@xmath11 shell , which potentially shields h@xmath11 dissociating photons @xcite . this mechanism is likely to work positively to form pop iii stars . on the other hand , the i - front can be accompanied with a shock for an optically - thick cloud @xcite . the shock affects significantly the collapse of cloud . this is a totally radiation hydrodynamic ( rhd ) process . such radiation hydrodynamic feedback has been investigated by 1d spherical rhd simulations @xcite , 2d cylindrical rhd simulations @xcite , and 3d rhd simulations @xcite . the results by 2d and 3d simulations are in good agreement with each other . it is found that ionizing radiation can bring positive feedback through the formation of h@xmath11 shell . @xcite investigated rhd feedback by a @xmath14 source star , and @xcite derived the feedback criterion . however , if a source star is less massive , the relative intensity of h@xmath11-dissociating radiation to ionizing radiation increases . then , the feedback tends to be more negative . in fact , the mass of first stars might be some @xmath15 owing to the variations of cosmological density fluctuations @xcite , the enhanced h@xmath11 cooling in pre - ionized gas @xcite , or the hd cooling in fossil hii regions ( e.g. , * ? ? ? * ; * ? ? ? * ; * ? ? ? * ; * ? ? ? * ; * ? ? ? * ; * ? ? ? * ) . also , the elemental abundance patterns of hyper - metal - poor stars well match the yields by supernova explosions with a progenitor mass of @xmath16 @xcite . the rhd feedback effects by pop iii stars less massive than @xmath17 have not been investigated so far , and no criterion has not been derived . in this paper , we perform 3d rhd simulations in order to investigate the radiative feedback effects from pop iii stars with various masses . we derive the criteria for the collapse of cloud cores irradiated by a neighboring pop iii star with 25,40,80 , or @xmath14 . in 2 , the simulation code and procedure are described . the simulation results are presented in 3 . finally , we summarize the conclusions in 4 . .properties of pop iii source stars [ cols="<,<,<,<",options="header " , ]

on the other hand , it is expected that the negative feedback by @xmath1-dissociating radiation can be predominant if a source star is less massive , since a ratio of the @xmath1-dissociating photon number to the ionizing photon number becomes higher . in order to investigate the radiative feedback effects from such less massive stars , , we find that if a source star is less massive than @xmath2 , the ionizing radiation can not suppress the negative feedback of @xmath1-dissociating radiation . [ firstpage ] early universe - galaxies : formation - radiative transfer - hydrodynamics

we explore the impact of ultraviolet ( uv ) radiation from massive population iii ( pop iii ) stars of 25 , 40 , 80 , and 120 @xmath0 on the subsequent pop iii star formation . in this paper , particular attention is paid to the dependence of radiative feedback on the mass of source pop iii star . uv radiation from the source star can work to impede the secondary star formation through the photoheating and photodissociation processes . recently , susa & umemura ( 2006 ) have shown that the ionizing radiation alleviates the negative effect by @xmath1-dissociating radiation from 120@xmath0 popiii star , since an @xmath1 shell formed ahead of an ionizing front can effectively shield @xmath1-dissociating radiation . on the other hand , it is expected that the negative feedback by @xmath1-dissociating radiation can be predominant if a source star is less massive , since a ratio of the @xmath1-dissociating photon number to the ionizing photon number becomes higher . in order to investigate the radiative feedback effects from such less massive stars , we perform three - dimensional radiation hydrodynamic simulations , incorporating the radiative transfer effect of ionizing and @xmath1-dissociating radiation . as a result , we find that if a source star is less massive than @xmath2 , the ionizing radiation can not suppress the negative feedback of @xmath1-dissociating radiation . therefore , the fate of the neighboring clouds around such less massive stars is determined solely by the flux of @xmath1-dissociating radiation from source stars . with making analytic estimates of @xmath1 shell formation and its shielding effect , we derive the criteria for radiation hydrodynamic feedback depending on the source star mass . [ firstpage ] early universe - galaxies : formation - radiative transfer - hydrodynamics

0902.2597

c

we have carried out rhd simulations to investigate the impact of uv radiation from a pop iii star on nearby collapsing cores . in particular , our attention has been paid to the dependence of uv feedback on the mass of pop iii star . the radiation hydrodynamic evolution of cloud core is determined by not only @xmath1-dissociating radiation but also ionizing radiation . as a result , we have found the critical stellar mass @xmath125 , above which an @xmath1 shell ahead of ionizing front can help clouds to collapse . owing to the fact that @xmath1-dissociating radiation becomes predominant for less massive source stars , the critical distance for the collapse of a neighboring core does not so strongly depend on the mass of source star . also , we have derived analytically the feedback criterion , @xmath124 , where @xmath123 is given by ( [ dcrsh ] ) and @xmath85 is a dynamical factor dependent on the the ratio of gravitational energy @xmath38 to internal energy @xmath39 of collapsing cloud . we have found @xmath86 for @xmath82 , and @xmath88 for @xmath87 . since @xmath85 is dependent on @xmath40 , a dark matter ( dm ) halo can influence the feedback criterion to a certain degree . in order to assess the effects of dm , we have calculated several models with a static nfw - type dark matter halo potential @xcite with @xmath126 and @xmath127 . in these runs , the ratios of dm mass ( @xmath128 ) to baryonic mass ( @xmath129 ) at the central regions of @xmath130pc are @xmath131 for @xmath54 , and @xmath132 for @xmath133 . as a result , we have found that the feedback criterion in the form of @xmath124 turns out to be still valid , and @xmath85 becomes smaller by a factor of 1.2 for @xmath54 and by a factor of 2 for @xmath133 . therefore , our main results are not changed so much by including dm . note that the dm density evolution is not treated consistently with the gas dynamics in these simulations . if the dm dynamics is solved with the evolution of gas clouds , the evolutionary path of core temperature might be changed . hence , for a more quantitative argument , the self - consistent treatment of dark matter would be requisite . in this paper , we have not considered the lifetime of source stars . the lifetime of pop iii star is @xmath134yr for 120@xmath0 , @xmath135yr for 80@xmath0 , @xmath136yr for 40@xmath0 , and @xmath137yr for 25@xmath0 @xcite . if the lifetime of source star is shorter than the free - fall time determined by @xmath43 , the feedback may be significantly changed before the cloud collapse . the density in which the free - fall time equals the stellar lifetime is @xmath138 for 120@xmath0 , @xmath139 for 80@xmath0 , @xmath140 for 40@xmath0 , and @xmath141 for 25@xmath0 . below these densities , arguments including the effects from the stellar lifetime are requisite . the fate of pop iii stars depends on the mass @xcite . pop iii stars with 120@xmath0 or 80@xmath0 may result in direct collapse to black holes ( bhs ) , while those with 40@xmath0 or 25@xmath0 may undergo type ii supernova explosions . in the case of direct bh formation , uv source disappears abruptly , and then already - formed @xmath1 molecules can promote the collapse of cloud cores ( e.g. , * ? ? ? * ; * ? ? ? * ; * ? ? ? * ; * ? ? ? * ) . in the case of type ii sn explosions , shock - driven hydrodynamic feedbacks could be significant @xcite .

we explore the impact of ultraviolet ( uv ) radiation from massive population iii ( pop iii ) stars of 25 , 40 , 80 , and 120 @xmath0 on the subsequent pop iii star formation . in this paper , particular attention is paid to the dependence of radiative feedback on the mass of source pop iii star . uv radiation from the source star can work to impede the secondary star formation through the photoheating and photodissociation processes . recently , susa & umemura ( 2006 ) have shown that the ionizing radiation alleviates the negative effect by @xmath1-dissociating radiation from 120@xmath0 popiii star , since an @xmath1 shell formed ahead of an ionizing front can effectively shield @xmath1-dissociating radiation . we perform three - dimensional radiation hydrodynamic simulations , incorporating the radiative transfer effect of ionizing and @xmath1-dissociating radiation . as a result therefore , the fate of the neighboring clouds around such less massive stars is determined solely by the flux of @xmath1-dissociating radiation from source stars . with making analytic estimates of @xmath1 shell formation and its shielding effect , we derive the criteria for radiation hydrodynamic feedback depending on the source star mass .

we explore the impact of ultraviolet ( uv ) radiation from massive population iii ( pop iii ) stars of 25 , 40 , 80 , and 120 @xmath0 on the subsequent pop iii star formation . in this paper , particular attention is paid to the dependence of radiative feedback on the mass of source pop iii star . uv radiation from the source star can work to impede the secondary star formation through the photoheating and photodissociation processes . recently , susa & umemura ( 2006 ) have shown that the ionizing radiation alleviates the negative effect by @xmath1-dissociating radiation from 120@xmath0 popiii star , since an @xmath1 shell formed ahead of an ionizing front can effectively shield @xmath1-dissociating radiation . on the other hand , it is expected that the negative feedback by @xmath1-dissociating radiation can be predominant if a source star is less massive , since a ratio of the @xmath1-dissociating photon number to the ionizing photon number becomes higher . in order to investigate the radiative feedback effects from such less massive stars , we perform three - dimensional radiation hydrodynamic simulations , incorporating the radiative transfer effect of ionizing and @xmath1-dissociating radiation . as a result , we find that if a source star is less massive than @xmath2 , the ionizing radiation can not suppress the negative feedback of @xmath1-dissociating radiation . therefore , the fate of the neighboring clouds around such less massive stars is determined solely by the flux of @xmath1-dissociating radiation from source stars . with making analytic estimates of @xmath1 shell formation and its shielding effect , we derive the criteria for radiation hydrodynamic feedback depending on the source star mass . [ firstpage ] early universe - galaxies : formation - radiative transfer - hydrodynamics

1004.2325

i

before we can reliably compute how galaxies form stars and evolve as a function of cosmic time , we must understand the physical processes that regulate the balance between neutral and molecular gas in their interstellar media . only if @xmath5 forms , will gravitationally unstable clouds cool and collapse to high enough densities to trigger star formation in the first galaxies . it is also generally believed that star formation occurs exclusively in molecular clouds in all galaxies at all epochs . many galaxy formation models adopt the so - called `` kennicutt - schmidt '' law ( hereafter k - s law , schmidt 1959 , kennicutt 1998 ) to prescribe the rate at which a disk galaxy of given cold gas mass and scale radius will form its stars . this has the form @xmath6 where @xmath7 represents the star formation rate surface density , @xmath8 is the total surface density of the cold gas in the disk , and the exponent @xmath9 is often adopted . some semi - analytic models also account for a critical density below which disks become gravitationally stable and star formation no longer occurs ( e.g kauffmann 1996 , de lucia & blaizot 2007 ) . in this case , @xmath10\ ] ] where the critical density @xmath11 is evaluated using the disk stability criterion given in toomre ( 1964 ) . in both equations ( [ eq : kslaw ] ) and ( [ eq : kslaw1 ] ) , the star formation rate surface density is proportional to the total surface density of cold gas ( i.e. both hi and h@xmath12 components ) in the galaxy . this prescription was motivated by the analysis of 97 nearby galaxies by kennicutt ( 1998 ) , which showed that star formation is more tightly correlated with @xmath8 than with @xmath13 . there have been studies in apparent disagreement with these conclusions ; for example , wong & blitz ( 2002 ) found that the relation between @xmath7 and @xmath13 is stronger than that between @xmath7 and @xmath14 in galaxies with high molecular gas fractions . in recent years , high quality , spatially - resolved maps of the cold gas have become available for samples of a few dozen nearby galaxies . examples of such data include hi maps from the hi nearby galaxy survey ( things ) and co maps from the berkeley - illinois - maryland association survey of nearby galaxies ( bima song ) and hera co - line extragalactic survey ( heracles ) . measurements of the rate at which stars are forming at different radii in the galaxy are provided by spitzer and galex observations . the combination of these different data sets has led to important new constraints on the relationship between star formation and gas in galactic disks . bigiel et al . ( 2008 ) studied 18 disk galaxies and showed that @xmath2 forms stars at a roughly constant efficiency in spirals at radii where it can be detected . their results suggest a star formation law of the form @xmath15 motivated by these findings , galaxy formation modelers are now progressing beyond a simple single - component view of the cold phase of the interstellar medium , and are attempting to model the formation of molecular hydrogen in galaxies . gnedin , tassis & kravtsov ( 2009 ) included a phenomenological model for @xmath5 formation in hydrodynamic simulations of disk galaxy formation . their model includes nonequilibrium formation of @xmath5 on dust and approximate treatment of both its self - shielding , and shielding by dust from the dissociating uv radiation field . dutton ( 2009 ) and dutton & van den bosch ( 2009 ) utilized the empirically - motivated hypothesis of blitz and rosolowsky ( 2004,2006 ) that hydrostatic pressure alone determines the ratio of atomic to molecular gas averaged over a particular radius in the disk in their analytic models of disk formation in a @xmath16cdm cosmology . they analyzed the radial distribution of stars and star formation in their disks , but did not focus very much on gas properties in their model . there have also been some attempts to predict the balance between atomic and molecular gas in galaxies at different redshifts by post - processing the publically available outputs of semi - analytic galaxy formation models ( e.g. obreschkow et al . this work also used the same blitz and rosolowsky ( 2004 , 2006 ) prescription to predict the fraction of molecular gas in disks . however , the obreschkow et al . approach is not self - consistent , because the simulations have been run assuming a `` standard '' kennicutt - schmidt law for star formation and the presence or absence of molecular gas has no influence on the actual evolution of the galaxies in the model . in this paper , we develop new semi - analytic models that follow gas cooling , supernova feedback , the assembly of galactic disks , the conversion of atomic gas into molecular gas as a function of radius within the disk , and the conversion of the gas into stars . in the 1990 s , semi - analytic models of galaxy formation were developed into a useful technique for interpreting observational data on galaxy populations ( e.g. kauffmann , white & guiderdoni 1993 ; cole et al . 1994 ; somerville & primack 1999 ) . in the first decade of the new millennium , considerable effort went into grafting these models on to large n - body simulations of the dark matter component of the universe . these efforts began with relatively low resolution simulations ( kauffmann et al . 1999 ) , but have rapidly progressed to simulations with high enough resolution to follow the detailed assembly histories of millions of galaxies with luminosities well below @xmath17 ( croton et al . 2006 ; bower et al . 2006 ; de lucia & bliazot 2007 ; guo et al . 2010 ) . our new models are an extension of the techniques described in croton et al . ( 2006 ) and de lucia & blaizot ( 2007 ) and are implemented using the merger trees from the millennium simulation ( springel et al . 2005 ) . we explore two different `` recipes '' for partitioning the cold gas into atomic and molecular form : a ) a prescription based on the analytic models of @xmath5 formation , dissociation and shielding developed by krumholz , mckee & tumlinson ( 2009 ) , in which the molecular fraction is a local function of the surface density and the metallicity of the cold gas , b ) the same pressure - based formulation explored by obreschkow et al . ( 2009 ) . we first use our models to calculate the hi , @xmath5 , stellar mass and sfr surface density profiles of disk galaxies that form in dark matter haloes with circular velocities @xmath18 200 km / s ( i.e. galaxies comparable to the milky way ) and we compare our results to the things / heracles observations presented in bigiel et al . ( 2008 ) . we then turn to the issue of the predicted _ scaling relations _ between atomic gas , molecular gas and stars for an ensemble of disk galaxies forming in dark matter haloes spanning a range of different circular velocities . we currently enjoy a rich and diverse array of scaling laws that describe the stellar components of galaxies . for example , the tully - fisher relation and the size - mass relation for local spiral galaxies play a crucial role in constraining current theories of disk galaxy formation . likewise , the scaling laws of bulge - dominated galaxies ( the fundamental plane ) provide important constraints on how these systems may have assembled through merging . in contrast , few well - established scaling laws exist describing how the cold gas is correlated with other global physical properties of galaxies . surveys of atomic and molecular gas in well - defined samples of a few hundred to a thousand galaxies are currently underway , and this paper will explore what can be learned about disk galaxy formation from the results . our paper is organized as follows . in section 2 , we briefly describe the simulation used in our study as well as the semi - analytic model used to track the formation of galaxies in the simulation . in section 3 , we describe the new aspects of the models presented in this paper , including our spatially resolved treatment of disk formation in radial bins , the recipes that prescribe how atomic gas is converted into molecular gas , and our new prescriptions for star formation and feedback . in section 4 , we compare the radial profiles in our models to observations from the things / heracles surveys , and present the global gas properties of the galaxies in our model , such as atomic and molecular gas mass functions . in section 5 , we introduce a set of scaling relations for the atomic and molecular gas fractions of galaxies and we clarify which aspects of the input physics are responsible for setting the slope and the scatter of these relations . finally , in section 6 we summarize our work and discuss our findings .

we extend existing semi - analytic models of galaxy formation to track atomic and molecular gas in disk galaxies . we include two simple prescriptions for molecular gas formation processes in our models : one is based on the analytic calculations by krumholz , mckee & tumlinson ( 2008 ) , and the other is a prescription where the @xmath2 fraction is determined by the pressure of the interstellar medium ( ism ) . motivated by the observational results of leroy et al . galaxies : evolution - stars : formation - galaxies : ism - ism : atoms - ism : molecules

we extend existing semi - analytic models of galaxy formation to track atomic and molecular gas in disk galaxies . simple recipes for processes such as cooling , star formation , supernova feedback , and chemical enrichment of the stars and gas are grafted on to dark matter halo merger trees derived from the millennium simulation . each galactic disk is represented by a series of concentric rings . we assume that surface density profile of infalling gas in a dark matter halo is exponential , with scale radius @xmath0 that is proportional to the virial radius of the halo times its spin parameter @xmath1 . as the dark matter haloes grow through mergers and accretion , disk galaxies assemble from the inside out . we include two simple prescriptions for molecular gas formation processes in our models : one is based on the analytic calculations by krumholz , mckee & tumlinson ( 2008 ) , and the other is a prescription where the @xmath2 fraction is determined by the pressure of the interstellar medium ( ism ) . motivated by the observational results of leroy et al . ( 2008 ) , we adopt a star formation law in which @xmath3 in the regime where the molecular gas dominates the total gas surface density , and @xmath4 where atomic hydrogen dominates . we then fit these models to the radial surface density profiles of stars , hi and @xmath2 drawn from recent high resolution surveys of stars and gas in nearby galaxies . we explore how the ratios of atomic gas , molecular gas and stellar mass vary as a function of global galaxy scale parameters , including stellar mass , stellar surface density , and gas surface density . we elucidate how the trends can be understood in terms of three variables that determine the partition of baryons in disks : the mass of the dark matter halo , the spin parameter of the halo , and the amount of gas recently accreted from the external environment . galaxies : evolution - stars : formation - galaxies : ism - ism : atoms - ism : molecules

1004.2325

i

in this paper , we extend existing semi - analytic models to follow atomic and molecular gas in galaxies . we study how the condensed baryons in present - day disk galaxies are partitioned between stars , hi and h@xmath12 as a function of radius within the disk . our new model is implemented in the l - galaxies semi - analytic code and is a modification of the models of croton et al . ( 2006 ) and de lucia & blaizot ( 2007 ) , in which dark matter halo merger trees derived from the millennium simulation form the `` skeleton '' , on which we graft simplified , but physically motivated , treatment of baryonic processes such as cooling , star formation , supernova feedback , and chemical enrichment of the stars and gas . we fit these models to the radial surface density profiles of stars , hi and @xmath5 derived from recent surveys of gas in nearby galaxies , making use of data from sings , things , heracles and the bima song surveys . we have used our models to explore how the relative mass fractions of atomic gas , molecular gas and stars are expected to vary as a function of global galaxy scale parameters , including stellar mass , mean stellar surface density , and mean gas surface density . we have attempted to elucidate how the trends can be understood in terms of the three variables that determine the partition of baryons in disks : a ) the mass of the dark matter halo , which determines the total mass of baryons that is able to cool and assemble in the disk , b ) the spin parameter of the halo , which sets the contraction factor of the gas , and thereby its surface density and molecular fraction , c ) the amount of gas that has been recently accreted from the external environment . the main changes we have made to earlier models are the following : \(i ) each galactic disk is represented by a series of concentric rings . we assume that surface density profile of infalling gas in a dark matter halo is exponential , with scale radius @xmath0 that is proportional to the virial radius of the halo times the spin parameter of the halo . as the universe evolves , the dark matter halo grows in mass through mergers and accretion and the scale radius of the infalling gas increases . disk galaxies thus form from the inside out in our models . the ring representation allows us to track the surface density _ profiles _ of the stars and gas as a function of cosmic time . \(ii ) we include simple prescriptions for molecular gas formation processes in our models . we adopt two different `` recipes '' : one based on the analytic calculations by krumholz et al . ( 2008 ) , in which @xmath102 is a function of the local surface density and metallicity of the cold gas , and the other motivated by the work of elmegreen ( 1989 & 1993 ) , blitz & rosolowsky ( 2006 ) , and obreschkow et al . ( 2009 ) , in which the @xmath5 fraction is determined by the pressure of the ism . \(iii ) motivated by the observational results of leroy et al . ( 2008 ) , we adopt a star formation law in which @xmath189 in the regime where the molecular gas dominates the total gas surface density , and @xmath190 where atomic hydrogen dominates . our work leads to the following conclusions : \(i ) a simple star formation law in which @xmath191 leads to gas consumption time - scales in the inner disk that are too short . in this paper , we simply patch over this problem by decreasing the efficiency of supernova feedback in the inner disk . \(ii ) the _ mean _ stellar , hi and @xmath5 surface density profiles of the disk galaxies in our model are only weakly sensitive to the adopted @xmath5 fraction prescription . the reason for this is that for typical @xmath17 disk galaxies , the local gas surface density is the main controlling parameter for both recipes . at low gas surface densities , the @xmath5 fraction depends sensitively on metallicity for the krumholz et al . prescription , but considerably less sensitively on stellar surface density @xmath172 for the pressure - based prescription . as a result , the correlation between molecular - to - atomic fraction and @xmath192 for local disk galaxies exhibits more scatter if the krumholz et al . model is correct . \(iii ) our results indicate that galaxies that have recently accreted a significant amount of gas from the external environment are characterized by higher - than - average _ total _ cold gas content . if the galaxy has high gas surface density , then this excess gas is an unambiguous signature of a recent accretion event , because the time - scale over which gas is consumed into stars is short in such systems . on the other hand , if the galaxy has low surface density , a higher - than - average total cold gas content could indicate a recent accretion event , but it may also mean that the galaxy has a higher - than - average spin parameter . higher spin parameters result in disk galaxies with more extended distributions of cold gas , lower - than - average molecular - to - atomic ratios , and low star formation efficiencies . for these ambiguous systems , one must seek additional evidence that the outer disks were assembled _ recently_. although these conclusions are somewhat open - ended , they do suggest avenues for further research . we believe that a more realistic way forward to solving the gas consumption timescale problem would be to model radial inflow of the gas . attempts have been made to construct phenomenological models that do include radial mixing of the stars and gas in disks as well as the effect of this mixing on the chemical evolution of the stars formed in the solar neighbourhood ( e.g schnrich & binney 2009 ) . results from hydrodynamical simulations also indicate that the gas tends to flow inwards , while the stars migrate outwards ( e.g rokar et al . 2008 ) . the main way to distinguish between different scenarios may be the predicted metallicity gradients . we intend to explore these issues in more detail in future work . in our model results , although the surface density profiles from the two @xmath5 fraction prescriptions are very similar , the models indicate that one should , in principle , be able to confirm the metallicity - dependence of the molecular gas fraction predicted by the krumholz prescription , if one measures the average gas - phase metallicities of nearby disk galaxies using emission lines . alternately , one can break the degeneracy by observing systems where the metallicity is low but the pressure is high ( fumagalli , krumholz & hunt 2010 ) . another interesting issue is whether a galaxy s location in the gas scaling relation diagrams can serve as a diagnostic as to whether it has accreted gas from the external environment . although the theory of gas accretion in galaxies has received considerable attention of late ( e.g. kere et al . 2005 ; dekel & birnboim 2006 ; dekel et al . 2009 ) , there is little _ observational evidence that this occurs in practice . this is true both for galaxies in the local universe and at high redshifts , where gas accretion rates are expected to be much higher . although average gas accretion rates are expected to be low at the present day , precise quantification of the expected scaling relations for equilibrium disk galaxies may allow us to identify a subset of systems which deviate significantly from the mean in terms of their gas content . following the conclusion ( iii ) , one may try to gain a better understanding of the observationally detectable signatures of a recent gas accretion episode . possible ways forward would be to look for signatures of recent accretion in the observed age gradients of the stars or in the metallicity gradients of the gas in the disk . one could also look for accretion signatures in the kinematics of the stars and the gas in the outer disks . alternatively , one could search for evidence of complex structure ( e.g. tidal streams or shells ) in the stellar haloes of gas - rich galaxies ( cooper at al 2010 ) . we intend to explore these possibilities in more detail in future work . ongoing and future surveys , such as the galex arecibo sloan survey ( gass ) ( catinella et al . 2010 ) and the cold gass survey carried out at the iram 30 m telescope ( saintonge et al . in preparation ) will enable us to quantify the scaling relations discussed in this paper in considerable detail . these surveys will provide interesting targets for follow - up programs , which may help us understand that extent to which galaxies still accrete gas at the present day . in the next few years , it will become possible to observe gas in galaxies at higher redshifts using facilities such as alma and square kilometer array pathfinder experiments such as askap or meerkat . we are certain that our simplified treatment of disk formation in concentric rings that undergo no radial mixing will not be a good way to describe the assembly of the clumpy , highly turbulent disks that are now known to exist at @xmath193 ( e.g. genzel et al . nevertheless , we believe that our models may still be useful in elucidating the gaseous and chemical evolution of disks over a somewhat smaller range in lookback time .

simple recipes for processes such as cooling , star formation , supernova feedback , and chemical enrichment of the stars and gas are grafted on to dark matter halo merger trees derived from the millennium simulation . each galactic disk is represented by a series of concentric rings . we assume that surface density profile of infalling gas in a dark matter halo is exponential , with scale radius @xmath0 that is proportional to the virial radius of the halo times its spin parameter @xmath1 . as the dark matter haloes grow through mergers and accretion , disk galaxies assemble from the inside out . ( 2008 ) , we adopt a star formation law in which @xmath3 in the regime where the molecular gas dominates the total gas surface density , and @xmath4 where atomic hydrogen dominates . we then fit these models to the radial surface density profiles of stars , hi and @xmath2 drawn from recent high resolution surveys of stars and gas in nearby galaxies . we explore how the ratios of atomic gas , molecular gas and stellar mass vary as a function of global galaxy scale parameters , including stellar mass , stellar surface density , and gas surface density . we elucidate how the trends can be understood in terms of three variables that determine the partition of baryons in disks : the mass of the dark matter halo , the spin parameter of the halo , and the amount of gas recently accreted from the external environment .

we extend existing semi - analytic models of galaxy formation to track atomic and molecular gas in disk galaxies . simple recipes for processes such as cooling , star formation , supernova feedback , and chemical enrichment of the stars and gas are grafted on to dark matter halo merger trees derived from the millennium simulation . each galactic disk is represented by a series of concentric rings . we assume that surface density profile of infalling gas in a dark matter halo is exponential , with scale radius @xmath0 that is proportional to the virial radius of the halo times its spin parameter @xmath1 . as the dark matter haloes grow through mergers and accretion , disk galaxies assemble from the inside out . we include two simple prescriptions for molecular gas formation processes in our models : one is based on the analytic calculations by krumholz , mckee & tumlinson ( 2008 ) , and the other is a prescription where the @xmath2 fraction is determined by the pressure of the interstellar medium ( ism ) . motivated by the observational results of leroy et al . ( 2008 ) , we adopt a star formation law in which @xmath3 in the regime where the molecular gas dominates the total gas surface density , and @xmath4 where atomic hydrogen dominates . we then fit these models to the radial surface density profiles of stars , hi and @xmath2 drawn from recent high resolution surveys of stars and gas in nearby galaxies . we explore how the ratios of atomic gas , molecular gas and stellar mass vary as a function of global galaxy scale parameters , including stellar mass , stellar surface density , and gas surface density . we elucidate how the trends can be understood in terms of three variables that determine the partition of baryons in disks : the mass of the dark matter halo , the spin parameter of the halo , and the amount of gas recently accreted from the external environment . galaxies : evolution - stars : formation - galaxies : ism - ism : atoms - ism : molecules

1310.3024

i

the drgt gravity @xcite is considered as a promising massive gravity model which yields einstein gravity in the massless limit . recently , it was shown that the stability of the schwarzschild black hole in the four dimensional drgt gravity could be determined by the gregory - laflamme ( gl ) instability @xcite of a five - dimensional black string . the small schwarzschild black hole with mass @xmath1 in the drgt gravity and its bi - gravity extension @xcite , and fourth - order gravity @xcite is unstable against metric and ricci tensor perturbations for @xmath2 and @xmath3 , respectively . these results may indicate that static black holes in massive gravity do not exist . interestingly , it turned out that in a massive theory of the einstein - weyl gravity , the linearized einstein tensor perturbations exhibit unstable modes of the schwarzschild - ads black hole featuring the gl instability of five - dimensional ads black string , in contrast to the stable schwarzschild - ads black hole in the einstein gravity @xcite . the linearized ricci tensor perturbations were employed to exhibit unstable modes of the schwarzschild - tangherlini ( higher dimensional schwarzschild ) black hole in higher - dimensional fourth order gravity which features the gl instability of higher dimensional black strings @xcite , in comparison with the stable schwarzschild - tangherlini black holes in higher - dimensional einstein gravity . these imply that the gl instability of the black holes in the massive gravity originates from the massiveness , but not a nature of the fourth - order gravity giving ghost states . also , one could avoid the ghost problem arising from the metric perturbations in the fourth - order gravity when using the linearized einstein and ricci tensors because their linearized equations become the second - order tensor equations . on the other hand , it was shown that the four - dimensional btz black string in einstein gravity is stable against metric perturbations regardless of the horizon size , which is also supported by a thermodynamic argument of gubser - mitra conjecture @xcite . later on , however , it was argued that the btz black string is not always stable against metric perturbations @xcite . in the literatures @xcite , there exists a threshold value for @xmath4 ( we use a different notation @xmath5 to avoid a confusion @xmath6 here ) which is related to the compactification of the extra dimension of the tensor perturbation . it was shown in @xcite that for @xmath7 with @xmath8 ads@xmath9 curvature radius , the btz black string is stable against @xmath0-mode metric perturbation , while for @xmath10 it is unstable . therefore , it seems to be necessary to point out which one is correct . the new massive gravity has been introduced as a fourth - order gravity with a healthy massive spin-2 mode and a massless spin-2 ghost mode , which is pure gauge only in three dimensions @xcite . this parity - even gravity describes two modes of helicity @xmath11 and @xmath12 [ 2 degrees of freedom ( dof ) ] of a massive graviton , but it has a drawback of serving as a unitary model of massive gravity only in three dimensions @xcite . for @xmath13 with @xmath6 the mass of graviton , the three - dimensional btz black hole in the new massive gravity is shown to be stable against @xmath0-mode metric perturbation @xcite when using the positivity of the potential outside the horizon . to this direction , it was recently reported that the stability of the btz black hole was mainly determined by the asymptotes of black hole spacetime : the condition of the @xmath0-mode stability is consistent with the generalized breitenlohner - freedman ( bf ) bound ( @xmath14 ) for metric perturbations on asymptotically ads@xmath9 spacetime @xcite . this result may imply that the stability condition is extended simply from @xmath13 to @xmath14 if @xmath6 is allowed to be a negative quantity . however , one expects that two different type of instabilities appears for the btz black hole in new massive gravity : one is from the bf bound based on the tensor propagation on asymptotically ads@xmath9 spacetime , while the other is the gl instability of a massive graviton propagating on the btz black hole spacetime . this is similar to two instabilities of ads black holes to trigger a holographic superconductor phase within the ads / cft correspondence @xcite . in these models , the ads@xmath15 black hole becomes unstable to form non - trivial fields outside its horizon when being close to extremality whose near - horizon geometry is ads@xmath16 . for a massive scalar with mass @xmath6 between @xmath17 and @xmath18 , two ads spacetimes are unstable @xcite . hence , it suggests strongly that the stability of btz black hole should be revisited in new massive gravity by observing the gl instability of four - dimensional black string . we will show that the instability of a massive graviton persists even in three - dimensional btz black hole . this establishes that the instability of the black holes in the @xmath19-dimensional massive gravity originates from the massiveness , but not a nature of the fourth - order gravity giving ghost states . as a byproduct , we will show that the four - dimensional btz black string is stable against the @xmath0-mode metric perturbation because its mass squared is positive ( @xmath4 ) .

this instability shows that the btz black hole could not exist as a stable static solution to the new massive gravity . for non - rotating btz black string in four dimensions , however , it is demonstrated that the btz black string can be stable against the metric perturbation .

we find the gregory - laflamme @xmath0-mode instability of the non - rotating btz black hole in new massive gravity . this instability shows that the btz black hole could not exist as a stable static solution to the new massive gravity . for non - rotating btz black string in four dimensions , however , it is demonstrated that the btz black string can be stable against the metric perturbation . + taeyoon moon and yun soo myung , + institute of basic sciences and department of computer simulation , inje university , gimhae 621 - 749 , korea + pacs numbers:04.30.nk , 04.70.bw

1504.00260

i

in a series of papers @xcite , the authors studied cluster algebras of finite type in terms of the combinatorics and geometry of finite coxeter groups , and in particular sortable elements and cambrian lattices . in @xcite , these constructions were extended to infinite coxeter groups . sortable elements and cambrian semilattices were shown in @xcite to produce combinatorial models of cluster algebras of infinite type , with an important limitation : sortable elements can only model the part of the exchange graph that corresponds to clusters whose @xmath0-vector cones intersect the interior of the tits cone . in this paper , we show how to extend the sortable / cambrian setup to obtain a complete combinatorial model when @xmath1 is acyclic and its cartan companion @xmath3 is of affine type . the basic idea can be illustrated by a very simple example . -vector fan for @xmath1 with @xmath3 of type @xmath4 and for @xmath2,title="fig : " ] and for @xmath2,title="fig : " ] suppose @xmath50 & 2 \\ -2 & 0 \end{bsmallmatrix*}$ ] . its cartan companion @xmath6 2 & -2 \\ -2 & 2 \end{bsmallmatrix*}$ ] is of type @xmath7 . figure [ a1tilde g ] shows the @xmath0-vector fan associated to @xmath1 . the left picture of figure [ a1tilde camb ] shows the cambrian fan associated to @xmath1 , while the right picture shows the cambrian fan associated to @xmath2 . in each cambrian fan picture , the tits cone is identified by light gray shading and the area outside the cambrian fan is identified by dark gray shading . two surprising things happen . first , the cambrian fan for @xmath1 is `` compatible '' with the image under the antipodal map of the cambrian fan for @xmath2 , in the sense that the union of these two fans is again a fan ( the * _ doubled cambrian fan _ * ) . second , the doubled cambrian fan coincides with the @xmath0-vector fan , so that the dual graph to the doubled cambrian fan is isomorphic to the exchange graph . the main results of the paper are that the first of these surprising things happens for all acyclic @xmath1 and that the second happens whenever @xmath1 is acyclic and @xmath3 is of affine type . for richer examples than the rank-@xmath8 example described above , see examples [ affineg2 ex ] , [ affineg2 frame ex ] , [ 344 ex ] and [ affineg2 slice ex ] . we now state our main results more formally . for each acyclic exchange matrix @xmath1 , we construct a doubled cambrian fan @xmath9 as the union of the cambrian fan for @xmath1 with the antipodal cambrian fan for @xmath2 . the * _ doubled cambrian framework _ * is the pair @xmath10 , where @xmath11 is the dual graph to @xmath9 and @xmath12 is a certain labeling of @xmath11 by roots . in the language of @xcite , the key result is the following . [ affinedoubleframework ] suppose that @xmath1 is acyclic and @xmath3 is of affine type . then @xmath10 is a complete , exact , well - connected , polyhedral , simply connected reflection framework . let @xmath13 be the principal - coefficients cluster algebra associated to @xmath1 . using results of @xcite ( as we explain in section [ frame and clus sec ] ) , the following corollaries are easily obtained . [ affine exch ] if @xmath1 is acyclic and @xmath3 is of affine type , then the exchange graph of the cluster algebra @xmath13 is isomorphic to @xmath11 . the isomorphism sends a vertex @xmath14 of @xmath11 to a seed whose @xmath15-vectors are ( simple - root coordinates of ) @xmath16 . [ affine g ] if @xmath1 is acyclic and @xmath3 is of affine type , then @xmath9 coincides with the fan of @xmath0-vector cones for the cluster algebra @xmath13 . corollary [ affine g ] refers to the @xmath0-vector cones defined by interpreting @xmath0-vectors as fundamental - weight coordinates of vectors in the weight lattice . see ( * ? ? ? * remark 5.17 ) and section [ ca background sec ] of the present paper . when @xmath1 is of infinite non - affine type , the doubled cambrian fan may be a proper subfan of the @xmath0-vector fan . ( see example [ 344 ex ] . ) however , the doubled cambrian fan coincides with the @xmath0-vector fan for all @xmath17 exchange matrices , even those of non - affine infinite type . ( see remark [ rank 2 ] . ) one of the initial motivations for this work was to prove the affine - type case of many of the standard structural conjectures on cluster algebras . indeed , theorems about frameworks from @xcite combined with the results stated above accomplish that task . ( see corollary [ affine type conj ] . ) many of the standard conjectures have been turned into theorems in full generality ( not merely the affine case ) using the machinery of scattering diagrams @xcite . see also the table at the end of ( * ? ? ? * section 3.3 ) for more on the previous status of these conjectures . the approach to cluster algebras via scattering diagrams makes it _ more _ important , not less important , to make explicit constructions in key special cases , like the affine case . scattering diagrams consist of a rational fan , decorated with certain rational functions , and containing the @xmath0-vector fan as a subfan . other constructions , notably semi - invariants ( see @xcite for a detailed treatment of the affine case , @xcite for the acyclic case and @xcite for the beginnings of an investigation of the general case ) and the mutation fan @xcite also yield fans that contain the @xmath0-vector fan . however , none of these methods give a direct combinatorial description of the fan , and it is difficult to use them to study the regions of the fan . scattering diagrams natively construct the walls of the fan and it is difficult to use them to discuss the chambers cut out by those walls . ( not impossible though ! see @xcite for some progress along these lines . ) semi - invariants also naturally construct the walls , although connections have been found to cluster tilting and @xmath18-tilting modules which correspond to the regions @xcite . neither method naturally connects the fan directly to lattice theory , although torsion classes form a lattice which has been related to semi - invariants @xcite . in contrast , our methods provide direct descriptions of the @xmath0-vector fan in the affine types in terms of the combinatorics of affine coxeter groups and root systems . we label the regions of the @xmath0-vector fan by sortable elements in those groups , which can be described either in terms of reduced words or in terms of pattern avoidance ( @xcite ) . and our methods are built on lattice theoretic and geometric properties which are well suited for proving global properties of the fans we study . the remainder of the paper is devoted to constructing the doubled cambrian framework and fan and proving theorem [ affinedoubleframework ] . we begin with background in section [ background sec ] . we define the doubled cambrian framework and fan for any acyclic exchange matrix in section [ double sec ] , where we also prove the part of theorem [ affinedoubleframework ] that does not need the hypothesis the @xmath3 is of affine type . the proof of theorem [ affinedoubleframework ] is completed in section [ affine sec ] . most of the affine dynkin diagrams are trees , and thus admit no non - acyclic orientations . the exception is @xmath19 ( @xmath20 ) , which is an @xmath21-cycle . thus , in almost every case when @xmath3 is of affine type , @xmath1 is acyclic and the doubled cambrian framework construction provides a complete framework for @xmath1 . however , the cyclic orientation in type @xmath19 ( @xmath20 ) does not fit into the doubled cambrian framework . in this case , the associated cluster algebra is of finite type @xmath22 . in @xcite , we construct a complete framework for the cyclically oriented @xmath21-cycle using the @xmath23 root system and a variation on the doubled cambrian framework idea .

we give a combinatorial model for the exchange graph and @xmath0-vector fan associated to any acyclic exchange matrix @xmath1 of affine type . the framework ( and in particular the @xmath0-vector fan ) is constructed by combining a copy of the cambrian fan for @xmath1 with an antipodal copy of the cambrian fan for @xmath2 .

we give a combinatorial model for the exchange graph and @xmath0-vector fan associated to any acyclic exchange matrix @xmath1 of affine type . more specifically , we construct a reflection framework for @xmath1 in the sense of [ n. reading and d. e. speyer , `` combinatorial frameworks for cluster algebras '' ] and establish good properties of this framework . the framework ( and in particular the @xmath0-vector fan ) is constructed by combining a copy of the cambrian fan for @xmath1 with an antipodal copy of the cambrian fan for @xmath2 .

0906.0823

c

in figure [ all ] , we compare the spatial distribution of the high - velocity @xmath3co ( @xmath4=32 ) emission , sio ( @xmath16=0 , @xmath4=21 ) emission , and the 3.3 mm dust continuum emission . the linearly extended feature in the sio emission coincides well with the blueshifted lobe of the molecular outflow driven by fir 6c . since the sio emission often traces shocked molecular gas caused by the interaction between the primary jet and the ambient molecular gas @xcite , this sio emission probably traces the well collimated outflow driven by fir 6c . furthermore , core 2 , 3 , and 4 in fir 6a clump surround the tip of component 1 in the sio emission , while the tip of component 2 locates even more downstream beyond fir 6a clump . in figure [ pv ] , we show position - velocity diagrams of the @xmath3co ( @xmath4=32 ) and sio ( @xmath16=0 , @xmath4=21 ) lines along the axis of the fir 6c outflow . it is obvious that there are two distinct outflow components in the @xmath3co and sio emission ; the velocity component with the higher blueshifted velocity corresponds to component 1 , while the other lower velocity component located away from fir 6c corresponds to component 2 . the sio emission of component 1 shows significant increase of the line width at the position of fir 6a clump . this increase of the sio line width , as well as the shell - like structure in fir 6a clump at the interface with component 1 , implies the presence of the interaction between the molecular outflow driven by fir 6c and fir 6a clump @xcite . we suggest that the two distinct sio components were ejected toward slightly different 3-dimensional directions , as seen in other protostellar jets @xcite , and that the direction of component 1 matches the direction to fir 6a clump from fir 6c . therefore , the jet component 1 interacts with fir 6a clump while component 2 keeps moving freely . on the assumption of the same jet propagation velocity , the lower line of sight velocity of component 2 implies that the jet axis of component 2 is closer to the plane of the sky than that of component 1 , which is consistent with the larger distance of component 2 from fir 6c . such an interaction associated with the outflow alters the physical condition of the surrounding medium through the c - type shock @xcite . @xcite have reported that a postshock density is 10 - 40 times more than a preshock density from their mhd simulation of the interaction . since the present gas density of fir 6a clump is estimated to be @xmath0 1.0 - 2.9 @xmath6 10@xmath11 @xmath12 , the preshock density of fir 6a clump is @xmath0 2.6 - 7.3 @xmath6 10@xmath45 @xmath12 on the assumption that a postshock density is 40 times more than a preshock density . the redshifted counterpart of the sio emission , on the other hand , was not detected . one of the possible reasons for the non - detection of the sio emission is that there is not sufficient dense - gas material at the south - west of fir 6c , and hence the reservoir of the sio production or amount of dust grains @xcite are not ample enough . in fact , the 1.3 mm dust continuum map in the fir 6 region by @xcite exhibits that there is asymmetric distribution of dusts around fir 6c , and that at the south - west of fir 6c the dust continuum emission becomes fainter while toward the north - east of fir 6c the dust continuum emission becomes stronger and shows a emission ridge . in section 4.1 . , we demonstrate that the outflow driven by fir 6c interacts with fir 6a clump . three cores in fir 6a clump locate around the tip of the fir 6c outflow , and it is possible that the interaction affects the physical evolution of these cores . in the following section , we discuss the possible effects of the interaction on these cores . first , we compare the time scale of the interaction to the time scale of fragmentation of fir 6a clump to produce the three cores . on the assumption that the interaction time scale @xmath46 is similar to the dynamical time - scale of the fir 6c outflow , i.e. @xmath46 @xmath0 @xmath47 , @xmath46 is estimated to be 1.2 - 1.9 @xmath6 10@xmath48 yr @xcite . the time scale of the fragmentation into the cores can be estimated on the assumption that the fragmentation time scale is the sound crossing time ; @xmath49 @xmath0 1.5 @xmath6 10@xmath50 yr . these two times scales are indistinguishable from each other and hence it is not straightforward to tell whether the interaction takes place before or after the production of the three cores . then we will discuss the following two cases ; * case 1 : the fir 6a cores were formed before the interaction occurs . * case 2 : the fir 6a cores were formed after the interaction occurs . in case 1 , the fir 6a cores could have been formed via spontaneous fragmentation or turbument fragmentation before the interaction @xcite . in this case , the outflow driven by fir 6c may externally affect the subsequent evolution of these cores . @xcite have compared the total force required to balance the gravity of the dense cores with the outflow momentum flux in the ngc 2264-c region , in order to assess whether the outflows influence the evolution of the neighboring cores . we follow the same argument for our case of the fir 6 region to investigate whether the blueshifted component of the fir 6c outflow influences the physical evolution of the fir 6a cores . the total force needed to balance gravity @xmath51 is expressed as @xmath52 ( eq.10 ; @xcite ) . since the average radius of the fir 6a cores and the mass are estimated to be @xmath53 = 0.0075 pc and @xmath54 = 1.3 -3.6 m@xmath2 , respectively ( see section 3.1 . ) , @xmath51 is calculated to be 1.0 - 7.7 @xmath6 10@xmath7 m@xmath2 km s@xmath5 yr@xmath5 . on the other hand , the outflow momentum flux of the blueshifted component of the fir 6c outflow @xmath55 is 2.4 @xmath6 10@xmath9 m@xmath2 km s@xmath5 yr@xmath5 @xcite , and hence the total force is @xmath0 10 times larger than the outflow momentum flux ( @xmath56 ) . therefore , it is unlikely that the interaction with the fir 6c outflow influences the subsequent physical evolution of the fir 6a cores . @xcite have also reported that the total momentum flux of eleven outflows in ngc 2264-c is insufficient to prevent the cores from collapsing . in case 2 , the fir 6a cores are considered to have been produced by the interaction . in fact , @xcite have demonstrated that the external shock compression could trigger the gravitational fragmentation of dense - gas clumps into cores . then , we compare the separation among core 2 , 3 , and 4 with the jeans length in order to investigate whether the fragmentation into the cores is caused by the gravitational instability . the mean projected separation ( @xmath25 @xmath57 ) among the fir 6a cores , corresponding to the lower limit of the real separation , is @xmath0 5 @xmath1 ( @xmath0 2.0 @xmath6 10@xmath10 au ) . the jeans length ( @xmath25 @xmath58 ) can be calculated with @xmath59 @xcite , where @xmath60 , g , and @xmath38 are the effective sound speed , gravitational constant , and the average gas density of fir 6a clump , respectively . we adopt a preshock density of @xmath0 2.6 - 7.3 @xmath6 10@xmath45 @xmath12 as an average gas density @xmath38 of fir 6a clump before the interaction . it is difficult , on the other hand , to observationally estimate @xmath60 , since there is no molecular emission , such as h@xmath42co@xmath43 ( @xmath4=10 ) and n@xmath61h@xmath43 ( @xmath4=10 ) , associated with fir 6a clump @xcite . hence , we simply assume that @xmath60 in fir 6a clump is same as that in fir 4 clump ( @xmath0 0.62 km s@xmath5 ) . with these values , the jeans length @xmath62 is estimated to be 5.0 - 8.4 @xmath63 au , which is comparable to the means separation among fir 6a cores . then , it is possible that the interaction triggers the jeans instability in fir 6a clump , which results in the fragmentation into fir 6a cores . furthermore , this interpretation is supported by the distribution of the dusty cores , which appears to delineate the outflow structure . our observational results can not distinguish precisely between case 1 and case 2 . in either case , however , fir 6a clump contains three cores with a mass of 0.18 - 1.6 m@xmath2 and a density of 0.2 - 5.8 @xmath64 @xmath12 , and these cores may be potential formation sites of the next - generation of cluster members .

appears abrupt increase of the sio line width ( @xmath0 15 km s@xmath5 ) , where the three resolved cores in fir 6a seem to delineate the tip . these results imply the presence of the interaction and the bowshock front between the fir 6c molecular outflow and fir 6a . fir 6a cores , with a mass of 0.18 - 1.6 m@xmath2 and a density of 0.2 - 5.8 @xmath6 10@xmath11 @xmath12 , might be potential formation sites of the next generation of cluster members .

we have conducted millimeter interferometric observations of the orion molecular cloud-2 ( omc-2 ) fir 6 region at an angular resolution of @xmath0 4@xmath1 - 7@xmath1 with the nobeyama millimeter array ( nma ) . in the 3.3 mm continuum emission we detected dusty core counterparts of the previously identified fir sources ( fir 6a , 6b , 6c , and 6d ) , and moreover , resolved fir 6a into three dusty cores . the size and mass of these cores are estimated to be 1100 - 5900 au and 0.19 - 5.5 m@xmath2 , respectively . we found that in the @xmath3co ( @xmath4=10 ) emission fir 6b , 6c , and 6d eject the molecular outflow and that the fir 6c outflow also exhibits at least two collimated jet - like components in the sio ( @xmath4=21 ) emission . at the tip of one of the sio components there appears abrupt increase of the sio line width ( @xmath0 15 km s@xmath5 ) , where the three resolved cores in fir 6a seem to delineate the tip . these results imply the presence of the interaction and the bowshock front between the fir 6c molecular outflow and fir 6a . if the interaction occurred after the formation of the fir 6a cores the influence of the fir 6c outflow on the fir 6a cores is minimal , since the total gravitational force in the fir 6a cores ( 1.0 - 7.7 @xmath6 10@xmath7 m@xmath2 km s@xmath8 yr@xmath5 ) is much larger than the outflow momentum flux ( 2.4 @xmath6 10@xmath9 m@xmath2 km s@xmath8 yr@xmath5 ) . on the other hand , it is also possible that the interaction caused the gravitational instability in fir 6a , and triggered the fragmentation into three cores , since the separation among these cores ( @xmath0 2.0 @xmath6 10@xmath10au ) is on the same order of the jeans length ( @xmath0 5.0 - 8.4 @xmath6 10@xmath10au ) . in either case , fir 6a cores , with a mass of 0.18 - 1.6 m@xmath2 and a density of 0.2 - 5.8 @xmath6 10@xmath11 @xmath12 , might be potential formation sites of the next generation of cluster members .

0906.0823

i

we have carried out high angular - resolution ( @xmath0 4@xmath1 - 7@xmath1 ) millimeter interferometric observations of the omc-2 fir 6 region with the nma in the @xmath3co ( @xmath4=10 ) and sio ( @xmath16=0 , @xmath4=21 ) lines as well as the 3.3 mm continuum emission . the main results of our new millimeter observations are summarized as follows ; 1 . we detected dusty counterparts of fir 6a - d in the 3.3 mm continuum emission . in particular we have first resolved fir 6a into three dusty cores and we totally detected six dusty cores . typical size , mass , and the average gas density of these cores is estimated to be @xmath0 1100 - 5900 au , @xmath0 0.18 - 5.5 m@xmath2 , and @xmath0 10@xmath65 @xmath12 , respectively . our nma observations in the @xmath3co ( @xmath4=10 ) emission have confirmed the presence of molecular outflows driven by fir 6b and 6c , which were previously identified with single - dish observations . furthermore , we have found a new outflow candidate whose driving source is fir 6d . previous single - dish observations could not find this outflow , because this outflow is hidden in the ambient cloud component . we detected at least two well - collimated sio ( @xmath16=0 , @xmath4=21 ) components aligned along the axis of the blue lobe of the fir 6c outflow , which probably traces the well - collimated jet components ejected by fir 6c . one of the sio components , component 1 , shows a higher blueshifted velocity ( -11.7 @xmath0 11.0 km s@xmath5 ) than the other , component 2 ( 3.4 @xmath0 14.2 km s@xmath5 ) , while the tip of component 2 locates more distant from the driving source . at the tip of component 1 , the line width of the sio emission shows abrupt increase and the cores in fir 6a clump form a shell - like feature , suggesting the presence of the bowshock front . we consider that component 1 is interacting with fir 6a clump while component 2 is propagating to the different direction freely . figure [ overview ] shows a schematic picture in the fir 6 region . the estimated time scale of the fragmentation of fir 6a clump into the three cores ( @xmath0 1.5 @xmath6 10@xmath50 yr ) is similar to the time scale of the interaction between the molecular outflow driven by fir 6c and fir 6a clump ( 1.2 - 1.9 @xmath6 10@xmath50 yr ) , and hence we can not tell whether the fragmentation of fir 6a clump into the cores occurs before or after the interaction . in the former case , the interaction with the fir 6c outflow is unlikely to affect the subsequent evolution of the fir 6a cores , since the momemtum flux of the fir 6c outflow is one order of magnitude smaller than the gravitational force in the fir 6a cores . in the latter case , it is possible that the interaction between the fir 6c outflow and fir 6a clump triggered the fragmentation into the cores by the gravitational instability . in either case , the fir 6a cores might be potential sites of the next - generation cluster formation in the fir 6 region . we are grateful to the staff at the nobeyama radio observatory ( nro ) for both operating the nma and helping us with the data reduction . nobeyama radio observatory is a branch of the national astronomical observatory , national institutes of natural sciences , japan . we thank d. johnstone for providing us the submillimeter continuum data taken with jcmt . moreover we acknowledge m. yamada , n. ikeda , y. kurono , and t. tsukagoshi for their helpful comments . we also acknowledge the anonymous referee for providing helpful suggestions to improve the paper . y. shimajiri was financially supported by global coe program `` the physical sciences frontier '' , mext , japan . s. takahashi is supported by a postdoctoral fellowship of the institute of astronomy and astrophysics , academia sinica . this work was supported by grant - in - aid for scientific research a 18204017 . s. takakuwa acknowledges a grant from the national science council of taiwan ( nsc 97 - 2112-m-001 - 003-my2 ) in support of this work . allen , l. , et al . 2007 , protostars and planets v , 361 aso , y. , tatematsu , k. , sekimoto , y. , nakano , t. , umemoto , t. , koyama , k. , & yamamoto , s. 2000 , , 131 , 465 avery , l. w. , & chiao , m. 1996 , , 463 , 642 bachiller , r. , martin - pintado , j. , & fuente , a. 1991 , , 243 , l21 bachiller , r. , prez gutirrez , m. , kumar , m. s. n. , & tafalla , m. 2001 , , 372 , 899 bergin , e. a. , neufeld , d. a. , & melnick , g. j. 1998 , , 499 , 777 castets , a. , & langer , w. d. 1995 , , 294 , 835 chini , r. , reipurth , b. , ward - thompson , d. , bally , j. , nyman , l .- a . , sievers , a. , & billawala , y. 1997 , , 474 , l135 elmegreen , b. g. 1998 , origins , 148 , 150 genzel , r. , & stutzki , j. 1989 , , 27 , 41 gueth , f. , bachiller , r. , & tafalla , m. 2003 , , 401 , l5 gusdorf , a. , cabrit , s. , flower , d. r. , & pineau des forts , g. 2008 , , 482 , 809 hildebrand , r. h. 1983 , , 24 , 267 hirano , n. , liu , s .- y . , shang , h. , ho , p. t. p. , huang , h .- c . , kuan , y .- j . , mccaughrean , m. j. , & zhang , q. 2006 , , 636 , l141 ikeda , n. , sunada , k. , & kitamura , y. 2007 , , 665 , 1194 inutsuka , s .- i . , & miyama , s. m. 1997 , , 480 , 681 johnstone , d. , & bally , j. 1999 , , 510 , l49 jrgensen , j. k. , et al . 2007 , , 659 , 479 kobayashi , n. , yasui , c. , tokunaga , a. t. , & saito , m. 2008 , , 683 , 178 koenig , x. p. , allen , l. e. , gutermuth , r. a. , hora , j. l. , brunt , c. m. , & muzerolle , j. 2008 , , 688 , 1142 lada , c. j. , & lada , e. a. 2003 , , 41 , 57 li , z .- y . , & nakamura , f. 2004 , , 609 , l83 maury , a. j. , andr , p. , & li , z. - . 2009 , arxiv:0902.1379 menten , k. m. , reid , m. j. , forbrich , j. , & brunthaler , a. 2007 , , 474 , 515 nakamura , f. , & li , z .- y . 2007 , , 662 , 395 nielbock , m. , chini , r. , mller , s. a. h. 2003 , , 408 , 245 okumura , s. k. , et al . 2000 , , 52 , 393 reipurth , b. , rodrguez , l. f. , & chini , r. 1999 , , 118 , 983 saito , m. , sunada , k. , kawabe , r. , kitamura , y. , & hirano , n. 1999 , , 518 , 334 saito , m. , kawabe , r. , kitamura , y. , & sunada , k. 2001 , , 547 , 840 sandstrom , k. m. , peek , j. e. g. , bower , g. c. , bolatto , a. d. , & plambeck , r. l. 2007 , , 667 , 1161 sandell , g. , & knee , l. b. g. 2001 , , 546 , l49 shimajiri , y. , takahashi , s. , takakuwa , s. , saito , m. , & kawabe , r. 2008 , , 683 , 255 takahashi , s. , saito , m. , takakuwa , s. , & kawabe , r. 2006 , , 651 , 933 takahashi , s. , saito , m. , takakuwa , s. , & kawabe , r. 2008a , , 313 , 165 takahashi , s. , saito , m. , ohashi , n. , kusakabe , n. , takakuwa , s. , shimajiri , y. , tamura , m. , & kawabe , r. 2008b , , 688 , 344 takakuwa , s. , kamazaki , t. , saito , m. , & hirano , n. 2003 , , 584 , 818 takakuwa , s. , et al . 2004 , , 616 , l15 takakuwa , s. , et al . 2007b , , 662 , 431 tatematsu , k. , kandori , r. , umemoto , t. , & sekimoto , y. 2008 , , 60 , 407 tsujimoto , m. , koyama , k. , tsuboi , y. , goto , m. , & kobayashi , n. 2003 , , 585 , 602 velusamy , t. , & langer , w. d. 1998 , , 392 , 685 whitworth , a. p. , bhattal , a. s. , chapman , s. j. , disney , m. j. , & turner , j. a. 1994 , , 290 , 421 williams , j. p. , plambeck , r. l. , & heyer , m. h. 2003 , , 591 , 1025 wilner , d. j. , & welch , w. j. 1994 , , 427 , 898 yokogawa , s. , kitamura , y. , momose , m. , & kawabe , r. 2003 , , 595 , 266 yu , k. c. , billawala , y. , smith , m. d. , bally , j. , & butner , h. m. 2000 , , 120 , 1974 lcc & @xmath3co ( @xmath4=10 ) & sio ( @xmath16=0 , @xmath4=21 ) + configuration & + baseline [ k@xmath28 ] & 3.9 - 31.4 & 3.3 - 27.0 + primary beam hpbw [ arcsec ] & 62 @xmath1 & 77 @xmath1 + synthesized beam hpbw [ arcsec ] & 6@xmath244 @xmath6 5@xmath244 & 8@xmath248 @xmath6 7@xmath241 + velocity resolution [ km s@xmath5 ] & 0.406 km s@xmath5 & 0.539 km s@xmath5 + gain calibrator & + bandpass calibrator & + system temperature in dsb [ k ] & 200 - 300 k & 100 - 300 k + rms noise level [ jy beam@xmath5 ] & 0.18 jy beam@xmath5 & 0.07 jy beam@xmath5 + lcc & figure [ dust]a & figure [ dust]b + configuration & + baseline [ k@xmath28 ] & + weighting & natural & uniform + beam size ( hpbw ) [ arcsec ] & 6@xmath246 @xmath6 4@xmath249 & 5@xmath241 @xmath6 3@xmath248 + p.a . of the beam [ @xmath68 & -15.7 & -24.0 + gain calibrator @xmath69 & + bandpass calibrator @xmath70 & + system temperature in dsb [ k ] & + rms noise level [ jy beam@xmath5 ] & 9.7 @xmath6 10@xmath7 jy beam@xmath5 & 1.2 @xmath6 10@xmath71 jy beam@xmath5 + lccccccc & & & d@xmath40 @xmath6 d@xmath41@xmath69 & p.a . & m@xmath30 @xmath70 & n + & @xmath17 & @xmath18 & ( @xmath610@xmath72 au ) & ( degree ) & m@xmath2 & ( @xmath12 ) + core 1 & 05@xmath73 35@xmath74 55@xmath756 & -05@xmath76 12@xmath77 3@xmath272 & 3.3 @xmath6 2.9 & 178.7 & 1.9 - 5.5 & 1.7 - 4.7 @xmath6 10@xmath11 + core 2 & 05 35 22.7 & -05 12 25.2 & 3.9 @xmath6 1.8 & 1.0 & 0.56 - 1.6 & 0.81 - 2.3 @xmath6 10@xmath11 + core 3 & 05 35 22.3 & -05 12 27.1 & 1.6 @xmath6 1.1 & 170.5 & 0.18 - 0.51 & 2.1 - 5.8 @xmath6 10@xmath11 + core 4 & 05 35 23.0 & -05 12 30.7 & 5.7 @xmath6 2.8 & 157.6 & 0.52 - 1.5 & 0.20 - 0.59 @xmath6 10@xmath11 + core 5 & 05 35 21.4 & -05 13 17.0 & 4.8 @xmath6 3.5 & 41.7 & 1.6 - 4.5 & 0.58 - 1.6 @xmath6 10@xmath11 + core 6 & 05 35 20.1 & -05 13 15.0 & 2.7 @xmath6 1.8 & 159.4 & 1.4 - 4.0 & 3.5 - 9.9 @xmath6 10@xmath11 +

we have conducted millimeter interferometric observations of the orion molecular cloud-2 ( omc-2 ) fir 6 region at an angular resolution of @xmath0 4@xmath1 - 7@xmath1 with the nobeyama millimeter array ( nma ) . in the 3.3 mm continuum emission we detected dusty core counterparts of the previously identified fir sources ( fir 6a , 6b , 6c , and 6d ) , and moreover , resolved fir 6a into three dusty cores . the size and mass of these cores are estimated to be 1100 - 5900 au and 0.19 - 5.5 m@xmath2 , respectively . if the interaction occurred after the formation of the fir 6a cores the influence of the fir 6c outflow on the fir 6a cores is minimal , since the total gravitational force in the fir 6a cores ( 1.0 - 7.7 @xmath6 10@xmath7 m@xmath2 km s@xmath8 yr@xmath5 ) is much larger than the outflow momentum flux ( 2.4 @xmath6 10@xmath9 m@xmath2 km s@xmath8 yr@xmath5 ) . on the other hand , it is also possible that the interaction caused the gravitational instability in fir 6a , and triggered the fragmentation into three cores , since the separation among these cores ( @xmath0 2.0 @xmath6 10@xmath10au ) is on the same order of the jeans length ( @xmath0 5.0 - 8.4 @xmath6 10@xmath10au ) . in either case ,

we have conducted millimeter interferometric observations of the orion molecular cloud-2 ( omc-2 ) fir 6 region at an angular resolution of @xmath0 4@xmath1 - 7@xmath1 with the nobeyama millimeter array ( nma ) . in the 3.3 mm continuum emission we detected dusty core counterparts of the previously identified fir sources ( fir 6a , 6b , 6c , and 6d ) , and moreover , resolved fir 6a into three dusty cores . the size and mass of these cores are estimated to be 1100 - 5900 au and 0.19 - 5.5 m@xmath2 , respectively . we found that in the @xmath3co ( @xmath4=10 ) emission fir 6b , 6c , and 6d eject the molecular outflow and that the fir 6c outflow also exhibits at least two collimated jet - like components in the sio ( @xmath4=21 ) emission . at the tip of one of the sio components there appears abrupt increase of the sio line width ( @xmath0 15 km s@xmath5 ) , where the three resolved cores in fir 6a seem to delineate the tip . these results imply the presence of the interaction and the bowshock front between the fir 6c molecular outflow and fir 6a . if the interaction occurred after the formation of the fir 6a cores the influence of the fir 6c outflow on the fir 6a cores is minimal , since the total gravitational force in the fir 6a cores ( 1.0 - 7.7 @xmath6 10@xmath7 m@xmath2 km s@xmath8 yr@xmath5 ) is much larger than the outflow momentum flux ( 2.4 @xmath6 10@xmath9 m@xmath2 km s@xmath8 yr@xmath5 ) . on the other hand , it is also possible that the interaction caused the gravitational instability in fir 6a , and triggered the fragmentation into three cores , since the separation among these cores ( @xmath0 2.0 @xmath6 10@xmath10au ) is on the same order of the jeans length ( @xmath0 5.0 - 8.4 @xmath6 10@xmath10au ) . in either case , fir 6a cores , with a mass of 0.18 - 1.6 m@xmath2 and a density of 0.2 - 5.8 @xmath6 10@xmath11 @xmath12 , might be potential formation sites of the next generation of cluster members .

hep-lat9608002

i

the 2-dimensional @xmath0 non - linear @xmath3-model is defined by the action @xmath4 together with the condition @xmath5 for all spacetime points @xmath6 . in this equation @xmath7 is the inverse of the bare coupling constant . perturbation theory @xmath8 predicts that this model is asymptotically free for @xmath9 . in particular the exponential correlation length @xmath10 on the lattice must scale as @xmath11 where @xmath12 are the corrections to universal scaling . here @xmath14 is a non - perturbative constant which for the standard action equals @xcite @xmath15 we define the magnetic susceptibility @xmath16 as the two - point correlation function at zero momentum . it scales as @xmath17 where again @xmath18 is a non - perturbative constant . from equations ( 2 ) and ( 4 ) we conclude that in @xmath19 the ratio @xmath20 tends to @xmath21 as we approach the continuum limit , @xmath22 . the corrections to asymptotic scaling @xmath23 depend on @xmath24 and @xmath25 . in a series of papers @xcite another scenario has been put forward for the model defined in ( 1 ) . under reasonable hypothesis the authors prove that there is no mass gap and that this model must undergo a kosterlitz - thouless - like ( @xmath26 ) phase transition at finite beta , @xmath27 . this implies that the ratio @xmath28 should be constant as one approaches @xmath27 from below . here @xmath29 is a critical exponent . for the @xmath30 model this exponent is @xmath31 . in @xcite the authors show that the @xmath2 model with the standard action on the lattice and @xmath31 gives a constant for @xmath32 while the data for @xmath33 displays a clear drop . here we will show a progress report from an extensive simulation performed on the @xmath1 model with standard action and the @xmath2 model with the tree - level improved symanzik action @xcite . if the constancy of @xmath32 for the @xmath2 model is a genuine physical effect , then also for the symanzik action we should see such a behaviour . the full account of our results with better statistics and using more corrections to asymptotic scaling can be found in @xcite . 0.3 cm 0.3 cm

we have performed a high statistics monte carlo simulation to investigate whether the two - dimensional @xmath0 non - linear sigma models are asymptotically free or they show a kosterlitz - thouless - like phase transition . we have calculated the mass gap and the magnetic susceptibility in the @xmath1 model with standard action and the @xmath2 model with symanzik action .

we have performed a high statistics monte carlo simulation to investigate whether the two - dimensional @xmath0 non - linear sigma models are asymptotically free or they show a kosterlitz - thouless - like phase transition . we have calculated the mass gap and the magnetic susceptibility in the @xmath1 model with standard action and the @xmath2 model with symanzik action . our results for @xmath1 support the asymptotic freedom scenario .

1401.8091

i

we have used the the 4000 break and h@xmath0 indices in combination with sfr/@xmath1 derived from emission line flux measurements , to constrain the recent star formation histories of galaxies in the stellar mass range @xmath67 . our main results can be summarized as follows . * the fraction of the total sfr density in galaxies with ongoing bursts declines with increasing stellar mass , from 0.85 at a stellar mass of @xmath3 to 0.25 at a stellar mass of @xmath10 . the duty cycle of bursts declines from 0.7 for @xmath56 galaxies to 0.1 for @xmath10 galaxies . * the median burst mass fraction in galaxies of all stellar masses is small , 5% or less . there is , however , a tail of low mass galaxies that are undergoing bursts that have formed as much as 50 - 60% of their present - day mass . the number of galaxies in this high mass fraction tail decreases as a function of stellar mass . * low mass galaxies are not all young . the distribution of half mass formation times for galaxies with stellar masses less than @xmath5 is broad , spanning the range from 1 to 10 gyr . this is quite different to what is obtained when colours or 4000 break strengths are used to estimate stellar population age , assuming continuous star formation histories . * the peak - to - trough variation in star formation rate among the bursting population ranges from a factor of 25 in the lowest mass galaxies in our sample to a factor of 10 for galaxies with @xmath68 . the average duration of bursts in low mass galaxies is comparable to their average dynamical time . * burst mass fraction is correlated with galaxy structure in quite different ways in low and high mass galaxies . high mass galaxies experiencing strong bursts are more centrally concentrated , indicating that bulge formation is likely at work . this is not seen in low mass galaxies . in low mass galaxies , we find that the stellar surface densities decrease as a function of @xmath7 . * gas phase metallicities decrease as a function of @xmath7 in galaxies of all stellar masses . these results are in rather good agreement with the observational predictions of teyssier et al ( 2013 ) and lend further credence to the idea that the cuspy halo problem can be solved by energy input from multiple starbursts triggered by gas cooling and supernova feedback cycles over the history of a low mass galaxy . we note that the analysis in this paper is confined to the stellar populations enclosed within the 3 arsecond diameter fiber aperture , which samples the central @xmath38 20 - 30 % of the total light from the galaxy . in future , it will be interesting to obtain resolved kinematic data for complete samples of low mass galaxies to understand the influence of bursts on galaxy and dark matter halo structure in more detail .

we have used 4000 break and h@xmath0 indices in combination with sfr/@xmath1 derived from emission line flux measurements , to constrain the recent star formation histories of galaxies with stellar masses in the range @xmath2 . the fraction of the total sfr density in galaxies with ongoing bursts is a strong function of stellar mass , declining from 0.85 at a stellar mass of @xmath3 to 0.25 for galaxies with @xmath4 . low mass galaxies are not all young . the distribution of half mass formation times for galaxies with stellar masses less than @xmath5 is broad , spanning the range 1 - 10 gyr . the peak - to - trough variation in star formation rate among the bursting population ranges lies in the range 10 - 25 . in low mass galaxies , the average duration of the burst bursts is comparable to the dynamical time of the galaxy . galaxy structure is correlated with estimated burst mass fraction , but in different ways in low and high mass galaxies . high mass galaxies with large burst mass fractions are more centrally concentrated , indicating that bulge formation is at work . in low mass galaxies , stellar surface densities @xmath6 decrease as a function of @xmath7 . these results are in good agreement with the observational predictions of teyssier et al ( 2013 ) and lend further credence to the idea that the cuspy halo problem can be solved by energy input from multiple starbursts over the lifetime of the galaxy .

we have used 4000 break and h@xmath0 indices in combination with sfr/@xmath1 derived from emission line flux measurements , to constrain the recent star formation histories of galaxies with stellar masses in the range @xmath2 . the fraction of the total sfr density in galaxies with ongoing bursts is a strong function of stellar mass , declining from 0.85 at a stellar mass of @xmath3 to 0.25 for galaxies with @xmath4 . low mass galaxies are not all young . the distribution of half mass formation times for galaxies with stellar masses less than @xmath5 is broad , spanning the range 1 - 10 gyr . the peak - to - trough variation in star formation rate among the bursting population ranges lies in the range 10 - 25 . in low mass galaxies , the average duration of the burst bursts is comparable to the dynamical time of the galaxy . galaxy structure is correlated with estimated burst mass fraction , but in different ways in low and high mass galaxies . high mass galaxies with large burst mass fractions are more centrally concentrated , indicating that bulge formation is at work . in low mass galaxies , stellar surface densities @xmath6 decrease as a function of @xmath7 . these results are in good agreement with the observational predictions of teyssier et al ( 2013 ) and lend further credence to the idea that the cuspy halo problem can be solved by energy input from multiple starbursts over the lifetime of the galaxy . we note that there is no compelling evidence for imf variations in the population of star - forming galaxies in the local universe . galaxies : star formation , galaxies : starburst , galaxies : structure , dark matter

1111.6538

i

anisotropic flow @xcite is one of the most important probes of ultrarelativistic nucleus - nucleus collisions . while early studies @xcite focused on elliptic flow generated by the almond shape of the interaction region in non - central collisions , most of the recent activity concerns the effect of fluctuations in the initial geometry @xcite . such fluctuations result in fluctuations of elliptic flow @xcite , and also in new types of flow , such as triangular flow @xcite and higher harmonics . these new flow observables have been recently measured at rhic @xcite and lhc @xcite . flow phenomena are best modeled with ideal @xcite or viscous @xcite hydrodynamics . event - by - event hydrodynamics @xcite provides a natural way of studying flow fluctuations : one typically supplies a set of initial conditions , then evolves these initial conditions through ideal @xcite or viscous @xcite hydrodynamics , then computes particle emission at the end . observables are finally averaged over a large number of initial conditions , much in the same way as they are averaged over events in an actual experiment . the largest source of uncertainty in these hydrodynamic models is the initial conditions @xcite that is , the state of the system after which it has sufficiently thermalized or isotropized for the hydrodynamic description to be valid . several models of initial geometry fluctuations have been proposed @xcite . the usual procedure is to choose one or two of these simple models for the initial conditions and calculate the resulting flow observables . significant progress has been made recently by simultaneously comparing to several of the newly - measured flow observables . with this approach , hydrodynamic calculations can be used to rule out a particular model of initial conditions if results do not match experimental data @xcite . but it does not tell us _ why _ a particular model fails . in order to constrain the initial state directly from data , we need to identify which properties of the initial state determine a given observable . these constraints can then provide valuable guidance in the construction of better , more sophisticated models of the early - time dynamics . it is well known that elliptic flow is largely determined by the participant eccentricity @xcite . teaney and yan @xcite have introduced a cumulant expansion of the initial density profile , in which the participant eccentricity is only the first term in an infinite series , and they have suggested that the hydrodynamic response may be improved by adding higher - order terms , but to our knowledge their suggestion has never been checked quantitatively . other expansions have also been suggested @xcite . as for triangular flow , @xmath10 , symmetry considerations have been used to argue that it should be created by an initial triangularity @xmath11 , but several definitions of @xmath11 are in use @xcite and it has never been investigated which is a better predictor of @xmath10 . finally , it has been shown that higher harmonics @xcite @xmath5 and @xmath6 are in general _ not _ proportional to the corresponding @xmath12 and @xmath13 . a possible better estimator was recently suggested @xcite , but it has not been checked quantitatively . the goal of this paper is to improve our understanding of the hydrodynamic response to initial fluctuations . we carry out event - by - event ideal hydrodynamic calculations with realistic initial conditions and then quantitatively compare the final values of @xmath0 with estimates derived from the initial density profile . we are thus able to systematically determine the best estimators of flow observables @xmath0 , @xmath14 25 from the initial transverse density profile .

we similarly study the importance of additional properties of the initial state . for example , we show that in order to correctly predict @xmath5 and @xmath6 for non - central collisions , one must take into account nonlinear terms proportional to @xmath7 and @xmath8 , respectively .

we investigate how the initial geometry of a heavy - ion collision is transformed into final flow observables by solving event - by - event ideal hydrodynamics with realistic fluctuating initial conditions . we study quantitatively to what extent anisotropic flow ( @xmath0 ) is determined by the initial eccentricity @xmath1 for a set of realistic simulations , and we discuss which definition of @xmath1 gives the best estimator of @xmath0 . we find that the common practice of using an @xmath2 weight in the definition of @xmath1 in general results in a poorer predictor of @xmath0 than when using @xmath3 weight , for @xmath4 . we similarly study the importance of additional properties of the initial state . for example , we show that in order to correctly predict @xmath5 and @xmath6 for non - central collisions , one must take into account nonlinear terms proportional to @xmath7 and @xmath8 , respectively . we find that it makes no difference whether one calculates the eccentricities over a range of rapidity , or in a single slice at @xmath9 , nor is it important whether one uses an energy or entropy density weight . this knowledge will be important for making a more direct link between experimental observables and hydrodynamic initial conditions , the latter being poorly constrained at present .

1111.6538

c

in this work , we have quantitatively tested to what extent anisotropic flow can be predicted from the initial density profile in event - by - event ideal hydrodynamics with realistic initial conditions . we have shown that the participant eccentricity @xmath25 gives a very good prediction of elliptic flow for all centralities . we have also shown that the definition of @xmath11 with @xmath115 weights @xcite gives a better prediction of triangular flow than the previous definition with @xmath2 weights . gubser s moments @xcite give worse results for both @xmath75 and @xmath10 . higher harmonics @xmath5 and @xmath6 can be well predicted from the corresponding eccentricities @xmath12 and @xmath13 ( again defined with @xmath116 and @xmath117 weights rather than with @xmath2 weights ) only for central collisions . for noncentral collisions , a good predictor of @xmath5 must include two terms , proportional to @xmath12 and @xmath7 . likewise , @xmath6 has contributions proportional to @xmath13 and @xmath8 . defining the eccentricities with energy or entropy density , or using the density at a midrapidity slice or over a finite longitudinal range is largely a matter of preference , and does not make a significant difference . these results provide an improved understanding of the hydrodynamic response to the initial state in realistic heavy - ion collisions , and provide a more direct link between experimental data and properties of the initial stage of the collision . this will allow for the construction of more realistic models for the early - time collision dynamics , and thus a significant reduction in the systematic uncertainties of extracted bulk properties of the system . this work is funded by `` agence nationale de la recherche '' under grant anr-08-blan-0093 - 01 , by cofecub under project uc ph 113/08;2007.1.875.43.9 , by fapesp under projects 09/50180 - 0 and 09/16860 - 3 , and by cnpq under project 301141/2010 - 0 . ml is supported by the european research council under the advanced investigator grant erc - ad-267258 . s. a. voloshin , a. m. poskanzer and r. snellings , arxiv:0809.2949 [ nucl - ex ] . j. -y . ollitrault , phys . d * 46 * , 229 ( 1992 ) . m. miller and r. snellings , nucl - ex/0312008 . b. alver _ et al . _ [ phobos collaboration ] , phys . lett . * 98 * , 242302 ( 2007 ) [ arxiv : nucl - ex/0610037 ] . b. alver and g. roland , phys . c * 81 * , 054905 ( 2010 ) [ erratum - ibid . c * 82 * , 039903 ( 2010 ) ] [ arxiv:1003.0194 [ nucl - th ] ] . a. adare _ et al . _ [ phenix collaboration ] , arxiv:1105.3928 [ nucl - ex ] . p. sorensen [ star collaboration ] , j. phys . g * 38 * , 124029 ( 2011 ) [ arxiv:1110.0737 [ nucl - ex ] ] . k. aamodt et al . 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we investigate how the initial geometry of a heavy - ion collision is transformed into final flow observables by solving event - by - event ideal hydrodynamics with realistic fluctuating initial conditions . this knowledge will be important for making a more direct link between experimental observables and hydrodynamic initial conditions , the latter being poorly constrained at present .

we investigate how the initial geometry of a heavy - ion collision is transformed into final flow observables by solving event - by - event ideal hydrodynamics with realistic fluctuating initial conditions . we study quantitatively to what extent anisotropic flow ( @xmath0 ) is determined by the initial eccentricity @xmath1 for a set of realistic simulations , and we discuss which definition of @xmath1 gives the best estimator of @xmath0 . we find that the common practice of using an @xmath2 weight in the definition of @xmath1 in general results in a poorer predictor of @xmath0 than when using @xmath3 weight , for @xmath4 . we similarly study the importance of additional properties of the initial state . for example , we show that in order to correctly predict @xmath5 and @xmath6 for non - central collisions , one must take into account nonlinear terms proportional to @xmath7 and @xmath8 , respectively . we find that it makes no difference whether one calculates the eccentricities over a range of rapidity , or in a single slice at @xmath9 , nor is it important whether one uses an energy or entropy density weight . this knowledge will be important for making a more direct link between experimental observables and hydrodynamic initial conditions , the latter being poorly constrained at present .

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understanding bar - formation and the secular effects that bars have on the stellar component is becoming central to our understanding of galaxy formation and evolution . once a bar forms it can change the scale length of the stellar component via scattering / mixing of stars in the radial direction and they can create an extended stellar distribution @xcite . bars can move a galaxy between morphological classes through the secular formation of pseudo - bulges @xcite and they can drive gas to the central black hole fuelling agn ( shlosman et al . 1989 ) . numerical simulations have shown that bars naturally arise from the secular evolution of discs @xcite . bars can also be triggered by dynamical interactions in the field @xcite . it has been shown that close galaxy companions are associated with bar formation , but primarily for early hubble - types @xcite . in galaxy clusters , gravitational encounters ( harassment ) can drive a morphological transformation from late type disks to dwarf ellipticals ( dsphs ) . in this scenario , encounters create a `` naked '' stellar bar which is subsequently heated , causing the remnants to become more spherical with time @xcite . is environment the key factor in determining why two similar galaxies may or may not have a bar or is the existence of a bar related to the initial conditions of galaxy formation ? the stability ( or instability ) of disks to bar formation may also depend on the baryon fraction , and in particular the mass of stars and gas in the disk . this varies across the hubble sequence and depends strongly on halo mass @xcite . this all suggests that in addition to local density , morphology and halo mass are also important principal parameters to investigate . another key observational result is the fact that the bar fraction is not changing significantly with redshift ( see @xcite , but also @xcite for a different result ) , however , most disk galaxies are not within dense environments so it would be difficult to disentangle the effects of environment , especially at higher redshifts . several studies have shown that there is no evidence for a dependence of bar frequency on galaxy environment @xcite , the same is true even if galaxies of different morphological type are considered independently @xcite . @xcite came to the same conclusion analyzing the clustering properties of barred and unbarred galaxies of similar stellar mass and finding it indistinguishable over all the scales probed ( from @xmath520 kpc to 30 mpc ) . more recently , the coma cluster was studied by @xcite : they find that the bar fraction does not vary significantly even when going from the center to the cluster outskirts . however , the coma cluster is such an extreme environment that most of its apparent spiral galaxy population may be field galaxies in projection . in the light of these observational results and motivation from numerical simulation studies , we aim at measuring the bar fraction ( as number of barred discs over the total number of discs ) as a function of environment and disc morphology , at @xmath0 in two carefully selected samples representative of a low - density environment ( the isolated galaxies from the amiga sample ) and of a moderately dense environment ( galaxies in the virgo cluster ) . to achieve this goal it is important to use homogeneous classifications since , as we have shown in giordano et al . , ( 2010 ) ( paperi hereafter ) , the bar fraction is very stable against sample selection but that some ( possibly spurious ) differences can arise if the comparison is based on samples classified using different methods ( for example visual classification versus automated profile fitting ) . in particular , the way the disc population is identified and isolated plays a crucial role , since , if no detailed morphological information is available , discs can easily be miscounted ( for example applying only color and/or magnitude cuts ) . in order to address this , we use data from the ukidss large area survey @xcite and from sdss dr7 @xcite , with the great advantage of combining optical ` r`gb images with near - infrared ( h - band ) imaging with excellent resolution for local universe studies , that allow us to visually inspect the images to provide detailed morphological classifications . ) , morphologically selected discs ( with hubble type ranging from s0 to sm ) . shaded histograms represent the barred discs.,scaledwidth=45.0% ] the outline of the paper is the following : in section [ sec.data ] we present the data that we are using , their classification and the selection of the samples based on local density estimation . the results about the bar fraction in the different cases are presented in section [ sec.results ] and discussed in section [ sec.discussion ] .

we investigate possible environmental and morphological trends in the @xmath0 bar fraction using two carefully selected samples representative of a low - density environment ( the isolated galaxies from the amiga sample ) and of a dense environment ( galaxies in the virgo cluster ) . galaxies span a stellar mass range from @xmath1 to @xmath2m@xmath3 and are visually classified using both high - resolution nir ( h - band ) imaging and optical ` rgb ` images . we find that the bar fraction in disk galaxies is independent of environment suggesting that bar formation may occur prior to the formation of galaxy clusters . the higher bar fraction in early type spirals may be due to the fact that a significant fraction of their bulges are pseudo - bulges which form via the buckling instability of a bar . i.e. a large part of the hubble sequence is due to secular processes which move disc galaxies from late to early types . there is a hint of a higher bar fraction with higher stellar masses which may be due to the susceptibility to bar instabilities as the baryon fractions increase in halos of larger masses . this supports the notion that @xmath8 form via the transformation of disk galaxies that enter the cluster environment .

we investigate possible environmental and morphological trends in the @xmath0 bar fraction using two carefully selected samples representative of a low - density environment ( the isolated galaxies from the amiga sample ) and of a dense environment ( galaxies in the virgo cluster ) . galaxies span a stellar mass range from @xmath1 to @xmath2m@xmath3 and are visually classified using both high - resolution nir ( h - band ) imaging and optical ` rgb ` images . we find that the bar fraction in disk galaxies is independent of environment suggesting that bar formation may occur prior to the formation of galaxy clusters . the bar fraction in early type spirals ( @xmath4 ) is @xmath550% , which is twice as high as the late type spirals ( @xmath6 ) . the higher bar fraction in early type spirals may be due to the fact that a significant fraction of their bulges are pseudo - bulges which form via the buckling instability of a bar . i.e. a large part of the hubble sequence is due to secular processes which move disc galaxies from late to early types . there is a hint of a higher bar fraction with higher stellar masses which may be due to the susceptibility to bar instabilities as the baryon fractions increase in halos of larger masses . overall , the @xmath7 population has a lower bar fraction than the @xmath4 galaxies and their barred fraction drops significantly with decreasing stellar mass . this supports the notion that @xmath8 form via the transformation of disk galaxies that enter the cluster environment . the gravitational harassment thickens the stellar disks , wiping out spiral patterns and eventually erasing the bar - a process that is more effective at lower galaxy masses .

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we present the first comprehensive study of barred disks as a function of environment that uses nir and ` rgb ` imaging to resolve bars ; the advantage of using near - infrared imaging from ukidss is that bar classifications are less affected by dust and bright star - forming regions . we expand on our study of bars in virgo by building a field sample using the kig catalog of isolated galaxies . our field and virgo disk populations are at @xmath31 , span a range in stellar mass from @xmath510@xmath32 to @xmath510@xmath33 m@xmath3 and hubble type ( @xmath34 ) , encompass a wide range in local densities and are analyzed in exactly the same manner . we find that the barred disk fraction is surprisingly constant at @xmath35% in both the field and virgo samples , i.e. the barred fraction for the disk population as a whole does not depend on environment . we test the robustness of our result by analyzing the na10 optically - selected sample of nearby galaxies in the same manner , and we again find a constant barred fraction across the full range of local galaxy density . the barred fraction is highest for early - type spirals ( @xmath4 ) regardless of environment : these galaxies are nearly twice as likely to be barred as late - type spirals ( @xmath6 ) . if a late type spiral forms a bar , then it may also form a pseudo - bulge via a buckling instability and its morphological class will change . indeed , the consensus is forming that our own galaxy has evolved across the hubble sequence in this fashion @xcite . if this is a common phenomenon , as numerical simulations indicate @xcite , then we naturally expect the bar fraction to be higher in early type spirals , that have a higher baryon fraction . this implies that a significant fraction of the bulges of early type galaxies are pseudo - bulges . the morphology - density relation @xcite can be explained by the notion that the cluster environment is creating s0 s from the infalling disc population . indeed , @xcite find that the bulge to disc ratios of s0 s is similar to that of early type galaxies . one might therefore expect the bar fraction to be the same in s0s and early type spirals , however averaged over the entire population it is significantly lower ( 25% versus 50% respectively ) . we note that the bar fraction in s0 s and early type discs with stellar masses above @xmath36 is similar ( @xmath5 50% ) , but this drops to less than 10% in the least massive s0 s . this supports a harassment scenario for the formation of the s0 population . gravitational encounters between galaxies and with the global cluster potential thicken the disks of massive early type spirals by an amount that is sufficient to suppress spiral patterns ( moore et al 1999 ) . for lower mass disks , the heating is more effective and will eventually erase the signatures of a preexisting bar . numerical simulations also indicate that infalling late type disks will undergo an environmentally driven bar instability , however this phase is short lived with the bar experiencing subsequent heating until it becomes a de / dsph . , g. , heckman , t. m. , white , s. d. m. , charlot , s. , tremonti , c. , brinchmann , j. , bruzual , g. , peng , e. w. , seibert , m. , bernardi , m. , blanton , m. , brinkmann , j. , castander , f. , csbai , i. , fukugita , m. , ivezic , z. , munn , j. a. , nichol , r. c. , padmanabhan , n. , thakar , a. r. , weinberg , d. h. , & york , d. 2003 , , 341 , 33 , a. , warren , s. j. , almaini , o. , edge , a. c. , hambly , n. c. , jameson , r. f. , lucas , p. , casali , m. , adamson , a. , dye , s. , emerson , j. p. , foucaud , s. , hewett , p. , hirst , p. , hodgkin , s. t. , irwin , m. j. , lodieu , n. , mcmahon , r. g. , simpson , c. , smail , i. , mortlock , d. , & folger , m. 2007 , , 379 , 1599 , k. , elmegreen , d. m. , elmegreen , b. g. , capak , p. , abraham , r. g. , athanassoula , e. , ellis , r. s. , mobasher , b. , salvato , m. , schinnerer , e. , scoville , n. z. , spalsbury , l. , strubbe , l. , carollo , m. , rich , m. , & west , a. a. 2008 , , 675 , 1141

the bar fraction in early type spirals ( @xmath4 ) is @xmath550% , which is twice as high as the late type spirals ( @xmath6 ) . the gravitational harassment thickens the stellar disks , wiping out spiral patterns and eventually erasing the bar - a process that is more effective at lower galaxy masses .

we investigate possible environmental and morphological trends in the @xmath0 bar fraction using two carefully selected samples representative of a low - density environment ( the isolated galaxies from the amiga sample ) and of a dense environment ( galaxies in the virgo cluster ) . galaxies span a stellar mass range from @xmath1 to @xmath2m@xmath3 and are visually classified using both high - resolution nir ( h - band ) imaging and optical ` rgb ` images . we find that the bar fraction in disk galaxies is independent of environment suggesting that bar formation may occur prior to the formation of galaxy clusters . the bar fraction in early type spirals ( @xmath4 ) is @xmath550% , which is twice as high as the late type spirals ( @xmath6 ) . the higher bar fraction in early type spirals may be due to the fact that a significant fraction of their bulges are pseudo - bulges which form via the buckling instability of a bar . i.e. a large part of the hubble sequence is due to secular processes which move disc galaxies from late to early types . there is a hint of a higher bar fraction with higher stellar masses which may be due to the susceptibility to bar instabilities as the baryon fractions increase in halos of larger masses . overall , the @xmath7 population has a lower bar fraction than the @xmath4 galaxies and their barred fraction drops significantly with decreasing stellar mass . this supports the notion that @xmath8 form via the transformation of disk galaxies that enter the cluster environment . the gravitational harassment thickens the stellar disks , wiping out spiral patterns and eventually erasing the bar - a process that is more effective at lower galaxy masses .

1406.1642

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stars habitually form in localised over - densities of cold gas , but predicting star formation ( sf ) remains challenging . kennicutt ( 1998 ) proposed that the star formation rate ( sfr ) correlates principally with the total ( i.e. h i@xmath1h@xmath2 ) gas surface mass density , with the gravitational collapse of sufficiently dense clouds in a turbulent ism being the dominant sf mechanism ( mac - low & glover 2012 ; renaud et al . alternatively , revisions of the sf law in favour of a metallicity- and h@xmath2-dependence have been advocated ( gao & solomon 2004 ; bigiel et al . 2008 ; gnedin & kravtsov 2011 ; kuhlen et al . 2012 ) . the apparent correlation of h@xmath2 and @xmath3 with mid - plane pressure in massive spirals ( wong & blitz 2002 ) implies that sf reflects the equilibrium between h@xmath2-formation by dust grain catalysis and dissociation by the fuv ( far ultra - violet ) background ( blitz & rosolowsky 2004 ) . the significance of this mechanism , relative to turbulence - regulated cloud - collapse , is disputed , particularly in light of some resolved sf regions exhibiting very low h@xmath2 content ( i.e. boissier et al . 2008 ) . these competing hypotheses both accommodate the inefficient sf found among metal - poor dwarves . on the one hand , a lack of or inefficiency of coolants in the ism can restrict supersonic turbulence to higher density thresholds , thus mitigating the shocks that lead to sf ( renaud et al . 2012 ) . on the other hand , weak h@xmath2 growth and protection from fuv in a metal - poor environment can push the h i@xmath4h@xmath2 transition to higher surface densities ( kuhlen et al . 2012 ) . interstellar dust plays a seminal role in the latter mechanism , being responsible for shielding and h@xmath2 formation ( cazaux & tielens 2002 ) . the properties of dust vary with environment ( cardelli et al . 1996 ) , manifesting in a dependence on the local metallicity and quotient of asymptotic giant branch ( agb ) stars and supernovae ( sne ) type 1a / ii ( matsuura et al . 2009 ; boyer et al . 2011 ) . sne ii ejecta are believed to synthesise significant dust mass ( lisenfeld & ferrara 1998 ; dwek 1998 ) , and are the favoured culprits for high observed extinction in the early ( @xmath5 ) universe ( dunne et al . 2003 ) , although the efficiency with which ejected metals condense remains subject to debate given the simultaneous grain destruction in the reverse shock . recent analytical models suggest sne ii are inefficient overall sources in dwarves , coupled with weak grain growth in the metal - poor ism , leading to the high gas - to - dust ratios in these systems ( zhukovska 2014 ) . understanding the relative rates at which dust mass growth is contributed to by stellar sources and the ism , as a function of metallicity , is key to elucidating conflicting observations of a _ universal _ dust - to - metal ratio ( i.e. zafar & wilson 2013 ; de cia et al . 2013 ; mattsson et al . 2014 ) . in this work , we examine the coupled h@xmath2 and dust lifecycles of the magellanic clouds over their recent ( @xmath0 ) past . as uniquely gas - rich and blue galaxies within our local group , these neighbouring galaxies are a convenient probe of star formation more common at higher redshifts ( tollerud et al . the low differential rotation in the mcs also permits the direct association between star formation and local conditions such as supergiant shells ( leroy et al . their proximity allows high resolution imaging of giant molecular clouds ( gmcs ; fukui et al . 2008 ) , where almost 300 individual gmcs have been resolved from the nanten @xmath6co(1 - 0 ) survey of the lmc ( fukui & kawamura 2010 ) . [ cols="^,^,^ " , ] to first - order , the global dust - to - gas ratios across our simulated lmc and smc follow a linear correlation with their respective mean metal abundances ( figure 23 ) , qualitatively matching previous numerical work ( b13 ) and an observed correlation in observational samples ( i.e. dwek 1998 ; zafar & wilson 2013 ) . this dust - to - metal ratio ( r@xmath7 ) is maintained by the model self - consistently ( i.e. not explicitly set as a constraint , except as an initial value ) as shown in the d - a@xmath8 phase space ( figure 24 ) this contrasts with present observational estimates of d in the smc , which are a factor of 5 to 14 less than the galactic ratio ( sofia et al . 2006 ; leroy et al . 2007 ; gordon et al . 2009 ) , and thus imply a deficit in dust when compared to the factor 4 to 5 expected from differences in mean metallicity . our calculation of r@xmath7 from simulations are free of line - of - sight uncertainties and selection bias towards warm dust . the line - of - sight morphology of the smc is complex where , besides tidal effects ( nidever et al . 2011 ; diaz & bekki 2012 ) , feedback within the ostensibly weak potential of the smc influences vertical structure and therefore measures of attenuation . this also makes a representative co - h@xmath2 conversion factor for the smc difficult to ascertain ( leroy et al . the presently low observed d could also be explained by an underestimation of the contribution from cold dust lying towards the limits of equilibrium ; leroy et al . ( 2007 ) derive an upper constraint on the dust mass at @xmath92 times the 10@xmath10 m@xmath11 mass commonly attributed to the smc . galametz et al . ( 2011 ) show that sub - millimetre data can be combined with sed analysis in low - metallicity dwarves to recover the universal r@xmath7 . in practice , dwarf galaxies exhibit wide dispersion in r@xmath7 , which various studies attribute to the variability in dust sources with metallicity , stellar outflows , sfh and destruction efficiencies ( lisenfeld & ferrara 1998 ; mattsson et al . furthermore , tidal perturbations disrupt the potential and drive gas dynamics , upon which the ism composition depends . mergers can reduce r@xmath7 following the triggered consumption of metal - rich gas ( hayward et al . 2011 ) , and tidal stripping appears to preferentially remove the metal - enriched h i over dust ( pappalardo et al . this manifests in our simulated stream and leading arms , which show negligible dust content ( figure 23 ) . however , observational estimates for d in the stream filaments ( coincident with sightlines fairall 9 and rbs 144 ; fox et al . 2013 ) far exceed that in our reference model by orders of magnitude ( figure 8) . in the following sections , we attempt to reconcile our results with the broader discussion of interstellar dust evolution . the contributions of different stellar sources to the metals and dust in the ism are not well understood for the mw / mcs ( gehrz 1989 ; boyer et al . agbs convey a variability cycle in mass loss ( srinivasan et al . 2009 ) and large scatter with metallicity ( boyer et al . 2012 ) , while the dust mass in sn remnants ranges from conservative lower limits of 0.01 m@xmath11 to an estimated @xmath90.5 m@xmath11 in sn 1987a in the lmc ( matsuura et al . the latter uncertainty largely prohibits a constraint on dust grain growth in the ism ( draine 2009 ; boyer et al . the relative delay in dust output from different stellar sources ( dwek 1998 ) is also a major complication in the mcs , which are presently experiencing starbursts and whose current dust output is compounded by the delayed products from prior starbursts in their very recent evolution ( harris & zaritksy 2009 ) . the evolution in dust sources can manifest in the c / o ratio ( dwek 1998 ; zhukovska & henning 2013 ) . given our adoption of simple ejecta yields ( dwek 1998 , instead of that from more recent work i.e. ferrarotti & gail 2006 ) , and the tracking of elemental abundances for only the 3.4 gyr of our simulations , we can not fully compare our results with more detailed analytical studies ( i.e. zhukovska & henning 2013 ) . nonetheless , we find the c / o ratio drops at commencement of the simulations , consistent with tidally - triggered starbursts that invoke large silicate production in short - lived massive stars . comparing the final c / o ratios of our mc models with the analytical galaxy model of dwek ( 1998 ) , we find consistency with an anticorrelation of oxygen abundance with metallicity among dirrs ( garnett et al . two observations of the mcs are further consistent with this result . first , the 2175 feature is weak in the lmc and absent in the smc ( gordon et al . 2003 ) with the implication that small carbonaceous grains are destroyed more efficiently in the harsher fuv background of the smc . secondly , matsuura et al . ( 2013 ) find substantial sne gas feedback in the mcs but more significantly so in the smc ( even when accounting for uncertainty in mass loss rates and the assumed agb gas - to - dust ratio ) , in accordance with relatively more enhanced sfr or weaker stellar winds in the more metal - poor environment . the dominant dust sources can be also revealed by constraining the variation of dust mass with metal abundance , since the yields of stellar winds and accretion efficiency are expected to vary with metallicity . for instance , zafar & wilson ( 2013 ) interpret a constant r@xmath7 ( similar to the galactic value adopted by dwek 1998 ) among a recent sample of grb / qsos across redshifts 0.1 to 0.63 , as evidence for rapid dust production . their metallicity range encompasses that of the mcs , appearing to support our adopted dust model parametrisations . a spatial correlation of extinction and stellar density ( grootes et al . 2013 ) , and the slow synthesis of dust by agbs , suggests sne are responsible for this production rate , as further demonstrated by our self - consistent work , analytical models ( lisenfeld & ferrara 1998 ; dwek 1998 ) , and other studies attempting to explain high redshift dust masses ( dunne et al . 2003 ) . on the other hand , de cia et al . ( 2013 ) find strong metallicity dependence of r@xmath7 among another sample of quasar foreground dlas . mattsson et al . ( 2014 ) try to reconcile these studies by proposing that while stellar yields vary with metallicity , rates of dust accretion and destruction by sne will tend towards an equilibrium that manifests in an apparent constant r@xmath7 . our models provide some support to the concept of an equilibrium state . figure 24 compares the evolutionary tracks , within the d - a@xmath8 phase space , of our reference lmc model l1 with additional models covering a small subset of the ism model parameter space . model l1 , with an initial r@xmath7 set at the galactic value ( @xmath90.4 , dwek 1998 ) , is self - consistently bound to this r@xmath7 throughout its evolution , similar to analytical models ( i.e. edmunds 2001 ) . the bottom panel highlights the substantial sensitivity of our simulations to characteristic timescales of ism processing , which we conveyed earlier in the amr ( figure 20 ) . our model is however robust to variations in the initial r@xmath7 ( figure 24 , top panel ) where , over the 3.4 gyr duration of the simulation , an initially dust poor model converges upon our reference model in which we had assumed almost complete condensation of gas - phase metals . our results thus far are consistent with efficient dust production by sne . however , a recent analytical model by zhukovska ( 2014 ) tracks the evolution of low metallicity galaxies in the d - a@xmath8 plane , from which she argues that the sne ii condensation efficiency is a governing parameter . hirashita ( 1999 ) similarly showed that larger efficiencies correspond almost linearly to higher d. for brevity , we adopted in this study the efficiencies derived by dwek ( 1998 ) , which are typically a order larger than those advocated in the cited one - zone studies ( i.e. 0.01 to 0.1 ) . it is presently unclear , for the purposes of self - consistent models , an appropriate choice of this parameter ; the dust yield from sne may be invariant over a metallicity range , but the condensation efficiency into its surroundings may depend indirectly on metallicity via cooling rates / shielding ( mattsson et al . moreover , elemental depletion observed in the vicinty of sn ejecta could indicate an additional cold dust component unaccounted for in the low efficiencies commonly derived ( morgan & edmunds 2003 ; and references therein ) . in the specific case of the mcs , however , dust output rates of sne / agbs are insufficient , by up to magnitude , to account for the global dust mass ( boyer et al . 2012 ; zhukovska & henning 2013 ) . this is supported by the spatial correlation of the dust surface density with atomic and molecular hydrogen ( roman - duval et al . 2010 ; sandstrom et al . 2010 ) indicating therefore the dominant role of dust growth in the ism . by contrast , we find @xmath12 is a weak parameter for our lmc models ( section 3.3.3 ) . we leave the task of reproducing the observed relative roles of dust growth by stellar sources and accretion to a subsequent paper . we generally find that the final dust mass is set by the sensitive balance of : the initial metallicity profile ( [ m / h]@xmath13 , @xmath14 ) , the initial dust - to - metal ratio ( r@xmath7 ) , reference dust accretion timescale ( @xmath15 ) , the adiabatic timescale of sn ( @xmath16 ) , the stellar dust yield and condensation efficiencies , and the tidal environment which triggers star formation and shapes the distribution of dust / h@xmath2 . to date , these factors are not well constrained for the metal - poor mcs , and thus we do not attempt further fine - tuning of our model parameters against observational constraints ( i.e. table 1 ) . @xmath172 ) , shorter dust accretion timescale ( @xmath15@xmath170.5 ) and a 1:1 ratio in destruction and accretion timescales ( @xmath18@xmath170.5 ) . the symbol colour tone varies from light ( 3.4 gyr ago ) to dark ( 0 gyr ago ) , highlighting how reference model l1 evolves with a near constant r@xmath7 , whereas deviations to the ism timescales can yield very different behaviour ; ( top ) a comparison of l1 and a model with initial r@xmath7 of 0.1 . note that both models converge after commencing from different locations in the d - a@xmath8 phase space . ] dwek ( 1998 ) derives the galactic accretion and destruction timescales independently ; the former depends on the time to accrete a typical layer thickness on dust grains and the mass fraction of molecular clouds ; the latter follows from modelling of radiative shocks . these factors were assumed constant over a hubble time evolution , despite a wide dynamical range in local conditions , leading to the canonical @xmath18@xmath192@xmath12 relation adopted in this work . this is a justifiable simplifying assumption , but the recent evolution of the mcs is clearly not steady . more recent studies have since argued for a decoupling of the timescales , where @xmath18 should directly reflect the local sn rate ( i.e. inoue 2003 ; zhukovska & henning 2013 ) . our simulations are the first to provide per - particle allocation of @xmath12 ( and @xmath18 ) , established per timestep from the local @xmath20 and thermal speed ( equation 7 ) . while not decoupled , our cursory parameter studies indicate the galaxy - wide amr depends more sensitively on the parametrized @xmath18 than @xmath12 ( section 3.3.3 ) , supporting our earlier assertion that sne are significant dust sources in our model . this conflicts with studies indicating the dominance of dust accretion over its production to accomodate the current budget in the mcs ( see section 4.1.1 ) . it is nonetheless instructive to compare destruction efficiencies in our lmc and smc models . observational studies have adopted the sn rate per unit surface area to establish the mean dust lifetime , implicitly assuming a constant sfr over the corresponding timescales . for the lmc , a range of 0.4 to 1.1 gyr , depending on grain type and subject to the error bounds of the sfr is obtained ( zhukovska & henning 2013 ) . by a similar method , matsuura et al . ( 2013 ) estimates lifetimes of @xmath90.4@xmath1710@xmath21 yr and @xmath91.4@xmath1710@xmath21 yr for the lmc and smc respectively . these data suggest dust destruction is less efficient in the smc by an approximate factor of 3 . our dust model does not explicitly account for microscopic - scale grain sputtering in the diffuse warm gas behind the sn remnant , since simulations can not at present distinguish this region due to resolution limitations . instead , dust destruction in our models , as parametrised by @xmath18 , is assumed to be most efficient in proximity to the thermal radiation ejected from sne emerging from dense clouds ( where equation 7 is imposed only on those gas particles lying within the smoothing length of a given sn ) . our parametrized @xmath18 is thus a proxy for a local sn rate dependence , with which we evaluate the global destruction timescale in our reference lmc and smc models , to compare with these observational estimates . we consider only gas particles lying in the line - of - sight region of the sky for which the integrated sfh histories ( a proxy for the sn rate , if combined with the imf ) of the mcs were established by harris & zaritsky ( 2004 ; 2009 ) . the main panel of figure 25 shows the pdf of @xmath18 for individual gas particle lifetimes ( at zero lookback time ) , ascertained with equation 7 and @xmath18@xmath192@xmath12 . the pdf peaks correspond to short @xmath18 on the order of the reference galactic value ( 5@xmath1710@xmath22 yr ; section 2.2.4 ) in regions of relatively large @xmath20/t ( i.e. the inner disc ) . the wider spread of the smc model s1 ( i.e. where @xmath18@xmath231 gyr ) , is largely attributable to diffuse gas particles in the line - of - sight stripped from the disc plane by tidal forces from the lmc / mw . this interpretation is further supported by the time - varying ratio of @xmath18 for the smc / lmc ( inset panel of fig . 26 ) , which shows peaks coinciding with pericentres in its complex orbits of the lmc and mw . nonetheless , our models are implied to have appropriately reproduced the ism density distribution given the underlying ratio of @xmath18 in the smc / lmc at present time ( @xmath93 ) is consistent with the aforementioned estimates . it is not clear from observation whether the magellanic stream and leading arms harbour significant extant dust mass ( i.e. fong et al . 1987 ; brns et al . 2005 ) , in spite of clear depletion patterns similar to the galaxy ( fox et al . the extraneous h i streams of our simulated mcs do not follow the universal dust - to - metal relation to which their parent discs are bound ( figure 23 ) , although we note that the tenuous tails test the limits of our galaxy - derived dust model . the lack of direct detection for stardust sources in the stream presently negates _ in situ _ formation , while accretion is limited by the available refractory elements . reprocessing of mantle into further core material provides a speculative remedy for dust growth in the stream . dwek ( 1998 ) invokes this process to explain the failure for the observationally - inferred destruction timescale by snr in the galaxy ( jones et al . 1996 ) to account for core depletion of iron . accretion may be further limited by the systematic absence of h@xmath2 in the observed and simulated stream ( figure 6 ) . zwaan & prochaska ( 2006 ) show for local galaxies a transition from h i to h@xmath2 at a column density of 10@xmath24 @xmath25 , which surpasses the peak observed densities of the magellanic stream ( putman et al . 2003 ; brns et al . our high - resolution simulations are presently insufficient for probing this transition in highly localised molecular clumps within the diffuse stream . this h@xmath2 dependence may be irrelevant ; lisenfeld & ferrara ( 1998 ) find in a sample of dwarf galaxies , strong depletion in spite of the lack of dense molecular clouds in which accretion would occur . moreover , at up to @xmath91.7 gyr old , the tails are not young ; extant dust could be long - lived with the relative lack of ionizing stars in the stream , but we do not incorporate ionization from hot halo interactions that can permeate the densest self - shielding regions of the stream . at relatively low mass , with strong sn activity as evidenced by a porous ism ( i.e. kim et al . 1998 ) , the mcs are susceptible to the outflow of heavy elements , a mechanism which has been proposed to explain dispersions in r@xmath7 for dwarf galaxies ( lisenfeld & ferrara 1998 ) . the existence of high velocity clouds on the periphery of , and traced to , the lmc ( staveley - smith et al . 2003 ) has also motivated previous studies to suggest the stream is a product of outflow ( olano 2004 ; nidever et al . this is partly in response to the paucity of stars in the stream , although our simulations suggest that the tidal h i will not necessarilty have a stellar counterpart . a further refutation arises from abundance measures of the metal - rich stream component ( fairall 9 ) . ejecta from sne type ii would show a deficiency in c , n and fe relative to o ( garnett 2002 ) , but this is not exhibited in the depletion analysis ( figure 8 of fox et al . 2013 ) . on the other hand , the mixing of dust and exchange with the gas - phase means that the observed depletion may be more a measure of grain survival than the progenitor stellar sources ( dwek 1998 ) . we posit two interpretations for the depletion level and apparent absence of dust in the stream , in the context of tidal / ram pressure stripping from the smc disc . first , the depletion level of the stream reflects that of the mcs ( prior to stripping 2 gyr ago ) which , in our simulations , depends sensitively on sf parameters , feedback , and dust lifetimes ( section 3.1.5 ) . moreover , dust typically traces metallicity ; an appropriate choice for the initial metallicity gradient is as yet ill - defined within observed ranges ( zaritsky et al . 1994 ) ; both mcs show flattened profiles at present time , but are likely to exhibited steeper gradients previously ( rubele et al . 2012 ) , before recent enivronmental influences in the local group and bar - driven gas inflow became significant . secondly , recent observations and simulations suggest that a group / cluster environment is more efficient at removing h i than h@xmath2/dust ( pappalardo et al . b13 interprets these results in terms of dust being locked within cool stabilised h@xmath2 regions , as opposed to its relatively loose h i envelope . a corollary of this preferential stripping is a positive radial gradient in the dust - to - gas ratio , which to date has not been reproduced numerically ( b13 ; this work ) . other evidence suggests however no such preference . stripped dust is evident in the smc tail ( gordon et al . 2009 ) ; the corresponding d in these regions is less than expected from metallicity , but the authors propose this as a consequence of local destruction . roussel et al . ( 2010 ) find stripped dust from m82 following a tidal interaction , which they distinguish from that swept out by superwinds , which is warmer and more diffuse . walter et al . ( 2007 ) also find substantial dust mass in the tidal arm of ngc 3077 ; this feature was pre - enriched before its stripping @xmath93@xmath1710@xmath26 yrs ago , given that the sfr within the arm is insufficient to form the dust . a more detailed study of the stripping efficiency of various subcomponents of the ism will comprise a future paper . , as calculated from equation 7 ) . the dotted line signifies the reference @xmath27 ( ) from the galaxy ; ( inset ) the ratio of mass - averaged @xmath18 ( ) in the s1 and l1 , as a function of lookback time . ] up to 20 per cent of the ir discharge of dust contaminated objects show emission lines corresponding to pahs ( smith et al . 2007 ) , but their origin is not well defined ( paradis et al . a recent census of pah - producing carbon stars in the lmc suggests that stellar sources provide a magnitude less than the total pah mass over their assumed lifetime ( matsuura et al . the implication is that the ism reprocesses grains , supported by the anti - correlation of pahs with carbon - rich stars in the lmcs ( sandstrom et al . 2010 ) and its preferential residence in dense molecular gas ( wiebe et al . 2011 ) . the production of pahs from the shattering of larger grains in shocks ( jones et al . 1996 ) is also proposed from the spatial anti - correlation of pahs and very small grains ( vsgs ) at the surfaces of molecular clouds ( paradis et al . 2009 ) . in this scenario , pahs are longer lived than larger grain species , perhaps explicating their spatial discordance with the original progenitor carbon stars . in the first self - consistent models of pahs , b13 delegated 5 per cent of the total carbonaceous dust in the ejecta of c - rich agb stars to new pahs , similar to the abundance fraction in the milky way ( 0.046 , li & draine 2001 ) . for the lmc , this model is reasonable given the majority of carbon - rich stars lie in the vicinity of the stellar bar ( matsuura et al . 2009 ) , coincident with a pah mass enhancement ( paradis et al . 2009 ; meixner et al . b13 postulates that this enhancement stems from tidal interactions triggering centralised starbursts ; the environment of the lmc could also explain its greater pah abundance over galaxies of comparable metallicity ( paradis et al . 2009 ) . in vindication of this model , b13 finds the pah - to - dust mass fraction varies with metallicity in accord with observations ( draine et al . 2007 ; muoz - mateos et al . 2009 ) . in a cursory diagnosis of our reference mc models , we find the pah - to - dust mass ratio overlaps with the observed @xmath91 - 2 per cent in star forming regions , to 0.6 per cent in diffuse ism and h@xmath28 regions ( sandstrom et al . 2011 ) . we note however that our models show positive pah abundance gradients , in conflict with observed samples of sdm and irr galaxies ( muoz - mateos et al . 2009 ) which show a preference for zero to negative gradients . this partly stems from the non - inclusion of old c - rich agbs ( age greater than our simulation duration of 3.4 gyr ) that would have settled towards the galaxy centre . nonetheless , pah destruction is likely the driving factor behind the apparent metallicity dependence ( bolatto et al . 2007 ) . observed spatial variations in pah emission strength , in particular those around 30 doradus , suggest that pahs tend to avoid bright h@xmath28 regions and are found instead near atomic and molecular gas ( wiebe et al . we thus advocate future models of the mcs to model the various evolutionary paths of pahs to further shed light on dust lifecycles in the mc ism . the global h@xmath2 mass fraction of our simulated lmc is consistent with observational estimates ( @xmath910 per cent ; israel 1997 ; fukui et al . 1999 ) , is comparable to wider samples of such galaxies ( young & scoville 1991 ) , and accordingly less than the galaxy . the simulated smc , under similar evolutionary parameters , produces an h@xmath2 abundance of up to 15 percent . this lies in excess of observational estimates ( again , @xmath910 percent ) , including those that account for a co - dark h@xmath2 component for @xmath29 ( leroy et al . 2007 ; wolfire et al . 2010 ; leroy et al . 2011 ) , in spite of a broad agreement between observations for the h i mass / metallicites of the mcs and our models . since h@xmath2 formation is sensitively bound to the dust abundance , this excess can be traced to oversimplifications in our adopted dust production model ( section 4.1.1 ) . furthermore , the flux density from irradiating massive stars is fixed to seds derived from the salpeter imf ( section 2.2.7 ) , ignoring the possibility for a top - heavy imf for lower metallicity galaxies ( maio et al . refinements in this direction would permit comparison with the varying hardness of the uv field ( cox et al . 2006 ) , especially that between individual clouds ( paradis et al . 2011 ) . greater regulation by photo - ionisation would manifest in an increasing average cloud column density with decreasing metallicity to attain equilibrium ( mckee 1989 ) . the ambient uv radiation is recognised as generally harsher than the mw , and clouds are accordingly hotter and smaller in the smc ( lequeux et al . 1994 ; leroy et al . 2007 ) . recent studies have suggested the metallicity - dependent balance between formation and dissociation is not as critical as ism turbulence ( walch et al . 2011 ; renaud et al . 2012 ) and local density enhancements ( mac low & glover 2012 ) . for example , gmcs and yso in the lmc are often enhanced and organized in the vicinity of supergiant shells and their colliding fronts ( dawson et al . the turbulent ism is also driven by successive tidal interactions that render the ism very porous ; several hundred supershells in the smc ( staveley - smith et al . 1997 ) conform to a turbulence spectrum driven by the recent close encounter ( goldman 2000 ) . detailed simulations of the mcs ( bekki & chiba 2007 ; besla et al . 2012 ; this work ) can not yet accurately reproduce the present distribution of star formation or h@xmath2 ; a clear example in our models is the concentration of h@xmath2 in the stellar bars , in a manner similar to massive barred spirals , but unlike the scattered fir / co emission in both mcs ( i.e. wong et al . moreover , numerical limtations restrict our capacity to address the possible preferential stripping of h@xmath2 over h i ( pappalardo et al . 2012 ) ; the stronger tidal actions acting on the lower mass smc may explain why its h@xmath2 gas mass fraction is broadly similar to that of the lmc in spite of a factor @xmath92.5 lower mean metallicity . on the other hand , figure 19 shows an analogue to the h i overdensity ( nidever et al . 2008 ) or molecular ridge , which at 100 - 200 pc wide and 1.8 kpc long ( ott et al . 2008 ) is argued to be a coherent structure , but kinematics and the discrepancy from the h i envelope would suggest otherwise . extending from one bar end , without a clear counterpart at the other , the structure forms in our simulations from strong recent lopsidedness ( section 3.3.2 ) of the bar resulting in the asymmetric collision of gas flows . the hydrodynamical collision of the lmc and smc or hot halo have also been proposed for its formation ( fujimoto & noguchi 1990 ; kim et al . 1998 ) , but which are not modelled here . significant molecular mass is also traced in the simulated bridge ( section 3.4 ) ; the stream , at comparable metallicity , is conversely devoid of h@xmath2 ( figure 6 ) . young stars with ages 10 to 40 myr are located throughout the bridge ( demers & battinelli 1998 ) , including young b - type stars with a low ( 0.1 z@xmath11 ) metallicity similar to the gas phase ( [ fe / h]@xmath19 - 1.7 to -0.9 ; lehner et al . the low metals abundance clearly does not preclude h@xmath2 formation and subsequent star formation in this h i - rich environment . in a similar bridge structure between massive spirals , gao et al . ( 2004 ) find the highest concentration of h@xmath30 near the _ intruder _ galaxy ( which in our simulations is the smc ) , due to the collisional nature of the gas - rich interaction . we propose that the observed amr is a complex function of the role played by dust evolution in quiescent and starburst epochs ; the modest but sustained enrichment of the mcs since 3.4 gyr ago ( weisz et al . 2013 ) disguises an underlying balance of competing growth and destructive processes in a tidally - driven ism , given the coupling of dust mass/ metallicity . in the following sections , we suggest refinements to our models and model analysis that would further elucidate the evolution of the mcs . the tidally - driven mcs would show evidence in their amr of not only the nominally secular balance of dust accretion and destruction , but also the infall and outflow of ism . tidal torques retard gas in the disc such that it encourages infall and fuels nuclear starburst and centrally concentrated growth , with the central starburst determined by the infall rate ( jog & das 1992 ) . in one - zone models , dispersions in the infall rate have been shown to perturb the derived r@xmath7 ( inoue 2003 ) , while the metallicity drops if the rate of gas accretion exceeds the sfr ( koppen & edmunds 1999 ) . the recent interaction history of the mcs provides multiple means of gas infall onto the galaxies with the implication of dilution , but most studies associate recent close encounters with rapid enrichment ( harris & zaritsky 2009 ; livanou et al . 2013 ) . this mirrors a broader debate on the role of interactions on metallicity : marquez et al . ( 2002 ) find in a large sample of isolated and interacting spirals that the gas - phase metallicity does not appear to correlate with the interaction state , while conversely kewley et al . ( 2006 ) find smaller galaxy separations correlated with lower metallicity . evidence for major infall events in the mcs lie first with the assertion by bekki & tsumjimoto ( 2012 ) that an apparent dip in the amr ( harris & zaritsky 2009 ) corresponds to stripped metal - poor gas from a less massive smc , consistent with a subpopulation of anomalous stars in the lmc which olsen et al . ( 2011 ) propose originate from the smc . the mass transfer invoked by bekki & tsujimoto ( 2012 ) to drive this dip exceeds that simulated in this work . alternatively , the timescale of this dip agrees with simulations of fly - by interactions ( montuori et al . 2010 ) , wherein inflows occur over a dynamical time ( @xmath910@xmath26 yr ) and the dilution of circumnuclear metallicities persist up to 10@xmath21 yrs ; the extent of the dip is also quantitatively similar to the 0.1 to 0.3 dex dilution established by rupke et al . ( 2010 ) . for the more recent close interaction ( @xmath90.2 gyr ago ) , bekki & chiba ( 2007 ) show that 10@xmath26 m@xmath11 of gas can be stripped from the smc and collide with the lmc . the relative velocity of gas transferred in this scenario ( @xmath960 kms@xmath31 ) is less than that of hvcs ( @xmath9160 kms@xmath31 ) and the circular velocity of the lmc disc ( @xmath980 - 120 kms@xmath31 ) , and would better explain the young ( @xmath910 myr ) subpopulation of nitrogen deficient stars than the timescales of accreting hvcs . gas accretion from the igm is another efficient driver of secular evolution ( dekel et al . the stellar bar of the lmc is barely traced by the ism ( mizuno et al . 2001 ) , suggesting it imparts a weak gravitational influence . the lifetime of bars with a dissipative medium is not well constrained , but weakening can occur gradually by cold gas accretion ( berentzen et al . 2004 ) . concurrently , accretion can enhance asymmetry in strength and longevity ( bournard et al . 2005 ) . the inner lmc and bar show strong lopsidedness ( van der marel et al . 2002 ) , the persistence of which is implied by carbon - rich stars which preferentially lie at one bar end for at least a gyr ( cioni , habing & israel 2000 ; matsuura et al . bekki & tsujimoto ( 2010 ) hypothesise that accreted hvcs are responsible for the low nitrogen content of h@xmath28 regions ( a factor of 7 lower than solar ) , which mix within a rotation time ( 10@xmath26 yr ) , and have minimal impact on other elemental abundances . the implications of a gas supply external to the mcs has yet to be modelled self - consistently and is advocated for future studies . the metallicity and kinematics of hvcs on the periphery of the lmc imply their origin from the gas disc , following superwind driven outflow ( staveley - smith et al . 2003 ) , which can also explain the various components of h i in the line - of - sight of the mcs . the metal - rich filament lying ahead of fairall 9 ( richter et al . 2013 ) also advocates the lmc as an origin to the stream ( olano 2004 ; nidever et al . 2010 ) , although the elemental abundance may negate this argument ( section 4.1.4 ) . alternatively , the stronger outflow from the lower mass smc could strip metal - rich ism from lmc to form this filament , a mechanism explored for generic low and intermediate mass galaxies by scannapieco & broadhurst ( 2001 ) . these arguments are consistent with the prominent role of sne in gas - rich , low mass galaxies with inefficient star formation akin to the smc ( dalcanton 2007 ) . lisenfeld & ferrara ( 1998 ) attribute the wide dispersion in r@xmath7 to outflow , where metals mixed in hot gas preferentially escape , while the cool ism is largely retained ( maclow & ferrara 1999 ) . the mass range susceptible to metal - enriched outflow ( @xmath3210@xmath33 m@xmath11 ; garnett 2002 ) includes our models for the smc and low mass lmc . strong feedback is also invoked to sustain the late - type spiral structure of the lmc , by mitigating the quenching , gas depletion and build - up of a nuclear bulge that follows strong starburst phases ( governato et al . this process shares a complex relationship with accretion mechanisms discussed in section 4.3.2 , where feedback drives out gas and mitigates subsequent infall through the dynamical heating of the halo ( dubois & teyssier 2008 ) . the multiple recent starbursts of the mcs can also mitigate outflow , where dynamical heating by previous feedback activity can oppose the motion of more recent superbubbles . the relationship between infall and outflow thus represents an important question for future simulations of magellanic - type galaxies , where presently adopted models are too primitive for this purpose . future work could follow from previous one - zone model considerations of [ @xmath30/fe ] as a means of constraining starburst epochs and gas outflow ( bekki & tsujimoto 2012 ) , who find variations from a salpeter imf , or outflows with preferential [ @xmath30/fe ] can explain elemental abundances .

we investigate the evolution of the interstellar medium ( ism ) in self - consistent , chemodynamical simulations of the magellanic clouds ( mcs ) during their recent ( @xmath0 ) past . we reproduce the age - metallicity relations , long gas depletion timescales , and presently observed dust and molecular hydrogen masses of the mcs to within their respective uncertainties . we find that these models enrichment depends sensitively on the processing of dust within the ism and the dynamical influence of external tides / stellar bars . our reference mc models tend to exhibit the disputed universal dust - to - metal ratio , which we argue stems from the adoption of high sne ii condensation efficiencies . our models are the first to reproduce the one - tenth solar metallicity of the stream / leading arm following tidal stripping of the smc ; the hypothesis that the lmc contributes a metal - rich filament to the stream , as implied by recent kinematic and abundance analyses , is also appraised in this study . [ firstpage ] galaxies : interactions galaxies : evolution galaxies : ism galaxies : magellanic clouds

we investigate the evolution of the interstellar medium ( ism ) in self - consistent , chemodynamical simulations of the magellanic clouds ( mcs ) during their recent ( @xmath0 ) past . an explicit modelling of dust and molecular hydrogen lifecycles enables us to compare our models against the observed properties of the ism , including elemental depletion from the gas - phase . combining this model with a tidal - dominated paradigm for the formation for the magellanic stream and bridge , we reproduce the age - metallicity relations , long gas depletion timescales , and presently observed dust and molecular hydrogen masses of the mcs to within their respective uncertainties . we find that these models enrichment depends sensitively on the processing of dust within the ism and the dynamical influence of external tides / stellar bars . the ratio of characteristic dust destruction timescales in our smc and lmc models , a governing parameter of our models evolution , is consistent with estimates based on observed supernova ( sn ) rates . our reference mc models tend to exhibit the disputed universal dust - to - metal ratio , which we argue stems from the adoption of high sne ii condensation efficiencies . our models are the first to reproduce the one - tenth solar metallicity of the stream / leading arm following tidal stripping of the smc ; the hypothesis that the lmc contributes a metal - rich filament to the stream , as implied by recent kinematic and abundance analyses , is also appraised in this study . [ firstpage ] galaxies : interactions galaxies : evolution galaxies : ism galaxies : magellanic clouds

1406.1642

c

we have investigated the recent chemodynamical evolution of the magellanic system with n - body / sph simulations , and the first self - consistent model of dust and h@xmath2 lifecycles . our models are broadly consistent with observations ; we discuss these results in terms of the metallicity - dependence of dust production , dynamical influences on h@xmath2-abundance , and future refinements to the numerical model . the principal results are summarised as follows : 1 . we simulate the magellanic clouds for their previous 3.4 gyr of chemodynamical evolution while in proximity to the galaxy , based on collisionless models originally developed in diaz & bekki ( 2012 ) . this timescale corresponds to a period of elevated star formation ( weisz et al . 2013 ) , which our models associate with strong mutual tidal perturbations operating within the lmc - smc - galaxy triplet . the past orbits of the mcs are reconstructed from recent proper motion measurements and constrained by the morphology of the magellanic stream , which is formed from tidal stripping of the smc commencing @xmath92 gyr ago . the mass composition of our smc model s1 ( which we assume includes most of the neutral hydrogen that presently comprises the magellanic stream , bridge and leading arms ) and lmc model l2 are thus constrained by that adopted in diaz & bekki ( 2012 ) wherein observed rotation curves were reproduced . we also investigate the evolution of a massive lmc model l1 whose mass more closely matches that predicted by pre - infall halo occupation models . 2 . our ism model , which explicitly follows the evolution of h@xmath2 and multi - elemental dust , incorporates parametrizations derived in the seminal work of dwek ( 1998 ) and similarly assumes the 2:1 coupling of dust destruction / accretion timescales . we calibrate this model , together with star formation criteria , against the observed star formation law and dust - to - metal abundance relations of the clouds . our reference model for the smc reproduces the present star formation rates inferred from fir and h@xmath30 emission ( i.e. bolatto et al . we find qualitative agreement with the observed age - metallicity relations and star formation histories of both mcs ( harris & zaritksy 2004 ; 2009 ; weisz et al . 2013 ) . for low and high mass lmc models , a recent ( @xmath32300 myr ago ) enhancement in sfh coincides with above - average asymmetry of the disc as observed ( van der marel et al . 2002 ) and representative of the wider class of magellanic irregulars . 3 . in a parameter study , we find the overall enrichment of the metal - poor clouds highly dependent on the choice of dust parameters , in particular the characteristic timescale for destruction by neighbouring sne . assuming destruction is most efficient in supernova remnants and is thus correlated with the recent star formation rate , the ratio of mean destruction timescales in our lmc and smc models is consistent with other observational and analytical studies . by adopting an initial dust - to - metal ratio of 0.4 ( the presumed metallicity - independent value for evolved systems ) our reference lmc / smc models match the observed ism abundances . moreover , the models are bound to this ratio throughout their evolution . commencing from a ratio of 0.1 converges upon the same abundances , implying the tendency towards an equilibrium state . observational estimates of the dust - to - gas ratio and oxygen abundance of the mcs and other metal - poor systems favour instead a non - linear metallicity dependence of dust abundance . we trace this discrepancy to the uncertainty regarding sne ii dust condensation efficiencies ; our adopted values from dwek ( 1998 ) are ostensibly too high , given recent evidence suggesting that dust growth in the ism is the primary source of the present dust mass . 5 . the morphology and low ( 0.1 z@xmath11 ) metallicity of the simulated magellanic stream and leading arms ( i.e. fox et al . 2013 ) are reproduced following the tidal stripping of our smc model by the mw / lmc . our simulations are the first to model these tidal features with an ism comprising h i , h@xmath2 and dust components ; we find they are dominated by h i , while h@xmath2 and dust make a negligible contribution . the h i shows a column density gradient along the stream , similar to that observed ( putman et al . 2003 ) and thus precludes the requirement for ram pressure interactions with the galaxy to explain this feature . the h i mass is however deficient by a factor of @xmath95 , similar to that found by other numerical sutides ( i.e. besla et al . this highlights a fundamental underestimation of the smcs original mass / gas budget . the dust - to - gas ratio and depletion of the gas phase to dust condensate is smaller in our simulated stream than that implied from sightline analysis , attributable to the stripped material being loose , unenriched metal / dust - poor gas from the peripehery of the smc . we show in additional models how the observed @xmath90.6 dex depletion level can be obtained from encouraging dust accretion in the smc gas disc prior to its stripping to the stream ; these models lead however to excessive h@xmath2 and dust abundances in the parent disc . we also address the recent hypothesis that a metal - rich and kinematically distinct filament in the stream was sourced from the lmc ( nidever et al . 2010 ; richter et al . 2013 ) . unlike our massive lmc model ( dynamical mass 6@xmath1710@xmath34 m@xmath11 ) , our low mass model ( 1@xmath1710@xmath34 m@xmath11 ) contributes a filament to the stream via stripping by the mw . this filament is less massive than that sourced from the smc by a magnitude , and does not readily match the metal or dust abundances of the aforementioned filament for the same reason as the smc - stream . 7 . in a subsequent paper , we aim to improve upon our reproduction of the mcs evolution and present abundances ( in a tidal - dominated scenario with the adopted dust / h@xmath2 model ) with the following major refinements : 1 ) uncoupling the relationship between dust accretion and destruction timescales to better reflect local ism conditions ; 2 ) calibrating our sne ii condensation efficiencies and characteristic timescales of dust growth against those estimated for metal - poor systems ; and 3 ) extending the method of diaz & bekki ( 2012 ) to larger lookback times ( assuming improved constraints on the mcs proper motions and dynamical masses become available ) , such that we can assert if a realistic ism abundance distribution at the onset of recent tidal stripping can accomodate the observed depletion of the stream .

an explicit modelling of dust and molecular hydrogen lifecycles enables us to compare our models against the observed properties of the ism , including elemental depletion from the gas - phase . combining this model with a tidal - dominated paradigm for the formation for the magellanic stream and bridge , the ratio of characteristic dust destruction timescales in our smc and lmc models , a governing parameter of our models evolution , is consistent with estimates based on observed supernova ( sn ) rates .

we investigate the evolution of the interstellar medium ( ism ) in self - consistent , chemodynamical simulations of the magellanic clouds ( mcs ) during their recent ( @xmath0 ) past . an explicit modelling of dust and molecular hydrogen lifecycles enables us to compare our models against the observed properties of the ism , including elemental depletion from the gas - phase . combining this model with a tidal - dominated paradigm for the formation for the magellanic stream and bridge , we reproduce the age - metallicity relations , long gas depletion timescales , and presently observed dust and molecular hydrogen masses of the mcs to within their respective uncertainties . we find that these models enrichment depends sensitively on the processing of dust within the ism and the dynamical influence of external tides / stellar bars . the ratio of characteristic dust destruction timescales in our smc and lmc models , a governing parameter of our models evolution , is consistent with estimates based on observed supernova ( sn ) rates . our reference mc models tend to exhibit the disputed universal dust - to - metal ratio , which we argue stems from the adoption of high sne ii condensation efficiencies . our models are the first to reproduce the one - tenth solar metallicity of the stream / leading arm following tidal stripping of the smc ; the hypothesis that the lmc contributes a metal - rich filament to the stream , as implied by recent kinematic and abundance analyses , is also appraised in this study . [ firstpage ] galaxies : interactions galaxies : evolution galaxies : ism galaxies : magellanic clouds

1201.6603

c

we have investigated prospects of determining dm annihilation final states with neutrino telescopes by using the spectrum of contained muon tracks from conversion of neutrinos that are produced in the annihilation of dm particles trapped inside the sun . our focus was on distinguishing neutrino final states from gauge boson and tau final states and on discriminating the flavor of final state neutrinos . gauge boson and tau final states are typically the dominant annihilation channels in supersymmetric models with neutralino dm , while direct annihilation into neutrinos can occur in models that connect dm to the neutrino sector . the theoretical motivation for the latter could provide the grounds for a dedicated analysis by the icecube collaboration to put stringent bounds on annihilation to primary neutrinos , similar to what has been done for annihilation to gauge bosons @xcite . primary neutrinos from dm annihilation result in a distinct peak in the muon spectrum at the dm mass . for dm masses below @xmath12 gev we can expect that the peak will be accessible to a detector the size of ic . the spectrum is smeared as a result of the experimental error in energy reconstruction , but primary neutrinos may be distinguished from gauge boson and tau final states after this effect is taken into account . we showed that for an energy resolution of 10 gev ( as in ic / dc ) and by making an optimal angular cut on the muons ( which we found to be @xmath117 ) , the branching ratios may be determined in the parameter space within the reach of the one - year sensitivity limits of ic / dc with a km@xmath58/yr of data . this is roughly equivalent to @xmath77 years of data for a detector with the same capabilities and effective volume as ic / dc . the regeneration of @xmath0 inside the sun may be used to distinguish the flavor of final state primary neutrinos . this effect becomes important for dm masses above @xmath12 gev and populates the spectrum with muons whose energy is well below the energy of primary neutrinos . for dm masses up to about @xmath107 gev , oscillations mix @xmath1 and @xmath0 effectively , which implies that regeneration affects final states with @xmath1 and @xmath0 similarly . final states with @xmath2 are therefore distinguishable within this mass range . for heavier dm particles , the @xmath101 oscillation becomes inefficient . as a result , @xmath0 final states are picked out by the regeneration effect for dm masses above @xmath107 gev . we showed that final states with @xmath0 stand out at a statistically significant level for dm masses as heavy as @xmath118 gev , even after normalizing the muon spectrum to the total event count ( to account for the unknown dm - nucleon elastic scattering cross section ) . again , such a distinction may be achieved with @xmath77 years of data from ic / dc . in summary , using the the ic / dc results in tandem with independent measurements of the dm mass ( for example , from the lhc ) , will allow us to identify the annihilation channels of dm with multi - year data . improved energy resolution and increased effective volume of the detector will greatly help in achieving this goal .

we investigate the prospects for distinguishing dark matter annihilation channels using the neutrino flux from gravitationally captured dark matter particles annihilating inside the sun . we show that , even with experimental error in energy reconstruction taken into account , the spectrum of contained muon tracks may be used to discriminate neutrino final states from the gauge boson / charged lepton final states and to determine their corresponding branching ratios . this effect as evidenced in the muon spectrum becomes important for dark matter masses above 300 gev . distinguishing primary neutrinos and their flavor may be achieved using multi - year data from a detector with the same capability and effective volume as the icecube / deepcore array .

we investigate the prospects for distinguishing dark matter annihilation channels using the neutrino flux from gravitationally captured dark matter particles annihilating inside the sun . we show that , even with experimental error in energy reconstruction taken into account , the spectrum of contained muon tracks may be used to discriminate neutrino final states from the gauge boson / charged lepton final states and to determine their corresponding branching ratios . we also discuss the effect of @xmath0 regeneration inside the sun as a novel method to distinguish the flavor of final state neutrinos . this effect as evidenced in the muon spectrum becomes important for dark matter masses above 300 gev . distinguishing primary neutrinos and their flavor may be achieved using multi - year data from a detector with the same capability and effective volume as the icecube / deepcore array . pacs numbers : 98.80.cq , 95.35.+d , 14.60.lm , 29.40.ka

1010.2927

i

production of exotic nuclei has opened the way to explore , in laboratory conditions , new aspects of nuclear structure and dynamics up to extreme ratios of neutron ( n ) to proton numbers ( z ) . an important issue addressed is the density dependence of the symmetry energy term in the nuclear equation of state ( eos ) , of interest also for the properties of astrophysical objects @xcite . by employing heavy ion collisions ( hic ) , at appropriate beam energy and centrality , the isospin dynamics at different densities of nuclear matter can be investigated @xcite . in this work we will focus the attention on the interplay of fusion vs. deep - inelastic mechanisms for dissipative hic with exotic nuclear beams at low energies , just above the coulomb barrier ( between @xmath2 and @xmath3 amev ) , where unstable ion beams with large asymmetry will be soon available . we will show that the competition between reaction mechanisms can be used to study properties of the symmetry energy term in a density range around the normal value . dissipative collisions at low energy are characterized by interaction times that are quite long and by a large coupling among various mean field modes that may eventually lead to the break - up of the system . hence the idea is to probe how the symmetry energy will influence such couplings in neutron - rich systems with direct consequences on the fusion probability . we will show that , within our approach , the reaction path is fully characterized by the fluctuations , at suitable time instants , of phase space quadrupole collective modes that lead the composite system either to fusion or to break - up . moreover , it is now well established that in the same energy range , for dissipative reactions between nuclei with different @xmath4 ratios , the charge equilibration process has a collective character resembling a large amplitude giant dipole resonance ( gdr ) , see the recent @xcite and refs . therein . the gamma yield resulting from the decay of such pre - equilibrium isovector mode can encode information about the early stage of the reaction @xcite . this collective response is appearing in the intermediate neck region , while the system is still in a highly deformed dinuclear configuration with large surface contributions , and so it will be sensitive to the density dependence of symmetry energy below saturation @xcite . here we will show that this mode is present also in break - up events , provided that a large dissipation is involved . in fact we see that the strength of such fast dipole emission is not much reduced passing from fusion to very deep - inelastic mechanisms . this can be expected from the fact that such excitation is related to an entrance channel collective oscillation . thus we suggest the interest of a study of the prompt gamma radiation , with its characteristic angular anisotropy @xcite , even in deep - inelastic collisions with radioactive beams . the paper is organized as follows . in sect.ii we present our transport approach to the low energy hic dynamics with description of the used symmetry effective potentials . sect.iii is devoted to the analysis of @xmath5 induced reactions with details about the procedure to select fusion vs. break - up events . in sect.iv we discuss symmetry energy effects on the competition between fusion and break - up ( fast - fission , deep - inelastic , ternary / quaternary - fragmentation ) mechanisms . the dependence on symmetry energy of the yield and angular distribution of the prompt dipole radiation , expected for entrance channels with large charge asymmetries , is presented in sect.v . finally in sect.vi we summarize the main results and we suggest some experiments to be performed at the new high intensity radioactive ion beam ( rib ) facilities in this low energy range .

we investigate the reaction path followed by heavy ion collisions with exotic nuclear beams at low energies . we will focus on the interplay between reaction mechanisms , fusion vs. break - up ( fast - fission , deep - inelastic ) , that in exotic systems is expected to be influenced by the symmetry energy term at densities around the normal value .

we investigate the reaction path followed by heavy ion collisions with exotic nuclear beams at low energies . we will focus on the interplay between reaction mechanisms , fusion vs. break - up ( fast - fission , deep - inelastic ) , that in exotic systems is expected to be influenced by the symmetry energy term at densities around the normal value . the evolution of the system is described by a stochastic mean field transport equation ( smf ) , where two parametrizations for the density dependence of symmetry energy ( asysoft and asystiff ) are implemented , allowing one to explore the sensitivity of the results to this ingredient of the nuclear interaction . the method described here , based on the event by event evolution of phase space quadrupole collective modes will nicely allow to extract the fusion probability at relatively early times , when the transport results are reliable . fusion probabilities for reactions induced by @xmath0sn on @xmath1ni targets at 10 amev are evaluated . we obtain larger fusion cross sections for the more n - rich composite system , and , for a given reaction , in the asysoft choice . finally a collective charge equilibration mechanism ( the dynamical dipole ) is revealed in both fusion and break - up events , depending on the stiffness of the symmetry term just below saturation .

1608.03539

c

the fits in section [ decomp ] reveal that ngc 2681 , ngc 3945 and ngc 4371 contain bulges that have srsic indices @xmath136 to @xmath137 . in addition , ngc 3945 and ngc 4371 have intermediate - scale disky ( @xmath138 ) pseudo - bulges that we modelled using the srsic model with low srsic indices @xmath139 and @xmath140 , respectively , rather than an exponential ( @xmath4 ) disk profile as done by laurikainen et al.(2010 ) , erwin et al . ( 2015 ) and gadotti et al . ( 2015 ) . forcing an exponential ( @xmath4 ) disk profile overestimates the actual luminosities of these low n ( @xmath141 ) pseudo - bulges which dominate the intermediate regions of the galaxies rather than at large radii like large - scale disks do . on the other hand , the bulge light in ngc 3945 and ngc 4371 dominates over the pseudo - bulge light at both small and large radii ( fig [ fig2 ] ) . as such these bulges do not reside within the pseudo - bulges ( although see erwin et al . 2015 ) . all of our bulges ( and pseudo - bulges ) have srsic indices @xmath142 ( and @xmath143 ) , in agreement with the ` pseudo - bulge ' ( @xmath144 ) versus ` classical bulges ' ( @xmath145 ) dichotomy ( e.g. , fisher & drory 2008 ) . however , the robustness of such a srsic index - based division among bulges is highly disputed ( e.g. , athanassoula 2005 ; graham 2013 , 2014 ) . the dichotomy in the properties between pseudo - bulges and classical bulges is attributed to their formation mechanisms . pseudo - bulges are thought to have formed via inward funnelling of disk materials catalysed by non - axisymmetric features , for example bars and rings ( e.g. , pfenniger & friedli 1991 ; kormendy & kennicutt 2004 ) while classical bulges ( hereafter referred to as bulges ) , akin to elliptical galaxies , are believed to be products of violent hierarchical merging processes ( e.g. , toomre & toomre 1972 ; kauffmann et al . 1996 ) or / and a rapid dissipative collapse ( eggen et al . 1962 ) . also , those massive present - day bulges , typically with @xmath146 and @xmath147 kpc , might be descendants of the compact , massive high - redshift ( @xmath148 ) early - type galaxies kpc , massive ( @xmath149 ) early - type galaxies at @xmath150 , noting the sizes of these objects are much smaller than local elliptical galaxies of comparable mass . ] ( graham 2013 , dullo & graham 2013 ; graham , dullo & savorgnan 2015 ; de la rosa et al . 2016 ) . table [ tab3 ] lists the fractional luminosities of the ( pseudo -)bulges plus other model components in ngc 2681 , ngc 3945 and ngc 4371 . for each component , the total integrated flux was computed using the best - fit ( major - axis ) structural parameters ( table [ tab2 ] ) and the corresponding ellipticity . these new flux measurements improve upon past works which used ground - based data or / and fitted a 2-component bulge plus disk model because our measurements are based on careful multi - component decompositions of high - resolution _ hst _ plus ground - based sdss data , and accounting for ( i ) the bulge , pseudo - bulge , disk , bar , lens , and point - source of the galaxies and ( ii ) the psf convolution . @xmath25-band bulge - to - total flux ( @xmath85 ) ratio of ngc 2681 is 0.33 , considerably higher than those of ngc 3945 ( @xmath25-band @xmath151 ) and ngc 4371 ( @xmath26-band @xmath152 ) , and broadly consistent with laurikainen et al . ( 2010 ; @xmath95-band @xmath153 ) . for ngc 2681 , the large - scale bar contains a significant fraction of the galaxy light ( @xmath1540.43 ) , compared to the bulge ( @xmath155 0.33 ) and the disk ( @xmath156 ) . the two smaller bars and the point source are relatively less luminous , adding up to 10% of the total galaxy flux . for ngc 3945 and ngc 4371 , the bulges are fainter than all the other components of the galaxies ( fig . [ fig2 ] , tables [ tab2 ] , [ tab3 ] ) . our @xmath85 ratios for these two galaxies ( @xmath157 ) are up to a factor of 3 higher than those reported by erwin et al . ( 2015 , @xmath158 @xmath7 0.06 , @xmath159 ) , their table 5 ) . on the other hand , the b / t ratio for ngc 4371 is in good agreement with laurikainen et al . ( 2010 , b / t = 0.20 ) , but because the 2d decomposition by laurikainen et al . did not identify the pseudo - bulge in ngc 3945 their @xmath160 ratio for that galaxy is higher than ours . it is worth noting that the bars , rings and the point source pertaining to our three galaxies add up to more than 20% of the total galaxy luminosities , underscoring the importance of including these components in the decomposition of multicomponent galaxies . before estimating the stellar masses of the bulges and pseudo - bulges in table [ tab4 ] , we corrected their luminosities for galactic extinction and surface brightness dimming . the bulges of ngc 2681 , ngc 3945 and ngc 4371 are compact ( i.e. , half - light radii @xmath161 pc to 385.4 pc ) and have stellar masses in the range @xmath1 @xmath2 . assuming a lower stellar mass limit of 1@xmath162 for compact , massive high - z galaxies ( e.g. , barro et al . 2013 ) , implies that the bulges of ngc 2681 and ngc 3945 ( see table [ tab4 ] ) might be local counterparts to compact high-@xmath26 galaxies ( dullo & graham 2013 , their fig . 5 ; graham , dullo & savorgnan 2015 , their fig . the bulge of ngc 4371 is less massive than the aforementioned mass limit . furthermore , the ( pseudo-)bulge - total flux ratios , masses and srsic indices @xmath163 of the bulges and pseudo - bulges of our three barred s0 galaxies are similar to those of other spiral and lenticular galaxies ( see e.g. , balcells et al . 2007 ; graham & worley 2008 ; laurikainen et al . 2010 , their figs . 4 , 5 , and 6 ; kormendy et al.2012 , their table 1 ; graham 2014 , his fig . 5 ; erwin et al . 2015 , their figs . 8 , 10 ) . this similarity is unsurprising because the ( pseudo-)bulge - to - total flux ratio for s0s can have any value between 1 and 0 ( e.g. , laurikainen et al . 2010 ) and it does not imply that multiple evolutionary paths are not possible for s0s ( e.g. , laurikainen et al . 2010 ; dullo & graham 2013 ; graham , dullo & savorgnan 2015 ; erwin et al . 2015 ) . given that the sizes ( as measured by the half - light radii @xmath51 ) of all the structural components of our galaxies , except the outer disks and the large - scale ring of ngc 3945 , are smaller than those of the large - scale bars , one can simply envisage that these galaxies are created via bar - related processes . small - scale bars and rings facilitate the gas supply to nuclear regions of the galaxies ( e.g. , shlosman et al . 1989 ) . in favor of this argument are ( i ) the presence of pseudo - bulges in ngc 3945 and ngc 4371 and ( ii ) the liner nuclear emission of the double- and triple - barred galaxies ( ngc 3945 and ngc 2681 ) , compared to the weak nuclear emission of the single - bar galaxy ngc 4371 ( section [ bpt ] ) . for ngc 2681 , the point source and the winding nuclear stellar spiral seen in continuum subtracted images ( figs . [ fig__line_image ] , [ fig_bpt ] ) are also consistent with a bar - driven formation scenario . however , bar - related mechanisms can not account for the bulges of ngc 2681 , ngc 3945 and ngc 4371 . for example , the bulge of ngc 2681 has a high central light concentration , as indicated by @xmath75 , suggestive of a classical ( @xmath164 ) bulge . similarly , the bulge of ngc 3945 with @xmath165 and a low ellipticity ( @xmath166 ) favors a merger - built scenario . also , the stellar kinematics by erwin et al . ( 2015 , their fig . 4d ) for ngc 3945 shows that the ratio of rotation velocity to velocity dispersion is low ( i.e. , @xmath167 ) in the inner regions where the bulge dominates ( i.e. , @xmath168 ) , supporting a merger origin for the galaxy s bulge . as noted above in section [ sec5.1 ] , the bulges of ngc 2681 and ngc 3945 occupy the same area as the @xmath169 compact spheroids in the size - mass diagram , although , all our bulges contain masses that are smaller than the conservative lower stellar mass limits adopted for high-@xmath26 compact galaxies ( 0.7@xmath170 ) , for example , by graham et al . ( 2015 , and references therein ) . therefore , our three galaxies may rather have had their bulges built at high redshift through violent major mergers , and the formation of the large - scale disks , pseudo - bulges , bars and rings subsequently ensues . in excellent agreement with this picture , the muse stellar population maps by gadotti et al . ( 2015 , their figs . 13 , 14 ) for ngc 4371 clearly show that the regions where the bulge dominates over the pseudo - bulge ( i.e. , the inner @xmath171 plus the region immediately outside the pseudo - bulge , see fig . [ fig2 ] ) have the highest concentration of old ( @xmath1728 gyr ) stars in the galaxy , as remarked upon by gadotti et al . ( 2015 ) . overall , our results suggest that the barred s0 galaxies ngc 2681 , ngc 3945 and ngc 4371 likely have a complex formation and evolutionary history . the pseudo - bulges have formed slowly out of the disk materials through the actions of bars and rings which drive gas inflow for fuelling the agn while the spheroidal components ( i.e. , bulges ) are consequences of violent mergers or a rapid gravitational collapse that happened earlier . further investigation of whether all the bulges that we have identified are actually dominated by stars that are older than those of the pseudo - bulges , bars , rings and outer disks , as is the case for ngc 4371 ( gadotti et al . 2015 ) together with the analysis of the age differences between the pseudo - bulges and the bars / outer disks are desirable .

ngc 3945 and ngc 4371 have intermediate - scale ` pseudo - bulges ' that are well described by a srsic model with low @xmath3 instead of an exponential ( @xmath4 ) profile as done in the past . our findings suggest that the three galaxies have experienced a complex evolutionary path .

we investigate three barred lenticular galaxies ( ngc 2681 , ngc 3945 and ngc 4371 ) which were previously reported to have complex central structures but without a detailed structural analysis of these galaxies high - resolution data . we have therefore performed four- to six - component ( pseudo-)bulge / disk / bar / ring / point source ) decompositions of the composite ( _ hubble space telescope _ plus ground - based ) surface brightness profiles . we find that ngc 2681 hosts three bars , while ngc 3945 and ngc 4371 are double- and single - barred galaxies , respectively , in agreement with past isophotal analysis . we find that the bulges in these galaxies are compact , and have srsic indices of @xmath0 and stellar masses of @xmath1 @xmath2 . ngc 3945 and ngc 4371 have intermediate - scale ` pseudo - bulges ' that are well described by a srsic model with low @xmath3 instead of an exponential ( @xmath4 ) profile as done in the past . we measure emission line fluxes enclosed within 9 different elliptical apertures , finding that ngc 2681 has a liner - type emission inside @xmath5 , but the emission line due to star formation is significant when aperture size is increased . in contrast , ngc 3945 and ngc 4371 have composite ( agn plus star forming)- and liner - type emissions inside and outside @xmath6 , respectively . our findings suggest that the three galaxies have experienced a complex evolutionary path . the bulges appear to be consequences of an earlier violent merging event while subsequent disk formation via gas accretion and bar - driven perturbations may account for the build - up of pseudo - bulges , bars , rings and point sources . [ firstpage ] galaxies : elliptical and lenticular , cd galaxies : fundamental parameter galaxies : nuclei galaxies : photometry galaxies : structure galaxies : individual . ngc 2681 , ngc 3945 and ngc 4371

1608.03539

c

we have extracted composite major - axis surface brightness profiles and isophotal parameters for three barred s0 galaxies ( ngc 2681 , ngc 3945 and ngc 4371 ) that have complex central structures using high - resolution _ hst _ wfpc2 , acs and nicmos plus ground - based sdss images . consistent with earlier published isophotal analysis , we found that ngc 2681 hosts three bars , while ngc 3945 and ngc 4371 are double- and single - barred galaxies , respectively . we performed detailed , four- to six - component ( pseudo-)bulge / disk / bar / ring / point source ) decompositions of the composite profiles covering a large radial range of @xmath173 , quantifying robustly the global and central structural properties of the galaxies . we fit an exponential function to the outer disk plus a gaussian function to the point source , and each of the other components is modelled with a srsic model . to our knowledge , this is the first time that such global decompositions have been made for these three galaxies . in addition , measuring the h@xmath22 @xmath234881 , [ o iii ] @xmath235032 , h@xmath24 @xmath236589 , [ n ii ] @xmath236613 , and [ s ii ] @xmath23@xmath236745 , 6757 line fluxes enclosed inside 9 different elliptical apertures of semi - major axes ( @xmath174@xmath58 , 2@xmath58.25 , 3@xmath58 , 4@xmath58 , 5@xmath58 , 8@xmath58 , 10@xmath58 , 15@xmath58 , and 20@xmath58 ) , we constructed the standard bpt diagnostic diagrams to distinguish between line emission produced by star formation , an agn or composite agn plus star formation processes . our principal findings are as follows . \(1 ) the decompositions yield good fits to the galaxy data . the average rms residual scatter is @xmath7 0.05 mag arcsec@xmath175 . we provide robust structural parameters for all the galaxy components . for our galaxies , we found that all the components except the outer bar , ring and disk have effective half - light radii @xmath176 kpc . \(2 ) an intermediate - scale disky ( @xmath138 ) component ( which we refer to as ` pseudo - bulge ' ) and a bulge coexist within ngc 3945 and ngc 4371 , confirming the conclusion of erwin et al . however , in contrast to past works we found that these pseudo - bulges follow a low @xmath163 ( @xmath141 ) srsic model profile instead of an exponential ( @xmath4 ) profile . fitting an exponential profile to what is actually a srsic profile with a low @xmath163 overestimates the luminosity and mass of the pseudo - bulge . the bulges of our three galaxies have srsic indices of @xmath177 \(3 ) we have presented new fractional luminosities for the ( pseudo-)bulges and other model components of ngc 2681 , ngc 3945 and ngc 4371 . we found that the bulges of our galaxies are compact ( i.e. , half - light radii @xmath161 pc to 385.4 pc ) and have stellar masses of @xmath1 @xmath2 . \(4 ) the nuclear regions of ngc 2681 , ngc 3945 and ngc 4371 lie well outside the pure star - forming galaxy zone in the bpt diagram . instead , ngc 2681 has liner - type emission inside @xmath5 but the emission lines due to star formation become increasingly significant when the aperture size is increased , consistent with the presence of the point source and nuclear bar in this galaxy . this trend is reversed for ngc 3945 and ngc 4371 where the contributions of the emission lines are dominated by the agn over @xmath133 . ngc 4371 has the weakest emission lines of the three galaxies . \(5 ) our results suggest that the bulges of the three galaxies have formed via an earlier violent merging while the disks form over time through gas accretion and bar - driven perturbations could create pseudo - bulges , bars , rings and point sources . nested bars are common , with around one third of all barred galaxies containing at least one additional smaller bar , and in future work we will analyse more of such systems in order to categorise them in more detail , and compare them in detail with dynamical models .

we investigate three barred lenticular galaxies ( ngc 2681 , ngc 3945 and ngc 4371 ) which were previously reported to have complex central structures but without a detailed structural analysis of these galaxies high - resolution data . we have therefore performed four- to six - component ( pseudo-)bulge / disk / bar / ring / point source ) decompositions of the composite ( _ hubble space telescope _ plus ground - based ) surface brightness profiles . we find that ngc 2681 hosts three bars , while ngc 3945 and ngc 4371 are double- and single - barred galaxies , respectively , in agreement with past isophotal analysis . we find that the bulges in these galaxies are compact , and have srsic indices of @xmath0 and stellar masses of @xmath1 @xmath2 . we measure emission line fluxes enclosed within 9 different elliptical apertures , finding that ngc 2681 has a liner - type emission inside @xmath5 , but the emission line due to star formation is significant when aperture size is increased . in contrast , ngc 3945 and ngc 4371 have composite ( agn plus star forming)- and liner - type emissions inside and outside @xmath6 , respectively . the bulges appear to be consequences of an earlier violent merging event while subsequent disk formation via gas accretion and bar - driven perturbations may account for the build - up of pseudo - bulges , bars , rings and point sources .

we investigate three barred lenticular galaxies ( ngc 2681 , ngc 3945 and ngc 4371 ) which were previously reported to have complex central structures but without a detailed structural analysis of these galaxies high - resolution data . we have therefore performed four- to six - component ( pseudo-)bulge / disk / bar / ring / point source ) decompositions of the composite ( _ hubble space telescope _ plus ground - based ) surface brightness profiles . we find that ngc 2681 hosts three bars , while ngc 3945 and ngc 4371 are double- and single - barred galaxies , respectively , in agreement with past isophotal analysis . we find that the bulges in these galaxies are compact , and have srsic indices of @xmath0 and stellar masses of @xmath1 @xmath2 . ngc 3945 and ngc 4371 have intermediate - scale ` pseudo - bulges ' that are well described by a srsic model with low @xmath3 instead of an exponential ( @xmath4 ) profile as done in the past . we measure emission line fluxes enclosed within 9 different elliptical apertures , finding that ngc 2681 has a liner - type emission inside @xmath5 , but the emission line due to star formation is significant when aperture size is increased . in contrast , ngc 3945 and ngc 4371 have composite ( agn plus star forming)- and liner - type emissions inside and outside @xmath6 , respectively . our findings suggest that the three galaxies have experienced a complex evolutionary path . the bulges appear to be consequences of an earlier violent merging event while subsequent disk formation via gas accretion and bar - driven perturbations may account for the build - up of pseudo - bulges , bars , rings and point sources . [ firstpage ] galaxies : elliptical and lenticular , cd galaxies : fundamental parameter galaxies : nuclei galaxies : photometry galaxies : structure galaxies : individual . ngc 2681 , ngc 3945 and ngc 4371

1006.5645

m

our aim is to obtain a reliable measurement of the real - space correlation length @xmath5 , the separation at which the 3d spatial correlation function satisfies @xmath107 . in the following description we will use the term redshift " to refer to photo - zs in the case of musyc data , and to refer to either photometric or spectroscopic redshifts in the case of the mock catalogues ( in this case , spectroscopic redshifts correspond to the true galaxy redshifts ) ; when analysing the latter , spectroscopic redshifts will be used to infer the true underlying clustering present in the mock samples . we will apply the following steps both to real and mock data : * measure the projected - angular cross - correlation function @xmath1 as a function of the comoving projected separation , @xmath108 . when calculating this correlation function one assumes that all tracers ( usually with no distance information ) lie at the known distance of the centre galaxy , given by its redshift ( spectroscopic or photometric ) . in our case this approach keeps the effect of distance measurement errors to a minimum by only using photometric redshifts to estimate comoving distances to the centre galaxies , and to restrict the range of redshifts of tracers ( i.e. we never calculate the relative distance between galaxies in the radial direction ) ; this is the main aim behind the choice of this cross - correlation function . + centre samples comprise galaxies selected by applying the cuts in redshift ( spectroscopic or photometric ) and absolute magnitude ( evaluated at the redshift of each individual galaxy ) defined in section [ sec : data ] . the tracer samples are characterised by the same cuts in rest - frame absolute magnitude ( calculated at the redshift of each individual galaxy ) and by redshifts @xmath109 ) , where @xmath110 and @xmath111 are the limits of the centre sample , and @xmath78 . the wider redshift range allowed for tracers results in an increase of the number of pairs around centre galaxies near @xmath110 and @xmath111 . + the estimator applied in this case is @xmath112 where @xmath113 and @xmath114 are counts of pairs of centre vs. tracer , and centre vs. random points , respectively . random points are extracted from random catalogues created to reproduce the angular geometry of the survey with constant density . since in the cross - correlation estimator adopted here the tracer sample is positioned at the distance of each centre galaxy , a random catalogue does not need to reproduce a radial selection function . * we find that the propagation of redshift errors onto magnitude , comoving distance and projected distance estimates , produces systematic effects on our measurements . we correct for these biases by modifying the projected separations involved in our calculations using a method tested with the mock catalogues . * we use @xmath1 to estimate the projected correlation function , @xmath2 , following padilla et al . ( 2001 ) , ratcliffe et al . ( 1998 ) and croft , dalton & efstathiou ( 1999 ) . our interest in the @xmath2 correlation function lies in that it can be used to obtain the real - space correlation function , our final objective . the functions @xmath1 and @xmath2 can be related via @xmath115 where the constant @xmath116 takes into account the selection function , @xmath117 , of the tracer sample and the individual comoving distances to the centre galaxies , @xmath118 in this equation , @xmath119 is the comoving distance to the @xmath120th centre galaxy calculated using its redshift ( spectroscopic or photometric ) , and the integration variable @xmath121 is comoving distance . in turn , the correlation function @xmath2 bears a close relationship to the real - space correlation function @xmath122 via @xmath123 where @xmath124 is the radial component of the 3d separation @xmath4 . * for the case of approximating the real - space correlation function by a power law with a slope @xmath125 , as @xmath126 , equation [ eq : xi ] simplifies to @xmath127 \sigma^{1-\gamma } , \label{eq : powerlaw}\ ] ] where @xmath128 is the gamma function . we use this relation to calculate the power law correlation length , @xmath5 , and slope , @xmath125 , for each subsample by minimising the quantity @xmath129 where the index @xmath120 runs over the bins in projected separation @xmath108 , @xmath130 is the measured projected correlation function , @xmath131 is the estimate from equation [ eq : powerlaw ] , and @xmath132 is the error in the measured correlation function calculated using the jacknife technique ( see section [ ssec : recovery ] ) . = 8.5truecm the method outlined above is a variant of the more common procedure of inverting the real - space correlation function from the angular correlation function @xmath133 ( where @xmath134 is the angular separation between a pair of galaxies ) using limber s equation ( limber , 1954 ) . in our case , however , the use of @xmath1 introduces the use of ( i ) the distance to centre galaxies which in this work come from photometric redshift estimates and ( ii ) the redshift distribution of tracers which also comes from photo - zs . this poses the question of whether photometric redshift errors introduce important systematics in our measurements ; this is answered in section 5 where we carry out several tests of the robustness of the method using mock catalogues . it should be stressed that the effect of the photo - z errors would still be similar in an inversion of the angular correlation function using limber s equation since in this case the photo - z errors would affect the redshift distribution of both , centres and tracers . our method has the advantage of allowing the use of different redshift ranges for tracers so as to maximise the number of pairs for centre galaxies near the borders of a redshift bin . in this subsection we present an attempt to understand the process of inferring a correlation length @xmath5 and power law slope @xmath125 using a theoretical projected cross - correlation function @xmath2 , paying particular attention at the relation between the parametrisation of this power - law and the physical quantities encoded in the correlation function . the actual shape of the real - space correlation function deviates from the power law proposed in section [ sec : method ] both in predictions from a @xmath3cdm model ( e.g. zheng et al . , 2005 ) and in observations ( e.g. zehavi et al . , 2004 ) . the meaning of @xmath5 in a power law correlation function is that of the separation at which the correlation function satisfies @xmath107 . in the case where the shape of @xmath122 is different than a power law , we will use the same equality to define @xmath5 . with respect to the power law slope @xmath125 , notice that its value will depend on the scales used to fit an estimate of a correlation function . we use theoretical estimates of the real - space and projected correlation functions for the @xmath3cdm cosmology obtained from non - linear power spectra using the smith et al . ( 2003 ) formalism . for real - space correlations we calculate the value of @xmath5 in three different ways , ( i ) searching the separation , @xmath135 , at which @xmath136 , ( ii ) by fitting a power law to the real - space correlation function @xmath122 between separations of @xmath137h@xmath8mpc@xmath138 , in which case we obtain @xmath139 ; additionally , this procedure also provides an estimate of the power law slope , @xmath140 . ( iii ) by using the method described in the third item of the previous section ( eq . 7 ) of fitting a power law to the projected correlation function between separations of @xmath141h@xmath8mpc@xmath138 ( corresponding to the scales we will use for the measured projected correlation functions ) . the value of @xmath135 can be considered as the true " underlying value of @xmath5 which will not depend on the parametrisation of @xmath122 . figure [ fig : xith ] shows projected correlation functions for different redshifts ( top line for @xmath17 to bottom line for @xmath142 ) ; the inset on the lower left shows the values of @xmath135 as a solid line ( true value ) , and of @xmath139 as a dotted line ; as can be seen both definitions of a correlation length agree to @xmath143h@xmath8mpc at @xmath17 and to @xmath144h@xmath8mpc at @xmath142 . the inset on the upper right shows as a dotted line the resulting values of @xmath140 . the procedure outlined in item ( iii ) of section [ sec : method ] recovers the correlation length and power law slope , @xmath5 and @xmath125 , shown as dashed lines in the lower left and upper right insets , respectively . this procedure reproduces the process that we will apply to our real data , and therefore can be used to put into context the meaning of the measured values of @xmath5 and @xmath125 in terms of the underlying values @xmath135 and @xmath139 and @xmath140 . as can be seen the recovered correlation length from the projected correlation function following the @xmath145 method , is consistent with the direct fit to the real - space correlation function . the power law slope , on the other hand , shows a systematic offset which could be taken into account when analysing the measured projected correlation functions . the origin of this offset comes from the mix of scales characterised by different correlation function slopes , produced by the integral over the radial direction . in this sense , the measured value of @xmath125 obtained from @xmath2 is a different quantity than @xmath140 , the average slope of the real - space correlation function . in our analysis of musyc data we will adopt a fixed value for this parameter of @xmath146 roughly consistent with previous estimates for galaxies at similar redshifts and also with theoretical values such as @xmath140 ; the statistics only allow one parameter to be obtained from this set of galaxies .

we use photometric redshift information to calculate the projected - angular correlation function , @xmath1 , from which we infer the projected correlation function @xmath2 . we demonstrate that this technique delivers accurate measurements of clustering even when large redshift measurement errors affect the data . to this aim

we measure the evolution of galaxy clustering out to a redshift of @xmath0 using data from two musyc fields , the extended hubble deep field south ( ehdf - s ) and the extended chandra deep field south ( ecdf - s ) . we use photometric redshift information to calculate the projected - angular correlation function , @xmath1 , from which we infer the projected correlation function @xmath2 . we demonstrate that this technique delivers accurate measurements of clustering even when large redshift measurement errors affect the data . to this aim we use two mock musyc fields extracted from a @xmath3cdm simulation populated with galform semi - analytic galaxies which allow us to assess the degree of accuracy of our estimates of @xmath2 and to identify and correct for systematic effects in our measurements . we study the evolution of clustering for volume limited subsamples of galaxies selected using their photometric redshifts and rest - frame @xmath4-band absolute magnitudes . we find that the real - space correlation length @xmath5 of bright galaxies , @xmath6 ( rest - frame ) can be accurately recovered out to @xmath0 , particularly for ecdf - s given its near - infrared photometric coverage . for these samples , the correlation length is consistent with a constant value of @xmath7h@xmath8mpc for the ecdf - s field , and @xmath9h@xmath8mpc for the ehdf - s field from a median redshift @xmath10 to @xmath11 . there is mild evidence for a luminosity dependent clustering in both fields at the low redshift samples ( up to @xmath12 ) , where the correlation length is higher for brighter galaxies by up to @xmath13 between median rest - frame r - band absolute magnitudes of @xmath14 to @xmath15 . as a result of the photometric redshift measurement , each galaxy is assigned a best - fit template ; we restrict to e and e@xmath16sbc types to construct subsamples of early type galaxies ( etgs ) . these etgs are separated into samples at different redshift intervals so that their passively evolved luminosities ( to @xmath17 ) are comparable . our etg samples show a strong increase in @xmath5 as the redshift increases , making it unlikely ( @xmath18 level ) that etgs at median redshift @xmath11 are the direct progenitors of etgs at @xmath10 with equivalent passively evolved luminosities . galaxies : distances and redshifts , galaxies : statistics , cosmology : observations , large - scale structure of the universe .

gr-qc0209072

i

this is the second in a series of papers aimed to establish a practical calculation scheme for the self force acting on a point particle in orbit around a black hole . this scheme referred to as the `` mode - sum method''stems from the general regularization prescription by mino , sasaki , and tanaka ( mst)@xcite and quinn and wald ( qw)@xcite . in effect , the mode - sum method re - formulates the mst - qw general result in the language of multipole modes , thereby making it accessible to standard numerical treatment . in practice , the application of this method involves two basic parts : ( i ) calculation of the `` full '' modes of the force , through numerical integration of the decoupled field equations ; and ( ii ) analytical derivation of certain parameters ( whose values depend on the orbit under consideration ) called the `` regularization parameters '' ( rp ) . previously , the explicit values of the rp were derived analytically in a few special cases of orbits in schwarzschild spacetime specifically , for circular and radial orbits in the scalar field case @xcite , and for radial trajectories in the gravitational case @xcite . in these works , the rp values where calculated through a rather cumbersome local expansion of the ( @xmath0-multipole ) green s function . the application of this technique to more general orbits appears a challenging task . in a recent letter @xcite , the joint groups of barack and ori ( bo ) and mino , nakano , and sasaki ( mns ) devised an alternative , more direct method for obtaining the rp . the new method is based on a multipole decomposition of the explicit `` direct '' part of the force ( see below ) . using this method , bo and mns were able to calculate the explicit rp values for both the scalar and gravitational self forces , for any geodesic orbit in schwarzschild spacetime . in a preceding paper @xcite ( hereafter referred to as `` paper i '' ) bo described the full details of the new calculation technique , as applied to the toy - model of the _ scalar _ self force acting on a scalar charge . the current paper deals with the more interesting case of the _ gravitational _ self force on a mass particle , and provides full details of the rp derivation in this case . in addition , we shall derive here the rp values for the _ electromagnetic _ self force acting on an electrically charged particle orbiting a schwarzschild black hole . ( bo and mns applied two slightly different methods in obtaining the rp ; mns describe their calculation in @xcite . ) the analysis presented in this paper relies greatly on the technique and results of paper i , to which we shall frequently refer the reader . though the basic idea of our calculation is the same as in the scalar toy model of paper i , some unavoidable technical complexities arise when coming to consider the gravitational or electromagnetic cases . in particular , one then has to consider an extension of the particle s four - velocity ( which takes part in constructing the `` direct force''see below ) off the worldline , and address the question of the rp dependence on the ( non - unique ) choice of such extension . another , more fundamental issue , is the gauge dependence of the gravitational self force and its implication to the mode sum scheme ( see ref . @xcite ) . most of our manuscript will concern with the ( most interesting ) gravitational case . our analytical technique is easily applicable to the ( simpler ) electromagnetic case , which we shall later consider in a separate section . the structure of this paper is as follows : in the rest of this introductory section we set up the physical scenario of a pointlike mass particle orbiting a schwarzschild black hole , introduce mst - qw s prescription for calculating the gravitational self force on this particle , and review the basics of the mode - sum method . in sec . [ secii ] we present mst s expression for the direct part of the gravitational self force , and analytically process this expression to extract the information relevant for deriving the rp . section [ seciii ] contains the heart of our calculation , namely , the derivation of all rp for any geodesic orbit , in the gravitational case . section [ secv ] deals with the electromagnetic case . in sec . [ secvi ] we summarize the prescription for calculating the gravitational and electromagnetic self forces via the mode - sum method , and give some concluding remarks . throughout this paper we use geometrized units ( with @xmath1 ) , metric signature @xmath2 , and the standard schwarzschild coordinates @xmath3 . we consider a pointlike particle of mass @xmath4 , moving freely in the vacuum exterior of a schwarzschild black hole with mass @xmath5 . ( qw @xcite discuss the extent to which the concept of a pointlike particle makes sense in the context of the radiation reaction problem . ) in the limit @xmath6 , the particle traces a geodesic @xmath7 of the schwarzschild background . due to angular momentum conservation , the geodesic orbit ( as well as the orbit under self - force effect ) is confined to a plain , which , without loss of generality , we shall take as the equatorial plain , @xmath8 . when the mass @xmath4 is finite , the particle no longer moves on a geodesic . in this case , it is useful to view the particle as being subject to a self force induced by its own gravitational field ( treated as a perturbation over the background geometry ) . the particle s equation of motion thus takes the form @xmath9 where @xmath10 , a semicolon denotes covariant differentiation with respect to the background geometry , and @xmath11 describes the leading - order self - force effect . in the following we shall consider the self force acting on the particle at an arbitrary point along its worldline , denoted by @xmath12 ( in our setup @xmath13 ) . we shall use the notation @xmath14 to represent a point in the neighborhood of @xmath15 . we will denote the metric of the perturbed spacetime as @xmath16 , where @xmath17 is the ( schwarzschild ) background metric and @xmath18 is the metric perturbation induced by the particle . following mst - qw , we consider the metric perturbation @xmath19 specifically in the harmonic gauge . we shall denote by @xmath20 the trace - reversed perturbation : @xmath21 mst and qw found that the gravitational self force on a particle freely moving in a vacuum spacetime can be formally constructed as @xcite @xmath22 where @xmath23 is the `` tail '' force , associated with the mere effect of waves scattered _ inside _ ( rather than propagating along ) the particle s past light cone . the tail force can be derived from the `` tail '' part of the metric perturbation , as defined by mst @xcite , through @xmath24 here , the tensor @xmath25 is any ( sufficiently regular ) extension of the tensor @xmath26 defined at @xmath27 , where @xmath28 and @xmath29 refer to the values of the four - velocity and the metric tensor at @xmath15 . [ later we shall employ a specific extension of @xmath30 ; note that the choice of extension does not affect the physical self force @xmath31 , though , obviously , it does affect the field @xmath32 off the worldline . ] the ( singular ) difference between the `` full '' perturbation @xmath33 and the tail part @xmath34 is associated with the instantaneous effect of waves propagating directly along the particle s light cone . this part is referred to as the `` direct '' perturbation : @xmath35 correspondingly , we define the `` direct '' force as @xmath36 defining also the `` full '' force , @xmath37 we then have @xmath38 the explicit form of the direct perturbation has been derived by mst @xcite ( see also @xcite ) . it is given below in eq.([ii-10 ] ) , and serves as the starting point for our analysis . note that both the direct force and the full force , which were defined above as vector fields in the neighborhood of @xmath15 , diverge as @xmath39 . however , their difference , yielding the tail force , admits a perfectly regular limit @xmath39 , which , according to mst - qw , represents the physical self force . in this respect , notice also the freedom one has in choosing the extension @xmath25 , as long as this extension is regular enough and reduces to @xmath40 in the limit @xmath39 . one has to make sure , though , that _ the same extension @xmath25 _ is applied to both the direct and the full forces . the mode - sum method was previously introduced @xcite as a practical method for calculating the mst - qw self force given in eq . ( [ i-30 ] ) @xcite . the method is reviewed in paper i ; here we merely describe the basic prescription ( as applied to the gravitational case ) and introduce the relevant notation . in the mode - sum scheme , one first formally expands the gravitational tail force , as well as the full and direct forces , into multipole @xmath0-modes , in the form @xmath41 here , precisely as in the scalar case , the modes @xmath42 , @xmath43 , and @xmath44 are obtained by decomposing ( each of the vectorial components of ) the corresponding quantities @xmath23 , @xmath45 , and @xmath46 into standard scalar spherical harmonics , and then , for any given multipole number @xmath0 , summing over all azimuthal numbers @xmath47 . it is important to emphasize here that the various @xmath0-modes introduced in eq . ( [ i-80 ] ) are defined in our scheme through a _ scalar _ harmonic decomposition . in this regard , recall that the ( full ) metric perturbation in schwarzschild spacetime is usually decomposed into _ harmonic modes in actual calculations . the construction of the full - force scalar - harmonic modes @xmath43 from the full perturbation tensor - harmonic modes can be prescribed in a straightforward manner ( as , e.g. , in @xcite ) . the basic prescription for constructing the gravitational self force via the mode - sum scheme is given by @xcite @xmath48 -d^{\alpha},\ ] ] where @xmath49 and the ( @xmath0-independent ) coefficients @xmath50 , @xmath51 , @xmath52 , and @xmath53 are the _ regularization parameters _ the rp @xmath50 , @xmath51 , and @xmath52 may be defined by the demand that the sum in eq . ( [ i-90 ] ) would converge . equivalently ( and more practically ) , one may define these parameters by requiring convergence of the sum @xmath54\equiv d^{\alpha}.\ ] ] this sum then defines the fourth parameter , @xmath53 . from the above definitions it is clear that the rp values may be derived through analysis of the direct force modes @xmath55 . ( [ i-90 ] ) constitutes a practical prescription for constructing the gravitational self force , given ( i ) the values of all necessary rp , and ( ii ) the full - force modes @xmath43 . in this paper we derive all rp for any ( equatorial ) geodesic orbit in schwarzschild spacetime , hence setting an analytical basis for calculations of the gravitational self force for all such orbits .

we obtain all `` regularization parameters '' ( rp ) needed for calculating the gravitational and electromagnetic self forces for an arbitrary geodesic orbit around a schwarzschild black hole . these rp values are required for implementing the previously introduced mode - sum method , which allows a practical calculation of the self force by summing over contributions from individual multipole modes of the particle s field . in the gravitational case , we provide here full details of the analytic method and results briefly reported in a recent letter [ phys . rev . lett . * 88 * , 091101 ( 2002 ) ] . in the electromagnetic case , the rp are obtained here for the first time .

we obtain all `` regularization parameters '' ( rp ) needed for calculating the gravitational and electromagnetic self forces for an arbitrary geodesic orbit around a schwarzschild black hole . these rp values are required for implementing the previously introduced mode - sum method , which allows a practical calculation of the self force by summing over contributions from individual multipole modes of the particle s field . in the gravitational case , we provide here full details of the analytic method and results briefly reported in a recent letter [ phys . rev . lett . * 88 * , 091101 ( 2002 ) ] . in the electromagnetic case , the rp are obtained here for the first time .

gr-qc0603056

i

inspiralling compact binaries of arbitrary mass ratio moving in _ quasi - circular _ orbits are the most plausible sources of gravitational radiation for the first generation ground - based interferometric detectors @xcite . the availability of highly accurate general relativistic theoretical waveforms required to extract the weak gw signals from the noise - dominated interferometric data is the main reason for the above understanding . the dynamics of long lived and isolated compact binaries can be modelled accurately in the pn approximation to general relativity as point particles moving in quasi - circular orbits . the pn approximation allows one to express the equations of motion of a compact binary as corrections to the newtonian equations of motion in powers of @xmath2 , where @xmath3 , @xmath4 , and @xmath5 are the characteristic orbital velocity , the total mass , and the typical orbital separation of the binary , respectively . recently , the orbital evolution of nonspinning compact binaries in quasi - circular orbits , under the action of general relativity , was computed up to the 3.5pn order in ref . the amplitude corrections to the gw polarizations @xmath0 and @xmath1 are also available to the 2.5pn order @xcite . however , a recent surge in astrophysically motivated investigations indicates that compact binaries of arbitrary mass ratio moving in inspiralling _ eccentric _ orbits are also plausible sources of gravitational radiation _ even _ for the ground - based gw interferometers . one of the earliest scenarios involves kozai oscillations , associated with hierarchical triplets that may be present in globular clusters @xcite . last year , it was pointed out that during the late stages of black hole neutron star inspiral the binary can become eccentric @xcite . this is because in general the neutron star is not disrupted at the first phase of mass transfer and what remains of the neutron star is left on a wider eccentric orbit from where it again inspirals back to the black hole . this scenario was very recently invoked to explain the light curve of the short gamma - ray burst grb @xmath6 @xcite . another scenario , reported in _ nature _ , suggests that at least partly short grbs are produced by the merger of binaries , formed in globular clusters by exchange interactions involving compact objects @xcite . a distinct feature of such binaries is that they have high eccentricities at short orbital separation [ see fig . 2 in ref . compact binaries that merge with some residual eccentricities may be present in galaxies too . chaurasia and bailes demonstrated that a natural consequence of an asymmetric kick imparted to neutron stars at birth is that the majority of binaries should possess highly eccentric orbits @xcite . further , the observed deficit of highly eccentric short - period binary pulsars was attributed to selection effects in pulsar surveys . the authors also pointed out that their conclusions are applicable to and binaries . yet another scenario that can create inspiralling eccentric binaries with short periods involves compact star clusters . it was noted that the interplay between gw - induced dissipation and stellar scattering in the presence of an intermediate - mass black hole can create short - period highly eccentric binaries @xcite . finally , a very recent attempt to model realistically compact clusters that are likely to be present in galactic centers indicates that compact binaries usually merge with eccentricities @xcite . these above mentioned scenarios force us to claim that compact binaries in inspiralling eccentric orbits are plausible sources of gravitatinal waves _ even _ for the ground - based gw interferometers . in order to do _ astrophysics _ with the proposed space - based gw interferometers , lisa @xcite , bbo @xcite , and decigo @xcite , it is required to have highly accurate gw polarizations , @xmath0 and @xmath1 , from compact binaries of arbitrary mass ratio moving in inspiralling eccentric orbits . recall , the earlier discussions also indicate that stellar - mass compact binaries in eccentric orbits are excellent sources for lisa . furthermore , it is expected that lisa will `` hear '' gravitational waves from intermediate - mass black holes moving in highly eccentric orbits @xcite . finally , several papers which appeared recently in the _ arxiv _ indicate that supermassive black - hole binaries , formed from galactic mergers , may coalesce with orbital eccentricity @xcite . it is interesting to note that these investigations employ different techniques and astrophysical scenarios to reach the above conlusion . the above mentioned astrophysically inspired investigations motivated us to extend the phasing formalism , developed and implemented with 2.5pn accuracy in ref . @xcite , to the next pn order , namely , the 3.5pn order . the phasing formalism provides a method to construct , almost analytically , templates for compact binaries of arbitrary mass ratio moving in inspiralling eccentric orbits . we recall that accurate templates for the detection of gravitational waves require _ phasing _ , i.e. , an accurate mathematical modelling of the continous time evolution of the gw polarizations . in the case of inspiralling eccentric binaries , the above modelling requires the combination of three different time scales present in the dynamics , namely , those associated with the radial motion ( orbital period ) , advance of periastron , and radiation reaction , without treating radiation reaction in an adiabatic mannner . in ref . @xcite , an improved _ method of variation of constants _ was presented to combine these three time scales and to obtain the phasing at the 2.5pn order . we note that the techniques adapted in ref . @xcite were influenced by the mathematical formulation , developed by damour @xcite , that gave the ( heavily employed ) accurate relativistic _ timing formula _ for binary pulsars @xcite . it is possible to extend the phasing to the 3.5pn order , mainly because of the recent determination of the 3pn accurate generalized quasi - keplerian parametric solution to the conservative dynamics of nonspinning compact binaries of arbitrary mass ratio moving in eccentric orbits @xcite . this parametrization , presented in ref . @xcite , allows one to solve analytically the 3pn accurate conservative dynamics of nonspinning compact binaries , computed both in adm - type coordinates @xcite and in harmonic coordinates @xcite , indicating the deterministic nature of the underlying dynamics @xcite . further , we recall that ref . @xcite extends the quasi - keplerian parametrization developed by damour and his collaborators @xcite , which is crucial to construct the timing formula relevant for relativistic binary pulsars @xcite . this observation clearly reveals the link , as envisaged by damour , connecting gw observations of inspiralling compact binaries to the timing of binary pulsars . in ref . @xcite , explicit computations to realize the phasing at the 2.5pn order were done in adm coordinates as at that time the 2pn accurate generalized quasi - keplerian parametrization , required by the method of variation of constants , was only available in adm coordinates . however , in this paper , computations required for the phasing at the 3.5pn order are done in harmonic coordinates . harmonic coordinates are preferred as computations that lead to ready to use search templates for compact binaries in quasi - circular orbits are usually performed in harmonic gauge @xcite . this paper has the following plan . in sec . [ phasing : phasingsec ] , we outline the procedure , detailed in ref . @xcite , to perform the phasing . section [ phasing : analex3.5pnsec ] provides explicit formulae required for the 3.5pn accurate phasing , which also include 3.5pn accurate equations for the secular and periodic variations of the orbital elements involved in the phasing . the pictorial representation of the main results and the related discussions are presented in sec . [ phasing : sec_visualization ] . finally , in sec . [ phasing : sec_conclusions ] , we give a brief summary and point out possible extensions . appendices [ phasing : appendix : vmu ] and [ phasing : appendix : pnadiabaticsec ] deal with computational details and some supplementary results .

d * 70 * , 064028 ( 2004 ) ] , and the 3pn accurate generalized quasi - keplerian parametric solution to the conservative dynamics of nonspinning compact binaries moving in eccentric orbits , available in [ r .- m . astrophysics _ with the proposed space - based gw interferometers like lisa , bbo , and decigo .

we obtain an efficient description for the dynamics of nonspinning compact binaries moving in inspiralling eccentric orbits to implement the phasing of gravitational waves from such binaries at the 3.5 post - newtonian ( pn ) order . our computation heavily depends on the phasing formalism , presented in [ t. damour , a. gopakumar , and b. r. iyer , phys . rev . d * 70 * , 064028 ( 2004 ) ] , and the 3pn accurate generalized quasi - keplerian parametric solution to the conservative dynamics of nonspinning compact binaries moving in eccentric orbits , available in [ r .- m . memmesheimer , a. gopakumar , and g. schfer , phys . rev . d * 70 * , 104011 ( 2004 ) ] . the gravitational - wave ( gw ) polarizations @xmath0 and @xmath1 with 3.5pn accurate phasing should be useful for the earth - based gw interferometers , current and advanced , if they plan to search for gravitational waves from inspiralling eccentric binaries . our results will be required to do _ astrophysics _ with the proposed space - based gw interferometers like lisa , bbo , and decigo .

gr-qc0603056

c

let us recapitulate . in this paper , we have incorporated the 3pn accurate conservative and the 1pn accurate reactive dynamics in harmonic coordinates into the phasing formalism to the 3.5pn order as a natural extension of the work presented in ref . this extension was possible due to the very recent determination of the 3pn accurate generalized quasi - keplerian parametrization for the conservative orbital motion of nonspinning compact binaries in eccentric orbits @xcite . we applied the method of ref . @xcite to construct , almost analytically , templates for gw signals emitted by compact binaries moving in inspiralling and slowly precessing _ eccentric _ orbits . an improved method of variation of arbitrary constants , explained in great detail in ref . @xcite , allowed us to combine the three different but relevant time scales , namely , those associated with the radial motion ( orbital period ) , advance of periastron , and radiation reaction , to the 3.5pn order without making the usual approximation of treating adiabatically the radiative time scale . in this context , we recall that the two - scale decomposition helped us to model accurately and efficiently the time evolution of the associated dynamical variables . we employed harmonic coordinates in this paper as calculations that provided search templates for compact binaries in quasi - circular orbits usually employ the harmonic gauge . the explicit computations provided in this paper will be required to construct accurate and efficient search templates for gravitational waves from compact binaries of arbitrary mass ratio moving in inspiralling eccentric orbits . our detailed calculations will have to be employed , if the earth - based gw interferometers plan to search for gravitational waves from compact binaries with residual eccentricities , motivated by a plethora of recent astrophysical investigations @xcite . the proposed space - based gw interferometers like lisa , bbo , and decigo will have to depend on our results to do astrophysics . it is interesting to note that our results will be required by lisa to search for gravitational waves from stellar - mass , intermediate - mass , and supermassive black - hole binaries as these binaries will likely to be in inspiralling eccentric orbits . another area where our computations can be quite effective will be the early stages of extreme mass ratio inspiral ( emri ) as relevant for lisa . our current results should be also useful to benchmark efforts that are required to obtain reliable emri templates @xcite . there are many avenues that will require detailed investigations in the near future and we list only a few of them below . in this paper , the conservative dynamics was restricted to compact binaries consisting of nonspinning point masses . naturally , it is desirable to include spin effects into our computations . a first step in this direction was taken in ref . @xcite , where the 3pn accurate generalized quasi - keplerian parametrization for the conservative dynamics of spinning compact binaries , moving in eccentric orbits , when the spin effects are restricted to the leading - order spin - orbit interaction , is presented . we also neglected , for simplicity , explicit pn corrections to the gw polarization amplitudes of @xmath0 and @xmath1 , and restricted them to their leading quadrupolar order . however , it is possible to obtain 2pn accurate corrections to these amplitudes , using refs . in order to make the numerical implementation of our computations more efficient and accurate , it is also desirable to provide better ways of solving the 3pn accurate kepler equation . another line of investigation should deal with a extension of these computations so that we have a dependable description for the orbital evolution near the lso . finally , these templates naturally trigger lots of data analysis investigations relevant for both ground - based and space - based gw interferometers . many of the above mentioned issues are currently under investigation . it is our pleasure to thank t. damour , b. r. iyer , and g. schfer for illuminating discussions and persistent encouragements . we are grateful to m. tessmer for carfully checking the typed equations . this work is supported by the deutsche forschungsgemeinschaft ( dfg ) through sfb / tr7 `` gravitationswellenastronomie '' . the algebraic computations , appearing in this paper , were performed using maple and mathematica .

we obtain an efficient description for the dynamics of nonspinning compact binaries moving in inspiralling eccentric orbits to implement the phasing of gravitational waves from such binaries at the 3.5 post - newtonian ( pn ) order . d * 70 * , 104011 ( 2004 ) ] . the gravitational - wave ( gw ) polarizations @xmath0 and @xmath1 with 3.5pn accurate phasing should be useful for the earth - based gw interferometers , current and advanced , if they plan to search for gravitational waves from inspiralling eccentric binaries . our results will be required to do _

we obtain an efficient description for the dynamics of nonspinning compact binaries moving in inspiralling eccentric orbits to implement the phasing of gravitational waves from such binaries at the 3.5 post - newtonian ( pn ) order . our computation heavily depends on the phasing formalism , presented in [ t. damour , a. gopakumar , and b. r. iyer , phys . rev . d * 70 * , 064028 ( 2004 ) ] , and the 3pn accurate generalized quasi - keplerian parametric solution to the conservative dynamics of nonspinning compact binaries moving in eccentric orbits , available in [ r .- m . memmesheimer , a. gopakumar , and g. schfer , phys . rev . d * 70 * , 104011 ( 2004 ) ] . the gravitational - wave ( gw ) polarizations @xmath0 and @xmath1 with 3.5pn accurate phasing should be useful for the earth - based gw interferometers , current and advanced , if they plan to search for gravitational waves from inspiralling eccentric binaries . our results will be required to do _ astrophysics _ with the proposed space - based gw interferometers like lisa , bbo , and decigo .

hep-ph9904510

i

a solution to the gauge hierarchy , based on extra spacial dimensions , was recently proposed by arkani - hamed , dimopoulos and dvali @xcite . they assumed the space - time is @xmath2 dimensional , with the standard model ( sm ) particles living on a brane . while the electromagnetic , strong , and weak forces are confined to this brane , gravity can propagate in the extra dimensions . to solve the gauge hierarchy problem they proposed the `` new '' planck scale @xmath3 is of the order of tev with very large extra dimensions . the size @xmath4 of these extra dimensions can be as large as 1 mm , which corresponds to a compactification scale @xmath5 as low as @xmath6 ev . the usual planck scale @xmath7 gev is related to this effective planck scale @xmath3 using the gauss s law : @xmath8 where @xmath9 is the number of extra dimensions . for @xmath10 it gives a large value for @xmath4 , which is already ruled out by gravitational experiments . on the other hand , @xmath11 gives @xmath12 mm , which is in the margin beyond the reach of present gravitational experiments . the graviton including its excitations in the extra dimensions can couple to the sm particles on the brane with an effective strength of @xmath13 ( instead of @xmath14 ) after summing the effect of all excitations collectively , and thus the gravitation interaction becomes comparable in strength to weak interaction at tev scale . hence , it can give rise to a number of phenomenological activities testable at existing and future colliders @xcite . so far , studies show that there are two categories of signals : direct and indirect . the indirect signal refers to exchanges of gravitons in the intermediate states , while direct refers to production or associated production of gravitons in the final state . indirect signals include fermion pair , gauge boson pair production , correction to precision variables , etc . there are also other astrophysical and cosmological signatures and constraints @xcite . among the constraints the cooling of supernovae by radiating gravitons places the strongest limit on the effective planck scale @xmath3 of order 50 tev for @xmath11 , which renders collider signatures for @xmath11 uninteresting . thus , we concentrate on @xmath15 . in this work , we perform a global analysis of the lepton - quark neutral current data on the low scale gravity model . the global data include hera neutral current deep - inelastic scattering , drell - yan production at the tevatron , and total hadronic , @xmath16 and @xmath17 pair cross sections at lepii . in addition , we also include the leptonic cross sections @xmath18 at lepii in our analysis . the @xmath19-n scattering data from ccfr and nutev have been shown by rizzo @xcite to be very insignificant in constraining the low scale gravity , and so we shall not include this data set in our analysis . we shall see that the drell - yan production , due to the large invariant mass data , provides the strongest constraint among the global data . by combining all data , the effective planck scale @xmath3 must be larger than about 1.12 tev for @xmath0 and 0.94 tev for @xmath1 at 95%cl . this is our main result . the organization of the paper is as follows . in the next section , we shall describe each set of data used in our global analysis and derive the effect of the low scale gravity . in sec . iii , we give the numerical results and interpretations for our fits , from which we can draw the limits on the effective planck scale .

we perform a global analysis of the lepton - quark neutral current data on the low scale gravity model , which arises from the extra dimensions . the global data include hera neutral current deep - inelastic scattering , drell - yan production at the tevatron , and fermion pair production at lepii . the drell - yan production , due to the large invariant mass data , provides the strongest constraint . combining all data , the effective planck scale must be larger than about 1.12 tev for @xmath0 and 0.94 tev for @xmath1 at 95%cl . date : global lepton - quark neutral current constraint on low scale gravity model + 0.7 cm kingman cheung + _ department of physics , university of california , davis , ca 95616 usa _

we perform a global analysis of the lepton - quark neutral current data on the low scale gravity model , which arises from the extra dimensions . the global data include hera neutral current deep - inelastic scattering , drell - yan production at the tevatron , and fermion pair production at lepii . the drell - yan production , due to the large invariant mass data , provides the strongest constraint . combining all data , the effective planck scale must be larger than about 1.12 tev for @xmath0 and 0.94 tev for @xmath1 at 95%cl . date : global lepton - quark neutral current constraint on low scale gravity model + 0.7 cm kingman cheung + _ department of physics , university of california , davis , ca 95616 usa _

astro-ph0609725

i

the importance of the oort constants is in their simple relation to the galactic potential , in the case of vanishing random motions . the circular orbits have velocity @xmath256 . if we could find the causes for the deviations , @xmath157 and @xmath156 , from the true " values , @xmath0 and @xmath1 , then we would provide a direct constraint on the galactic potential . in this paper we have investigated the effect of spiral structure on the measurements of the oc @xmath0 , @xmath1 , @xmath2 , and @xmath3 . we have performed test - particle simulations with an initially cold or hot stellar disk and an imposed two - armed spiral density wave perturbation . variations of simulated measurements of the oc with pattern speed , galactic azimuth , and sample depth have been explored . we find that systematic errors due to the presence of spiral structure _ are _ likely to affect the measurements of the oort constants . moderate strength spiral structure causes errors of order 5 km / s in @xmath0 and @xmath1 . axisymmetric , high velocity dispersion disks also yield errors in the simulated measurements of oort s @xmath0 ( as a result of the asymmetric drift ) , but they are smaller , of order 2 km / s ( see [ sec : axi_hot ] ) . if the sun is located near the corotation resonance then , regardless of the phase angle , we would measure @xmath169 and thus get no information about the spiral structure . if , in addition , we constrain @xmath175 , or @xmath257 , all oc would have values within the current measurement error . as the lindblad resonances are neared , @xmath2 varies strongly with phase angle and has an increased value . in [ sec : sample_depth ] we investigated the effect of sample depth on the measurements of the oc . we found that for an initially cold disk , spiral structure can give rise to marked variations of all oc with the average heliocentric distance of the sample . for @xmath0 and @xmath1 this results from an oscillating average @xmath203 , whereas @xmath2 is sensitive to variations in the radial velocity and its gradient . we find that for phase angles placing the sun near the convex arm negative values for the axisymmetric drift are possible for low velocity dispersion stars . unlike the @xmath18 induced asymmetric drift in a hot axisymmetric disk , in a cold disk it is the spiral structure that causes it . it is possible the reason for never observing @xmath223 could be our proximity to the concave spiral arm . our result for the variation of @xmath2 with velocity dispersion is distinctly different than the observational measurement of @xmath2 done by o&d . whereas in our simulations the absolute value of @xmath2 decreases with increasing velocity dispersion , the opposite trend is observed in fig . 6 by o&d . in the same paper the authors suggest that it is possible that the galactic bar is responsible for this behavior . since orbits change orientation at the 2:1 olr of the bar , at this location the bar is expected to most strongly distort the local kinematics . as discussed by o&d , stars from inside the olr should produce @xmath258 . if the sun s location is just outside the olr then we would sample more stars giving rise to negative @xmath2 with increasing sample depth . to test this possibility , o&d analyzed only stars brighter than @xmath259 which yielded a decrease in the phase mixing " corrected value of @xmath2 from @xmath260 to @xmath261 km / s . another way to try to explain it is to consider the combined effect of spiral structure and bar perturbations . other possibilities are the effects from minor mergers , or those due to a triaxial halo @xcite . future work should aim at understanding this unusual behavior for @xmath2 . we would like to thank jason nordhaus for helpful comments . support for this work was in part provided by national science foundation grant asst-0406823 , and the national aeronautics and space administration under grant no . nng04gm12 g issued through the origins of solar systems program . lccccc [ fig : cont_u00 ] & @xmath262 & @xmath263 & 0 & 0.8 + [ fig : cont_u40 ] & @xmath262 & @xmath263 & 40 & 0.8 + [ fig : o06](solid / dashed ) & @xmath262 & 0.6 & 0/40 & 0.8 + [ fig : o07](solid / dashed ) & @xmath262 & 0.7 & 0/40 & 0.8 + [ fig : o10](solid / dashed ) & @xmath262 & 1.0 & 0/40 & 0.8 + [ fig : o07_19](solid / dashed ) & @xmath264 & 0.7 & 0/40 & @xmath265 + [ fig : o07_45](solid / dashed ) & @xmath266 & 0.7 & 0/40 & @xmath265 + [ fig : o10_45](solid / dashed ) & @xmath266 & 1.0 & 0/40 & @xmath265 + [ fig : v_vs_r](top / mid / bottom ) & @xmath264/@xmath266/@xmath266 & 0.7/0.7/1.0 & 0 &

we get relations between the fourier coefficients and some galactic parameters , such as the phase angle of the solar neighborhood and the spiral pattern speed . we show that systematic errors due to the presence of spiral structure are likely to affect the measurements of the oort constants . moderate strength spiral structure causes errors of order 5 km / s / kpc in @xmath0 and @xmath1 . we find variations of the fourier coefficients with velocity dispersion , pattern speed , and sample depth . for a sample at an average heliocentric distance of 0.8 kpc we can summarize our findings as follows : ( i ) if our location in the galaxy is near corotation then we expect a vanishing value for @xmath2 for all phase angles ; ( ii ) for a hot disk , spiral structure induced errors for all oort constants vanish at , and just inward of the corotation radius ; ( iii ) as one approaches the 4:1 lindblad resonances @xmath4 increases and so does its variation with galactic azimuth ; ( iv ) for all simulations @xmath4 , on average , is larger for lower stellar velocity dispersions , contrary to recent measurements .

we perform test - particle simulations in a 2d , differentially rotating stellar disk , subjected to a two - armed steady state spiral density wave perturbation in order to estimate the influence of spiral structure on the local velocity field . by using levenberg - marquardt least - squares fit we decompose the local velocity field ( as a result of our simulations ) into fourier components to fourth order . thus we obtain simulated measurements of the oort constants , @xmath0 , @xmath1 , @xmath2 , and @xmath3 . we get relations between the fourier coefficients and some galactic parameters , such as the phase angle of the solar neighborhood and the spiral pattern speed . we show that systematic errors due to the presence of spiral structure are likely to affect the measurements of the oort constants . moderate strength spiral structure causes errors of order 5 km / s / kpc in @xmath0 and @xmath1 . we find variations of the fourier coefficients with velocity dispersion , pattern speed , and sample depth . for a sample at an average heliocentric distance of 0.8 kpc we can summarize our findings as follows : ( i ) if our location in the galaxy is near corotation then we expect a vanishing value for @xmath2 for all phase angles ; ( ii ) for a hot disk , spiral structure induced errors for all oort constants vanish at , and just inward of the corotation radius ; ( iii ) as one approaches the 4:1 lindblad resonances @xmath4 increases and so does its variation with galactic azimuth ; ( iv ) for all simulations @xmath4 , on average , is larger for lower stellar velocity dispersions , contrary to recent measurements .

astro-ph0409689

i

in x - rays , obscured agn may be classified into _ compton - thin _ and _ compton - thick _ , according to the column of absorbing matter covering the active nucleus . the threshold corresponds to a column density @xmath4 @xmath3 . the fact that compton - thick seyfert 2s are a substantial fraction of the whole population of seyfert 2 galaxies , maybe as high as 50% ( risaliti et al . 1999 ) , suggests that the covering fraction of the absorbing matter is large . if a single absorber covers a steady - state active nucleus , the classification of individual objects is not expected to be time - dependent . a review on the observational properties of compton - thick seyfert 2 galaxies has been recently published by comastri ( 2004 ) . _ bona fide _ compton - thick seyfert 2 galaxies are observed in x - rays also at energies lower than the photoelectric cut - off . this x - ray emission is probably due to reprocessing of the nuclear emission by compton - thick matter surrounding the nucleus @xcite , and/or by hot plasma in the nuclear environment @xcite . we define hereafter _ reprocessing - dominated _ seyfert 2 galaxies those , whose x - ray emission in the xmm - newton energy band ( @xmath5 kev ) is dominated by reprocessing . the common wisdom so far has been to * identify reprocessing - dominated seyferts with compton - thick agn*. however , very recently transitions between `` compton - thin '' and `` compton - thick '' spectral states have been serendipitously discovered in a few x - ray bright seyfert 2 galaxies ( matt et al . 2003b , and references therein ) . in ugc 4203 , for instance ( guainazzi et al . 2001 ; ohno et al . 2004 ) , an xmm - newton observation detected a bright ( 210 kev flux @xmath6 erg @xmath3 s@xmath1 ) agn , with a low - energy photoelectric cutoff ( corresponding to @xmath7 @xmath3 ) . in asca observations , performed about six years earlier , the weaker continuum and the huge k@xmath8 fluorescent iron line ( equivalent width , @xmath9 kev ) can be instead best explained if the spectrum is dominated by the compton echo of an otherwise invisible nuclear emission . such transitions have been observed in both directions , and are normally accompanied by substantial changes in the observed 210 kev flux . this discovery stimulates some fundamental questions on the nature of reprocessing - dominated seyfert 2 galaxies . these transitions could be due in principle to a change of the intervening absorption . alternatively , seyfert 2 x - ray spectral states dominated by reprocessing may represent phases of low- or totally absent activity in the life of an active nucleus , as observed , for instance , in ngc 4051 ( guainazzi et al . 1998 ) , ngc 2992 ( gilli et al . 2000 ) , and ngc 6300 ( guainazzi 2002 ) . in these cases , the observed transitions require a change by at least one order of magnitude of the nuclear activity level . transitions between `` compton - thin '' and `` compton - thick '' spectral states have been observed in 4 seyfert 2 galaxies so far ( see matt et al . 2003b , and references therein ) , out of about 40 objects for which multiple x - ray spectroscopic measurements are available ( bassani et al . 1999 ; risaliti et al . 2001 ) . however , the `` parent sample '' is neither homogeneous , nor complete , being substantially biased toward brighter ( and therefore less absorbed ) objects ( see the discussion in risaliti et al . 1999 ) . we are carrying on a xmm - newton survey of an optically defined and complete - albeit small - sample of seyfert galaxies , classified as compton - thick according to observations prior to the launch of _ chandra _ and xmm - newton . the primary goal of this study is to determine the rate of transmission- " ( _ i.e. _ compton - thin ) to reprocessing - dominated " transitions , and their typical timescale on the soundest possible statistical basis . this rate might be related to the duty - cycle of the active galactic nuclei ( agn ) phenomenon , at least in the local universe , if these transitions are due to large changes of the overall x - ray agn energy output @xcite . the results of this survey are the main subject of this paper .

we present _ chandra _ and xmm - newton observations of a small sample ( 11 objects ) of optically - selected seyfert 2 galaxies , for which asca and bepposax had suggested compton - thick obscuration of the active nucleus ( agn ) . this indicates a typical occurrence rate of at least @xmath00.02 years@xmath1 . these transitions could be due to large changes of the obscuring gas column density , or to a transient dimming of the agn activity , the latter scenario being supported by detailed analysis of the best studied events . galaxies : active galaxies : nuclei galaxies : seyfert x - rays : galaxies

we present _ chandra _ and xmm - newton observations of a small sample ( 11 objects ) of optically - selected seyfert 2 galaxies , for which asca and bepposax had suggested compton - thick obscuration of the active nucleus ( agn ) . the main goal of this study is to estimate the rate of transitions between `` transmission- '' and `` reprocessing - dominated '' states . we discover one new transition in ngc 4939 , with a possible additional candidate in ngc 5643 . this indicates a typical occurrence rate of at least @xmath00.02 years@xmath1 . these transitions could be due to large changes of the obscuring gas column density , or to a transient dimming of the agn activity , the latter scenario being supported by detailed analysis of the best studied events . independently of the ultimate mechanism , comparison of the observed spectral dynamics with monte - carlo simulations demonstrates that the obscuring gas is largely inhomogeneous , with multiple absorbing components possibly spread through the whole range of distances from the nucleus between a fraction of parsecs up to several hundreds parsecs . as a by - product of this study , we report the first measurement ever of the column density covering the agn in ngc 3393 ( @xmath2 @xmath3 ) , and the discovery of soft x - ray extended emission , apparently aligned along the host galaxy main axis in ngc 5005 . the latter object hosts most likely an historically misclassified low - luminosity compton - thin agn . galaxies : active galaxies : nuclei galaxies : seyfert x - rays : galaxies

astro-ph0409689

c

the main result of this paper is the estimate of the occurrence rate of transmission- " to reprocessing - dominated " state transitions , on the most unbiased and complete existing sample of compton - thick seyfert 2 galaxies ( cf . [ fig9 ] ) . we have discovered 1 ( new ) transition out of a sample of 10 _ bona - fide _ compton - thick objects , with an average time span between pre- and post xmm - newton and _ chandra _ launch observations of about 5 years . the statistics is still too small to determine anything more accurate than an order - of - magnitude estimate for the occurrence rate . bearing this caveat in mind , it seems that once or twice every century we might be forced to change our x - ray absorption classification for each highly obscured agn . with respect to the mechanism responsible for these transitions , our results are consistent with the discussion in matt et al . ( 2003b ) . although an explanation in terms of varying line - of - sight column density can not be ruled out , the fact that in the best studied cases these transitions are associated with large ( @xmath8210 ) fluctuations of the agn x - ray output suggests that they are due to a change of the optical path through which we observe the nucleus . for the transition specifically discussed in this paper - ngc 4939 - the factor of 2 variation of the observed 210 kev band flux hides a larger variation of the agn intrinsic power , as its true luminosity in the reprocessing - dominated state is unknown . if this is the correct interpretation , the transition occurrence rate translates immediately into a duty - cycle of the agn phenomenon in the local universe . independently of the ultimate mechanism responsible for these transitions , comparison of their spectral properties with monte - carlo simulations demonstrates that obscuring gas in absorbed agn can not be distributed in a space- or time- homogeneous structure . again , a compact but inhomogeneous torus " can not be ruled out . however , there is mounting evidence that gas in regions of intense star formation and dust in the host galaxy play a major role , and might be ultimately responsible for the bulk of compton - thin x - ray absorption in agn .

independently of the ultimate mechanism , comparison of the observed spectral dynamics with monte - carlo simulations demonstrates that the obscuring gas is largely inhomogeneous , with multiple absorbing components possibly spread through the whole range of distances from the nucleus between a fraction of parsecs up to several hundreds parsecs . as a by - product of this study , we report the first measurement ever of the column density covering the agn in ngc 3393 ( @xmath2 @xmath3 ) , and the discovery of soft x - ray extended emission , apparently aligned along the host galaxy main axis in ngc 5005 . the latter object hosts most likely an historically misclassified low - luminosity compton - thin agn .

we present _ chandra _ and xmm - newton observations of a small sample ( 11 objects ) of optically - selected seyfert 2 galaxies , for which asca and bepposax had suggested compton - thick obscuration of the active nucleus ( agn ) . the main goal of this study is to estimate the rate of transitions between `` transmission- '' and `` reprocessing - dominated '' states . we discover one new transition in ngc 4939 , with a possible additional candidate in ngc 5643 . this indicates a typical occurrence rate of at least @xmath00.02 years@xmath1 . these transitions could be due to large changes of the obscuring gas column density , or to a transient dimming of the agn activity , the latter scenario being supported by detailed analysis of the best studied events . independently of the ultimate mechanism , comparison of the observed spectral dynamics with monte - carlo simulations demonstrates that the obscuring gas is largely inhomogeneous , with multiple absorbing components possibly spread through the whole range of distances from the nucleus between a fraction of parsecs up to several hundreds parsecs . as a by - product of this study , we report the first measurement ever of the column density covering the agn in ngc 3393 ( @xmath2 @xmath3 ) , and the discovery of soft x - ray extended emission , apparently aligned along the host galaxy main axis in ngc 5005 . the latter object hosts most likely an historically misclassified low - luminosity compton - thin agn . galaxies : active galaxies : nuclei galaxies : seyfert x - rays : galaxies

1006.4901

i

x - ray observations of edge - on spiral galaxies revealed the existence of hot gas at temperatures of @xmath6 10@xmath7 k extending a few kpc beyond the disk ( e.g. @xcite ) . the origin of energy and material in such a hot halo has not been clarified . feedback from supernovae ( sne ) as galactic wind or fountain and heated primordial gas are possible candidates @xcite . in any cases , halo gas plays important roles in galactic evolution through chemical circulation and interaction between galaxies and the intergalactic medium . the hot gaseous halo in and around the milky - way has been investigated for a long time . for instance , rosat all sky survey ( rass ) quantitatively mapped the spatial distribution of the soft x - ray background emission ( sxb ; @xcite ) . the cosmic x - ray background ( cxb ) component extrapolated from the discrete hard x - ray sources could explain only about half of the sxb , leaving the soft x - ray emission below 1 kev being of a diffuse origin . with the high resolution x - ray microcalorimeter flying on a sounding rocket , @xcite detected emission lines of hydrogen- and helium - like oxygen , neon , and iron ions from about 1 steradian of the sky , which suggests that the emitting gas is of a thermal nature and at temperatures of t@xmath8 k. the existence of the hot gas in and around the milky - way is consistent with the _ chandra _ observations of nearby edge - on spiral galaxies . however , because these emission data carry very little distance information , the properties of the global hot gas , like its density , temperature , and their distributions , are still poorly understood . a combined analysis of high resolution absorption and emission data provides us with a powerful diagnostic of properties of the absorbing / emitting plasma . absorption lines measure the column density of the absorbing material , which is an integration of the density of the absorbing ions along a sight line . in contrast , emission line intensity is sensitive to the emission measure , which is proportional to the density square of the emitting plasma . thus , a combination of the emission and absorption data naturally yields the density and the size of the corresponding absorbing / emitting gas . with significantly improved spectral resolution of current x - ray instruments , we are now able to observe the needed high resolution absorption and emission lines produced in the hot plasma . for instance , the x - ray absorption lines at @xmath9 , in particular the helium- and hydrogen - like o and o lines , are detected in spectra of many galactic and extragalactic sources ( e.g. @xcite ) . recently , @xcite and @xcite find that the o absorption line can always be detected in an agn spectrum as long as the spectrum is of high signal - to - noise ratio . on the other hand , the x - ray imaging spectrometer ( xis ) aboard _ suzaku _ can also resolve emission lines produced in a diffuse emitting plasma at temperatures of t@xmath8 k. and indeed , the o and o lines have been detected in nearly all directions ( e.g. , @xcite ) . recently , a systematical study of emission lines of the hot gas in and around the galaxy has been conducted by @xcite , who report the o and o lines in 14 blank sky observations with the xis and conclude that the line - of - sight mean temperatures of the emitting gas has a narrow distribution around @xmath10 k. since the ion fractions of o and o and their k - transition emissivities are very sensitive to gas temperature at @xmath11 k , a combined analysis of these emission and absorption lines will also constrain the gas temperature and its distribution without the complexity of relative chemical abundances of metal elements . although this combined analysis method has long been applied in the ultraviolet wavelength band @xcite , its application in the x - ray band just began . complementing the high resolution absorption data observed with _ chandra _ with the broadband emission data obtained with rass , @xcite firstly attempted to conduct the combined analysis in the x - ray band to infer the hot gas properties in our galaxy . they also proposed a model for the galactic disk assuming the temperature and density of the hot gas fading off exponentially along the vertical direction . they concluded that the o and o absorption lines observed along the mrk 421 sight line are consistent with the galactic disk origin . @xcite further constrained this disk model by jointly analyzing the high resolution absorption data obtained with _ chandra _ along the lmc x-3 sight line and emission data observed with _ suzaku _ in the vicinity of the sight line . they estimated gas temperature and density at the galactic plane and their scale heights as 3.6 ( + 0.8 , @xmath120.7 ) @xmath13 k and 1.4 ( + 2.0 , @xmath121.0 ) @xmath14 @xmath3 and 1.4 ( + 3.8 , @xmath121.2 ) kpc and 2.8 ( + 3.6 , @xmath121.8 ) kpc , respectively . these results are consistent with the early findings by @xcite , i.e. , the sxb can be explained by a kpc - scale halo around our galaxy . in this paper , we present the second case study of the combined analysis of high resolution absorption and emission lines . the absorption lines are observed with _ chandra _ along a blazer , pks 2155304 sight line and the emission lines are obtained with _ suzaku _ observations of the vicinity of the sight line . in section 2 , we describe our observations and data reduction process . we perform our data analysis in section 3 and discuss our results in section 4 .

we present a detailed spectroscopic study of the hot gas in the galactic halo toward the direction of a blazer pks 2155 - 304 ( @xmath00.117 ) . the o and o absorption lines are measured with the low and high energy transmission grating spectrographs aboard _ chandra _ , and the o , o , and ne emission lines produced in the adjacent field of the pks 2155 - 304 direction are observed with the x - ray imaging spectrometer aboard _ suzaku_. assuming vertically exponential distributions of the gas temperature and the density , we perform a combined analysis of the absorption and emission data .

we present a detailed spectroscopic study of the hot gas in the galactic halo toward the direction of a blazer pks 2155 - 304 ( @xmath00.117 ) . the o and o absorption lines are measured with the low and high energy transmission grating spectrographs aboard _ chandra _ , and the o , o , and ne emission lines produced in the adjacent field of the pks 2155 - 304 direction are observed with the x - ray imaging spectrometer aboard _ suzaku_. assuming vertically exponential distributions of the gas temperature and the density , we perform a combined analysis of the absorption and emission data . the gas temperature and density at the galactic plane are determined to be @xmath1 k and @xmath2 @xmath3 and the scale heights of the gas temperature and density are @xmath4 kpc and @xmath5 kpc , respectively . these values are consistent with those obtained in the lmc x-3 direction .

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we have analyzed high resolution x - ray absorption / emission data observed by _ chandra _ and _ suzaku _ to determine the physical state of the global hot gas along the pks 2155 - 304 direction . 1 . suzaku clearly detected o k@xmath28 , o k@xmath28 and o k@xmath29 lines . the surface brightnesses of o and o in this direction can be understood in the same scheme as obtained by other 14 observations ( @xcite ) . 2 . by the absorption analysis , column density is measured as 3.9 ( @xmath244 ) @xmath3 pc and temperature is measured as 1.91 ( @xmath245 ) @xmath13 k. by the emission analysis , emission measure is measured as 3.0 ( @xmath246 ) @xmath14 @xmath119 pc and temperature is measured as 2.14 ( @xmath247 ) @xmath248 k. 3 . combined analysis using the exponential disk model gives a good fit with @xmath45/dof of 789.65/756 to both emission and absorption spectra . the gas temperature and density at the galactic plane are determined to be @xmath249 k and @xmath2 @xmath3 and the scale heights of the gas temperature and density @xmath250 kpc and @xmath251 kpc , respectively . 4 . the results obtained by the combined analysis are consistent with those for the lmc x-3 direction . this suggest that the global hot gas surrounding our galaxy has common structure . part of this work was financially supported by grant - in - aid for scientific research ( kakenhi ) by mext , no . 20340041 , 20340068 , and 20840051 . th appreciates the support from the jsps research fellowship and the global coe program `` the physical sciences frontier '' , mext , japan anders , e. , & grevesse , n. 1989 , geochim . cosmo chim . acta , 53 , 197 berkhuijsen , e. m. , haslam , c. g. t. , & salter , c. j. 1971 , , 14 , 252 bregman , j. n. , & lloyd - davies , e. j. 2007 , , 669 , 990 cox , d. p. 2005 , , 43 , 337 fang , t. , mckee , c.f . , canizares , c.r . , wolfire , m. 2006 , , 644 , 174 ferrire , k. 1998 , , 497 , 759 fujimoto , r. , et al . 2007 , , 59 , s133 futamoto , k. , mitsuda , k. , takei , y. , fujimoto , r. , & yamasaki , n. y. 2004 , , 605 , 793 henley , d. b. , shelton , r. l. , & kuntz , k. d. 2007 , , 661 , 304 ishisaki , y. , et al . 2007 , , 59 , 113 kalberla , p. m. w. , burton , w. b. , hartmann , d. , arnal , e. m. , bajaja , e. , morras , r. , p&oumlppel , w. g. l. 2005 , , 440 , 775 kharchenko , v. , rigazio , m. , dalgarno , a. , & krasnopolsky , v. a. 2003 , , 585 , l73 koutroumpa , d. , acero , f. , lallement , r. , ballet , j. , & kharchenko , v. 2007 , a&a , 475 , 901 koyama , k. , et al . 2007 , , 59 , 23 lallement , r. , raymond , j.c . , vallerga , j. , lemoine , m. , dalaudier , f. , & vertaux , j.l . 2004 , a&a , 426 , 875 li , j .- , li , z. , wang , q. d. , irwin , j. a. , & rossa , j. 2008 , , 390 , 59 masui , k. , mitsuda , k. , yamasaki , n. y. , takei , y. , kimura , s. , yoshino , t. , & mccammon , d. 2009 , , 61 , 115 mccammon , d. , 2002 , , 576 , 188 mitsuda , k. , et al . 2007 , , 59 , 1 norman , c. a. , & ikeuchi , s. 1989 , , 345 , 372 sembach , k.r , savage , b.d.m tripp , t.d . 1997 , , 480 , 216 shelton , r. l. , shallmen , s. m. , & jenkins , e. b. 2007 , , 659 , 365 shull , j. m. , & slavin , j. d. 1994 , , 427 , 784 smith , r. k. , 2007 , , 59 , s141 snowden , s. l. , egger , r. , freyberg , m. j. , mccammon , d. , plucinsky , p.p . , sanders , w.t . , schmitt , j.h.m.m . , trmper , j. , & voges , w. 1997 , , 485 , 125 strickland , d. k. , heckman , t. m. , colbert , e. j. m. , hoopes , c. g. , & weaver , k. a. 2004 , , 151 , 193 sutherland , r. s. , & dopita , m. a. 1993 , , 88 , 253 tawa , n. et al , 2008 , , 60 , s22 williams , r. j. , mathur , s. , nicastro , f. , & elvis , m. 2007 , , 665 , 247 wang , q.d . , immler , s. , walterbos , r. , lauroesch , j. t , breitschwerdt , d. 2001 , , 555 , 99 wang , q.d . , chaves , t. , irwin , j.d . 2003 , , 598 , 969 yamasaki , n. y. , sato , k. , mitsuishi , i. , & ohashi , t. 2009 , , 61 , 291 yao , y. , & wang , q. d. , 2005 , , 624 , 751 yao , y. , & wang , q. d. , 2007 , , 658 , 1088 yao , y. , wang , q. d. , hagihara , t. , mitsuda , k. , mccammon , d. , & yamasaki , n. y. 2009 , , 690 , 143 yoshino , t. , et al . 2009 , , 61 , 805

the gas temperature and density at the galactic plane are determined to be @xmath1 k and @xmath2 @xmath3 and the scale heights of the gas temperature and density are @xmath4 kpc and @xmath5 kpc , respectively . these values are consistent with those obtained in the lmc x-3 direction .

we present a detailed spectroscopic study of the hot gas in the galactic halo toward the direction of a blazer pks 2155 - 304 ( @xmath00.117 ) . the o and o absorption lines are measured with the low and high energy transmission grating spectrographs aboard _ chandra _ , and the o , o , and ne emission lines produced in the adjacent field of the pks 2155 - 304 direction are observed with the x - ray imaging spectrometer aboard _ suzaku_. assuming vertically exponential distributions of the gas temperature and the density , we perform a combined analysis of the absorption and emission data . the gas temperature and density at the galactic plane are determined to be @xmath1 k and @xmath2 @xmath3 and the scale heights of the gas temperature and density are @xmath4 kpc and @xmath5 kpc , respectively . these values are consistent with those obtained in the lmc x-3 direction .

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`` kerckhoffs principle '' @xcite and shannon s assumption `` the enemy knows the system '' @xcite established the basis for modern cryptography and enhanced secure communication between two parties . with the proposal of the `` one time pad '' @xcite , the security aspect shifted from secure communication to secure key distribution between these two parties . quantum key distribution ( qkd ) , first proposed 1984 @xcite , offers a way to exchange a secret key using the quantum mechanical properties of light as the carrier of information . the security is thereby based on fundamental physical concepts . first proof of principle experiments for qkd @xcite were followed by practical implementations over long and extremely long distances @xcite . in parallel to these discrete - variable qkd systems , continuous - variable qkd using homodyne detection was proposed @xcite . it was shown , that the limit of 3db channel attenuation can be overcome by the concept of postselection @xcite and the postprocessing method reverse reconciliation @xcite . continuous - variable qkd has been tested on quantum channels of up to 25 km length @xcite using homodyne detection and basis switching . besides using a single homodyne detection , also simultaneous detection of both conjugate quadratures of the signal was demonstrated @xcite . homodyne detection of conjugate quadratures referred to as heterodyne detection is particularly interesting for three reasons : * random numbers are not needed in the receiver s setup . * the trojan - horse attack @xcite , where eve gains information by reading the basis choice in bob s setup , is not possible . * the heterodyne detection strategy achieves higher secure bit rates than schemes with homodyne detection in some qkd protocols @xcite . experiments using heterodyne detection on a long fiber channel , however , had not yet been demonstrated . in this paper , we present a fiber - based qkd - system using a double - homodyne detection setup . as in previous experiments @xcite , we use binary encoded continuous - variable quantum states consisting of a signal mode and a local oscillator mode . we adapt our previous polarization - based experiments to a fiber channel . to this end , our two mode states are sent through the quantum channel using a combination of time @xcite and polarization multiplexing @xcite of signal and local oscillator ( lo ) . therefore , detrimental effects from photon - phonon interactions ( gawbs ) are avoided @xcite . by describing the sent quantum information in the stokes space @xcite , it is possible to verify effective entanglement in the measurement data according to the method in @xcite . in contrast to all previous experiments , not only the signal but also the strong reference beam ( lo ) is considered in this security analysis . we show how to measure conjugate stokes parameters with a freely drifting interferometric phase . the phase drift is monitored by additional classical calibration pulses on the quantum channel . subsequently , bob remaps his measurement data , similar to @xcite . finally , monitoring the intensity of the local oscillator at the detection stage allows us to unambiguously demonstrate the generation of quantum - correlated data . the paper is organized as follows . in section [ protocol ] , we introduce our protocol and the stokes formalism . in section [ experiment ] , we describe the setup focusing on the implementation of the detection part . in section [ verification ] , noise characteristics of the system and the transmitted signal states are presented . finally , the entanglement criterion is applied .

, a quantum signal of two non - orthogonal weak optical coherent states is sent through a fiber - based quantum channel . c. shannon , `` communication theory of secrecy systems , '' the bell system technical journal * 28 * , 656715 ( 1949 ) . g. vernam , `` cipher printing telegraph systems for secret wire and radio telegraphic communications , '' j. amer . quantum cryptography : public key distribution and coin tossing , '' proceedings of ieee international conference on computers systems and signal processing , bangarore india pp . 175179 ( 1984 ) . c. bennett , f. bessette , g. brassard , l. salvail , and j. smolin , `` experimental quantum cryptography , '' journal of cryptology * 5 * , 328 ( 1992 ) . a. ekert , j. rarity , p. tapster , and g. palma , `` practical quantum cryptography based on 2-photon interferometry , '' phys . a. muller , j. breguet , and n. gisin , `` experimental demonstration of quantum cryptography using polarized photons in optical - fiber over more than 1 km , '' europhys . d. stucki , n. gisin , o. guinnard , g. ribordy , and h. zbinden , `` quantum key distribution over 67 km with a plug&play system , '' new j. phys . d. rosenberg , j. w. harrington , p. r. rice , p. a. hiskett , c. g. peterson , r. j. hughes , a. e. lita , s. w. nam , and j. e. nordholt , `` long - distance decoy - state quantum key distribution in optical fiber , '' phys . r. ursin , f. tiefenbacher , t. schmitt - manderbach , h. weier , t. scheidl , m. lindenthal , b. blauensteiner , t. jennewein , j. perdigues , p. trojek , b. mer , m. frst , m. meyenburg , j. rarity , z. sodnik , c. barbieri , h. weinfurter , and a. zeilinger , `` entanglement - based quantum communication over 144 km , '' nat . phys . * 3 * , 481486 ( 2007 ) . t. schmitt - manderbach , h. weier , m. frst , r. ursin , f. tiefenbacher , t. scheidl , j. perdigues , z. sodnik , c. kurtsiefer , j. g. rarity , a. zeilinger , and h. weinfurter , `` experimental demonstration of free - space decoy - state quantum key distribution over 144 km , '' phys . * 98 * , 010504 ( 2007 ) . t. c. ralph , `` continuous variable quantum cryptography , '' phys . f. grosshans , g. v. assche , j. wenger , r. brouri , n. j. cerf , and p. grangier , `` quantum key distribution using gaussian - modulated coherent states , '' nature * 421 * , 238241 ( 2003 ) . j. lodewyck , m. bloch , r. garcia - patron , s. fossier , e. karpov , e. diamanti , t. debuisschert , n. j. cerf , r. tualle - brouri , s. w. mclaughlin , and p. grangier , `` quantum key distribution over 25 km with an all - fiber continuous - variable system , '' phys . a * 76 * , 04230510 ( 2007 ) . b. qi , l. huang , l. qian , and h. lo , `` experimental study on the gaussian - modulated coherent - state quantum key distribution over standard telecommunication fibers , '' phys . s. lorenz , n. korolkova , and g. leuchs , `` continuous - variable quantum key distribution using polarization encoding and post selection , '' appl . . a. m. lance , t. symul , v. sharma , c. weedbrook , t. c. ralph , and p. k. lam , `` no - switching quantum key distribution using broadband modulated coherent light , '' phys . n. gisin , s. fasel , b. kraus , h. zbinden , and g. ribordy , `` trojan - horse attacks on quantum - key - distribution systems , '' phys . s. pirandola , s. mancini , s. lloyd , and s. l. braunstein , `` continuous - variable quantum cryptography using two - way quantum communication , '' nat . phys . * 4 * , 726730 ( 2008 ) . c. weedbrook , a. m. lance , w. p. bowen , t. symul , t. c. ralph , and p. k. lam , `` coherent - state quantum key distribution without random basis switching , '' phys j. lodewyck and p. grangier , `` tight bound on the coherent - state quantum key distribution with heterodyne detection , '' phys . d. elser , t. bartley , b. heim , c. wittmann , d. sych , and g. leuchs , `` feasibility of free space quantum key distribution with coherent polarization states , '' new j. phys . * 11 * , 045014 ( 2009 ) h. hseler , t. moroder , and n. ltkenhaus , `` testing quantum devices : practical entanglement verification in bipartite optical systems , '' phys . . lett . * 15 * , 17461748 ( 2003 ) . c. h. bennett , `` quantum cryptography using any two nonorthogonal states , '' phys . y. zhao , m. heid , j. rigas , and n. ltkenhaus , `` asymptotic security of binary modulated continuous - variable quantum key distribution under collective attacks , '' phys . m. curty , m. lewenstein , and n. ltkenhaus , `` entanglement as a precondition for secure quantum key distribution , '' phys . lett . * 92 * , 217903 ( 2004 ) . c. h. bennett , g. brassard , and n. d. mermin , `` quantum cryptography without bell s theorem , '' phys . j. rigas , o. ghne , and n. ltkenhaus , `` entanglement verification for quantum - key - distribution systems with an underlying bipartite qubit - mode structure , '' phys . u. leonhardt , _ measuring the quantum state of light _ ( cambridge university press , 1997 ) . m. legr ' e , h. zbinden , and n. gisin , `` implementation of continuous variable quantum cryptography in optical fibres using a go-&-return configuration , '' quantum inf . j. shapiro and s. wagner , `` phase and amplitude uncertainties in heterodyne detection , '' ieee j. quantum electron . * 20 * , 803813 ( 1984 ) . h. bachor and t. ralph , _ a guide to experiments in quantum optics _

we present a fiber - based continuous - variable quantum key distribution system . in the scheme , a quantum signal of two non - orthogonal weak optical coherent states is sent through a fiber - based quantum channel . the receiver simultaneously measures conjugate quadratures of the light using two homodyne detectors . from the measured q - function of the transmitted signal , we estimate the attenuation and the excess noise caused by the channel . the estimated excess noise originating from the channel and the channel attenuation including the quantum efficiency of the detection setup is investigated with respect to the detection of effective entanglement . the local oscillator is considered in the verification . we witness effective entanglement with a channel length of up to @xmath0 . 10 a. kerckhoffs , _ la cryptographie militaire _ ( journal des sciences militaires , vol . ix , pp . 5 - 38 , 1883 ) . c. shannon , `` communication theory of secrecy systems , '' the bell system technical journal * 28 * , 656715 ( 1949 ) . g. vernam , `` cipher printing telegraph systems for secret wire and radio telegraphic communications , '' j. amer . inst . elect . eng . p. 109 ( 1926 ) . c. bennett and g. brassard , `` quantum cryptography : public key distribution and coin tossing , '' proceedings of ieee international conference on computers systems and signal processing , bangarore india pp . 175179 ( 1984 ) . c. bennett , f. bessette , g. brassard , l. salvail , and j. smolin , `` experimental quantum cryptography , '' journal of cryptology * 5 * , 328 ( 1992 ) . a. ekert , j. rarity , p. tapster , and g. palma , `` practical quantum cryptography based on 2-photon interferometry , '' phys . rev . lett . * 69 * , 12931295 ( 1992 ) . a. muller , j. breguet , and n. gisin , `` experimental demonstration of quantum cryptography using polarized photons in optical - fiber over more than 1 km , '' europhys . lett . * 23 * , 383388 ( 1993 ) . d. stucki , n. gisin , o. guinnard , g. ribordy , and h. zbinden , `` quantum key distribution over 67 km with a plug&play system , '' new j. phys . * 4 * , 41 ( 2002 ) . d. rosenberg , j. w. harrington , p. r. rice , p. a. hiskett , c. g. peterson , r. j. hughes , a. e. lita , s. w. nam , and j. e. nordholt , `` long - distance decoy - state quantum key distribution in optical fiber , '' phys . rev . lett . * 98 * , 10503 ( 2007 ) . r. ursin , f. tiefenbacher , t. schmitt - manderbach , h. weier , t. scheidl , m. lindenthal , b. blauensteiner , t. jennewein , j. perdigues , p. trojek , b. mer , m. frst , m. meyenburg , j. rarity , z. sodnik , c. barbieri , h. weinfurter , and a. zeilinger , `` entanglement - based quantum communication over 144 km , '' nat . phys . * 3 * , 481486 ( 2007 ) . t. schmitt - manderbach , h. weier , m. frst , r. ursin , f. tiefenbacher , t. scheidl , j. perdigues , z. sodnik , c. kurtsiefer , j. g. rarity , a. zeilinger , and h. weinfurter , `` experimental demonstration of free - space decoy - state quantum key distribution over 144 km , '' phys . rev . lett . * 98 * , 010504 ( 2007 ) . t. c. ralph , `` continuous variable quantum cryptography , '' phys . rev . a * 61 * , 010303 ( 1999 ) . c. silberhorn , t. c. ralph , n. ltkenhaus , and g. leuchs , `` continuous variable quantum cryptography : beating the 3 db loss limit , '' phys . rev . lett . * 89 * , 167901 ( 2002 ) . f. grosshans , g. v. assche , j. wenger , r. brouri , n. j. cerf , and p. grangier , `` quantum key distribution using gaussian - modulated coherent states , '' nature * 421 * , 238241 ( 2003 ) . j. lodewyck , m. bloch , r. garcia - patron , s. fossier , e. karpov , e. diamanti , t. debuisschert , n. j. cerf , r. tualle - brouri , s. w. mclaughlin , and p. grangier , `` quantum key distribution over 25 km with an all - fiber continuous - variable system , '' phys . rev . a * 76 * , 04230510 ( 2007 ) . b. qi , l. huang , l. qian , and h. lo , `` experimental study on the gaussian - modulated coherent - state quantum key distribution over standard telecommunication fibers , '' phys . rev . a * 76 * , 0523239 ( 2007 ) . s. lorenz , n. korolkova , and g. leuchs , `` continuous - variable quantum key distribution using polarization encoding and post selection , '' appl . phys . b * 79 * , 273277 ( 2004 ) . a. m. lance , t. symul , v. sharma , c. weedbrook , t. c. ralph , and p. k. lam , `` no - switching quantum key distribution using broadband modulated coherent light , '' phys . rev . lett . * 95 * , 1805034 ( 2005 ) . n. gisin , s. fasel , b. kraus , h. zbinden , and g. ribordy , `` trojan - horse attacks on quantum - key - distribution systems , '' phys . rev . a * 73 * , 0223206 ( 2006 ) . s. pirandola , s. mancini , s. lloyd , and s. l. braunstein , `` continuous - variable quantum cryptography using two - way quantum communication , '' nat . phys . * 4 * , 726730 ( 2008 ) . c. weedbrook , a. m. lance , w. p. bowen , t. symul , t. c. ralph , and p. k. lam , `` coherent - state quantum key distribution without random basis switching , '' phys . rev . a * 73 * , 0223169 ( 2006 ) . j. lodewyck and p. grangier , `` tight bound on the coherent - state quantum key distribution with heterodyne detection , '' phys . rev . a * 76 * , 0223328 ( 2007 ) . d. elser , t. bartley , b. heim , c. wittmann , d. sych , and g. leuchs , `` feasibility of free space quantum key distribution with coherent polarization states , '' new j. phys . * 11 * , 045014 ( 2009 ) . d. elser , c. wittmann , u. l. andersen , o. glckl , s. lorenz , c. marquardt , and g. leuchs , `` guided acoustic wave brillouin scattering in photonic crystal fibers , '' j. phys . conf . ser . * 92 * , 012108 ( 2007 ) . n. korolkova , g. leuchs , r. loudon , t. c. ralph , and c. silberhorn , `` polarization squeezing and continuous - variable polarization entanglement , '' phys . rev . a * 65 * , 052306 ( 2002 ) . h. hseler , t. moroder , and n. ltkenhaus , `` testing quantum devices : practical entanglement verification in bipartite optical systems , '' phys . rev . a * 77 * , 03230311 ( 2008 ) . c. dorrer , d. kilper , h. stuart , g. raybon , and m. raymer , `` linear optical sampling , '' ieee photonics technol . lett . * 15 * , 17461748 ( 2003 ) . c. h. bennett , `` quantum cryptography using any two nonorthogonal states , '' phys . rev . lett . * 68 * , 3121 ( 1992 ) . y. zhao , m. heid , j. rigas , and n. ltkenhaus , `` asymptotic security of binary modulated continuous - variable quantum key distribution under collective attacks , '' phys . rev . a * 79 * , 01230714 ( 2009 ) . m. curty , m. lewenstein , and n. ltkenhaus , `` entanglement as a precondition for secure quantum key distribution , '' phys . rev . lett . * 92 * , 217903 ( 2004 ) . c. h. bennett , g. brassard , and n. d. mermin , `` quantum cryptography without bell s theorem , '' phys . rev . lett . * 68 * , 557 ( 1992 ) . j. rigas , o. ghne , and n. ltkenhaus , `` entanglement verification for quantum - key - distribution systems with an underlying bipartite qubit - mode structure , '' phys . rev . a * 73 * , 0123416 ( 2006 ) . u. leonhardt , _ measuring the quantum state of light _ ( cambridge university press , 1997 ) . m. legr ' e , h. zbinden , and n. gisin , `` implementation of continuous variable quantum cryptography in optical fibres using a go-&-return configuration , '' quantum inf . comput . * 6 * , 326335 ( 2006 ) . j. a. nelder and r. mead , `` a simplex method for function minimization , '' the computer journal * 7 * , 308313 ( 1965 ) . j. shapiro and s. wagner , `` phase and amplitude uncertainties in heterodyne detection , '' ieee j. quantum electron . * 20 * , 803813 ( 1984 ) . s. stenholm , `` simultaneous measurement of conjugate variables , '' ann . phys . * 218 * , 233254 ( 1992 ) . u. leonhardt and h. paul , `` realistic optical homodyne measurements and quasi - probability distributions , '' phys . rev . a * 48 * , 45984604 ( 1993 ) . h. hansen , t. aichele , c. hettich , p. lodahl , a. lvovsky , j. mlynek , and s. schiller , `` ultrasensitive pulsed , balanced homodyne detector : application to time - domain quantum measurements , '' opt . lett . * 26 * , 17141716 ( 2001 ) . u. leonhardt , j. a. vaccaro , b. bhmer , and h. paul , `` canonical and measured phase distributions , '' phys . rev . a * 51 * , 84 ( 1995 ) . h. bachor and t. ralph , _ a guide to experiments in quantum optics _ ( wiley - vch verlag , 2004 ) .

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r

in this section , we first describe alice s and bob s optical hardware . we then separately discuss the detection scheme and finally explain the control software . the optical setup of our qkd - system is shown in fig . [ fig : setup ] . the alice module consists of a diode laser ( _ slt5411 _ from _ sumitomo electronic industries _ as used in @xcite ) pulsed by a self - made pulsed current supply . the laser pulses are approximately 100ns long and have a wavelength of 1549.3 nm . the line width is 6.6ghz at -10db of optical power and the coherence time is estimated with self - homodyning to be 0.2ns . the laser pulses are split asymmetrically in the lo and the signal arm . the smaller fraction is used for the signal preparation . the signal arm consists of a delay fiber , a mach - zehnder modulator for amplitude modulation , a monitor detector , and an optical attenuator . this results in a shot noise limited weak signal at the single photon level . in the second fiber beamsplitter ( bs ) the lo pulses and the signal pulses are spatially combined with a 500ns time shift . additionally , the polarization of the pulses is chosen orthogonal . the last component in the alice setup is a computer controlled polarization controller pre - compensating the slow polarization drift in the fiber channel . in the bob module the signal is demultiplexed with a polarizing beamsplitter ( pbs ) . we control the second port of the pbs with a physical block to ensure the second input mode is in a vacuum state . the lo passes a delay fiber , while the signal is directly sent to the free - space detection setup . a monitor diode behind a highly reflective mirror measures the lo energy pulse by pulse . the polarization control is set such that the power on the monitor diode is maximized . finally the signal is measured with our detection scheme shown in ( fig . [ fig : setup ] ( right ) ) . the detection system in fig . [ fig : setup ] ( right ) consists of two homodyne detectors detecting two conjugate quadratures of the signal mode simultaneously . this was first investigated in @xcite . our scheme consists of free - space optics and therefore allows for easy and lossless manipulations of the polarization . the lo s polarization is then chosen to be circular . the signal s polarization is tilted by 45@xmath31 with respect to h and v polarization . both beams interfere on a polarization independent 50:50 beam splitter with acute angle of incidence . for the h - polarized component , we label the relative phase between the signal and the bright lo @xmath32 , where @xmath33 originates from interferometer drifts in sender and receiver modules . the phase shift of @xmath34 between two orthogonally polarized lo components results in a relative phase for the v - components of @xmath35 . both beams propagate to a pbs , which separates the h- and v - polarization . the reflected v - components impinge on the first homodyne detector ( hd1 ) , while the transmitted h - components impinge on the second homodyne detector ( hd2 ) . the difference of the photo currents is recorded . commonly , homodyne detectors are treated as quadrature detectors . we calculate the photon number difference @xmath36 detected by hd1 using the linearized field operators @xmath37 and @xmath38 . we assume that @xmath39 and @xmath40 are real and @xmath41 . additionally , the modes @xmath42 and @xmath43 , the modes orthogonally polarized to signal and lo , are in a vacuum state , i.e. @xmath44 and @xmath45 . the last assumption is justified , since the other input port of the pbs is under bob s control . the detected signal is found after a straightforward calculation to be @xmath46 where @xmath47 is a quadrature operator for mode @xmath48 with a phase @xmath49 . this quadrature measurement is derived analogously for hd2 . it reads @xmath50 the vacuum input @xmath42 at the pbs adds additional 3db noise to the variance of the measurement . therefore our setup is equivalent to a standard heterodyne detection . we do not stabilize the interferometric phase @xmath33 but let it drift freely . however , we have an inherent stabilization of the relative phase of @xmath51 . therefore two random but conjugate quadratures are measured with hd1 and hd2 . l ( a ) lissajous figure of a phase randomized signal is measured for different settings of the qwp in the setup . if the measured quadratures @xmath52 and @xmath53 are not orthogonal , the shape of the graph will be elliptical . we demonstrate that orthogonal quadratures are measured for the correct qwp angle ( orange trace ) . ( b ) the phase is estimated from blocks of calibration pulses . the figure shows the standard deviation of the phase drift between different calibration blocks.,title="fig:",width=196 ] ( a ) lissajous figure of a phase randomized signal is measured for different settings of the qwp in the setup . if the measured quadratures @xmath52 and @xmath53 are not orthogonal , the shape of the graph will be elliptical . we demonstrate that orthogonal quadratures are measured for the correct qwp angle ( orange trace ) . ( b ) the phase is estimated from blocks of calibration pulses . the figure shows the standard deviation of the phase drift between different calibration blocks.,title="fig:",width=287 ] + ( a)(b ) + the simultaneous measurement of two conjugate quadratures depends strongly on the proper choice of the polarization of signal and lo in the detection setup . for balancing , a linearly polarized lo is equally split to both homodyne detectors . a weak signal beam is then sent into the detection scheme . the quadrature measurements of 4000 signals are averaged and the mean values are plotted in the two - dimensional measurement space of fig . [ fig : detection](a ) . phase drifts of the interferometric phase will result in elliptical or circular graphs , depending on the angle of the quarter wave plate ( qwp ) in the lo path , corresponding to largely correlated measurements ( elliptical ) and uncorrelated measurements ( circular ) . it is easy to show , that by turning the qwp , two quadratures with arbitrary relative angle can be measured . we desire uncorrelated measurements ( orange trace in fig . [ fig : detection](a ) ) . in the following , we describe the electronic hardware , the control software and the steps in the postprocessing . the alice electronics is essentially a 14-bit - d / a - converter to prepare the signal with a sampling rate of 20ms / s . one port drives the laser with a pulse rate of 1 mhz . another port produces rectangular pulses for the amplitude modulator . a third port synchronizes bob s experiment with an electronic clock signal at approximately 1khz . the clock could be substituted for a synchronization using the lo monitor diode and calibration pulses as time stamp in future experiments . a quaternary modulation is applied to the amplitude modulator to create the states @xmath54 , @xmath55 , @xmath56 and @xmath57 , where @xmath40 is the signal amplitude and @xmath58 is the amplitude of brighter `` classical '' calibration pulses sent along with the signal . the pulse pattern consists of four calibration pulses followed by 28 signal pulses . to pre - compensate the polarization drift , we inserted the polarization control in alice s setup . an optimal separation of signal and lo is obtained by maximizing the lo power on the monitor diode . the power is maximized either manually or with bob s pc using a simplex method @xcite . this demultiplexing method is very stable . it is furthermore lossless as opposed to a coupler with fixed splitting ratio @xcite . in the following , we describe the electronic circuits . the difference signal in the homodyne detectors is amplified by charge sensitive amplifiers as in the design by @xcite . the electrical pulse duration produced by the detectors is set to 400ns ( foot ) , which allows for repetition rates up to 2mhz while maintaining linear amplification . the linearity was confirmed for all four photodiodes independently . due to limitations of computing power , and an electronic signal due to lo light leaking into the signal arm , we run the experiment at 1mhz . when varying the lo power for balanced homodyne detection of vacuum , we find a linear behavior of the signal variance versus the lo intensity . for typical lo power of @xmath59 , the electronic noise is 20 db below the signals variance . the common mode rejection ratio is always better that 40db . the detection efficiency of the homodyne detectors was 70% , including the quantum efficiency of the diodes ( 86% ) , the mode matching efficiency ( @xmath60 ) and the loss in optical components ( 10% ) . bob s 12-bit - a / d - converter digitizes the signal and the lo monitor detectors with 16ms / s . we reduce the number of samples by neglecting samples in between the pulses and averaging 8 samples ( approximately the electronic pulse length ) . these mean values are used to estimate the shot noise level , as shown in eqn . ( [ s1est ] ) . in the postprocessing , we estimate the mean value of the stokes operators @xmath61 and @xmath62 for 1024 signal states . the displacement with respect to this mean value is considered as quantum signal . long term fluctuations of the detector are thereby compensated . the interferometric phase @xmath33 is estimated with the four bright calibration pulses in each 32-pulse - frame . to measure the phase noise , we calculate the phase drift between two calibration steps . we show the standard deviation of the phase drift in fig . [ fig : detection](b ) . we find that for weak calibration pulses the standard deviation depends on the calibration pulse amplitude . this stems from the limit for the phase estimation of weak coherent states @xcite . for stronger amplitudes , the standard deviation of the phase drift is measured to be 4 degree for calibration times of @xmath63s . with the estimated phase , we remap the coordinate system of the measured frame to the phase space of alice s signal states . subsequently , the data can be analyzed as described in the next section . the computational power needed for the complete postprocessing is high , but at 1mhz repetition rate the system runs continuously in realtime , as required for practical use in a qkd system .

10 a. kerckhoffs , _ la cryptographie militaire _ ( journal des sciences militaires , vol . ix , pp . 5 - 38 , 1883 ) . inst . elect . eng . p. 109 ( 1926 ) . c. bennett and g. brassard , `` rev . lett . * 69 * , 12931295 ( 1992 ) . lett . * 23 * , 383388 ( 1993 ) . * 4 * , 41 ( 2002 ) . rev . lett . * 98 * , 10503 ( 2007 ) . rev . lett . rev . a * 61 * , 010303 ( 1999 ) . c. silberhorn , t. c. ralph , n. ltkenhaus , and g. leuchs , `` continuous variable quantum cryptography : beating the 3 db loss limit , '' phys . rev . lett . * 89 * , 167901 ( 2002 ) . rev . rev . a * 76 * , 0523239 ( 2007 ) . phys . b * 79 * , 273277 ( 2004 ) rev . lett . * 95 * , 1805034 ( 2005 ) . rev . a * 73 * , 0223206 ( 2006 ) . . rev . a * 73 * , 0223169 ( 2006 ) . rev . a * 76 * , 0223328 ( 2007 ) . . d. elser , c. wittmann , u. l. andersen , o. glckl , s. lorenz , c. marquardt , and g. leuchs , `` guided acoustic wave brillouin scattering in photonic crystal fibers , '' j. phys . conf . ser . * 92 * , 012108 ( 2007 ) . n. korolkova , g. leuchs , r. loudon , t. c. ralph , and c. silberhorn , `` polarization squeezing and continuous - variable polarization entanglement , '' phys . rev . a * 65 * , 052306 ( 2002 ) . rev . a * 77 * , 03230311 ( 2008 ) . c. dorrer , d. kilper , h. stuart , g. raybon , and m. raymer , `` linear optical sampling , '' ieee photonics technol rev . lett . * 68 * , 3121 ( 1992 ) . rev . a * 79 * , 01230714 ( 2009 ) . rev . rev . lett . * 68 * , 557 ( 1992 ) . rev . a * 73 * , 0123416 ( 2006 ) . comput . * 6 * , 326335 ( 2006 ) . j. a. nelder and r. mead , `` a simplex method for function minimization , '' the computer journal * 7 * , 308313 ( 1965 ) . s. stenholm , `` simultaneous measurement of conjugate variables , '' ann . phys . * 218 * , 233254 ( 1992 ) . rev . a * 48 * , 45984604 ( 1993 ) . h. hansen , t. aichele , c. hettich , p. lodahl , a. lvovsky , j. mlynek , and s. schiller , `` ultrasensitive pulsed , balanced homodyne detector : application to time - domain quantum measurements , '' opt . lett . * 26 * , 17141716 ( 2001 ) . u. leonhardt , j. a. vaccaro , b. bhmer , and h. paul , `` canonical and measured phase distributions , '' phys . rev . a * 51 * , 84 ( 1995 ) . ( wiley - vch verlag , 2004 ) .

we present a fiber - based continuous - variable quantum key distribution system . in the scheme , a quantum signal of two non - orthogonal weak optical coherent states is sent through a fiber - based quantum channel . the receiver simultaneously measures conjugate quadratures of the light using two homodyne detectors . from the measured q - function of the transmitted signal , we estimate the attenuation and the excess noise caused by the channel . the estimated excess noise originating from the channel and the channel attenuation including the quantum efficiency of the detection setup is investigated with respect to the detection of effective entanglement . the local oscillator is considered in the verification . we witness effective entanglement with a channel length of up to @xmath0 . 10 a. kerckhoffs , _ la cryptographie militaire _ ( journal des sciences militaires , vol . ix , pp . 5 - 38 , 1883 ) . c. shannon , `` communication theory of secrecy systems , '' the bell system technical journal * 28 * , 656715 ( 1949 ) . g. vernam , `` cipher printing telegraph systems for secret wire and radio telegraphic communications , '' j. amer . inst . elect . eng . p. 109 ( 1926 ) . c. bennett and g. brassard , `` quantum cryptography : public key distribution and coin tossing , '' proceedings of ieee international conference on computers systems and signal processing , bangarore india pp . 175179 ( 1984 ) . c. bennett , f. bessette , g. brassard , l. salvail , and j. smolin , `` experimental quantum cryptography , '' journal of cryptology * 5 * , 328 ( 1992 ) . a. ekert , j. rarity , p. tapster , and g. palma , `` practical quantum cryptography based on 2-photon interferometry , '' phys . rev . lett . * 69 * , 12931295 ( 1992 ) . a. muller , j. breguet , and n. gisin , `` experimental demonstration of quantum cryptography using polarized photons in optical - fiber over more than 1 km , '' europhys . lett . * 23 * , 383388 ( 1993 ) . d. stucki , n. gisin , o. guinnard , g. ribordy , and h. zbinden , `` quantum key distribution over 67 km with a plug&play system , '' new j. phys . * 4 * , 41 ( 2002 ) . d. rosenberg , j. w. harrington , p. r. rice , p. a. hiskett , c. g. peterson , r. j. hughes , a. e. lita , s. w. nam , and j. e. nordholt , `` long - distance decoy - state quantum key distribution in optical fiber , '' phys . rev . lett . * 98 * , 10503 ( 2007 ) . r. ursin , f. tiefenbacher , t. schmitt - manderbach , h. weier , t. scheidl , m. lindenthal , b. blauensteiner , t. jennewein , j. perdigues , p. trojek , b. mer , m. frst , m. meyenburg , j. rarity , z. sodnik , c. barbieri , h. weinfurter , and a. zeilinger , `` entanglement - based quantum communication over 144 km , '' nat . phys . * 3 * , 481486 ( 2007 ) . t. schmitt - manderbach , h. weier , m. frst , r. ursin , f. tiefenbacher , t. scheidl , j. perdigues , z. sodnik , c. kurtsiefer , j. g. rarity , a. zeilinger , and h. weinfurter , `` experimental demonstration of free - space decoy - state quantum key distribution over 144 km , '' phys . rev . lett . * 98 * , 010504 ( 2007 ) . t. c. ralph , `` continuous variable quantum cryptography , '' phys . rev . a * 61 * , 010303 ( 1999 ) . c. silberhorn , t. c. ralph , n. ltkenhaus , and g. leuchs , `` continuous variable quantum cryptography : beating the 3 db loss limit , '' phys . rev . lett . * 89 * , 167901 ( 2002 ) . f. grosshans , g. v. assche , j. wenger , r. brouri , n. j. cerf , and p. grangier , `` quantum key distribution using gaussian - modulated coherent states , '' nature * 421 * , 238241 ( 2003 ) . j. lodewyck , m. bloch , r. garcia - patron , s. fossier , e. karpov , e. diamanti , t. debuisschert , n. j. cerf , r. tualle - brouri , s. w. mclaughlin , and p. grangier , `` quantum key distribution over 25 km with an all - fiber continuous - variable system , '' phys . rev . a * 76 * , 04230510 ( 2007 ) . b. qi , l. huang , l. qian , and h. lo , `` experimental study on the gaussian - modulated coherent - state quantum key distribution over standard telecommunication fibers , '' phys . rev . a * 76 * , 0523239 ( 2007 ) . s. lorenz , n. korolkova , and g. leuchs , `` continuous - variable quantum key distribution using polarization encoding and post selection , '' appl . phys . b * 79 * , 273277 ( 2004 ) . a. m. lance , t. symul , v. sharma , c. weedbrook , t. c. ralph , and p. k. lam , `` no - switching quantum key distribution using broadband modulated coherent light , '' phys . rev . lett . * 95 * , 1805034 ( 2005 ) . n. gisin , s. fasel , b. kraus , h. zbinden , and g. ribordy , `` trojan - horse attacks on quantum - key - distribution systems , '' phys . rev . a * 73 * , 0223206 ( 2006 ) . s. pirandola , s. mancini , s. lloyd , and s. l. braunstein , `` continuous - variable quantum cryptography using two - way quantum communication , '' nat . phys . * 4 * , 726730 ( 2008 ) . c. weedbrook , a. m. lance , w. p. bowen , t. symul , t. c. ralph , and p. k. lam , `` coherent - state quantum key distribution without random basis switching , '' phys . rev . a * 73 * , 0223169 ( 2006 ) . j. lodewyck and p. grangier , `` tight bound on the coherent - state quantum key distribution with heterodyne detection , '' phys . rev . a * 76 * , 0223328 ( 2007 ) . d. elser , t. bartley , b. heim , c. wittmann , d. sych , and g. leuchs , `` feasibility of free space quantum key distribution with coherent polarization states , '' new j. phys . * 11 * , 045014 ( 2009 ) . d. elser , c. wittmann , u. l. andersen , o. glckl , s. lorenz , c. marquardt , and g. leuchs , `` guided acoustic wave brillouin scattering in photonic crystal fibers , '' j. phys . conf . ser . * 92 * , 012108 ( 2007 ) . n. korolkova , g. leuchs , r. loudon , t. c. ralph , and c. silberhorn , `` polarization squeezing and continuous - variable polarization entanglement , '' phys . rev . a * 65 * , 052306 ( 2002 ) . h. hseler , t. moroder , and n. ltkenhaus , `` testing quantum devices : practical entanglement verification in bipartite optical systems , '' phys . rev . a * 77 * , 03230311 ( 2008 ) . c. dorrer , d. kilper , h. stuart , g. raybon , and m. raymer , `` linear optical sampling , '' ieee photonics technol . lett . * 15 * , 17461748 ( 2003 ) . c. h. bennett , `` quantum cryptography using any two nonorthogonal states , '' phys . rev . lett . * 68 * , 3121 ( 1992 ) . y. zhao , m. heid , j. rigas , and n. ltkenhaus , `` asymptotic security of binary modulated continuous - variable quantum key distribution under collective attacks , '' phys . rev . a * 79 * , 01230714 ( 2009 ) . m. curty , m. lewenstein , and n. ltkenhaus , `` entanglement as a precondition for secure quantum key distribution , '' phys . rev . lett . * 92 * , 217903 ( 2004 ) . c. h. bennett , g. brassard , and n. d. mermin , `` quantum cryptography without bell s theorem , '' phys . rev . lett . * 68 * , 557 ( 1992 ) . j. rigas , o. ghne , and n. ltkenhaus , `` entanglement verification for quantum - key - distribution systems with an underlying bipartite qubit - mode structure , '' phys . rev . a * 73 * , 0123416 ( 2006 ) . u. leonhardt , _ measuring the quantum state of light _ ( cambridge university press , 1997 ) . m. legr ' e , h. zbinden , and n. gisin , `` implementation of continuous variable quantum cryptography in optical fibres using a go-&-return configuration , '' quantum inf . comput . * 6 * , 326335 ( 2006 ) . j. a. nelder and r. mead , `` a simplex method for function minimization , '' the computer journal * 7 * , 308313 ( 1965 ) . j. shapiro and s. wagner , `` phase and amplitude uncertainties in heterodyne detection , '' ieee j. quantum electron . * 20 * , 803813 ( 1984 ) . s. stenholm , `` simultaneous measurement of conjugate variables , '' ann . phys . * 218 * , 233254 ( 1992 ) . u. leonhardt and h. paul , `` realistic optical homodyne measurements and quasi - probability distributions , '' phys . rev . a * 48 * , 45984604 ( 1993 ) . h. hansen , t. aichele , c. hettich , p. lodahl , a. lvovsky , j. mlynek , and s. schiller , `` ultrasensitive pulsed , balanced homodyne detector : application to time - domain quantum measurements , '' opt . lett . * 26 * , 17141716 ( 2001 ) . u. leonhardt , j. a. vaccaro , b. bhmer , and h. paul , `` canonical and measured phase distributions , '' phys . rev . a * 51 * , 84 ( 1995 ) . h. bachor and t. ralph , _ a guide to experiments in quantum optics _ ( wiley - vch verlag , 2004 ) .

0911.3032

c

in conclusion , we present a fiber - based continuous - variable quantum key distribution system . we demonstrate a receiver module , which simultaneously measures conjugate stokes operators of light . this is the first simultaneous detection of conjugate stokes operator of a quantum signal after a fiber channel . from the measured q - function of the transmitted signal , we estimate the attenuation and the excess noise caused by the channel . for the measured amount of excess noise , the theory has not progressed far enough to generate an unconditionally secure and secret key . nevertheless , we successfully witness effective entanglement with a channel length of up to @xmath0 considering both parts of the quantum signal , the signal and the lo mode .

we present a fiber - based continuous - variable quantum key distribution system . in the scheme the receiver simultaneously measures conjugate quadratures of the light using two homodyne detectors . from the measured q - function of the transmitted signal , we estimate the attenuation and the excess noise caused by the channel . the estimated excess noise originating from the channel and the channel attenuation including the quantum efficiency of the detection setup is investigated with respect to the detection of effective entanglement . we witness effective entanglement with a channel length of up to @xmath0 .

we present a fiber - based continuous - variable quantum key distribution system . in the scheme , a quantum signal of two non - orthogonal weak optical coherent states is sent through a fiber - based quantum channel . the receiver simultaneously measures conjugate quadratures of the light using two homodyne detectors . from the measured q - function of the transmitted signal , we estimate the attenuation and the excess noise caused by the channel . the estimated excess noise originating from the channel and the channel attenuation including the quantum efficiency of the detection setup is investigated with respect to the detection of effective entanglement . the local oscillator is considered in the verification . we witness effective entanglement with a channel length of up to @xmath0 . 10 a. kerckhoffs , _ la cryptographie militaire _ ( journal des sciences militaires , vol . ix , pp . 5 - 38 , 1883 ) . c. shannon , `` communication theory of secrecy systems , '' the bell system technical journal * 28 * , 656715 ( 1949 ) . g. vernam , `` cipher printing telegraph systems for secret wire and radio telegraphic communications , '' j. amer . inst . elect . eng . p. 109 ( 1926 ) . c. bennett and g. brassard , `` quantum cryptography : public key distribution and coin tossing , '' proceedings of ieee international conference on computers systems and signal processing , bangarore india pp . 175179 ( 1984 ) . c. bennett , f. bessette , g. brassard , l. salvail , and j. smolin , `` experimental quantum cryptography , '' journal of cryptology * 5 * , 328 ( 1992 ) . a. ekert , j. rarity , p. tapster , and g. palma , `` practical quantum cryptography based on 2-photon interferometry , '' phys . rev . lett . * 69 * , 12931295 ( 1992 ) . a. muller , j. breguet , and n. gisin , `` experimental demonstration of quantum cryptography using polarized photons in optical - fiber over more than 1 km , '' europhys . lett . * 23 * , 383388 ( 1993 ) . d. stucki , n. gisin , o. guinnard , g. ribordy , and h. zbinden , `` quantum key distribution over 67 km with a plug&play system , '' new j. phys . * 4 * , 41 ( 2002 ) . d. rosenberg , j. w. harrington , p. r. rice , p. a. hiskett , c. g. peterson , r. j. hughes , a. e. lita , s. w. nam , and j. e. nordholt , `` long - distance decoy - state quantum key distribution in optical fiber , '' phys . rev . lett . * 98 * , 10503 ( 2007 ) . r. ursin , f. tiefenbacher , t. schmitt - manderbach , h. weier , t. scheidl , m. lindenthal , b. blauensteiner , t. jennewein , j. perdigues , p. trojek , b. mer , m. frst , m. meyenburg , j. rarity , z. sodnik , c. barbieri , h. weinfurter , and a. zeilinger , `` entanglement - based quantum communication over 144 km , '' nat . phys . * 3 * , 481486 ( 2007 ) . t. schmitt - manderbach , h. weier , m. frst , r. ursin , f. tiefenbacher , t. scheidl , j. perdigues , z. sodnik , c. kurtsiefer , j. g. rarity , a. zeilinger , and h. weinfurter , `` experimental demonstration of free - space decoy - state quantum key distribution over 144 km , '' phys . rev . lett . * 98 * , 010504 ( 2007 ) . t. c. ralph , `` continuous variable quantum cryptography , '' phys . rev . a * 61 * , 010303 ( 1999 ) . c. silberhorn , t. c. ralph , n. ltkenhaus , and g. leuchs , `` continuous variable quantum cryptography : beating the 3 db loss limit , '' phys . rev . lett . * 89 * , 167901 ( 2002 ) . f. grosshans , g. v. assche , j. wenger , r. brouri , n. j. cerf , and p. grangier , `` quantum key distribution using gaussian - modulated coherent states , '' nature * 421 * , 238241 ( 2003 ) . j. lodewyck , m. bloch , r. garcia - patron , s. fossier , e. karpov , e. diamanti , t. debuisschert , n. j. cerf , r. tualle - brouri , s. w. mclaughlin , and p. grangier , `` quantum key distribution over 25 km with an all - fiber continuous - variable system , '' phys . rev . a * 76 * , 04230510 ( 2007 ) . b. qi , l. huang , l. qian , and h. lo , `` experimental study on the gaussian - modulated coherent - state quantum key distribution over standard telecommunication fibers , '' phys . rev . a * 76 * , 0523239 ( 2007 ) . s. lorenz , n. korolkova , and g. leuchs , `` continuous - variable quantum key distribution using polarization encoding and post selection , '' appl . phys . b * 79 * , 273277 ( 2004 ) . a. m. lance , t. symul , v. sharma , c. weedbrook , t. c. ralph , and p. k. lam , `` no - switching quantum key distribution using broadband modulated coherent light , '' phys . rev . lett . * 95 * , 1805034 ( 2005 ) . n. gisin , s. fasel , b. kraus , h. zbinden , and g. ribordy , `` trojan - horse attacks on quantum - key - distribution systems , '' phys . rev . a * 73 * , 0223206 ( 2006 ) . s. pirandola , s. mancini , s. lloyd , and s. l. braunstein , `` continuous - variable quantum cryptography using two - way quantum communication , '' nat . phys . * 4 * , 726730 ( 2008 ) . c. weedbrook , a. m. lance , w. p. bowen , t. symul , t. c. ralph , and p. k. lam , `` coherent - state quantum key distribution without random basis switching , '' phys . rev . a * 73 * , 0223169 ( 2006 ) . j. lodewyck and p. grangier , `` tight bound on the coherent - state quantum key distribution with heterodyne detection , '' phys . rev . a * 76 * , 0223328 ( 2007 ) . d. elser , t. bartley , b. heim , c. wittmann , d. sych , and g. leuchs , `` feasibility of free space quantum key distribution with coherent polarization states , '' new j. phys . * 11 * , 045014 ( 2009 ) . d. elser , c. wittmann , u. l. andersen , o. glckl , s. lorenz , c. marquardt , and g. leuchs , `` guided acoustic wave brillouin scattering in photonic crystal fibers , '' j. phys . conf . ser . * 92 * , 012108 ( 2007 ) . n. korolkova , g. leuchs , r. loudon , t. c. ralph , and c. silberhorn , `` polarization squeezing and continuous - variable polarization entanglement , '' phys . rev . a * 65 * , 052306 ( 2002 ) . h. hseler , t. moroder , and n. ltkenhaus , `` testing quantum devices : practical entanglement verification in bipartite optical systems , '' phys . rev . a * 77 * , 03230311 ( 2008 ) . c. dorrer , d. kilper , h. stuart , g. raybon , and m. raymer , `` linear optical sampling , '' ieee photonics technol . lett . * 15 * , 17461748 ( 2003 ) . c. h. bennett , `` quantum cryptography using any two nonorthogonal states , '' phys . rev . lett . * 68 * , 3121 ( 1992 ) . y. zhao , m. heid , j. rigas , and n. ltkenhaus , `` asymptotic security of binary modulated continuous - variable quantum key distribution under collective attacks , '' phys . rev . a * 79 * , 01230714 ( 2009 ) . m. curty , m. lewenstein , and n. ltkenhaus , `` entanglement as a precondition for secure quantum key distribution , '' phys . rev . lett . * 92 * , 217903 ( 2004 ) . c. h. bennett , g. brassard , and n. d. mermin , `` quantum cryptography without bell s theorem , '' phys . rev . lett . * 68 * , 557 ( 1992 ) . j. rigas , o. ghne , and n. ltkenhaus , `` entanglement verification for quantum - key - distribution systems with an underlying bipartite qubit - mode structure , '' phys . rev . a * 73 * , 0123416 ( 2006 ) . u. leonhardt , _ measuring the quantum state of light _ ( cambridge university press , 1997 ) . m. legr ' e , h. zbinden , and n. gisin , `` implementation of continuous variable quantum cryptography in optical fibres using a go-&-return configuration , '' quantum inf . comput . * 6 * , 326335 ( 2006 ) . j. a. nelder and r. mead , `` a simplex method for function minimization , '' the computer journal * 7 * , 308313 ( 1965 ) . j. shapiro and s. wagner , `` phase and amplitude uncertainties in heterodyne detection , '' ieee j. quantum electron . * 20 * , 803813 ( 1984 ) . s. stenholm , `` simultaneous measurement of conjugate variables , '' ann . phys . * 218 * , 233254 ( 1992 ) . u. leonhardt and h. paul , `` realistic optical homodyne measurements and quasi - probability distributions , '' phys . rev . a * 48 * , 45984604 ( 1993 ) . h. hansen , t. aichele , c. hettich , p. lodahl , a. lvovsky , j. mlynek , and s. schiller , `` ultrasensitive pulsed , balanced homodyne detector : application to time - domain quantum measurements , '' opt . lett . * 26 * , 17141716 ( 2001 ) . u. leonhardt , j. a. vaccaro , b. bhmer , and h. paul , `` canonical and measured phase distributions , '' phys . rev . a * 51 * , 84 ( 1995 ) . h. bachor and t. ralph , _ a guide to experiments in quantum optics _ ( wiley - vch verlag , 2004 ) .

1405.3234

i

optical fields with non - zero orbital angular momentum ( oam ) , which show a non - gaussian transverse amplitude and phase profiles @xcite , are of great interest in a myriad of scientific and technological applications , such as secure communications @xcite , ultra - precise measurements @xcite , nano - particle manipulation @xcite or quantum computing @xcite . these applications push forward the development of new methods aimed at the preparation of optical fields with oam in both the classical and quantum ( i.e. single - photon ) regimes . paired photons with nonzero oam are widely generated nowadays via the nonlinear optical process of spontaneous parametric down - conversion ( spdc ) , where photons are generated in pairs ( signal and idler ) . such paired photons can show quantum correlations ( entanglement ) in several degrees of freedom including polarization , frequency , or momentum . entanglement may occur also in the oam degree of freedom @xcite , as experimentally demonstrated in @xcite . states with the winding numbers around 300 have already been observed in volume optics @xcite . dimensions of this entanglement reaching even @xmath3 are theoretically predicted in @xcite . however , the generation of oam entanglement in optical fibers still represents a challenge , which solution could open the door for many applications that would benefit from using guided modes ( low losses in optical elements , long transmission distances ) . recently , guided oam states in fibers with the winding numbers up to 1 have been observed @xcite . there are mainly two problems to overcome . on the one hand , the presence of inverse symmetry in ideally cylindrically - shaped silicon optical fibers excludes the existence of @xmath1 nonlinearity . for this reason , photon pairs in optical fibers are generally generated by means of an alternative nonlinear process ( four - wave mixing ) which utilizes instead the third - order nonlinearity of silicon @xcite . small values of the elements of @xmath4 nonlinear tensor can be compensated by increasing the interaction length to give higher photon - pair fluxes . unfortunately , this is accompanied by equal enhancement of other effects , i.e. , raman scattering , that cause unwanted higher noise contributions to the generated flux . nevertheless , silicon optical fibers can become nonlinear using the method of thermal poling @xcite which provides a nonzero @xmath1 susceptibility and also enables to employ quasi - phase - matching ( qpm ) reached via uv erasure @xcite . on the other hand , the propagation of photons with oam in the usual step - index long optical fibers do not prevent cross - talk among modes with different oam from being strong , which results in the fast deterioration of the purity of the oam propagating modes . however , modern technology suggest also a solution in the form of ring and vortex fibers with ring - shaped cores @xcite that are more resistant against cross - talk . here , we show that entangled photon pairs in oam modes can be generated in this type of silica fiber with thermal poling .

g. puentes , n. hermosa , and j. p. torres , `` weak measurements with orbital - angular - momentum pointer states , '' phys . guo , `` demonstration of one - dimensional quantum random walks using orbital angular momentum of photons , '' phys . a * 75 * , 052310 ( 2007 ) . j. svozilk , j. peina jr . , and j. p. torres , `` high spatial entanglement via chirped quasi - phase - matched optical parametric down - conversion , '' phys . rev . a * 86 * , 052318 ( 2012 ) . x. li , p. l. voss , j. e. sharping , and p. kumar , `` optical - fiber source of polarization - entangled photons in the 1550 nm telecom band , '' phys . e. y. zhu , l. qian , l. g. helt , m. liscidini , j. e. sipe , c. corbari , a. canagasabey , m. ibsen , and p. g. kazansky , `` measurement of @xmath2(2 ) symmetry in a poled fiber , '' opt . kazansky , p. tapster , and j. rarity , `` parametric fluorescence in periodically poled silica fibers , '' appl . k. p. huy , a. t. nguyen , e. brainis , m. haelterman , p. emplit , c. corbari , a. canagasabey , p. g. kazansky , o. deparis , a. a. fotiadi , p. mgret , and s. massar , `` photon pair source based on parametric fluorescence in periodically poled twin - hole silica fiber , '' opt . yang , l. zhang , y. ren , h. huang , k. m. birnbaum , b. i. erkmen , s. dolinar , m. tur , and a. e. willner , `` mode properties and propagation effects of optical orbital angular momentum ( oam ) modes in a ring fiber , '' ieee photonics j. * 4 * , 535 - 543 ( 2012 ) . a. w. snyder and j. love , _ optical waveguide theory _ , ( springer , 1983 ) . v. brckner , _ elements of optical networking _ ( springer , 2011 ) . m. j. collins , c. xiong , i. h. rey , t. d. vo , j. he , s. shahnia , b. j. eggleton,(2013 ) .

we present a method for the generation of correlated photon pairs in desired orbital - angular - momentum states using a non - linear silica ring fiber and spontaneous parametric down - conversion . photon - pair emission under quasi - phase - matching conditions with quantum conversion efficiency @xmath0 is found in a 1-m long fiber with a thermally induced @xmath1 nonlinearity in a ring - shaped core . 10 l. allen , s. m. barnett , and m. j. padgett , _ optical angularmomentum _ ( crc press , 2003 ) . j. p. torres and l. torner , _ twisted photons : applications of light with orbital angular momentum _ ( john wiley & sons , 2011 ) . n. bozinovic , y. yue , y. ren , m. tur , p. kristensen , h. huang , a. e. willner , and s. ramachandran , `` terabit - scale orbital angular momentum mode division multiplexing in fibers , '' science * 340 * , 1545 - 1548 ( 2013 ) . g. molina - terriza , j. p. torres , and l. torner , `` twisted photons , '' nature physics * 3 * , 305 - 310 ( 2007 ) . g. puentes , n. hermosa , and j. p. torres , `` weak measurements with orbital - angular - momentum pointer states , '' phys . rev . lett . * 109 * , 040401 ( 2012 ) . m. padgett and r. bowman , `` tweezers with a twist , '' nature photonics * 5 * , 343 - 348 ( 2011 ) . p. zhang , x .- f . ren , x .- b . zou , b .- h . liu , y .- f . huang , and g .- c . guo , `` demonstration of one - dimensional quantum random walks using orbital angular momentum of photons , '' phys . rev . a * 75 * , 052310 ( 2007 ) . a. mair , a. vaziri , g. weihs , and a. zeilinger , `` entanglement of the orbital angular momentum states of photons , '' nature * 412 * , 313 - 316 ( 2001 ) . a. c. dada , j. leach , g. s. buller , m. j. padgett , and e. andersson , `` experimental high - dimensional two - photon entanglement and violations of generalized bell inequalities , '' nature physics * 7 * , 677 - 680 ( 2011 ) . r. fickler , r. lapkiewicz , w. n. plick , m. krenn , c. schaeff , s. ramelow , and a. zeilinger , `` quantum entanglement of high angular momenta , '' science * 338 * , 640 - 643 ( 2012 ) . j. svozilk , j. peina jr . , and j. p. torres , `` high spatial entanglement via chirped quasi - phase - matched optical parametric down - conversion , '' phys . rev . a * 86 * , 052318 ( 2012 ) . x. li , p. l. voss , j. e. sharping , and p. kumar , `` optical - fiber source of polarization - entangled photons in the 1550 nm telecom band , '' phys . rev . lett . * 94 * , 053601 ( 2005 ) . j. fulconis , o. alibart , w. wadsworth , p. russell , and j. rarity , `` high brightness single mode source of correlated photon pairs using a photonic crystal fiber , '' opt . express * 13 * , 7572 - 7582 ( 2005 ) . j. fan , a. migdall , and l. wang , `` efficient generation of correlated photon pairs in a microstructure fiber , '' opt . lett . * 30 * , 3368 - 3370 ( 2005 ) . r. a. myers , n. mukherjee , and s. r. j. brueck , `` large second - order nonlinearity in poled fused silica , '' opt . lett . * 16 * , 1732 - 1734 ( 1991 ) . e. y. zhu , l. qian , l. g. helt , m. liscidini , j. e. sipe , c. corbari , a. canagasabey , m. ibsen , and p. g. kazansky , `` measurement of @xmath2(2 ) symmetry in a poled fiber , '' opt . lett . * 35 * , 1530 - 1532 ( 2010 ) . g. bonfrate , v. pruneri , p. kazansky , p. tapster , and j. rarity , `` parametric fluorescence in periodically poled silica fibers , '' appl . . lett . * 75 * , 2356 - 2358 ( 1999 ) . k. p. huy , a. t. nguyen , e. brainis , m. haelterman , p. emplit , c. corbari , a. canagasabey , p. g. kazansky , o. deparis , a. a. fotiadi , p. mgret , and s. massar , `` photon pair source based on parametric fluorescence in periodically poled twin - hole silica fiber , '' opt . express * 15 * , 4419 - 4426 ( 2007 ) . e. y. zhu , z. tang , l. qian , l. g. helt , m. liscidini , j. e. sipe , c. corbari , a. canagasabey , m. ibsen , and p. g. kazansky , `` direct generation of polarization - entangled photon pairs in a poled fiber , '' phys . rev . lett . * 108 * , 213902 ( 2012 ) . y. yue , y. yan , n. ahmed , j .- y . yang , l. zhang , y. ren , h. huang , k. m. birnbaum , b. i. erkmen , s. dolinar , m. tur , and a. e. willner , `` mode properties and propagation effects of optical orbital angular momentum ( oam ) modes in a ring fiber , '' ieee photonics j. * 4 * , 535 - 543 ( 2012 ) . a. canagasabey , c. corbari , a. v. gladyshev , f. liegeois , s. guillemet , y. hernandez , m. v. yashkov , a. kosolapov , e. m. dianov , m. ibsen , and p. g. kazansky , `` high - average - power second - harmonic generation from periodically poled silica fibers , '' opt . lett . * 34 * , 2483 - 2485 ( 2009 ) . a. w. snyder and j. love , _ optical waveguide theory _ , ( springer , 1983 ) . v. brckner , _ elements of optical networking _ ( springer , 2011 ) . m. j. collins , c. xiong , i. h. rey , t. d. vo , j. he , s. shahnia , b. j. eggleton,(2013 ) . _ integrated spatial multiplexing of heralded single - photon sources _ , nat . commun . * 4 * , 1 - 7 ( 2013 ) .

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( a ) as it depends on signal wavelength @xmath72 for three different combinations of eigenmodes fulfilling the oam selection rule . the horizontal grey line indicates the maximum of spatial spectrum of @xmath73 modulation expressed in @xmath74 . the period of modulation @xmath75 m is chosen such that quasi - phase - matching occurs for @xmath76 @xmath77 m and process @xmath78 . ( b ) signal photon - number density @xmath79 as a function of signal wavelength @xmath72 for a 1 m - long fiber with period @xmath75 m . different modes recognized in the signal field are indicated.,title="fig:",width=230](b ) as it depends on signal wavelength @xmath72 for three different combinations of eigenmodes fulfilling the oam selection rule . the horizontal grey line indicates the maximum of spatial spectrum of @xmath73 modulation expressed in @xmath74 . the period of modulation @xmath75 m is chosen such that quasi - phase - matching occurs for @xmath76 @xmath77 m and process @xmath78 . ( b ) signal photon - number density @xmath79 as a function of signal wavelength @xmath72 for a 1 m - long fiber with period @xmath75 m . different modes recognized in the signal field are indicated.,title="fig:",width=230 ] in the analysis , we consider a silica fiber with a ring - shaped core created by doping the base material with 19.3 mol% of @xmath80 ( for details , see @xcite ) . the spdc process is pumped by a monochromatic beam of wavelength @xmath81 m . the fiber was designed such that photon pairs are emitted around the wavelength @xmath82 m used in fiber communication systems . a right - handed circularly polarized he@xmath83 mode with oam number @xmath84 ( composed of he@xmath85 and he@xmath86 modes , see @xcite ) has been found suitable for the pump beam . it gives minimal crosstalk with other pump modes ( namely tm@xmath87 ) at the given wavelength . importantly , according to the full - vector numerical model , the propagation constants of eigenmodes he@xmath85 and he@xmath86 for pump ( signal ) field differ only by 3.88@xmath88 ( 1.14@xmath88 ) rad / m in an anisotropic fiber with @xmath89 . the generated signal and idler photons fulfil the energy conservation law ( @xmath90 ) and also the selection rule for oam numbers ( @xmath91 ) that originates in the radial symmetry of the nonlinear interaction . under these conditions , efficient photon - pair generation has been found for a signal photon in mode he@xmath92 ( @xmath93 ) and an idler photon in mode he@xmath94 or he@xmath95 ( @xmath96 ) which represent the right- and left - handed polarization variants of the same spatial mode . as the phase - matching curves in fig . [ fig:2](a ) show , also other efficient combinations of signal and idler modes are possible , namely he@xmath97 te@xmath98 @xmath99he@xmath100 and he@xmath97 tm@xmath98 @xmath99 he@xmath100 . however , qpm reached via the periodic modulation of @xmath1 nonlinearity allows to separate different processes . the right choice of period @xmath101 of @xmath1 nonlinearity tunes the desired process that is exclusively selected provided that the @xmath102 spatial spectrum is sufficiently narrow . for our fiber , the @xmath73 spatial spectrum has to be narrower than @xmath103 @xmath104m@xmath105 . this is achieved in general for fibers longer than 1 cm . the analyzed fiber 1 m long with the width of spatial spectrum equal to @xmath106 @xmath104m@xmath107 allows to separate the desired process from the other ones with the precision better than 1:100 . according to fig . [ fig:2](b ) the greatest values of signal photon - number density @xmath108 occur for mode he@xmath92 with an oam number @xmath109 around the wavelength @xmath110 m . the full width at the half of maximum of the peak equals @xmath111 nm . the second largest contribution belongs to the processes involving modes he@xmath112 and he@xmath113 that interact with mode he@xmath114 . they build a common peak found at the wavelength @xmath115 @xmath104 m . in signal photon - number density @xmath116 , there also exists two peaks of mode he@xmath112 that form pairs with the peaks created by modes tm@xmath87 and te@xmath87 . these peaks are shifted towards lower and larger wavelengths , respectively , due to their propagation constants . whereas the peak belonging to mode tm@xmath98 occurs at the lower wavelength @xmath117 @xmath77 m , the peak given by mode te@xmath98 is located at the longer wavelength @xmath118 @xmath119 m . spectral shifts of these peaks allow their efficient separation by frequency filtering . the generated photon - pair field is then left in the state with a signal photon in mode he@xmath92 and an idler photon either in state he@xmath94 or he@xmath120 . the weights of both possible idler states he@xmath94 and he@xmath120 in quantum superposition are the same which gives linear polarization of the overall idler field . also , pump - field leakage into modes te@xmath121 and tm@xmath121 caused by imperfect fiber coupling may occur . this gives extra peaks in the signal photon - number density @xmath122 that are spectrally separated from those discussed above by 15 nm . the fiber 1 m long provides around 240 photon pairs per 1 s and @xmath123w of pumping in the analyzed modes . for comparison , the fibre 10-cm long generates around 20 photon pairs per 1 s and @xmath123w of pumping in the same configuration . this means that a slightly better than linear increase of photon - pair numbers with the fiber length occurs . strong correlations between the signal and idler frequencies result in fast temporal correlations between the signal and idler detection times occurring in a time window 7 ps long . we notice , that the process can also be considered in its left - handed polarization variant in which the pump beam propagates as a he@xmath124 mode . both variants provide photon pairs suitable , e.g. , for quantum metrology or heralded single - photon sources @xcite giving fock states with non - zero oam numbers . quasi - phase matching allows also other efficient combinations of modes . for example , the pump beam in mode he@xmath125 ( or he@xmath126 ) with @xmath127 provides spectrally broad - band spdc that may give photon pairs with temporal correlations at fs time - scale . also photon pairs entangled in oam numbers can be obtained in this configuration in which the signal ( idler ) photon propagates either as he@xmath128 ( he@xmath129 ) mode or he@xmath130 ( he@xmath131 ) . we note that vortex fibers @xcite are also suitable for spdc as they provide similar conditions for photon - pair generation as the analyzed ring fibers . moreover , their additional core gives better stability to fundamental modes participating in the nonlinear interaction . both ring and vortex fibers thus have a large potential to serve as versatile fiber sources of photon pairs in oam states useful in optical information processing .

photon - pair emission under quasi - phase - matching conditions with quantum conversion efficiency @xmath0 is found in a 1-m long fiber with a thermally induced @xmath1 nonlinearity in a ring - shaped core . 10 l. allen , s. m. barnett , and m. j. padgett , _ optical angularmomentum _ ( crc press , 2003 ) . ( john wiley & sons , 2011 ) . rev . lett . * 109 * , 040401 ( 2012 ) . m. padgett and r. bowman , `` tweezers with a twist , '' nature photonics * 5 * , 343 - 348 ( 2011 ) . ren , x .- b . zou , b .- h . huang , and g .- c . rev . rev . lett . * 94 * , 053601 ( 2005 ) . j. fulconis , o. alibart , w. wadsworth , p. russell , and j. rarity , `` high brightness single mode source of correlated photon pairs using a photonic crystal fiber , '' opt . j. fan , a. migdall , and l. wang , `` efficient generation of correlated photon pairs in a microstructure fiber , '' opt . lett . * 30 * , 3368 - 3370 ( 2005 ) . . lett . * 16 * , 1732 - 1734 ( 1991 ) . lett . * 35 * , 1530 - 1532 ( 2010 ) . . lett . * 75 * , 2356 - 2358 ( 1999 ) . rev . lett . * 108 * , 213902 ( 2012 ) . a. canagasabey , c. corbari , a. v. gladyshev , f. liegeois , s. guillemet , y. hernandez , m. v. yashkov , a. kosolapov , e. m. dianov , m. ibsen , and p. g. kazansky , `` high - average - power second - harmonic generation from periodically poled silica fibers , '' opt . lett . * 34 * , 2483 - 2485 ( 2009 ) . _ integrated spatial multiplexing of heralded single - photon sources _ , nat . commun . * 4 * , 1 - 7 ( 2013 ) .

we present a method for the generation of correlated photon pairs in desired orbital - angular - momentum states using a non - linear silica ring fiber and spontaneous parametric down - conversion . photon - pair emission under quasi - phase - matching conditions with quantum conversion efficiency @xmath0 is found in a 1-m long fiber with a thermally induced @xmath1 nonlinearity in a ring - shaped core . 10 l. allen , s. m. barnett , and m. j. padgett , _ optical angularmomentum _ ( crc press , 2003 ) . j. p. torres and l. torner , _ twisted photons : applications of light with orbital angular momentum _ ( john wiley & sons , 2011 ) . n. bozinovic , y. yue , y. ren , m. tur , p. kristensen , h. huang , a. e. willner , and s. ramachandran , `` terabit - scale orbital angular momentum mode division multiplexing in fibers , '' science * 340 * , 1545 - 1548 ( 2013 ) . g. molina - terriza , j. p. torres , and l. torner , `` twisted photons , '' nature physics * 3 * , 305 - 310 ( 2007 ) . g. puentes , n. hermosa , and j. p. torres , `` weak measurements with orbital - angular - momentum pointer states , '' phys . rev . lett . * 109 * , 040401 ( 2012 ) . m. padgett and r. bowman , `` tweezers with a twist , '' nature photonics * 5 * , 343 - 348 ( 2011 ) . p. zhang , x .- f . ren , x .- b . zou , b .- h . liu , y .- f . huang , and g .- c . guo , `` demonstration of one - dimensional quantum random walks using orbital angular momentum of photons , '' phys . rev . a * 75 * , 052310 ( 2007 ) . a. mair , a. vaziri , g. weihs , and a. zeilinger , `` entanglement of the orbital angular momentum states of photons , '' nature * 412 * , 313 - 316 ( 2001 ) . a. c. dada , j. leach , g. s. buller , m. j. padgett , and e. andersson , `` experimental high - dimensional two - photon entanglement and violations of generalized bell inequalities , '' nature physics * 7 * , 677 - 680 ( 2011 ) . r. fickler , r. lapkiewicz , w. n. plick , m. krenn , c. schaeff , s. ramelow , and a. zeilinger , `` quantum entanglement of high angular momenta , '' science * 338 * , 640 - 643 ( 2012 ) . j. svozilk , j. peina jr . , and j. p. torres , `` high spatial entanglement via chirped quasi - phase - matched optical parametric down - conversion , '' phys . rev . a * 86 * , 052318 ( 2012 ) . x. li , p. l. voss , j. e. sharping , and p. kumar , `` optical - fiber source of polarization - entangled photons in the 1550 nm telecom band , '' phys . rev . lett . * 94 * , 053601 ( 2005 ) . j. fulconis , o. alibart , w. wadsworth , p. russell , and j. rarity , `` high brightness single mode source of correlated photon pairs using a photonic crystal fiber , '' opt . express * 13 * , 7572 - 7582 ( 2005 ) . j. fan , a. migdall , and l. wang , `` efficient generation of correlated photon pairs in a microstructure fiber , '' opt . lett . * 30 * , 3368 - 3370 ( 2005 ) . r. a. myers , n. mukherjee , and s. r. j. brueck , `` large second - order nonlinearity in poled fused silica , '' opt . lett . * 16 * , 1732 - 1734 ( 1991 ) . e. y. zhu , l. qian , l. g. helt , m. liscidini , j. e. sipe , c. corbari , a. canagasabey , m. ibsen , and p. g. kazansky , `` measurement of @xmath2(2 ) symmetry in a poled fiber , '' opt . lett . * 35 * , 1530 - 1532 ( 2010 ) . g. bonfrate , v. pruneri , p. kazansky , p. tapster , and j. rarity , `` parametric fluorescence in periodically poled silica fibers , '' appl . . lett . * 75 * , 2356 - 2358 ( 1999 ) . k. p. huy , a. t. nguyen , e. brainis , m. haelterman , p. emplit , c. corbari , a. canagasabey , p. g. kazansky , o. deparis , a. a. fotiadi , p. mgret , and s. massar , `` photon pair source based on parametric fluorescence in periodically poled twin - hole silica fiber , '' opt . express * 15 * , 4419 - 4426 ( 2007 ) . e. y. zhu , z. tang , l. qian , l. g. helt , m. liscidini , j. e. sipe , c. corbari , a. canagasabey , m. ibsen , and p. g. kazansky , `` direct generation of polarization - entangled photon pairs in a poled fiber , '' phys . rev . lett . * 108 * , 213902 ( 2012 ) . y. yue , y. yan , n. ahmed , j .- y . yang , l. zhang , y. ren , h. huang , k. m. birnbaum , b. i. erkmen , s. dolinar , m. tur , and a. e. willner , `` mode properties and propagation effects of optical orbital angular momentum ( oam ) modes in a ring fiber , '' ieee photonics j. * 4 * , 535 - 543 ( 2012 ) . a. canagasabey , c. corbari , a. v. gladyshev , f. liegeois , s. guillemet , y. hernandez , m. v. yashkov , a. kosolapov , e. m. dianov , m. ibsen , and p. g. kazansky , `` high - average - power second - harmonic generation from periodically poled silica fibers , '' opt . lett . * 34 * , 2483 - 2485 ( 2009 ) . a. w. snyder and j. love , _ optical waveguide theory _ , ( springer , 1983 ) . v. brckner , _ elements of optical networking _ ( springer , 2011 ) . m. j. collins , c. xiong , i. h. rey , t. d. vo , j. he , s. shahnia , b. j. eggleton,(2013 ) . _ integrated spatial multiplexing of heralded single - photon sources _ , nat . commun . * 4 * , 1 - 7 ( 2013 ) .

1405.3234

c

a ring fiber with thermally induced @xmath132 nonlinearity and periodical poling has been presented as a promising source of photon pairs being in eigenmodes of orbital angular momentum . spontaneous parametric down - conversion has been pumped by a beam with nonzero orbital angular momentum that has been transferred into one of the down - converted beams . several mutually competing nonlinear processes exploiting different modes can be spectrally separated . other configurations also allow for the emission of spectrally broad - band photon pairs as well as photon pairs entangled in orbital - angular - momentum numbers . this makes the analyzed ring fiber useful for many integrated fiber - based applications .

we present a method for the generation of correlated photon pairs in desired orbital - angular - momentum states using a non - linear silica ring fiber and spontaneous parametric down - conversion . j. p. torres and l. torner , _ twisted photons : applications of light with orbital angular momentum _ n. bozinovic , y. yue , y. ren , m. tur , p. kristensen , h. huang , a. e. willner , and s. ramachandran , `` terabit - scale orbital angular momentum mode division multiplexing in fibers , '' science * 340 * , 1545 - 1548 ( 2013 ) . a. mair , a. vaziri , g. weihs , and a. zeilinger , `` entanglement of the orbital angular momentum states of photons , '' nature * 412 * , 313 - 316 ( 2001 ) . e. y. zhu , z. tang , l. qian , l. g. helt , m. liscidini , j. e. sipe , c. corbari , a. canagasabey , m. ibsen , and p. g. kazansky , `` direct generation of polarization - entangled photon pairs in a poled fiber , '' phys .

we present a method for the generation of correlated photon pairs in desired orbital - angular - momentum states using a non - linear silica ring fiber and spontaneous parametric down - conversion . photon - pair emission under quasi - phase - matching conditions with quantum conversion efficiency @xmath0 is found in a 1-m long fiber with a thermally induced @xmath1 nonlinearity in a ring - shaped core . 10 l. allen , s. m. barnett , and m. j. padgett , _ optical angularmomentum _ ( crc press , 2003 ) . j. p. torres and l. torner , _ twisted photons : applications of light with orbital angular momentum _ ( john wiley & sons , 2011 ) . n. bozinovic , y. yue , y. ren , m. tur , p. kristensen , h. huang , a. e. willner , and s. ramachandran , `` terabit - scale orbital angular momentum mode division multiplexing in fibers , '' science * 340 * , 1545 - 1548 ( 2013 ) . g. molina - terriza , j. p. torres , and l. torner , `` twisted photons , '' nature physics * 3 * , 305 - 310 ( 2007 ) . g. puentes , n. hermosa , and j. p. torres , `` weak measurements with orbital - angular - momentum pointer states , '' phys . rev . lett . * 109 * , 040401 ( 2012 ) . m. padgett and r. bowman , `` tweezers with a twist , '' nature photonics * 5 * , 343 - 348 ( 2011 ) . p. zhang , x .- f . ren , x .- b . zou , b .- h . liu , y .- f . huang , and g .- c . guo , `` demonstration of one - dimensional quantum random walks using orbital angular momentum of photons , '' phys . rev . a * 75 * , 052310 ( 2007 ) . a. mair , a. vaziri , g. weihs , and a. zeilinger , `` entanglement of the orbital angular momentum states of photons , '' nature * 412 * , 313 - 316 ( 2001 ) . a. c. dada , j. leach , g. s. buller , m. j. padgett , and e. andersson , `` experimental high - dimensional two - photon entanglement and violations of generalized bell inequalities , '' nature physics * 7 * , 677 - 680 ( 2011 ) . r. fickler , r. lapkiewicz , w. n. plick , m. krenn , c. schaeff , s. ramelow , and a. zeilinger , `` quantum entanglement of high angular momenta , '' science * 338 * , 640 - 643 ( 2012 ) . j. svozilk , j. peina jr . , and j. p. torres , `` high spatial entanglement via chirped quasi - phase - matched optical parametric down - conversion , '' phys . rev . a * 86 * , 052318 ( 2012 ) . x. li , p. l. voss , j. e. sharping , and p. kumar , `` optical - fiber source of polarization - entangled photons in the 1550 nm telecom band , '' phys . rev . lett . * 94 * , 053601 ( 2005 ) . j. fulconis , o. alibart , w. wadsworth , p. russell , and j. rarity , `` high brightness single mode source of correlated photon pairs using a photonic crystal fiber , '' opt . express * 13 * , 7572 - 7582 ( 2005 ) . j. fan , a. migdall , and l. wang , `` efficient generation of correlated photon pairs in a microstructure fiber , '' opt . lett . * 30 * , 3368 - 3370 ( 2005 ) . r. a. myers , n. mukherjee , and s. r. j. brueck , `` large second - order nonlinearity in poled fused silica , '' opt . lett . * 16 * , 1732 - 1734 ( 1991 ) . e. y. zhu , l. qian , l. g. helt , m. liscidini , j. e. sipe , c. corbari , a. canagasabey , m. ibsen , and p. g. kazansky , `` measurement of @xmath2(2 ) symmetry in a poled fiber , '' opt . lett . * 35 * , 1530 - 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our ability to measure the spin of a black hole ( bh ) has increased substantially over the last decade . apart from exploring a fundamental prediction concerning orbits around spinning compact objects , spin measurements may hold the key to understanding how relativistic jets are launched . as such , spin is a very important quantity to measure . it is also a very difficult quantity to measure , because in order to do so one must observe the effects that the bh has on nearby material in an accretion disk , and infer information indirectly about the hole itself . currently , two reliable methods are used to measure the spins of accreting black holes using the x - ray spectrum . the first is the continuum fitting method ( zhang , cui , & chen 1997 ; shafee et al . 2006 ; mcclintock et al . 2006 ; etc . ) . in this method , one fits spectra with models that estimate an inner radius of the disk , which is assumed to exist at the innermost stable circular orbit ( isco ) . the radius of the isco is determined by the spin and mass , and thus the spin can be determined , if the mass is already known . the distance to the source and the inclination of the inner disk must also be known when performing this method in order to infer the inner radius of the disk from the observed flux . the mass , distance , and binary inclination can be reliably measured via independant methods ( some examples of such methods applied to various black hole systems can be found in miller - jones et al . 2009 ; gelino et al . 2001 ; orosz et al . however in cases where the spin vector of the black hole is misaligned with the binary s orbital angular momentum , the inclination of the inner disk may be misaligned with the orbital inclination since it aligns instead with the spin of the black hole ( bardeen & petterson 1975 ) . the other method for measuring black hole spin using the x - ray spectrum is by modeling spectral features produced via reflection from material in the inner disk ( tanaka et al . 1995 ; miller et al . 2002 ; miller et al . 2004 ; for a comprehensive review , see reynolds 2013 ) . in particular , one examines asymetric blurring of the iron k shell emission lines caused by the strong gravity and by doppler shifts from orbits within that potential . additionally , other features are produced by reflection that one must account for properly in order to declare their measurement credible . use of this method has led to spin measurements for both supermassive black holes and bhbs because it does not necessitate a strong disk component to be observed in the x - rays . this method also does not require prior constraints on the mass or distance , since the shape of the line is determined by the metric ( reynolds 2013 ) . additionally , the observed shape of the line is affected by the inclination of the inner disk with respect to the observer in such a way that the inner disk inclination can be robustly constrained using this method ( reynolds 2013 ) . for bhbs , both methods have found evidence for both extreme and moderate spins . generally , when applied to the same sources , they provide results that are in agreement ( miller et al . 2011 ) . however there remain two cases for which such an agreement is not found : gro j1655 - 40 and 4u 1543 - 47 ( reynolds 2013 ) . resolving the discrepancy for gro j1655 - 40 is difficult because the spectrum shows evidence of strong absorption by winds which complicates modeling of the continuum spectrum , and possible strong misalignment between the binary ( greene et al . 2001 ) , the jet ( maccarone 2002 ) , and possibly the inner disk as well ( reis et al . 2009 ) . however , 4u 1543 - 47 shows very little evidence for the same complications . furthermore , the discrepancy is @xmath2 for 4u 1543 - 47 , but only @xmath3 for gro j1655 - 40 , making resolving the disagreement in 4u 1543 - 475 the more pressing concern . we note that both past work and recent studies have demonstrated the potential for x - ray timing to measure black hole spin , if observations can eventually determine the mechanism for quasi - period oscillations ( strohmayer 2001 ; wagoner 2012 ; motta et al . 2014a , b ; bambi et al . 2014 ; dexter and blaes 2014 ) . in this work , we shall examine spectra obtained during the 2002 outburst of 4u 1543 - 47 in an attempt to measure its spin . we use models that combine disk reflection and continuum fitting . our data reduction and data selection procedures are described in section 2 . our analysis methods and results are presented in section 3 . we discuss these results in section 4 , and list our conclusions in section 5 .

we focus on observations in the high / soft state , and attempt to measure the `` spin '' of the black hole by simultaneously fitting the thermal disk continuum and by modeling the broadened iron k - shell emission lines and additional blurred reflection features . [ firstpage ]

we present a new analysis of rossi x - ray timing explorer observations of the 2002 outburst of the transient x - ray nova 4u 1543 - 47 . we focus on observations in the high / soft state , and attempt to measure the `` spin '' of the black hole by simultaneously fitting the thermal disk continuum and by modeling the broadened iron k - shell emission lines and additional blurred reflection features . previous works have found that use of these methods individually returns contradictory values for the dimensionless spin parameter @xmath0 . we find that when used in conjunction with each other , a moderate spin is obtained ( @xmath1 ) that is actually consistent with both other values within errors . we discuss limitations of our analysis , systematic uncertainties , and implications of this measurement , and compare our result to those previously claimed for 4u 1543 - 47 . [ firstpage ]

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we have performed a thorough examination of rxte data of the 2002 outburst of the soft x - ray transient 4u 1543 - 74 . using a combination of continuum - fitting , and disk reflection modeling , we have measured the spin to be @xmath1 . prior works measuring the spin of 4u 1543 - 74 which used both of these methods separately had found conflicting values of @xmath22 ( 0.75 - 0.85 by shafee et al . 2006 ; @xmath111 by miller et al . our measured spin is lower than that obtained by shafee et al . ( 2006 ) , primarily because they assumed that the binary inclination is equal to the inclination of the disk . we instead used the iron line to constrain the inclination of the disk , since there is evidence of potential misalignment of varying degrees in other systems , and since the data clearly favor a higher inclination when self - consistent reflection features are considered . additionally , our model uses _ simpl _ rather than a power - law , which avoids a systematic overestimate of the spin due to the divergence of a power - law at low energy ( see e.g. steiner et al . last , our model replaces the _ edge _ and _ smedge _ functions adopted by shafee et al . ( 2006 ) with newer model components that treat absorption and emission features self - consistently while also properly taking relativistic effects into account . [ fig:1543contours ] our measurement is consistent with that from miller et al . our method differs from this prior work in that we require the normalization of _ kerrbb _ to be fixed to 1 , and we use a different combination of models to explain the reflected continuum . we also examine a different set of observations , focusing specifically on spectra which meet all the criteria necessary for use of the continuum fitting method . additionally we use _ kerrbb2 _ which provides its own method of determining the value of @xmath11 to input to _ kerrbb_. to make a direct comparison , we decided to fit spectra for 16 evenly spaced values of @xmath23 and 31 evenly spaced values of @xmath22 , for the range @xmath112 and @xmath113 using the _ steppar _ feature in xspec ( this range was refined from our original range , which included the binary inclination @xmath114 and stepped @xmath22 between 0 and 0.998 ) . in all of these fits , values of @xmath115 and @xmath116 were allowed to vary within the range allowed by our grid , and were jointly determined by all 15 spectra . the resulting contours of @xmath13 are shown in figure [ fig:1543contours ] . it is clear that when the mass and distance are allowed to vary , the best - fitting spin is equivalent to that determined by miller et al . thus , our model aggrees with both shafee et al . ( 2006 ) and with miller et al . ( 2009 ) when similar parameter constraints are applied . [ fig : jetpower ] 4u 1543 - 47 was also detected during outburst in the radio by park et al . ( 2004 ) . assuming that this radio emission is tied to a jet , we can use the peak radio luminosity obtained as an approximation of the power launched in the jet , and we can compare this particular source to existing models of jet production in black hole binaries . one such model is that from narayan & mcclintock ( 2012 ) , who find that the jet power , when scaled to account for the different masses and distances of different sources , is related to the spin of the black hole . their quantity for jet power @xmath117 is simply the observed beam - corrected radio flux . @xmath118 scaled by the mass and distance of the black hole , as well as a correction for frequency ( @xmath119 ) at which the source was observed . @xmath120 the quantities @xmath121 and @xmath10 are the doppler factor and the radio spectral index respectively . the doppler factor is determined by the velocity of the jet ( @xmath122 ) , the lorentz factor ( @xmath123 ) , and the inclination ( @xmath23 ) . @xmath124)^{-1}\ ] ] the radio spectral index is usually determined empirically , using multiwavelength observations of the source . for 4u 1543 - 47 , we used @xmath125 ( king et al . 2013 ) . the peak flux reported in park et al . ( 2004 ) is @xmath126 at 1.03 ghz . using the mass and distance to the source and the inclination as measured by our model , we have calculated the approximate jet power for two different values of the lorentz factor . they are both plotted in figure [ fig : jetpower ] . the uncertainties are equivalent to half of the measured @xmath117 since @xmath10 is uncertain , and since the peak radio flux produced may be higher than that observed . also plotted are the spins and @xmath117 values for six additional black holes , whose spins have been measured by continuum fitting ( steiner et al . 2013 and references therein , morningstar et al . 2014 ) . it is clear that , although the other six sources are well described by the narayan & mcclintock ( 2012 ) model , 4u 1543 - 47 is not . narayan & mcclintock ( 2012 ) suggest that the observed radio flux of 4u 1543 - 47 may only be a lower limit , since the source was not examined during the entirety of its outburst . therefore it is still possible that at some point the power in the jet was sufficient to be represented by their model , although the flux would have needed to be considerably larger ( @xmath127 for @xmath128 , or @xmath129 for @xmath130 ) .

we present a new analysis of rossi x - ray timing explorer observations of the 2002 outburst of the transient x - ray nova 4u 1543 - 47 . previous works have found that use of these methods individually returns contradictory values for the dimensionless spin parameter @xmath0 . we discuss limitations of our analysis , systematic uncertainties , and implications of this measurement , and compare our result to those previously claimed for 4u 1543 - 47 .

we present a new analysis of rossi x - ray timing explorer observations of the 2002 outburst of the transient x - ray nova 4u 1543 - 47 . we focus on observations in the high / soft state , and attempt to measure the `` spin '' of the black hole by simultaneously fitting the thermal disk continuum and by modeling the broadened iron k - shell emission lines and additional blurred reflection features . previous works have found that use of these methods individually returns contradictory values for the dimensionless spin parameter @xmath0 . we find that when used in conjunction with each other , a moderate spin is obtained ( @xmath1 ) that is actually consistent with both other values within errors . we discuss limitations of our analysis , systematic uncertainties , and implications of this measurement , and compare our result to those previously claimed for 4u 1543 - 47 . [ firstpage ]

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interacting and merging galaxies are among the most fascinating astronomical objects in the universe . these galaxy systems span a wide range of configurations , from single distant encounters to close encounters which may result in a single merged system . typical morphologies include bridges between the interacting partners and tidal tails . these structures are usually associated with sites of strong star formation resulting in dense star clusters or even dwarf galaxy sized objects . additionally , a central star burst might be triggered by tidally induced bars which funnel matter to the galactic center . this coupling between galactic dynamics and star formation processes provides a unique tool for a deeper understanding of galactic evolution . from a theoretical standpoint , interactions and mergers are considered to be major drivers of galactic evolution , affecting morphological and spectral characteristics , gas - dynamics , high - energy processes , and nuclear activity . a merger sequence for the formation of elliptical galaxies from interacting spirals was first proposed by @xcite based on numerical simulations . inclusion of gas dynamics and star formation using tree - sph codes is now the state of the art ( cf . @xcite ) and allows a variety of predictions for the induced star formation and dynamical phenomena to be compared with observations . a review of these processes and of the growing evidence that mergers play a major role in the delayed formation of elliptical and early - type disk galaxies both in the field and in clusters can be found in @xcite . observations of galaxy pairs at intermediate redshifts have revealed a larger number of such systems in the past ( @xcite , but see also @xcite ) , confirming that merging plays an important role in galaxy evolution . this is suggested , for example , by the excess of blue star - forming galaxies at intermediate redshifts @xcite . however , most previous work has been limited to small samples of objects covering a small area on the sky , thus making the statistical analyses less than ideal . the best known catalogs of interacting and merging pairs of galaxies are , course , those by vorontsov - velyaminov @xcite and @xcite , and many interacting and merging pairs can also be found in @xcite s _ atlas of peculiar galaxies_. the vorontsov - velyaminov catalog of interacting galaxies , updated in a web edition in 1999 by r. i. noskova & v. p. arkhipova of the sternberg astronomical insitute , contains 2014 systems , mostly confined to declinations north of @xmath2 , complete for galaxies brighter than @xmath3 . the vorontsov - velyaminov catalog is not restricted to isolated galaxy pairs , but also contains peculiar single galaxies , tight groups , `` nests '' @xcite , and chains of galaxies . @xcite , on the other hand , searched explicitly for galaxy pairs that were isolated . using @xcite s _ catalogue of galaxies & clusters of galaxies _ as his source for galaxy positions and magnitudes , he identified 603 isolated pairs north of @xmath4 for galaxies down to @xmath5 . due to its size , completeness , and relatively unbiased selection , this catalog has been a popular sample for studies of isolated galaxy pairs ( @xcite ; among others ) . other catalogs of galaxy pairs include an extension of the karachentsev catalog by @xcite , which netted 409 candidate isolated pairs , 214 of which lie in the southern hemisphere , and a catalog of 621 southern isolated pairs identified by @xcite using a surface density enhancement method . both these catalogs were extacted from the _ the surface photometry catalogue of the eso - uppsala galaxies _ @xcite , which is a galaxy catalog complete to @xmath6 @xcite . finally , the advent of large redshift surveys has made it possible to hunt down large , homogeneous samples of galaxy pairs in velocity - space . important among these are the samples by @xcite , who found 251 close pairs in the cfa2 redshift survey , and by @xcite , who found 1258 pairs in the 100 k public release of the 2df galaxy survey . here , we present a catalog of 1479 merging pairs of galaxies extracted from the approximately 462 sq deg of imaging data from the sloan digital sky survey early data release ( sdss edr ; @xcite ) . we provide an overview of the sdss edr in [ sec : data ] , present our selection criteria in [ sec : selectioncriteria ] , describe the construction of the catalog in [ sec : construction ] , present the catalog itself in [ sec : prop ] , and draw conclusions in [ sec : conclusion ] .

we present a new catalog of merging galaxies obtained through an automated systematic search routine . the 1479 new pairs of merging galaxies were found in @xmath0 462 sq deg of the sloan digital sky survey early data release ( sdss edr ; @xcite ) photometric data , and the pair catalog is complete for galaxies in the magnitude range @xmath1 .

we present a new catalog of merging galaxies obtained through an automated systematic search routine . the 1479 new pairs of merging galaxies were found in @xmath0 462 sq deg of the sloan digital sky survey early data release ( sdss edr ; @xcite ) photometric data , and the pair catalog is complete for galaxies in the magnitude range @xmath1 . the selection algorithm , implementing a variation on the original @xcite criteria , proved to be very efficient and fast . merging galaxies were selected such that the inter - galaxy separations were less than the sum of the component galaxies radii . we discuss the characteristics of the sample in terms of completeness , pair separation , and the holmberg effect . we also present an online atlas of images for the sdss edr pairs obtained using the corrected frames from the sdss edr database . the atlas images also include the relevant data for each pair member . this catalog will be useful for conducting studies of the general characteristics of merging galaxies , their environments , and their component galaxies . the redshifts for a subset of the interacting and merging galaxies and the distribution of angular sizes for these systems indicate the sdss provides a much deeper sample than almost any other wide - area catalog to date .

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we have presented an algorithm for the automated identification of merging galaxy pair candidates from the sdss data . the algorithm , which implements a variation of @xcite s isolated pair criteria , proves to be very efficient and fast . within the @xmath0462 sq deg of the sdss edr photometric data set , we have identified 1479 merging galaxy pair candidates for galaxies in the magnitude range @xmath86 , where we define _ a merging pair _ as one in which the two galaxy centers are separated by less than the sum of the members petrosian radii . by our definition , we estimate that approximately 0.5% of sdss edr galaxies are members of merging pairs . we provide a catalog and an online atlas of all 1479 merging pair candidates . analysis indicates that the merging pair galaxies tend to be slightly bluer than a corresponding field sample from the sdss edr . furthermore , compared to the field sample , the merging pair sample is weighted toward later type galaxies . we take this result of active star formation occurring within merging pair galaxies . finally , we studied the color concordance of galaxy members in each pair . using much smaller samples , @xcite and others have found the linear correlation coefficient for the @xmath69 colors of pair galaxies to be @xmath87 . we find that the strength of the color concordance varies drastically with color index , with the @xmath72 colors of pair galaxies showing the strongest and most significant concordance ( @xmath88 ) and the @xmath77 colors showing the weakest and least significant concordance ( @xmath89 ) . surprisingly , although @xmath90 for stellar populations , we find that the @xmath72 color concordance we measure is only about half the strength of the @xmath69 color concordance measured in other samples . we expect that the difference is due to sample properties : the galaxies in an sdss edr merging pair are on average much closer together than the galaxies in a pair from one of these other samples . it may be that the galaxies in sdss edr merging pairs are undergoing more vigorous and chaotic star formation compared with the galaxies in the generally wider pairs characteristic of these other samples . funding for the creation and distribution of the sdss archive has been provided by the alfred p. sloan foundation , the participating institutions , the national aeronautics and space administration , the national science foundation , the u.s . department of energy , the japanese monbukagakusho , and the max planck society . the sdss web site is http://www.sdss.org/. the sdss is managed by the astrophysical research consortium ( arc ) for the participating institutions . the participating institutions are the university of chicago , fermilab , the institute for advanced study , the japan participation group , the johns hopkins university , los alamos national laboratory , the max - planck - institute for astronomy ( mpia ) , the max - planck - institute for astrophysics ( mpa ) , new mexico state university , university of pittsburgh , princeton university , the united states naval observatory , and the university of washington . this research has made use of the nasa / ipac extragalactic database ( ned ) , which is operated by the jet propulsion laboratory , caltech , under contract with the national aeronautics and space administration . rrrrrr 94 & 83 & 119107 & 590 & 7.1 & 0.0050 + 125 & 83 & 117235 & 378 & 4.55 & 0.0032 + 752 & 114 & 142785 & 716 & 4.53 & 0.0050 + 756 & 114 & 141124 & 958 & 8.4 & 0.0068 + 1336 & 16 & 20217 & 92 & 5.75 & 0.0046 + 1339 & 16 & 19379 & 84 & 5.25 & 0.0043 + 1356 & 17 & 20191 & 80 & 4.7 & 0.0040 + 1359 & 19 & 19610 & 60 & 3.15 & 0.0031 + total & 462 & 458524 & 2958 & 6.4 & 0.0065 + c@c@c@c@c@c@c@c@c@c@c@c@c@c 1 & 00:02:49.25 & + 00:45:05.77 & 18.544 & 16.367 & 15.369 & 14.818 & 14.463 & 5.856 & sdss j000249.06 + 004504.83 & 0.086497 & sdss j000249.43 + 004506.72 & - + 2 & 00:03:57.29 & + 00:28:29.21 & 19.137 & 17.788 & 16.944 & 16.509 & 16.193 & 5.708 & sdss j000357.27 + 002832.06 & 0.084922 & sdss j000357.30 + 002826.37 & - + 3 & 00:06:46.67 & -00:36:55.26 & 20.487 & 19.401 & 18.725 & 18.411 & 18.128 & 5.633 & sdss j000646.74 - 003652.62 & - & sdss j000646.60 - 003657.90 & - + 4 & 00:07:17.63 & + 00:50:20.14 & 18.257 & 16.706 & 15.912 & 15.491 & 15.143 & 12.453 & sdss j000717.23 + 005018.52 & 0.102078 & sdss j000718.03 + 005021.76 & - + 5 & 00:07:20.49 & + 00:29:34.40 & 18.113 & 16.128 & 15.122 & 14.666 & 14.309 & 8.690 & sdss j000720.21 + 002933.20 & - & sdss j000720.77 + 002935.60 & 0.091190 + 6 & 00:07:55.69 & + 00:32:55.12 & 19.589 & 18.458 & 17.962 & 17.659 & 17.540 & 5.530 & sdss j000755.59 + 003252.81 & - & sdss j000755.79 + 003257.44 & - + 7 & 00:08:26.77 & + 00:22:13.31 & 19.042 & 17.578 & 16.918 & 16.458 & 16.076 & 11.506 & sdss j000826.52 + 002209.00 & 0.054646 & sdss j000827.02 + 002217.61 & - + 8 & 00:08:32.70 & + 01:02:20.20 & 18.806 & 17.235 & 16.564 & 16.083 & 15.824 & 4.089 & sdss j000832.83 + 010219.86 & 0.060147 & sdss j000832.56 + 010220.54 & - + 9 & 00:09:43.89 & -00:06:12.18 & 20.268 & 18.506 & 17.386 & 16.902 & 16.557 & 4.151 & sdss j000943.83 - 000610.34 & - & sdss j000943.96 - 000614.03 & - + 10 & 00:10:11.01 & -00:14:30.51 & 18.060 & 16.345 & 15.496 & 15.052 & 14.791 & 3.726 & sdss j001011.13 - 001430.82 & 0.113350 & sdss j001010.89 - 001430.19 & - + 11 & 00:10:19.49 & + 00:56:32.56 & 19.056 & 18.128 & 17.238 & 16.918 & 16.570 & 6.544 & sdss j001019.64 + 005630.31 & - & sdss j001019.33 + 005634.81 & 0.157578 + 12 & 00:10:38.99 & + 00:28:25.37 & 19.212 & 17.482 & 16.500 & 16.038 & 15.748 & 7.011 & sdss j001039.11 + 002828.39 & 0.105247 & sdss j001038.87 + 002822.35 & - + 13 & 00:10:45.51 & -00:07:43.94 & 18.049 & 16.895 & 16.431 & 16.093 & 15.845 & 7.854 & sdss j001045.54 - 000740.04 & 0.086649 & sdss j001045.47 - 000747.84 & - + 14 & 00:11:28.26 & + 01:04:02.53 & 20.077 & 18.686 & 17.733 & 17.263 & 17.024 & 4.373 & sdss j001128.38 + 010401.34 & - & sdss j001128.13 + 010403.72 & - + 15 & 00:11:43.89 & + 00:31:23.88 & 16.811 & 15.908 & 15.580 & 15.289 & 15.236 & 6.562 & sdss j001144.08 + 003125.34 & - & sdss j001143.69 + 003122.41 & 0.072570 + 16 & 00:12:29.90 & + 00:39:09.88 & 21.658 & 18.900 & 17.415 & 16.892 & 16.585 & 3.435 & sdss j001229.84 + 003911.32 & 0.250288 & sdss j001229.97 + 003908.44 & - + 17 & 00:12:38.11 & + 00:49:51.93 & 18.644 & 17.065 & 16.406 & 15.988 & 15.743 & 5.658 & sdss j001238.04 + 004949.34 & 0.064733 & sdss j001238.19 + 004954.53 & - + 18 & 00:12:40.44 & -00:02:47.60 & 19.243 & 18.383 & 18.320 & 18.180 & 18.147 & 6.407 & sdss j001240.56 - 000250.21 & - & sdss j001240.32 - 000244.99 & - + 19 & 00:12:50.94 & + 00:17:22.94 & 19.624 & 17.675 & 16.592 & 16.125 & 15.758 & 4.411 & sdss j001250.98 + 001725.08 & 0.147479 & sdss j001250.90 + 001720.81 & - + 20 & 00:12:54.68 & -00:32:54.91 & 19.732 & 18.213 & 17.282 & 17.022 & 16.869 & 4.590 & sdss j001254.53 - 003255.52 & - & sdss j001254.82 - 003254.31 & - + 21 & 00:12:56.94 & + 00:19:10.84 & 20.569 & 18.851 & 17.916 & 17.413 & 17.186 & 3.167 & sdss j001256.86 + 001909.84 & - & sdss j001257.03 + 001911.84 & - + 22 & 00:13:15.11 & + 00:02:43.32 & 17.729 & 16.334 & 15.470 & 15.268 & 15.135 & 7.712 & sdss j001315.28 + 000240.48 & 0.090181 & sdss j001314.93 + 000246.16 & - + 23 & 00:13:47.22 & + 00:46:07.25 & 18.404 & 16.325 & 15.176 & 14.633 & 14.181 & 11.532 & sdss j001347.32 + 004601.68 & - & sdss j001347.12 + 004612.82 & 0.155520 + 24 & 00:13:54.68 & -00:36:33.33 & 18.436 & 17.127 & 16.554 & 16.093 & 15.799 & 10.153 & sdss j001354.91 - 003629.68 & - & sdss j001354.44 - 003636.98 & - + 25 & 00:14:27.29 & + 01:15:15.10 & 19.315 & 18.239 & 17.936 & 17.664 & 17.560 & 6.223 & sdss j001427.47 + 011516.74 & - & sdss j001427.11 + 011513.46 & - + 26 & 00:15:26.70 & -00:58:15.74 & 19.070 & 18.064 & 17.421 & 16.961 & 16.683 & 5.370 & sdss j001526.78 - 005818.10 & 0.167064 & sdss j001526.61 - 005813.38 & - + 27 & 00:15:30.47 & -00:48:06.60 & 18.224 & 16.138 & 15.266 & 14.740 & 14.425 & 17.741 & sdss j001531.05 - 004805.65 & - & sdss j001529.88 - 004807.56 & 0.155471 + 28 & 00:17:28.49 & + 01:06:48.88 & 19.897 & 19.088 & 18.465 & 18.135 & 18.058 & 3.208 & sdss j001728.50 + 010650.47 & - & sdss j001728.47 + 010647.30 & - + 29 & 00:17:53.87 & + 01:13:54.08 & 18.707 & 17.492 & 16.507 & 16.103 & 15.814 & 5.854 & sdss j001753.98 + 011351.70 & - & sdss j001753.76 + 011356.46 & - + 30 & 00:17:54.30 & + 00:27:52.09 & 20.503 & 18.601 & 17.334 & 16.908 & 16.548 & 5.899 & sdss j001754.39 + 002754.71 & - & sdss j001754.21 + 002749.46 & - + 31 & 00:18:02.89 & -00:34:30.26 & 20.867 & 19.198 & 18.252 & 17.808 & 17.533 & 3.082 & sdss j001802.87 - 003431.77 & - & sdss j001802.91 - 003428.75 & - + 32 & 00:18:10.22 & -00:04:28.62 & 18.234 & 17.225 & 16.873 & 16.818 & 16.613 & 7.455 & sdss j001810.47 - 000428.73 & - & sdss j001809.97 - 000428.51 & - + 33 & 00:18:28.20 & -00:34:11.45 & 16.725 & 15.791 & 15.331 & 14.950 & 14.754 & 3.681 & sdss j001828.30 - 003410.51 & 0.069362 & sdss j001828.09 - 003412.38 & 0.069319 + 34 & 00:18:28.56 & -00:19:58.66 & 18.966 & 17.011 & 15.927 & 15.517 & 15.157 & 9.518 & sdss j001828.45 - 001954.17 & - & sdss j001828.66 - 002003.14 & 0.157433 + 35 & 00:18:29.31 & -00:32:21.20 & 17.788 & 16.362 & 15.728 & 15.316 & 14.999 & 5.328 & sdss j001829.48 - 003221.15 & 0.069018 & sdss j001829.13 - 003221.24 & - + 36 & 00:19:06.45 & -01:08:23.33 & 19.629 & 18.017 & 16.955 & 16.486 & 16.286 & 5.213 & sdss j001906.34 - 010825.33 & 0.151968 & sdss j001906.56 - 010821.33 & - + 37 & 00:19:30.96 & -00:36:08.16 & 17.050 & 16.297 & 15.974 & 15.791 & 15.574 & 9.202 & sdss j001930.68 - 003606.35 & 0.032851 & sdss j001931.25 - 003609.97 & - + 38 & 00:20:00.33 & -00:50:42.56 & 18.919 & 17.222 & 16.153 & 15.715 & 15.379 & 7.720 & sdss j002000.12 - 005044.66 & 0.188464 & sdss j002000.55 - 005040.47 & - + 39 & 00:20:10.89 & -00:48:56.86 & 18.366 & 16.615 & 15.593 & 15.135 & 14.758 & 10.396 & sdss j002010.67 - 004852.85 & 0.141251 & sdss j002011.11 - 004900.87 & - + 40 & 00:20:31.52 & + 00:22:19.07 & 19.518 & 18.693 & 18.205 & 17.918 & 17.843 & 4.068 & sdss j002031.46 + 002220.86 & - & sdss j002031.58 + 002217.27 & - + 41 & 00:20:55.03 & -00:32:33.40 & 20.626 & 19.476 & 19.032 & 18.849 & 18.788 & 2.759 & sdss j002055.05 - 003234.76 & - & sdss j002055.02 - 003232.03 & - + 42 & 00:20:56.23 & -00:01:12.96 & 19.172 & 18.316 & 17.882 & 17.673 & 17.431 & 4.605 & sdss j002056.17 - 000115.13 & - & sdss j002056.28 - 000110.79 & - + 43 & 00:21:43.84 & -00:51:14.43 & 19.237 & 16.914 & 15.923 & 15.483 & 15.172 & 4.092 & sdss j002143.74 - 005115.71 & - & sdss j002143.95 - 005113.16 & - + 44 & 00:22:08.76 & + 00:22:01.62 & 17.996 & 15.991 & 15.112 & 14.652 & 14.271 & 3.096 & sdss j002208.69 + 002200.48 & - & sdss j002208.83 + 002202.76 & 0.070563 + 45 & 00:22:17.60 & + 00:39:53.60 & 19.548 & 18.225 & 17.658 & 17.265 & 17.127 & 4.148 & sdss j002217.47 + 003952.63 & - & sdss j002217.72 + 003954.56 & - + 46 & 00:22:55.43 & -00:08:45.95 & 19.740 & 17.913 & 16.901 & 16.401 & 16.012 & 6.352 & sdss j002255.59 - 000848.16 & 0.160888 & sdss j002255.28 - 000843.75 & - + 47 & 00:23:01.70 & + 01:11:03.66 & 18.051 & 16.541 & 16.195 & 15.836 & 15.731 & 7.982 & sdss j002301.76 + 011059.77 & - & sdss j002301.64 + 011107.54 & - + 48 & 00:23:05.32 & + 00:00:29.80 & 20.068 & 19.119 & 18.708 & 18.467 & 18.593 & 2.718 & sdss j002305.28 + 000028.57 & - & sdss j002305.36 + 000031.02 & - + 49 & 00:23:15.35 & -01:10:43.69 & 19.008 & 17.372 & 16.561 & 16.140 & 15.890 & 4.937 & sdss j002315.36 - 011041.23 & 0.063074 & sdss j002315.35 - 011046.16 & - + 50 & 00:23:16.36 & -01:01:14.39 & 19.796 & 18.932 & 18.526 & 18.342 & 18.225 & 7.878 & sdss j002316.21 - 010117.65 & - & sdss j002316.51 - 010111.13 & - + 51 & 00:25:40.91 & -00:27:06.19 & 19.407 & 18.730 & 18.312 & 18.205 & 18.247 & 3.194 & sdss j002540.87 - 002704.68 & - & sdss j002540.94 - 002707.69 & - + 52 & 00:25:50.59 & + 00:30:01.10 & 17.568 & 16.260 & 15.486 & 15.396 & 15.271 & 4.225 & sdss j002550.65 + 003002.99 & 0.063879 & sdss j002550.52 + 002959.22 & - + 53 & 00:26:15.70 & -00:26:47.30 & 19.589 & 18.431 & 17.833 & 17.484 & 17.231 & 6.524 & sdss j002615.81 - 002650.13 & - & sdss j002615.59 - 002644.46 & - + 54 & 00:26:30.87 & + 00:16:00.67 & 20.748 & 19.520 & 18.566 & 18.177 & 17.815 & 3.080 & sdss j002630.95 + 001601.60 & - & sdss j002630.79 + 001559.73 & - + 55 & 00:27:58.77 & -00:06:31.16 & 17.473 & 16.156 & 15.598 & 15.263 & 14.951 & 11.750 & sdss j002758.54 - 000626.42 & - & sdss j002759.00 - 000635.90 & 0.060550 + 56 & 00:28:02.72 & + 00:49:37.85 & 17.860 & 16.664 & 16.154 & 15.808 & 15.574 & 3.753 & sdss j002802.83 + 004937.21 & 0.082002 & sdss j002802.60 + 004938.49 & - + 57 & 00:28:18.45 & -00:10:13.02 & 20.043 & 18.904 & 18.237 & 17.902 & 17.619 & 3.273 & sdss j002818.46 - 001014.66 & - & sdss j002818.45 - 001011.38 & - + 58 & 00:28:35.83 & -00:36:57.00 & 20.102 & 18.728 & 18.197 & 17.843 & 17.460 & 11.061 & sdss j002835.64 - 003652.24 & - & sdss j002836.01 - 003701.75 & - + 59 & 00:28:38.64 & -00:52:36.60 & 19.352 & 18.367 & 18.038 & 17.768 & 17.706 & 2.417 & sdss j002838.67 - 005237.72 & - & sdss j002838.61 - 005235.47 & - + 60 & 00:28:55.11 & -00:04:21.43 & 17.507 & 16.139 & 15.446 & 15.061 & 14.800 & 8.449 & sdss j002854.85 - 000422.95 & - & sdss j002855.37 - 000419.91 & 0.063224 + 61 & 00:28:56.84 & + 00:40:37.01 & 19.274 & 17.396 & 16.415 & 15.930 & 15.579 & 1.830 & sdss j002856.80 + 004037.69 & 0.089929 & sdss j002856.88 + 004036.33 & - + 62 & 00:29:01.57 & + 00:19:26.31 & 18.334 & 16.770 & 16.021 & 15.878 & 15.600 & 8.980 & sdss j002901.86 + 001927.06 & - & sdss j002901.27 + 001925.57 & - + 63 & 00:29:16.80 & -01:00:23.25 & 16.652 & 15.946 & 15.716 & 15.729 & 15.720 & 3.894 & sdss j002916.79 - 010025.20 & 0.013459 & sdss j002916.81 - 010021.31 & - + 64 & 00:29:27.58 & -00:11:48.04 & 19.104 & 18.006 & 17.728 & 17.611 & 17.770 & 5.537 & sdss j002927.74 - 001149.52 & - & sdss j002927.43 - 001146.56 & - + 65 & 00:29:37.84 & -00:06:15.28 & 20.838 & 19.529 & 18.674 & 18.181 & 17.917 & 4.359 & sdss j002937.99 - 000615.20 & - & sdss j002937.70 - 000615.37 & - + 66 & 00:30:04.61 & -00:29:27.08 & 19.874 & 18.827 & 18.243 & 17.774 & 17.573 & 4.645 & sdss j003004.62 - 002929.41 & - & sdss j003004.61 - 002924.76 & - + 67 & 00:30:20.56 & -01:06:47.39 & 19.920 & 18.124 & 16.811 & 16.237 & 15.871 & 2.734 & sdss j003020.54 - 010646.04 & 0.226033 & sdss j003020.57 - 010648.74 & - + 68 & 00:30:25.59 & -00:42:00.78 & 18.423 & 17.445 & 16.953 & 16.538 & 16.368 & 2.766 & sdss j003025.66 - 004201.64 & 0.107380 & sdss j003025.51 - 004159.92 & - + 69 & 00:31:07.62 & + 00:00:33.89 & 19.817 & 18.801 & 18.388 & 18.123 & 17.936 & 6.586 & sdss j003107.50 + 000031.12 & - & sdss j003107.74 + 000036.65 & - + 70 & 00:31:22.43 & + 00:18:39.66 & 18.134 & 16.510 & 15.719 & 15.287 & 14.874 & 8.321 & sdss j003122.49 + 001843.70 & 0.094798 & sdss j003122.36 + 001835.62 & - + 71 & 00:32:02.51 & + 00:17:44.82 & 18.705 & 16.725 & 15.783 & 15.323 & 14.876 & 8.105 & sdss j003202.44 + 001748.74 & 0.081327 & sdss j003202.58 + 001740.90 & - + 72 & 00:32:10.59 & -00:52:40.86 & 19.679 & 17.792 & 16.747 & 16.331 & 15.948 & 8.205 & sdss j003210.32 - 005241.40 & 0.096586 & sdss j003210.86 - 005240.32 & - + 73 & 00:32:14.52 & + 00:29:37.91 & 20.286 & 18.760 & 18.231 & 17.890 & 17.629 & 3.763 & sdss j003214.55 + 002936.06 & - & sdss j003214.50 + 002939.75 & - + 74 & 00:32:36.06 & + 00:06:52.30 & 18.333 & 17.525 & 17.198 & 17.132 & 17.252 & 8.240 & sdss j003235.84 + 000654.78 & - & sdss j003236.28 + 000649.83 & - + 75 & 00:33:11.37 & -00:36:45.36 & 19.496 & 18.434 & 17.863 & 17.573 & 17.460 & 3.577 & sdss j003311.40 - 003647.08 & - & sdss j003311.34 - 003643.63 & - + 76 & 00:33:33.23 & -00:50:01.27 & 19.213 & 17.859 & 16.924 & 16.536 & 16.201 & 6.017 & sdss j003333.06 - 004959.68 & 0.119782 & sdss j003333.40 - 005002.86 & - + 77 & 00:33:39.76 & -00:55:20.37 & 20.803 & 19.518 & 18.730 & 18.380 & 17.969 & 4.931 & sdss j003339.85 - 005522.37 & - & sdss j003339.66 - 005518.36 & - + 78 & 00:34:10.00 & -00:17:15.86 & 18.708 & 17.661 & 17.378 & 17.167 & 17.082 & 5.790 & sdss j003409.94 - 001718.63 & 0.057981 & sdss j003410.05 - 001713.09 & - + 79 & 00:35:24.10 & + 00:23:58.98 & 19.900 & 18.593 & 17.450 & 16.963 & 16.449 & 2.569 & sdss j003524.12 + 002400.21 & - & sdss j003524.07 + 002357.76 & - + 80 & 00:35:46.88 & + 01:08:09.04 & 17.737 & 16.589 & 16.058 & 15.639 & 15.388 & 8.697 & sdss j003547.00 + 010805.10 & 0.055626 & sdss j003546.76 + 010812.98 & - + 81 & 00:36:01.26 & -00:06:40.54 & 20.202 & 18.206 & 17.021 & 16.473 & 15.988 & 6.141 & sdss j003601.08 - 000641.74 & - & sdss j003601.45 - 000639.34 & - + 82 & 00:36:50.33 & + 00:02:03.11 & 17.837 & 17.126 & 16.809 & 16.314 & 16.330 & 3.660 & sdss j003650.42 + 000201.92 & 0.111705 & sdss j003650.24 + 000204.31 & - + 83 & 00:37:11.73 & + 00:05:46.92 & 20.604 & 18.598 & 17.059 & 16.507 & 16.214 & 3.532 & sdss j003711.82 + 000545.69 & 0.258729 & sdss j003711.65 + 000548.16 & - + 84 & 00:37:36.65 & + 00:00:18.25 & 20.110 & 17.860 & 16.750 & 16.258 & 15.828 & 9.229 & sdss j003736.96 + 000018.49 & - & sdss j003736.34 + 000018.01 & - + 85 & 00:38:14.41 & + 00:14:19.75 & 19.563 & 18.350 & 17.479 & 17.063 & 16.876 & 5.617 & sdss j003814.59 + 001420.69 & - & sdss j003814.24 + 001418.81 & - + 86 & 00:39:11.31 & + 00:16:40.96 & 20.203 & 19.427 & 19.114 & 18.861 & 18.959 & 3.158 & sdss j003911.25 + 001639.70 & - & sdss j003911.38 + 001642.22 & - + 87 & 00:39:11.49 & -00:57:51.74 & 18.580 & 16.776 & 15.861 & 15.412 & 15.094 & 7.624 & sdss j003911.34 - 005754.83 & 0.080994 & sdss j003911.64 - 005748.65 & - + 88 & 00:39:37.34 & + 00:12:34.29 & 18.680 & 17.100 & 16.269 & 15.926 & 15.722 & 7.514 & sdss j003937.28 + 001237.96 & 0.080166 & sdss j003937.39 + 001230.62 & - + 89 & 00:39:40.48 & -00:33:32.18 & 18.070 & 17.247 & 16.878 & 16.533 & 16.324 & 8.019 & sdss j003940.30 - 003329.13 & 0.116745 & sdss j003940.65 - 003335.22 & - + 90 & 00:40:12.61 & -01:14:13.32 & 19.831 & 18.643 & 17.399 & 16.942 & 16.648 & 6.843 & sdss j004012.84 - 011413.20 & - & sdss j004012.38 - 011413.45 & - + 91 & 00:40:49.48 & + 00:01:52.53 & 17.810 & 16.579 & 16.027 & 15.700 & 15.546 & 7.210 & sdss j004049.24 + 000152.72 & 0.034640 & sdss j004049.72 + 000152.34 & - + 92 & 00:41:14.41 & + 00:00:11.92 & 17.996 & 16.209 & 15.318 & 14.914 & 14.548 & 3.728 & sdss j004114.44 + 000013.71 & 0.109246 & sdss j004114.37 + 000010.14 & - + 93 & 00:42:17.62 & + 01:09:29.05 & 19.485 & 18.266 & 17.939 & 17.814 & 17.926 & 6.170 & sdss j004217.83 + 010929.44 & - & sdss j004217.42 + 010928.65 & - + 94 & 00:43:43.94 & + 01:02:16.04 & 17.968 & 16.785 & 16.222 & 15.858 & 15.668 & 4.737 & sdss j004344.08 + 010215.07 & - & sdss j004343.80 + 010217.01 & 0.106895 + 95 & 00:44:04.18 & + 01:11:20.27 & 20.451 & 18.643 & 17.704 & 17.230 & 16.825 & 3.560 & sdss j004404.29 + 011119.53 & - & sdss j004404.08 + 011121.01 & - + 96 & 00:44:17.67 & + 00:08:47.41 & 20.946 & 18.835 & 17.547 & 17.010 & 16.745 & 3.242 & sdss j004417.56 + 000847.36 & - & sdss j004417.78 + 000847.46 & - + 97 & 00:44:18.87 & + 01:07:39.09 & 19.386 & 17.626 & 16.679 & 16.264 & 15.916 & 6.120 & sdss j004419.08 + 010739.14 & - & sdss j004418.67 + 010739.03 & - + 98 & 00:44:45.78 & -00:58:00.93 & 19.157 & 18.480 & 18.270 & 17.998 & 17.919 & 4.323 & sdss j004445.67 - 005759.50 & - & sdss j004445.88 - 005802.37 & - + 99 & 00:44:59.62 & -01:01:24.87 & 17.345 & 16.020 & 15.240 & 14.833 & 14.515 & 11.930 & sdss j004459.23 - 010124.31 & 0.107010 & sdss j004500.02 - 010125.42 & - + 100 & 00:45:15.56 & -01:13:17.81 & 18.231 & 17.323 & 16.922 & 16.641 & 16.642 & 3.244 & sdss j004515.67 - 011317.90 & - & sdss j004515.45 - 011317.72 & 1.597980 + 101 & 00:45:24.08 & -01:14:09.36 & 19.306 & 17.489 & 16.430 & 15.981 & 15.786 & 5.578 & sdss j004524.26 - 011408.66 & 0.118817 & sdss j004523.90 - 011410.06 & - + 102 & 00:46:05.08 & -00:58:36.91 & 19.263 & 17.602 & 16.244 & 15.829 & 15.447 & 3.029 & sdss j004605.16 - 005835.85 & - & sdss j004605.01 - 005837.97 & 0.111324 + 103 & 00:46:11.10 & -00:05:10.80 & 17.994 & 16.653 & 15.995 & 15.663 & 15.293 & 7.837 & sdss j004611.35 - 000509.77 & 0.114100 & sdss j004610.84 - 000511.84 & - + 104 & 00:46:12.57 & + 00:01:40.10 & 19.197 & 17.344 & 16.367 & 15.910 & 15.713 & 4.409 & sdss j004612.72 + 000140.54 & 0.115360 & sdss j004612.43 + 000139.66 & - + 105 & 00:46:22.47 & + 00:45:35.26 & 20.106 & 18.636 & 17.624 & 17.132 & 16.726 & 4.921 & sdss j004622.63 + 004534.50 & - & sdss j004622.32 + 004536.02 & - + 106 & 00:46:39.37 & + 01:08:27.00 & 19.090 & 17.369 & 16.730 & 16.266 & 16.194 & 4.076 & sdss j004639.28 + 010825.40 & - & sdss j004639.45 + 010828.60 & - + 107 & 00:46:44.32 & -00:36:55.68 & 19.823 & 18.731 & 18.026 & 17.607 & 17.365 & 4.644 & sdss j004644.25 - 003657.74 & - & sdss j004644.40 - 003653.63 & - + 108 & 00:47:20.56 & + 00:25:16.19 & 19.973 & 17.191 & 16.070 & 15.586 & 15.117 & 4.404 & sdss j004720.64 + 002514.27 & - & sdss j004720.49 + 002518.11 & 0.129092 + 109 & 00:47:26.00 & -00:56:53.01 & 20.373 & 18.294 & 17.131 & 16.726 & 16.381 & 5.023 & sdss j004726.16 - 005653.92 & - & sdss j004725.84 - 005652.09 & - + 110 & 00:47:49.87 & + 00:34:51.37 & 18.381 & 17.460 & 17.190 & 16.861 & 16.715 & 5.762 & sdss j004749.68 + 003451.44 & 0.068672 & sdss j004750.06 + 003451.29 & - + 111 & 00:48:02.74 & + 00:46:09.89 & 19.274 & 17.277 & 16.260 & 15.797 & 15.386 & 3.858 & sdss j004802.64 + 004610.93 & - & sdss j004802.85 + 004608.84 & - + 112 & 00:48:45.78 & + 01:09:41.40 & 20.996 & 19.491 & 18.467 & 18.051 & 17.828 & 3.457 & sdss j004845.84 + 010939.92 & - & sdss j004845.72 + 010942.87 & - + 113 & 00:49:33.99 & -00:57:27.27 & 20.153 & 19.318 & 18.425 & 18.085 & 17.611 & 3.130 & sdss j004933.96 - 005728.74 & - & sdss j004934.03 - 005725.80 & - + 114 & 00:50:12.00 & -00:34:59.29 & 18.284 & 17.337 & 16.859 & 16.903 & 17.390 & 6.550 & sdss j005012.21 - 003458.81 & - & sdss j005011.78 - 003459.77 & - + 115 & 00:50:57.42 & + 01:09:09.59 & 17.974 & 15.842 & 14.948 & 14.510 & 14.166 & 4.070 & sdss j005057.38 + 010911.55 & 0.065331 & sdss j005057.45 + 010907.63 & - + 116 & 00:51:14.02 & + 00:20:48.16 & 17.969 & 16.054 & 15.157 & 15.049 & 14.207 & 3.305 & sdss j005114.11 + 002049.23 & 0.112633 & sdss j005113.94 + 002047.09 & - + 117 & 00:51:18.73 & + 00:13:07.43 & 19.649 & 17.886 & 16.685 & 16.145 & 15.752 & 8.304 & sdss j005118.45 + 001307.11 & 0.190183 & sdss j005119.00 + 001307.74 & - + 118 & 00:51:44.42 & -01:05:39.91 & 19.631 & 17.595 & 16.475 & 15.961 & 15.612 & 9.793 & sdss j005144.52 - 010544.59 & 0.132042 & sdss j005144.32 - 010535.23 & - + 119 & 00:52:06.58 & -00:28:34.68 & 19.823 & 17.820 & 16.735 & 16.234 & 15.792 & 7.670 & sdss j005206.74 - 002831.64 & 0.134547 & sdss j005206.43 - 002837.72 & - + 120 & 00:53:40.04 & + 01:07:12.14 & 19.951 & 17.899 & 16.670 & 16.222 & 15.782 & 8.310 & sdss j005340.32 + 010711.78 & 0.172041 & sdss j005339.76 + 010712.50 & - + 121 & 00:53:55.74 & + 01:02:02.41 & 19.205 & 17.945 & 17.076 & 16.663 & 16.372 & 3.118 & sdss j005355.82 + 010203.33 & - & sdss j005355.65 + 010201.50 & - + 122 & 00:54:11.77 & -00:30:54.59 & 20.464 & 19.796 & 19.345 & 19.069 & 18.590 & 4.258 & sdss j005411.64 - 003053.81 & - & sdss j005411.90 - 003055.37 & - + 123 & 00:54:42.84 & + 00:35:51.61 & 19.314 & 17.163 & 16.712 & 16.532 & 16.542 & 7.029 & sdss j005442.79 + 003555.05 & 0.046319 & sdss j005442.88 + 003548.17 & - + 124 & 00:54:53.37 & -00:59:09.77 & 18.203 & 17.369 & 16.601 & 16.190 & 15.945 & 6.220 & sdss j005453.56 - 005908.59 & 0.146665 & sdss j005453.18 - 005910.95 & - + 125 & 00:54:59.38 & + 00:21:29.20 & 19.074 & 18.540 & 18.102 & 17.993 & 17.430 & 3.749 & sdss j005459.30 + 002130.59 & - & sdss j005459.47 + 002127.81 & - + 126 & 00:55:17.65 & -01:13:56.94 & 19.983 & 18.373 & 17.544 & 17.100 & 16.976 & 6.233 & sdss j005517.44 - 011356.35 & - & sdss j005517.85 - 011357.54 & - + 127 & 00:55:18.51 & -00:49:27.17 & 19.942 & 18.604 & 18.150 & 17.840 & 17.626 & 5.429 & sdss j005518.69 - 004927.45 & - & sdss j005518.33 - 004926.88 & - + 128 & 00:55:19.57 & -00:48:39.78 & 19.729 & 18.451 & 17.935 & 17.637 & 17.411 & 4.035 & sdss j005519.46 - 004838.58 & - & sdss j005519.68 - 004840.98 & - + 129 & 00:55:19.77 & + 00:15:12.63 & 20.254 & 19.003 & 18.230 & 17.794 & 17.414 & 3.275 & sdss j005519.87 + 001511.85 & - & sdss j005519.68 + 001513.41 & - + 130 & 00:55:23.73 & + 01:10:42.58 & 20.760 & 18.906 & 17.705 & 17.206 & 16.917 & 3.844 & sdss j005523.78 + 011040.80 & - & sdss j005523.68 + 011044.36 & - + 131 & 00:55:58.24 & -00:07:54.40 & 18.973 & 17.270 & 16.463 & 16.012 & 15.626 & 6.355 & sdss j005558.22 - 000757.56 & - & sdss j005558.27 - 000751.24 & - + 132 & 00:56:05.32 & -01:08:10.71 & 18.702 & 17.252 & 16.408 & 16.109 & 15.853 & 11.105 & sdss j005604.96 - 010809.42 & 0.044830 & sdss j005605.68 - 010812.01 & - + 133 & 00:56:07.87 & -01:00:56.59 & 19.456 & 17.735 & 16.654 & 16.154 & 15.751 & 9.817 & sdss j005607.80 - 010101.38 & 0.173589 & sdss j005607.94 - 010051.80 & - + 134 & 00:56:09.72 & + 00:06:20.72 & 18.341 & 17.097 & 16.412 & 15.978 & 15.708 & 6.662 & sdss j005609.88 + 000622.89 & 0.044641 & sdss j005609.55 + 000618.54 & - + 135 & 00:56:17.42 & -00:22:09.69 & 17.712 & 15.884 & 15.140 & 14.774 & 14.517 & 3.208 & sdss j005617.35 - 002208.50 & - & sdss j005617.49 - 002210.88 & 0.044591 + 136 & 00:57:23.70 & + 00:43:57.93 & 19.352 & 17.900 & 16.976 & 16.501 & 16.356 & 4.891 & sdss j005723.54 + 004357.22 & - & sdss j005723.85 + 004358.64 & - + 137 & 00:57:31.74 & + 00:46:00.35 & 17.948 & 15.995 & 15.108 & 14.673 & 14.280 & 11.526 & sdss j005731.48 + 004556.00 & 0.063330 & sdss j005731.99 + 004604.70 & - + 138 & 00:58:35.74 & -00:32:55.64 & 21.740 & 19.509 & 18.139 & 17.589 & 17.200 & 5.548 & sdss j005835.59 - 003254.15 & - & sdss j005835.90 - 003257.13 & - + 139 & 00:58:45.27 & + 00:23:01.26 & 18.821 & 17.116 & 16.421 & 16.038 & 15.639 & 6.527 & sdss j005845.16 + 002258.43 & 0.062080 & sdss j005845.38 + 002304.09 & - + 140 & 00:58:48.66 & + 01:12:08.98 & 20.740 & 18.493 & 17.185 & 16.697 & 16.427 & 3.538 & sdss j005848.57 + 011207.74 & - & sdss j005848.74 + 011210.22 & - + 141 & 00:58:51.76 & -00:57:45.16 & 19.385 & 18.180 & 17.522 & 17.034 & 16.726 & 2.465 & sdss j005851.84 - 005745.75 & - & sdss j005851.69 - 005744.57 & - + 142 & 00:59:51.22 & -00:16:20.57 & 18.695 & 17.774 & 16.684 & 16.312 & 16.094 & 2.468 & sdss j005951.28 - 001621.42 & - & sdss j005951.16 - 001619.73 & - + 143 & 00:59:56.60 & -00:22:25.68 & 19.410 & 17.443 & 16.247 & 15.741 & 15.348 & 11.320 & sdss j005956.23 - 002226.63 & 0.170915 & sdss j005956.97 - 002224.73 & - + 144 & 01:00:11.94 & -00:17:52.47 & 20.525 & 17.575 & 16.669 & 16.209 & 15.844 & 9.278 & sdss j010011.64 - 001753.59 & 0.113563 & sdss j010012.24 - 001751.34 & - + 145 & 01:00:57.56 & -01:00:07.79 & 19.516 & 18.035 & 17.381 & 16.921 & 16.551 & 8.336 & sdss j010057.84 - 010007.30 & 0.051065 & sdss j010057.28 - 010008.28 & - + 146 & 01:00:57.81 & + 00:31:13.46 & 20.043 & 18.445 & 17.047 & 16.545 & 16.208 & 2.767 & sdss j010057.79 + 003112.12 & - & sdss j010057.84 + 003114.79 & - + 147 & 01:01:04.65 & + 01:03:48.70 & 21.858 & 19.256 & 17.823 & 16.914 & 16.457 & 2.596 & sdss j010104.58 + 010349.42 & - & sdss j010104.72 + 010347.98 & - + 148 & 01:01:24.92 & -00:03:05.88 & 17.706 & 16.290 & 15.423 & 15.178 & 14.854 & 6.154 & sdss j010124.74 - 000307.36 & 0.109630 & sdss j010125.10 - 000304.41 & - + 149 & 01:01:43.00 & -00:30:28.86 & 20.795 & 19.640 & 18.670 & 18.111 & 17.660 & 4.419 & sdss j010142.86 - 003029.33 & - & sdss j010143.15 - 003028.40 & - + 150 & 01:01:55.68 & + 01:08:05.51 & 20.243 & 18.966 & 18.216 & 17.751 & 17.551 & 2.507 & sdss j010155.72 + 010806.54 & - & sdss j010155.63 + 010804.48 & - + 151 & 01:02:06.30 & -00:57:12.43 & 21.004 & 18.924 & 17.668 & 17.117 & 16.696 & 6.608 & sdss j010206.09 - 005713.68 & - & sdss j010206.50 - 005711.19 & - + 152 & 01:02:22.35 & + 00:25:42.47 & 19.492 & 17.508 & 16.572 & 16.079 & 15.647 & 3.855 & sdss j010222.41 + 002540.77 & 0.078651 & sdss j010222.29 + 002544.18 & - + 153 & 01:03:05.08 & -00:22:28.47 & 18.648 & 17.328 & 16.744 & 16.477 & 16.376 & 10.792 & sdss j010304.96 - 002223.38 & 0.064721 & sdss j010305.20 - 002233.56 & - + 154 & 01:03:15.92 & + 00:29:16.76 & 20.376 & 18.964 & 17.836 & 17.390 & 17.179 & 2.798 & sdss j010315.88 + 002918.05 & - & sdss j010315.96 + 002915.47 & - + 155 & 01:03:48.60 & + 00:39:33.48 & 20.263 & 19.089 & 17.870 & 17.385 & 16.980 & 2.948 & sdss j010348.60 + 003934.96 & - & sdss j010348.60 + 003932.01 & 0.314855 + 156 & 01:03:53.54 & -00:50:03.69 & 18.606 & 16.768 & 15.933 & 15.509 & 15.150 & 5.983 & sdss j010353.37 - 005002.07 & 0.066220 & sdss j010353.71 - 005005.30 & - + 157 & 01:03:53.82 & -00:26:29.42 & 18.551 & 16.900 & 16.148 & 15.750 & 15.452 & 8.212 & sdss j010354.02 - 002626.68 & 0.017437 & sdss j010353.61 - 002632.16 & - + 158 & 01:04:03.91 & -00:31:18.24 & 19.857 & 19.072 & 18.214 & 17.832 & 17.463 & 3.924 & sdss j010403.86 - 003116.42 & - & sdss j010403.96 - 003120.07 & - + 159 & 01:04:04.83 & + 01:16:02.44 & 20.269 & 19.400 & 18.615 & 18.393 & 18.088 & 2.296 & sdss j010404.82 + 011601.30 & - & sdss j010404.84 + 011603.57 & - + 160 & 01:04:05.52 & -01:12:31.57 & 20.374 & 18.655 & 17.393 & 16.863 & 16.532 & 8.625 & sdss j010405.76 - 011233.94 & - & sdss j010405.28 - 011229.19 & - + 161 & 01:04:25.53 & -00:22:05.04 & 18.597 & 16.692 & 15.797 & 15.380 & 15.025 & 8.029 & sdss j010425.68 - 002208.42 & 0.051175 & sdss j010425.39 - 002201.65 & - + 162 & 01:04:35.11 & + 01:15:54.21 & 19.013 & 17.877 & 17.380 & 17.019 & 16.736 & 7.412 & sdss j010434.99 + 011557.45 & - & sdss j010435.23 + 011550.97 & - + 163 & 01:06:35.38 & + 01:15:55.09 & 18.014 & 16.181 & 15.137 & 14.627 & 14.282 & 6.119 & sdss j010635.18 + 011555.04 & 0.050220 & sdss j010635.59 + 011555.15 & - + 164 & 01:07:05.54 & -00:23:15.54 & 19.323 & 18.262 & 17.365 & 16.991 & 16.677 & 2.501 & sdss j010705.47 - 002314.91 & 0.240929 & sdss j010705.61 - 002316.17 & - + 165 & 01:07:15.22 & + 01:06:38.55 & 19.446 & 18.431 & 17.597 & 17.221 & 17.017 & 7.137 & sdss j010715.24 + 010642.12 & - & sdss j010715.21 + 010634.99 & - + 166 & 01:07:47.55 & + 00:45:14.17 & 20.517 & 18.455 & 17.158 & 16.696 & 16.527 & 3.647 & sdss j010747.66 + 004515.01 & - & sdss j010747.44 + 004513.34 & - + 167 & 01:07:56.29 & + 00:05:56.25 & 20.906 & 19.590 & 18.455 & 18.024 & 17.690 & 2.373 & sdss j010756.23 + 000555.48 & - & sdss j010756.35 + 000557.03 & - + 168 & 01:08:03.72 & + 01:05:00.00 & 17.912 & 16.717 & 15.897 & 15.889 & 15.727 & 5.231 & sdss j010803.55 + 010500.70 & 0.043195 & sdss j010803.88 + 010459.30 & - + 169 & 01:08:52.33 & + 00:24:13.38 & 19.479 & 17.392 & 16.334 & 15.863 & 15.450 & 3.959 & sdss j010852.36 + 002411.48 & 0.121886 & sdss j010852.29 + 002415.29 & - + 170 & 01:09:29.89 & -00:18:29.16 & 19.294 & 17.558 & 16.648 & 16.281 & 15.952 & 3.805 & sdss j010930.00 - 001828.17 & 0.101981 & sdss j010929.78 - 001830.16 & - + 171 & 01:10:12.72 & + 00:30:31.34 & 19.089 & 18.075 & 17.832 & 17.605 & 17.711 & 7.245 & sdss j011012.48 + 003030.93 & - & sdss j011012.96 + 003031.74 & - + 172 & 01:11:19.81 & -00:02:26.70 & 17.521 & 16.549 & 16.186 & 16.124 & 16.006 & 8.668 & sdss j011119.96 - 000223.05 & - & sdss j011119.65 - 000230.35 & - + 173 & 01:12:03.78 & -00:02:13.02 & 20.779 & 18.810 & 17.769 & 17.189 & 16.717 & 7.248 & sdss j011203.72 - 000216.53 & - & sdss j011203.84 - 000209.51 & - + 174 & 01:12:38.07 & + 00:05:14.80 & 18.913 & 17.065 & 16.193 & 15.738 & 15.419 & 9.404 & sdss j011237.92 + 000510.72 & 0.067638 & sdss j011238.23 + 000518.87 & - + 175 & 01:12:58.58 & -00:52:39.76 & 18.936 & 17.912 & 17.613 & 17.390 & 17.341 & 9.367 & sdss j011258.27 - 005239.57 & - & sdss j011258.89 - 005239.95 & - + 176 & 01:13:55.53 & -01:05:25.92 & 20.365 & 18.314 & 17.161 & 16.643 & 16.374 & 6.488 & sdss j011355.72 - 010524.43 & - & sdss j011355.34 - 010527.42 & - + 177 & 01:13:56.80 & -00:11:33.52 & 18.245 & 17.060 & 16.605 & 16.311 & 15.960 & 9.126 & sdss j011357.09 - 001134.99 & - & sdss j011356.52 - 001132.06 & 0.092871 + 178 & 01:14:49.40 & -00:29:40.80 & 17.054 & 16.014 & 15.334 & 15.351 & 15.140 & 14.150 & sdss j011448.98 - 002937.58 & - & sdss j011449.82 - 002944.02 & - + 179 & 01:15:36.24 & + 00:23:30.93 & 19.135 & 17.580 & 17.277 & 17.045 & 16.817 & 4.352 & sdss j011536.38 + 002330.67 & - & sdss j011536.09 + 002331.19 & - + 180 & 01:15:40.98 & -00:08:26.85 & 19.483 & 17.379 & 16.515 & 16.105 & 15.698 & 3.543 & sdss j011540.87 - 000826.13 & - & sdss j011541.08 - 000827.57 & 0.090482 + 181 & 01:15:53.58 & -00:10:52.39 & 20.158 & 18.988 & 18.016 & 17.496 & 17.141 & 3.522 & sdss j011553.64 - 001050.87 & - & sdss j011553.52 - 001053.90 & - + 182 & 01:16:14.38 & + 00:00:15.90 & 19.252 & 18.302 & 17.869 & 17.662 & 17.224 & 3.773 & sdss j011614.30 + 000017.30 & - & sdss j011614.47 + 000014.49 & - + 183 & 01:16:50.85 & + 00:26:08.90 & 20.854 & 18.955 & 17.852 & 17.377 & 17.078 & 6.005 & sdss j011650.97 + 002606.50 & - & sdss j011650.73 + 002611.30 & - + 184 & 01:16:55.96 & -00:46:09.29 & 19.922 & 19.077 & 18.580 & 18.233 & 17.933 & 5.347 & sdss j011655.80 - 004610.18 & - & sdss j011656.13 - 004608.40 & - + 185 & 01:16:59.38 & + 00:19:34.76 & 17.713 & 15.925 & 15.116 & 14.659 & 14.275 & 10.139 & sdss j011659.71 + 001936.20 & 0.077302 & sdss j011659.06 + 001933.31 & - + 186 & 01:17:01.66 & + 00:31:52.24 & 19.642 & 18.450 & 17.767 & 17.360 & 17.160 & 4.723 & sdss j011701.60 + 003150.06 & - & sdss j011701.72 + 003154.43 & - + 187 & 01:17:10.71 & -00:10:11.33 & 20.641 & 19.265 & 18.472 & 18.055 & 17.773 & 5.980 & sdss j011710.65 - 001014.18 & - & sdss j011710.77 - 001008.47 & - + 188 & 01:17:26.10 & + 00:39:14.36 & 20.236 & 19.227 & 18.816 & 18.470 & 18.495 & 1.924 & sdss j011726.08 + 003915.30 & - & sdss j011726.11 + 003913.41 & - + 189 & 01:19:04.05 & + 00:26:24.13 & 17.964 & 15.907 & 14.955 & 14.525 & 14.182 & 12.599 & sdss j011904.03 + 002630.42 & 0.077477 & sdss j011904.08 + 002617.84 & - + 190 & 01:19:55.51 & -00:10:04.53 & 18.500 & 17.425 & 16.780 & 16.578 & 16.443 & 6.598 & sdss j011955.39 - 001007.29 & - & sdss j011955.63 - 001001.76 & - + 191 & 01:20:22.70 & -00:01:55.73 & 19.692 & 17.527 & 16.367 & 15.818 & 15.364 & 8.459 & sdss j012022.51 - 000152.64 & 0.174803 & sdss j012022.89 - 000158.83 & - + 192 & 01:20:45.12 & -00:31:41.62 & 18.580 & 17.497 & 16.965 & 16.688 & 16.559 & 4.606 & sdss j012045.04 - 003143.66 & - & sdss j012045.19 - 003139.59 & - + 193 & 01:22:00.64 & -00:51:55.58 & 19.176 & 17.586 & 16.661 & 16.200 & 15.864 & 3.603 & sdss j012200.52 - 005155.51 & 0.163656 & sdss j012200.76 - 005155.66 & - + 194 & 01:22:22.50 & -00:11:13.05 & 19.252 & 18.100 & 17.487 & 17.078 & 16.792 & 4.580 & sdss j012222.56 - 001115.16 & 0.093562 & sdss j012222.44 - 001110.95 & - + 195 & 01:23:04.06 & + 00:19:04.53 & 20.772 & 18.772 & 17.797 & 17.210 & 16.755 & 3.460 & sdss j012304.08 + 001906.25 & - & sdss j012304.05 + 001902.81 & - + 196 & 01:23:31.20 & + 01:10:45.08 & 18.685 & 17.228 & 16.648 & 16.246 & 15.927 & 6.219 & sdss j012331.27 + 011048.00 & 0.017635 & sdss j012331.12 + 011042.16 & - + 197 & 01:24:08.82 & -00:22:27.04 & 18.999 & 17.741 & 17.459 & 17.274 & 17.350 & 4.785 & sdss j012408.95 - 002225.70 & - & sdss j012408.68 - 002228.38 & - + 198 & 01:24:17.25 & -01:14:34.87 & 21.022 & 19.071 & 17.856 & 17.388 & 17.110 & 4.238 & sdss j012417.23 - 011436.96 & - & sdss j012417.28 - 011432.78 & - + 199 & 01:24:23.31 & + 00:29:31.32 & 19.805 & 18.200 & 17.201 & 16.739 & 16.529 & 4.799 & sdss j012423.18 + 002929.96 & - & sdss j012423.44 + 002932.67 & - + 200 & 01:26:13.92 & -00:52:13.43 & 20.199 & 19.073 & 18.183 & 17.812 & 17.560 & 5.607 & sdss j012613.80 - 005211.28 & - & sdss j012614.04 - 005215.58 & - + 201 & 01:30:38.05 & + 00:06:59.18 & 18.433 & 16.460 & 15.544 & 15.112 & 14.819 & 11.984 & sdss j013038.18 + 000653.52 & 0.079526 & sdss j013037.92 + 000704.83 & - + 202 & 01:30:42.87 & + 00:46:30.65 & 20.953 & 19.049 & 17.752 & 17.213 & 16.938 & 4.070 & sdss j013042.74 + 004631.12 & - & sdss j013043.00 + 004630.18 & - + 203 & 01:31:45.19 & + 00:00:57.47 & 20.130 & 18.937 & 18.335 & 18.137 & 17.790 & 5.682 & sdss j013145.36 + 000056.16 & - & sdss j013145.02 + 000058.78 & - + 204 & 01:31:57.24 & -00:45:02.03 & 19.829 & 17.821 & 16.626 & 16.122 & 15.784 & 3.751 & sdss j013157.28 - 004503.76 & 0.167436 & sdss j013157.19 - 004500.30 & - + 205 & 01:32:13.00 & -00:03:05.02 & 19.294 & 18.041 & 17.446 & 17.091 & 16.926 & 6.706 & sdss j013212.79 - 000305.88 & - & sdss j013213.22 - 000304.15 & - + 206 & 01:32:50.38 & + 00:48:24.12 & 20.210 & 19.369 & 18.280 & 17.873 & 17.321 & 5.432 & sdss j013250.20 + 004823.83 & - & sdss j013250.56 + 004824.42 & - + 207 & 01:34:49.50 & -00:36:41.64 & 18.083 & 16.479 & 15.495 & 15.034 & 14.675 & 10.854 & sdss j013449.82 - 003639.22 & 0.080116 & sdss j013449.17 - 003644.05 & - + 208 & 01:35:00.58 & + 01:10:25.17 & 18.985 & 18.141 & 17.870 & 17.643 & 17.706 & 2.941 & sdss j013500.55 + 011026.54 & 0.153254 & sdss j013500.62 + 011023.80 & - + 209 & 01:35:11.96 & -00:53:20.38 & 19.506 & 17.699 & 16.761 & 16.319 & 16.035 & 3.986 & sdss j013512.09 - 005320.15 & 0.153254 & sdss j013511.83 - 005320.61 & - + 210 & 01:35:34.46 & -01:07:54.82 & 20.766 & 19.354 & 18.410 & 17.948 & 17.700 & 4.415 & sdss j013534.48 - 010752.64 & - & sdss j013534.44 - 010757.00 & - + 211 & 01:36:41.53 & -00:58:13.50 & 18.822 & 17.448 & 16.653 & 16.268 & 15.889 & 7.448 & sdss j013641.35 - 005810.94 & 0.079594 & sdss j013641.71 - 005816.07 & - + 212 & 01:36:46.46 & + 00:41:38.69 & 19.742 & 17.906 & 16.968 & 16.554 & 16.143 & 5.380 & sdss j013646.41 + 004136.10 & - & sdss j013646.51 + 004141.29 & - + 213 & 01:36:57.97 & -00:24:42.33 & 20.272 & 19.031 & 18.488 & 18.170 & 18.098 & 3.318 & sdss j013657.86 - 002441.97 & - & sdss j013658.08 - 002442.69 & - + 214 & 01:37:07.06 & + 01:03:12.11 & 19.201 & 17.531 & 16.641 & 16.189 & 15.937 & 4.865 & sdss j013706.91 + 010312.78 & 0.043293 & sdss j013707.22 + 010311.44 & - + 215 & 01:37:07.27 & + 00:07:11.59 & 19.297 & 17.823 & 16.797 & 16.378 & 16.101 & 5.787 & sdss j013707.22 + 000708.78 & - & sdss j013707.32 + 000714.39 & - + 216 & 01:39:04.94 & -01:01:50.35 & 19.929 & 18.625 & 18.048 & 17.741 & 17.602 & 5.649 & sdss j013904.84 - 010152.78 & - & sdss j013905.04 - 010147.92 & - + 217 & 01:39:05.08 & + 00:17:46.48 & 19.243 & 17.321 & 16.279 & 15.772 & 15.334 & 5.472 & sdss j013904.94 + 001748.16 & 0.123558 & sdss j013905.23 + 001744.80 & - + 218 & 01:39:25.08 & -00:54:55.19 & 17.299 & 16.152 & 15.582 & 15.367 & 15.209 & 8.150 & sdss j013925.17 - 005451.38 & 0.082491 & sdss j013924.98 - 005459.01 & - + 219 & 01:39:35.52 & -00:31:33.25 & 18.810 & 17.658 & 17.073 & 16.688 & 16.406 & 25.456 & sdss j013935.92 - 003122.09 & 0.055750 & sdss j013935.11 - 003144.41 & - + 220 & 01:39:49.98 & + 01:13:05.48 & 22.011 & 19.693 & 18.149 & 17.632 & 17.307 & 3.606 & sdss j013950.08 + 011304.69 & - & sdss j013949.87 + 011306.27 & - + 221 & 01:40:12.67 & + 00:00:21.82 & 20.944 & 19.666 & 19.078 & 18.704 & 18.443 & 4.411 & sdss j014012.52 + 000022.26 & - & sdss j014012.81 + 000021.37 & - + 222 & 01:40:12.86 & + 00:24:23.92 & 21.612 & 19.894 & 18.566 & 18.056 & 17.718 & 2.886 & sdss j014012.76 + 002423.82 & - & sdss j014012.96 + 002424.01 & - + 223 & 01:40:19.46 & -00:52:01.38 & 20.202 & 19.248 & 19.037 & 18.829 & 18.803 & 2.568 & sdss j014019.39 - 005200.68 & - & sdss j014019.53 - 005202.07 & - + 224 & 01:40:22.22 & -00:04:40.57 & 17.707 & 16.316 & 15.346 & 15.028 & 14.747 & 10.417 & sdss j014022.56 - 000439.26 & 0.161523 & sdss j014021.88 - 000441.89 & - + 225 & 01:41:02.85 & + 01:16:14.59 & 19.188 & 18.280 & 18.090 & 17.877 & 17.780 & 3.802 & sdss j014102.73 + 011613.98 & - & sdss j014102.97 + 011615.20 & - + 226 & 01:41:11.61 & -00:11:20.25 & 19.478 & 18.476 & 18.299 & 18.038 & 17.957 & 3.128 & sdss j014111.61 - 001118.69 & - & sdss j014111.61 - 001121.82 & - + 227 & 01:41:26.01 & + 00:05:53.57 & 19.682 & 18.277 & 17.237 & 16.799 & 16.397 & 6.220 & sdss j014126.18 + 000551.75 & 0.125571 & sdss j014125.84 + 000555.39 & - + 228 & 01:41:29.59 & -00:41:56.01 & 18.289 & 17.389 & 17.167 & 16.876 & 16.776 & 4.916 & sdss j014129.47 - 004157.68 & 0.068770 & sdss j014129.71 - 004154.33 & - + 229 & 01:42:26.84 & + 00:12:45.59 & 18.822 & 17.074 & 16.224 & 15.748 & 15.414 & 5.868 & sdss j014226.76 + 001242.94 & - & sdss j014226.92 + 001248.24 & - + 230 & 01:43:35.05 & -01:06:49.03 & 19.024 & 17.276 & 16.583 & 16.368 & 16.454 & 10.463 & sdss j014334.70 - 010649.39 & - & sdss j014335.40 - 010648.67 & - + 231 & 01:44:12.16 & -01:09:20.55 & 19.814 & 18.746 & 18.127 & 17.785 & 17.590 & 8.036 & sdss j014411.90 - 010919.87 & - & sdss j014412.43 - 010921.24 & - + 232 & 01:44:26.12 & -00:18:58.84 & 19.678 & 18.910 & 18.750 & 18.436 & 18.510 & 4.670 & sdss j014426.06 - 001900.99 & - & sdss j014426.18 - 001856.68 & - + 233 & 01:44:59.25 & + 00:45:15.87 & 21.081 & 19.067 & 18.016 & 17.501 & 17.163 & 3.808 & sdss j014459.16 + 004514.62 & - & sdss j014459.35 + 004517.11 & - + 234 & 01:45:00.52 & + 00:13:47.90 & 19.412 & 17.577 & 16.647 & 16.168 & 15.779 & 3.294 & sdss j014500.45 + 001349.14 & 0.059642 & sdss j014500.60 + 001346.66 & - + 235 & 01:46:31.18 & + 00:53:36.33 & 21.048 & 19.067 & 17.748 & 17.251 & 16.962 & 4.819 & sdss j014631.34 + 005335.76 & - & sdss j014631.03 + 005336.91 & - + 236 & 01:46:36.39 & -00:28:49.55 & 18.065 & 16.787 & 16.117 & 15.717 & 15.436 & 6.388 & sdss j014636.24 - 002851.73 & 0.083278 & sdss j014636.55 - 002847.38 & - + 237 & 01:46:48.20 & + 00:41:07.58 & 18.467 & 17.463 & 17.299 & 17.090 & 16.992 & 9.086 & sdss j014648.50 + 004108.21 & 0.057675 & sdss j014647.90 + 004106.96 & - + 238 & 01:47:27.99 & + 00:51:34.84 & 20.094 & 18.358 & 17.113 & 16.656 & 16.294 & 3.454 & sdss j014727.88 + 005135.44 & 0.193447 & sdss j014728.10 + 005134.24 & - + 239 & 01:47:38.17 & -01:03:05.40 & 19.720 & 17.705 & 16.546 & 16.046 & 15.755 & 5.760 & sdss j014738.23 - 010308.13 & - & sdss j014738.11 - 010302.66 & 0.161445 + 240 & 01:49:20.25 & -00:10:49.03 & 18.813 & 17.555 & 16.956 & 16.635 & 16.390 & 5.598 & sdss j014920.40 - 001047.25 & - & sdss j014920.11 - 001050.81 & - + 241 & 01:49:28.47 & + 00:47:22.73 & 20.087 & 18.619 & 17.741 & 17.207 & 16.853 & 4.098 & sdss j014928.36 + 004721.48 & - & sdss j014928.58 + 004723.99 & - + 242 & 01:49:40.35 & -00:40:20.69 & 18.951 & 17.709 & 16.823 & 16.471 & 16.117 & 2.757 & sdss j014940.29 - 004021.73 & - & sdss j014940.41 - 004019.65 & - + 243 & 01:50:24.38 & + 00:31:38.30 & 19.321 & 18.051 & 17.276 & 16.896 & 16.596 & 5.646 & sdss j015024.31 + 003135.69 & - & sdss j015024.45 + 003140.91 & - + 244 & 01:50:46.94 & -00:37:27.83 & 20.348 & 18.631 & 17.268 & 16.719 & 16.339 & 4.347 & sdss j015047.08 - 003727.59 & 0.208155 & sdss j015046.80 - 003728.07 & - + 245 & 01:50:47.80 & -01:03:26.19 & 21.225 & 19.219 & 18.216 & 17.836 & 17.593 & 4.613 & sdss j015047.95 - 010327.00 & - & sdss j015047.66 - 010325.38 & - + 246 & 01:50:48.80 & + 00:11:48.46 & 19.484 & 18.080 & 17.432 & 17.031 & 16.860 & 5.299 & sdss j015048.72 + 001150.79 & 0.081155 & sdss j015048.88 + 001146.13 & - + 247 & 01:51:10.74 & -00:52:32.77 & 20.085 & 18.484 & 17.477 & 16.932 & 16.613 & 5.459 & sdss j015110.72 - 005235.49 & - & sdss j015110.75 - 005230.04 & - + 248 & 01:51:14.58 & -01:11:17.53 & 21.440 & 19.265 & 17.976 & 17.483 & 17.126 & 2.775 & sdss j015114.54 - 011118.81 & - & sdss j015114.61 - 011116.26 & - + 249 & 01:51:32.60 & + 00:53:52.80 & 20.230 & 18.973 & 18.072 & 17.717 & 17.398 & 3.324 & sdss j015132.49 + 005353.17 & - & sdss j015132.71 + 005352.43 & - + 250 & 01:51:33.22 & -00:36:38.56 & 17.919 & 16.764 & 16.280 & 15.905 & 15.694 & 10.268 & sdss j015133.48 - 003635.08 & 0.059885 & sdss j015132.97 - 003642.03 & - + 251 & 01:51:53.29 & + 00:55:22.26 & 20.899 & 19.099 & 18.040 & 17.548 & 17.218 & 2.539 & sdss j015153.20 + 005522.10 & - & sdss j015153.37 + 005522.41 & - + 252 & 01:52:32.86 & -00:57:47.08 & 18.164 & 16.451 & 15.634 & 15.212 & 14.864 & 7.570 & sdss j015233.04 - 005744.43 & 0.059958 & sdss j015232.68 - 005749.74 & - + 253 & 01:52:38.31 & + 00:34:20.81 & 19.068 & 17.555 & 16.667 & 16.217 & 15.883 & 7.524 & sdss j015238.52 + 003423.00 & 0.120276 & sdss j015238.11 + 003418.62 & - + 254 & 01:53:13.11 & + 00:01:51.66 & 19.409 & 18.751 & 18.479 & 18.161 & 18.155 & 3.845 & sdss j015313.15 + 000153.50 & - & sdss j015313.08 + 000149.81 & - + 255 & 01:53:29.04 & + 00:49:51.00 & 19.067 & 17.677 & 17.029 & 16.733 & 16.455 & 7.281 & sdss j015328.92 + 004947.83 & 0.059317 & sdss j015329.16 + 004954.16 & - + 256 & 01:53:41.64 & + 00:50:24.56 & 19.935 & 18.515 & 17.791 & 17.446 & 17.112 & 2.578 & sdss j015341.64 + 005025.85 & - & sdss j015341.64 + 005023.28 & - + 257 & 01:53:42.55 & + 00:44:57.93 & 21.269 & 19.227 & 17.753 & 17.381 & 17.012 & 3.391 & sdss j015342.55 + 004456.24 & - & sdss j015342.55 + 004459.63 & - + 258 & 01:54:02.02 & -01:01:42.29 & 20.607 & 19.463 & 18.780 & 18.379 & 18.045 & 8.377 & sdss j015401.87 - 010138.82 & - & sdss j015402.18 - 010145.76 & - + 259 & 01:54:09.46 & + 00:07:27.90 & 18.399 & 17.076 & 16.496 & 16.085 & 15.801 & 7.235 & sdss j015409.36 + 000724.67 & 0.087382 & sdss j015409.57 + 000731.14 & - + 260 & 01:56:18.33 & + 01:03:33.78 & 20.020 & 18.164 & 17.327 & 16.912 & 16.646 & 5.486 & sdss j015618.45 + 010335.85 & - & sdss j015618.21 + 010331.71 & - + 261 & 01:56:34.44 & -00:10:08.58 & 19.418 & 17.967 & 17.193 & 16.726 & 16.353 & 5.591 & sdss j015634.27 - 001007.37 & - & sdss j015634.60 - 001009.78 & - + 262 & 01:56:59.98 & -00:55:52.54 & 19.194 & 17.995 & 17.236 & 16.883 & 16.555 & 6.293 & sdss j015659.78 - 005553.27 & - & sdss j015700.19 - 005551.80 & - + 263 & 01:57:11.80 & -00:28:23.99 & 17.974 & 16.131 & 15.243 & 14.851 & 14.499 & 14.489 & sdss j015711.35 - 002826.38 & 0.080266 & sdss j015712.26 - 002821.60 & - + 264 & 01:57:15.13 & + 00:15:17.76 & 19.775 & 18.146 & 17.065 & 16.602 & 16.340 & 4.574 & sdss j015715.00 + 001516.62 & 0.136880 & sdss j015715.26 + 001518.91 & - + 265 & 01:57:31.26 & -01:03:42.53 & 20.802 & 19.286 & 18.593 & 18.185 & 18.019 & 5.033 & sdss j015731.36 - 010340.60 & - & sdss j015731.15 - 010344.46 & - + 266 & 01:58:16.26 & -00:31:20.01 & 17.933 & 16.364 & 15.722 & 15.272 & 14.996 & 3.908 & sdss j015816.36 - 003118.92 & 0.080296 & sdss j015816.15 - 003121.10 & - + 267 & 02:00:53.26 & -00:10:49.94 & 20.608 & 18.720 & 17.573 & 17.147 & 16.852 & 3.156 & sdss j020053.32 - 001048.65 & - & sdss j020053.20 - 001051.24 & - + 268 & 02:01:26.35 & -01:01:16.82 & 19.542 & 17.813 & 16.833 & 16.335 & 15.930 & 5.001 & sdss j020126.49 - 010115.56 & 0.125846 & sdss j020126.20 - 010118.08 & - + 269 & 02:01:27.62 & + 00:25:30.34 & 19.551 & 18.132 & 17.271 & 16.748 & 16.463 & 10.967 & sdss j020127.57 + 002535.78 & - & sdss j020127.67 + 002524.91 & - + 270 & 02:01:30.48 & + 00:49:48.27 & 20.515 & 18.506 & 17.414 & 16.951 & 16.591 & 7.330 & sdss j020130.72 + 004948.96 & - & sdss j020130.24 + 004947.58 & - + 271 & 02:01:42.34 & -00:48:17.44 & 19.389 & 17.486 & 16.523 & 16.106 & 15.726 & 4.299 & sdss j020142.31 - 004815.36 & 0.120919 & sdss j020142.38 - 004819.53 & - + 272 & 02:01:50.66 & -00:50:52.31 & 19.736 & 18.382 & 17.643 & 17.157 & 16.948 & 3.812 & sdss j020150.66 - 005050.40 & - & sdss j020150.66 - 005054.22 & - + 273 & 02:01:52.39 & -00:33:11.57 & 19.695 & 18.070 & 16.972 & 16.470 & 16.098 & 9.456 & sdss j020152.17 - 003315.01 & - & sdss j020152.60 - 003308.12 & - + 274 & 02:01:52.95 & + 01:12:01.94 & 18.672 & 16.686 & 15.635 & 15.180 & 14.806 & 14.422 & sdss j020153.28 + 011207.27 & 0.129504 & sdss j020152.63 + 011156.61 & - + 275 & 02:02:46.33 & + 01:14:26.71 & 17.878 & 16.026 & 15.187 & 14.727 & 14.410 & 12.141 & sdss j020246.70 + 011429.11 & - & sdss j020245.96 + 011424.32 & - + 276 & 02:04:16.03 & -00:11:30.32 & 19.064 & 17.969 & 17.775 & 17.522 & 16.286 & 8.554 & sdss j020415.86 - 001133.78 & - & sdss j020416.20 - 001126.86 & - + 277 & 02:04:20.47 & -00:45:33.26 & 21.096 & 19.466 & 18.226 & 17.716 & 17.228 & 6.651 & sdss j020420.68 - 004534.02 & - & sdss j020420.25 - 004532.51 & - + 278 & 02:04:31.52 & + 00:13:39.02 & 17.239 & 15.937 & 14.999 & 14.787 & 14.428 & 7.448 & sdss j020431.32 + 001341.14 & 0.163089 & sdss j020431.72 + 001336.90 & - + 279 & 02:04:42.50 & -00:17:47.70 & 18.957 & 17.425 & 16.574 & 16.134 & 15.773 & 5.528 & sdss j020442.36 - 001749.43 & 0.111874 & sdss j020442.64 - 001745.98 & - + 280 & 02:05:11.28 & + 00:05:27.47 & 18.383 & 16.654 & 15.789 & 15.397 & 15.108 & 9.511 & sdss j020511.16 + 000531.87 & 0.076353 & sdss j020511.40 + 000523.06 & - + 281 & 02:05:25.38 & + 00:15:16.92 & 18.612 & 16.680 & 15.516 & 15.054 & 14.613 & 8.297 & sdss j020525.22 + 001513.50 & - & sdss j020525.53 + 001520.35 & - + 282 & 02:05:34.08 & + 00:36:36.52 & 19.187 & 18.092 & 17.799 & 17.637 & 17.580 & 7.256 & sdss j020534.27 + 003634.31 & - & sdss j020533.88 + 003638.73 & - + 283 & 02:05:36.40 & -00:58:51.70 & 18.652 & 17.375 & 16.481 & 16.043 & 15.722 & 7.374 & sdss j020536.19 - 005853.46 & - & sdss j020536.62 - 005849.94 & - + 284 & 02:05:51.80 & -00:32:30.81 & 17.629 & 16.137 & 15.385 & 14.885 & 14.570 & 4.742 & sdss j020551.91 - 003232.55 & 0.063742 & sdss j020551.69 - 003229.08 & - + 285 & 02:05:56.72 & + 00:01:02.82 & 19.037 & 17.060 & 15.846 & 15.378 & 15.012 & 12.238 & sdss j020556.66 + 000108.87 & - & sdss j020556.78 + 000056.77 & 0.172998 + 286 & 02:06:12.40 & -00:01:28.25 & 18.915 & 16.950 & 15.805 & 15.378 & 15.035 & 16.097 & sdss j020611.90 - 000125.49 & 0.112975 & sdss j020612.91 - 000131.01 & - + 287 & 02:06:20.83 & + 00:30:32.04 & 19.216 & 18.132 & 17.731 & 17.536 & 17.274 & 7.143 & sdss j020620.80 + 003028.48 & - & sdss j020620.85 + 003035.59 & - + 288 & 02:06:28.38 & -00:53:51.21 & 18.755 & 17.141 & 16.211 & 15.745 & 15.379 & 13.866 & sdss j020627.93 - 005353.14 & - & sdss j020628.82 - 005349.28 & - + 289 & 02:06:59.42 & + 01:00:49.05 & 18.264 & 16.879 & 16.562 & 16.329 & 16.224 & 15.154 & sdss j020659.92 + 010048.52 & 0.019783 & sdss j020658.92 + 010049.57 & - + 290 & 02:07:16.10 & -01:00:42.46 & 18.277 & 16.027 & 14.964 & 14.478 & 14.114 & 5.626 & sdss j020716.08 - 010045.25 & - & sdss j020716.12 - 010039.67 & 0.115449 + 291 & 02:07:29.18 & -00:18:21.80 & 19.936 & 18.828 & 18.095 & 17.806 & 17.463 & 5.361 & sdss j020729.01 - 001822.71 & - & sdss j020729.35 - 001820.89 & - + 292 & 02:08:25.10 & + 00:30:37.53 & 18.642 & 17.578 & 17.289 & 17.110 & 16.996 & 3.731 & sdss j020825.20 + 003036.35 & 0.067201 & sdss j020825.00 + 003038.72 & - + 293 & 02:08:37.29 & + 00:47:39.32 & 20.225 & 18.885 & 17.849 & 17.446 & 17.164 & 5.174 & sdss j020837.39 + 004737.17 & - & sdss j020837.20 + 004741.47 & - + 294 & 02:08:50.49 & + 00:34:04.58 & 19.394 & 17.314 & 16.481 & 16.038 & 15.643 & 9.100 & sdss j020850.30 + 003408.10 & 0.068017 & sdss j020850.68 + 003401.05 & - + 295 & 02:08:59.36 & + 00:09:40.37 & 20.973 & 19.544 & 18.536 & 17.474 & 16.826 & 8.366 & sdss j020859.64 + 000940.97 & - & sdss j020859.08 + 000939.78 & - + 296 & 02:09:08.74 & -00:21:36.09 & 20.561 & 18.839 & 17.997 & 17.465 & 17.268 & 1.972 & sdss j020908.80 - 002136.49 & - & sdss j020908.68 - 002135.69 & - + 297 & 02:09:39.18 & -00:46:08.55 & 19.426 & 18.068 & 17.228 & 16.763 & 16.475 & 6.481 & sdss j020939.14 - 004605.36 & - & sdss j020939.21 - 004611.75 & - + 298 & 02:10:05.97 & + 00:53:16.38 & 19.512 & 17.672 & 16.653 & 16.236 & 15.946 & 6.191 & sdss j021005.78 + 005315.24 & 0.140885 & sdss j021006.16 + 005317.52 & - + 299 & 02:10:35.23 & + 00:30:03.22 & 18.227 & 17.195 & 16.552 & 16.296 & 16.094 & 6.832 & sdss j021035.11 + 003000.31 & - & sdss j021035.35 + 003006.12 & - + 300 & 02:10:36.94 & + 00:17:37.70 & 20.842 & 18.626 & 17.358 & 16.808 & 16.425 & 2.878 & sdss j021037.03 + 001738.39 & - & sdss j021036.86 + 001737.00 & - + 301 & 02:10:37.15 & -00:35:31.93 & 20.611 & 19.482 & 18.920 & 18.890 & 18.800 & 3.747 & sdss j021037.05 - 003530.73 & - & sdss j021037.24 - 003533.12 & - + 302 & 02:11:25.53 & -01:01:57.97 & 20.193 & 18.359 & 17.283 & 16.753 & 16.413 & 7.038 & sdss j021125.65 - 010200.99 & 0.175588 & sdss j021125.41 - 010154.94 & - + 303 & 02:12:26.84 & -00:50:48.06 & 19.708 & 17.773 & 16.883 & 16.511 & 16.247 & 3.928 & sdss j021226.88 - 005046.17 & 0.097383 & sdss j021226.80 - 005049.95 & - + 304 & 02:13:26.60 & + 00:00:31.43 & 19.944 & 19.393 & 18.488 & 18.187 & 17.808 & 4.064 & sdss j021326.59 + 000033.45 & - & sdss j021326.61 + 000029.40 & - + 305 & 02:13:41.95 & + 00:12:24.18 & 18.100 & 16.014 & 15.027 & 14.572 & 14.211 & 16.138 & sdss j021341.52 + 001228.99 & - & sdss j021342.38 + 001219.37 & 0.099408 + 306 & 02:13:55.50 & + 00:27:57.01 & 21.310 & 19.666 & 18.434 & 18.036 & 17.593 & 3.550 & sdss j021355.39 + 002756.28 & - & sdss j021355.60 + 002757.73 & - + 307 & 02:13:56.55 & + 00:31:44.55 & 17.476 & 16.095 & 15.374 & 14.941 & 14.635 & 16.696 & sdss j021356.76 + 003152.32 & 0.040614 & sdss j021356.35 + 003136.78 & - + 308 & 02:14:11.46 & -00:11:48.03 & 20.110 & 18.385 & 17.430 & 17.034 & 16.702 & 3.248 & sdss j021411.40 - 001146.68 & - & sdss j021411.52 - 001149.38 & - + 309 & 02:14:12.50 & -00:11:19.60 & 19.576 & 17.594 & 16.494 & 16.034 & 15.816 & 3.716 & sdss j021412.62 - 001119.14 & 0.140781 & sdss j021412.38 - 001120.06 & - + 310 & 02:14:43.47 & + 00:32:24.47 & 20.710 & 19.246 & 18.265 & 17.718 & 17.532 & 3.015 & sdss j021443.56 + 003223.64 & - & sdss j021443.39 + 003225.30 & - + 311 & 02:15:06.68 & + 00:53:43.58 & 17.821 & 16.605 & 15.845 & 15.547 & 15.330 & 7.325 & sdss j021506.79 + 005340.30 & 0.142031 & sdss j021506.57 + 005346.87 & - + 312 & 02:16:21.20 & -00:23:09.79 & 19.956 & 18.418 & 17.284 & 16.753 & 16.434 & 5.542 & sdss j021621.16 - 002307.08 & - & sdss j021621.24 - 002312.51 & - + 313 & 02:16:47.60 & -00:39:05.77 & 17.938 & 17.091 & 16.941 & 16.883 & 16.810 & 10.533 & sdss j021647.68 - 003910.88 & 0.020532 & sdss j021647.52 - 003900.65 & - + 314 & 02:17:14.00 & + 00:15:17.64 & 21.097 & 18.998 & 17.895 & 17.421 & 17.149 & 2.746 & sdss j021714.06 + 001516.60 & - & sdss j021713.94 + 001518.67 & - + 315 & 02:18:37.28 & + 00:10:44.96 & 20.464 & 18.607 & 17.710 & 17.302 & 17.078 & 4.132 & sdss j021837.24 + 001046.95 & - & sdss j021837.32 + 001042.97 & - + 316 & 02:19:35.67 & -00:17:02.15 & 18.977 & 17.930 & 17.563 & 17.457 & 17.046 & 18.810 & sdss j021935.76 - 001652.83 & - & sdss j021935.59 - 001711.47 & - + 317 & 02:19:58.29 & + 00:51:04.40 & 19.963 & 18.146 & 17.170 & 16.722 & 16.345 & 14.782 & sdss j021958.00 + 005058.40 & - & sdss j021958.58 + 005110.40 & - + 318 & 02:20:22.42 & -00:38:15.87 & 20.247 & 19.322 & 18.278 & 17.815 & 17.396 & 4.037 & sdss j022022.41 - 003813.86 & - & sdss j022022.44 - 003817.88 & - + 319 & 02:22:50.86 & -00:53:53.00 & 20.160 & 18.903 & 18.188 & 17.801 & 17.616 & 2.395 & sdss j022250.92 - 005352.21 & - & sdss j022250.80 - 005353.79 & - + 320 & 02:23:02.43 & -00:08:34.58 & 17.989 & 16.428 & 15.654 & 15.237 & 14.990 & 7.511 & sdss j022302.61 - 000831.97 & 0.073479 & sdss j022302.25 - 000837.19 & - + 321 & 02:25:05.01 & + 00:54:30.65 & 19.537 & 17.529 & 16.426 & 15.952 & 15.672 & 3.884 & sdss j022504.96 + 005428.85 & - & sdss j022505.06 + 005432.45 & - + 322 & 02:26:25.46 & -00:01:03.52 & 18.272 & 16.659 & 15.862 & 15.522 & 15.209 & 8.201 & sdss j022625.36 - 000107.36 & 0.072984 & sdss j022625.56 - 000059.68 & - + 323 & 02:27:09.04 & -00:33:44.59 & 17.382 & 16.246 & 15.642 & 15.439 & 15.199 & 20.093 & sdss j022709.09 - 003354.61 & 0.058911 & sdss j022709.00 - 003334.57 & - + 324 & 02:27:12.66 & -00:02:59.94 & 17.334 & 16.318 & 15.959 & 16.023 & 16.277 & 3.310 & sdss j022712.76 - 000300.28 & - & sdss j022712.55 - 000259.60 & 0.025918 + 325 & 02:28:42.45 & -00:50:52.38 & 17.812 & 15.924 & 15.033 & 14.580 & 14.237 & 11.494 & sdss j022842.64 - 005057.35 & - & sdss j022842.26 - 005047.40 & 0.085310 + 326 & 02:29:09.96 & + 01:00:43.39 & 19.888 & 18.066 & 17.156 & 16.790 & 16.434 & 7.231 & sdss j022910.20 + 010043.74 & - & sdss j022909.72 + 010043.05 & - + 327 & 02:29:22.24 & -00:38:46.66 & 19.191 & 17.278 & 16.241 & 15.786 & 15.410 & 5.010 & sdss j022922.12 - 003844.92 & 0.116381 & sdss j022922.36 - 003848.40 & - + 328 & 02:31:19.20 & + 00:29:07.11 & 20.290 & 19.336 & 18.727 & 18.419 & 18.490 & 6.276 & sdss j023119.08 + 002904.54 & - & sdss j023119.32 + 002909.68 & - + 329 & 02:31:26.49 & -00:47:34.54 & 17.312 & 16.224 & 15.856 & 15.744 & 15.712 & 4.327 & sdss j023126.64 - 004734.67 & 0.040612 & sdss j023126.35 - 004734.41 & - + 330 & 02:31:56.07 & -00:00:32.11 & 19.800 & 17.896 & 16.673 & 16.186 & 15.908 & 4.418 & sdss j023156.08 - 000029.91 & - & sdss j023156.06 - 000034.31 & - + 331 & 02:32:24.03 & -01:04:11.49 & 19.553 & 16.475 & 15.443 & 14.941 & 14.580 & 15.065 & sdss j023223.78 - 010404.98 & 0.071063 & sdss j023224.28 - 010418.01 & - + 332 & 02:35:10.24 & + 00:01:03.10 & 20.787 & 19.317 & 18.236 & 17.785 & 17.513 & 5.291 & sdss j023510.17 + 000100.69 & - & sdss j023510.32 + 000105.52 & - + 333 & 02:35:13.05 & -01:12:04.15 & 19.049 & 17.498 & 16.440 & 15.965 & 15.592 & 9.536 & sdss j023512.74 - 011205.07 & 0.119035 & sdss j023513.36 - 011203.24 & - + 334 & 02:35:34.58 & -00:34:54.39 & 21.758 & 19.867 & 18.456 & 17.897 & 17.466 & 4.599 & sdss j023534.65 - 003452.35 & - & sdss j023534.51 - 003456.42 & - + 335 & 02:35:49.94 & + 00:18:01.19 & 21.114 & 19.439 & 18.296 & 17.901 & 17.499 & 2.134 & sdss j023549.92 + 001800.18 & - & sdss j023549.96 + 001802.19 & - + 336 & 02:35:58.26 & + 01:15:27.84 & 18.594 & 16.780 & 15.985 & 15.530 & 15.194 & 3.126 & sdss j023558.20 + 011529.12 & - & sdss j023558.32 + 011526.56 & 0.124362 + 337 & 02:36:03.97 & -00:23:54.06 & 20.844 & 19.579 & 18.817 & 18.555 & 18.197 & 3.299 & sdss j023603.96 - 002355.70 & - & sdss j023603.98 - 002352.42 & - + 338 & 02:36:32.84 & + 00:57:12.47 & 18.843 & 17.668 & 16.972 & 16.567 & 16.349 & 5.434 & sdss j023632.97 + 005714.33 & - & sdss j023632.71 + 005710.61 & - + 339 & 02:37:08.62 & -00:30:07.54 & 19.272 & 17.425 & 16.298 & 15.785 & 15.466 & 4.516 & sdss j023708.59 - 003005.35 & - & sdss j023708.66 - 003009.73 & 0.185720 + 340 & 02:37:39.16 & + 00:38:58.21 & 18.999 & 17.221 & 16.482 & 15.998 & 15.712 & 2.916 & sdss j023739.09 + 003857.23 & - & sdss j023739.24 + 003859.19 & - + 341 & 02:37:42.60 & + 00:38:35.53 & 18.875 & 17.024 & 16.075 & 15.653 & 15.356 & 8.269 & sdss j023742.33 + 003834.35 & 0.126086 & sdss j023742.86 + 003836.72 & - + 342 & 02:37:50.64 & + 00:34:24.71 & 18.146 & 16.369 & 15.468 & 15.031 & 14.721 & 8.390 & sdss j023750.73 + 003428.65 & 0.062951 & sdss j023750.54 + 003420.77 & - + 343 & 02:37:53.30 & + 00:45:22.80 & 20.967 & 19.131 & 18.022 & 17.595 & 17.246 & 3.338 & sdss j023753.20 + 004521.96 & - & sdss j023753.40 + 004523.65 & - + 344 & 02:37:58.58 & + 00:53:04.50 & 19.955 & 18.940 & 18.288 & 17.984 & 17.766 & 7.481 & sdss j023758.48 + 005307.95 & - & sdss j023758.68 + 005301.05 & - + 345 & 02:38:32.49 & -00:11:08.60 & 17.579 & 16.288 & 15.756 & 15.500 & 15.305 & 11.441 & sdss j023832.13 - 001106.72 & 0.026744 & sdss j023832.85 - 001110.49 & - + 346 & 02:39:02.77 & -00:31:50.86 & 18.652 & 17.300 & 16.568 & 16.190 & 15.919 & 2.725 & sdss j023902.85 - 003151.38 & 0.136064 & sdss j023902.68 - 003150.35 & - + 347 & 02:39:58.33 & -00:31:49.18 & 17.830 & 16.850 & 16.702 & 16.587 & 16.585 & 6.840 & sdss j023958.56 - 003149.18 & 0.051669 & sdss j023958.10 - 003149.18 & - + 348 & 02:40:36.21 & -01:01:14.14 & 19.510 & 18.478 & 18.004 & 17.650 & 17.423 & 7.638 & sdss j024036.36 - 010110.99 & - & sdss j024036.07 - 010117.29 & - + 349 & 02:40:48.30 & + 01:06:18.34 & 17.772 & 16.724 & 16.381 & 16.324 & 16.267 & 6.312 & sdss j024048.09 + 010617.56 & 0.023431 & sdss j024048.50 + 010619.11 & - + 350 & 02:41:49.34 & -00:51:54.99 & 21.288 & 19.288 & 17.968 & 17.489 & 17.141 & 5.018 & sdss j024149.34 - 005157.50 & - & sdss j024149.34 - 005152.48 & - + 351 & 02:43:29.20 & + 00:38:35.52 & 20.354 & 17.851 & 17.209 & 16.840 & 16.770 & 4.485 & sdss j024329.11 + 003833.80 & - & sdss j024329.30 + 003837.24 & 0.218196 + 352 & 02:43:58.99 & + 00:33:24.57 & 18.869 & 17.867 & 17.711 & 17.565 & 17.489 & 3.944 & sdss j024358.94 + 003326.40 & - & sdss j024359.04 + 003322.73 & - + 353 & 02:44:02.40 & -01:04:31.08 & 19.120 & 17.862 & 17.024 & 16.616 & 16.309 & 5.667 & sdss j024402.23 - 010432.37 & - & sdss j024402.56 - 010429.78 & 0.179604 + 354 & 02:44:02.84 & + 00:33:41.88 & 18.753 & 17.785 & 17.531 & 17.344 & 17.228 & 9.101 & sdss j024403.14 + 003341.20 & - & sdss j024402.54 + 003342.56 & - + 355 & 02:44:05.34 & -00:21:13.12 & 18.130 & 17.030 & 16.446 & 16.087 & 15.885 & 8.427 & sdss j024405.08 - 002111.26 & 0.133108 & sdss j024405.59 - 002114.99 & - + 356 & 02:44:27.42 & + 01:13:21.45 & 20.845 & 19.037 & 18.058 & 17.625 & 17.393 & 2.724 & sdss j024427.40 + 011322.80 & - & sdss j024427.43 + 011320.10 & - + 357 & 02:45:26.24 & + 00:14:36.83 & 20.332 & 18.102 & 16.855 & 16.335 & 16.032 & 3.463 & sdss j024526.35 + 001436.21 & 0.182166 & sdss j024526.13 + 001437.44 & - + 358 & 02:45:53.30 & -00:05:31.71 & 19.616 & 18.565 & 18.133 & 17.843 & 17.740 & 2.403 & sdss j024553.25 - 000530.74 & - & sdss j024553.35 - 000532.67 & - + 359 & 02:45:57.38 & -00:45:09.19 & 17.134 & 16.152 & 15.805 & 15.644 & 15.628 & 6.466 & sdss j024557.45 - 004512.24 & 0.054013 & sdss j024557.31 - 004506.15 & - + 360 & 02:46:36.72 & -00:03:43.86 & 19.982 & 17.891 & 16.678 & 16.190 & 15.761 & 8.068 & sdss j024636.88 - 000347.01 & - & sdss j024636.55 - 000340.71 & 0.182135 + 361 & 02:46:46.83 & -00:41:40.62 & 19.906 & 18.610 & 17.750 & 17.207 & 16.916 & 5.401 & sdss j024646.65 - 004140.57 & - & sdss j024647.01 - 004140.67 & - + 362 & 02:47:07.26 & -01:03:58.95 & 19.667 & 18.346 & 17.476 & 17.015 & 16.679 & 9.819 & sdss j024706.93 - 010359.65 & 0.113242 & sdss j024707.58 - 010358.24 & - + 363 & 02:49:10.20 & -01:00:10.20 & 20.734 & 18.737 & 17.508 & 16.991 & 16.720 & 2.917 & sdss j024910.10 - 010010.44 & - & sdss j024910.29 - 010009.97 & - + 364 & 02:49:26.66 & + 00:01:25.82 & 18.742 & 17.117 & 16.081 & 15.599 & 15.290 & 11.490 & sdss j024926.47 + 000130.79 & 0.150226 & sdss j024926.85 + 000120.85 & - + 365 & 02:51:40.02 & -00:45:20.55 & 16.940 & 16.057 & 15.719 & 15.506 & 15.324 & 6.857 & sdss j025139.79 - 004520.31 & 0.028373 & sdss j025140.24 - 004520.80 & - + 366 & 02:51:58.15 & -00:12:17.37 & 20.346 & 19.653 & 19.255 & 18.982 & 19.148 & 3.831 & sdss j025158.08 - 001215.79 & - & sdss j025158.22 - 001218.96 & - + 367 & 02:52:44.24 & -00:02:38.02 & 20.084 & 18.566 & 17.570 & 17.030 & 16.690 & 5.614 & sdss j025244.20 - 000240.78 & - & sdss j025244.28 - 000235.27 & - + 368 & 02:52:54.67 & + 00:43:47.21 & 20.667 & 18.467 & 17.173 & 16.670 & 16.245 & 8.108 & sdss j025254.55 + 004343.57 & 0.185988 & sdss j025254.79 + 004350.84 & - + 369 & 02:53:06.66 & + 01:09:43.90 & 17.338 & 16.350 & 15.999 & 15.821 & 15.790 & 5.053 & sdss j025306.50 + 010944.85 & 0.058854 & sdss j025306.81 + 010942.94 & - + 370 & 02:54:16.92 & + 01:12:05.07 & 17.618 & 15.962 & 14.884 & 14.448 & 13.989 & 15.701 & sdss j025416.44 + 011208.20 & - & sdss j025417.40 + 011201.94 & 0.067698 + 371 & 02:54:30.24 & + 01:00:04.55 & 20.482 & 18.239 & 17.064 & 16.590 & 16.077 & 2.907 & sdss j025430.14 + 010004.75 & - & sdss j025430.33 + 010004.35 & - + 372 & 02:58:56.46 & -00:58:59.14 & 18.312 & 17.104 & 16.775 & 16.935 & 16.049 & 4.510 & sdss j025856.37 - 005857.27 & - & sdss j025856.54 - 005901.01 & - + 373 & 02:59:42.55 & + 00:01:39.69 & 17.495 & 16.466 & 15.754 & 15.694 & 15.583 & 4.670 & sdss j025942.67 + 000141.18 & 0.043107 & sdss j025942.43 + 000138.21 & - + 374 & 03:00:51.18 & + 00:49:00.37 & 19.252 & 17.545 & 16.740 & 16.348 & 16.077 & 5.481 & sdss j030051.26 + 004857.94 & 0.044221 & sdss j030051.09 + 004902.80 & - + 375 & 03:01:44.07 & -00:34:45.83 & 20.155 & 19.456 & 19.046 & 18.728 & 18.593 & 4.691 & sdss j030144.11 - 003443.55 & - & sdss j030144.04 - 003448.11 & - + 376 & 03:02:21.00 & + 00:23:28.92 & 21.139 & 18.756 & 17.272 & 16.761 & 16.253 & 7.056 & sdss j030221.19 + 002330.96 & - & sdss j030220.80 + 002326.89 & - + 377 & 03:02:25.92 & + 00:06:23.49 & 19.037 & 17.530 & 16.689 & 16.251 & 15.933 & 7.285 & sdss j030226.16 + 000624.05 & 0.087482 & sdss j030225.68 + 000622.93 & - + 378 & 03:02:51.06 & + 00:26:25.85 & 19.740 & 18.011 & 17.173 & 16.774 & 16.457 & 1.987 & sdss j030251.12 + 002625.42 & 0.174660 & sdss j030251.00 + 002626.27 & - + 379 & 03:03:56.29 & + 00:50:17.56 & 17.402 & 16.288 & 15.816 & 15.660 & 15.432 & 8.173 & sdss j030356.49 + 005020.27 & 0.020074 & sdss j030356.08 + 005014.85 & - + 380 & 03:03:56.67 & + 00:43:38.50 & 20.475 & 18.984 & 17.919 & 17.367 & 16.940 & 6.059 & sdss j030356.61 + 004341.40 & - & sdss j030356.73 + 004335.61 & - + 381 & 03:04:19.63 & + 01:09:07.75 & 20.635 & 18.830 & 17.777 & 17.311 & 16.954 & 4.867 & sdss j030419.53 + 010909.72 & - & sdss j030419.72 + 010905.79 & - + 382 & 03:04:32.71 & -00:13:21.73 & 19.452 & 18.393 & 17.927 & 17.598 & 17.628 & 4.362 & sdss j030432.61 - 001320.10 & - & sdss j030432.80 - 001323.37 & - + 383 & 03:04:38.74 & + 01:11:19.05 & 20.512 & 18.392 & 17.376 & 16.923 & 16.609 & 3.249 & sdss j030438.83 + 011120.07 & - & sdss j030438.66 + 011118.02 & - + 384 & 03:05:01.45 & + 00:23:01.39 & 18.494 & 17.668 & 17.212 & 17.006 & 16.653 & 6.105 & sdss j030501.48 + 002304.39 & 0.019487 & sdss j030501.41 + 002258.38 & - + 385 & 03:05:37.86 & -00:40:01.12 & 19.985 & 17.952 & 16.809 & 16.292 & 15.848 & 4.012 & sdss j030537.72 - 004001.44 & 0.110011 & sdss j030537.99 - 004000.79 & - + 386 & 03:06:19.23 & + 00:14:06.24 & 19.967 & 18.836 & 18.060 & 17.667 & 17.505 & 3.306 & sdss j030619.34 + 001405.91 & - & sdss j030619.12 + 001406.57 & - + 387 & 03:06:20.88 & + 00:48:04.02 & 20.066 & 18.360 & 17.574 & 17.182 & 16.847 & 3.758 & sdss j030620.76 + 004804.56 & - & sdss j030621.00 + 004803.48 & - + 388 & 03:06:28.52 & -00:17:37.21 & 21.443 & 18.233 & 17.212 & 15.916 & 14.903 & 1.802 & sdss j030628.58 - 001737.25 & - & sdss j030628.46 - 001737.16 & - + 389 & 03:06:30.68 & -00:49:20.48 & 20.137 & 18.880 & 17.975 & 17.499 & 17.338 & 3.655 & sdss j030630.57 - 004919.63 & - & sdss j030630.79 - 004921.32 & - + 390 & 03:08:18.62 & + 00:47:13.72 & 19.727 & 18.078 & 17.047 & 16.529 & 16.234 & 2.271 & sdss j030818.69 + 004714.07 & 0.155895 & sdss j030818.55 + 004713.36 & - + 391 & 03:08:56.95 & -00:35:02.19 & 18.107 & 17.138 & 16.837 & 16.776 & 16.959 & 7.336 & sdss j030856.71 - 003502.89 & - & sdss j030857.19 - 003501.48 & - + 392 & 03:09:01.03 & -00:44:22.07 & 18.550 & 17.172 & 16.372 & 15.806 & 15.577 & 8.810 & sdss j030901.17 - 004418.24 & 0.078201 & sdss j030900.88 - 004425.91 & - + 393 & 03:09:17.42 & -00:22:02.23 & 19.468 & 17.840 & 16.590 & 16.062 & 15.725 & 9.936 & sdss j030917.71 - 002159.78 & 0.207172 & sdss j030917.13 - 002204.69 & - + 394 & 03:09:45.96 & + 00:21:33.93 & 19.629 & 18.790 & 18.415 & 18.347 & 18.127 & 4.817 & sdss j030946.10 + 002134.99 & - & sdss j030945.81 + 002132.86 & - + 395 & 03:11:09.09 & -00:30:04.53 & 18.938 & 17.729 & 16.912 & 16.461 & 16.114 & 7.172 & sdss j031108.97 - 003001.43 & 0.135339 & sdss j031109.21 - 003007.63 & - + 396 & 03:11:12.28 & -00:17:07.29 & 20.249 & 18.270 & 17.356 & 16.895 & 16.675 & 4.235 & sdss j031112.36 - 001705.47 & - & sdss j031112.21 - 001709.11 & - + 397 & 03:11:21.45 & -00:37:25.54 & 18.708 & 17.360 & 16.059 & 15.683 & 15.335 & 8.636 & sdss j031121.69 - 003723.15 & 0.206868 & sdss j031121.21 - 003727.92 & - + 398 & 03:12:34.04 & -00:29:53.77 & 19.118 & 18.015 & 17.652 & 17.384 & 17.223 & 7.650 & sdss j031233.81 - 002952.06 & - & sdss j031234.27 - 002955.48 & - + 399 & 03:12:43.71 & -00:53:38.94 & 19.256 & 18.316 & 17.788 & 17.447 & 17.233 & 6.120 & sdss j031243.72 - 005341.99 & - & sdss j031243.70 - 005335.88 & - + 400 & 03:12:48.37 & -01:00:26.37 & 18.760 & 16.949 & 15.985 & 15.516 & 15.105 & 14.655 & sdss j031248.26 - 010033.51 & - & sdss j031248.48 - 010019.22 & - + 401 & 03:12:54.61 & -00:52:12.16 & 20.200 & 18.197 & 16.868 & 16.348 & 15.972 & 6.160 & sdss j031254.81 - 005212.51 & 0.211980 & sdss j031254.40 - 005211.80 & - + 402 & 03:14:19.38 & -00:59:31.76 & 19.329 & 18.091 & 17.504 & 17.119 & 16.996 & 4.732 & sdss j031419.22 - 005932.11 & 0.139650 & sdss j031419.53 - 005931.41 & - + 403 & 03:15:09.86 & -01:11:02.95 & 17.973 & 16.545 & 15.788 & 14.958 & 14.605 & 2.222 & sdss j031509.91 - 011102.11 & - & sdss j031509.81 - 011103.80 & - + 404 & 03:15:45.57 & -00:29:46.67 & 18.380 & 16.368 & 15.393 & 14.950 & 14.522 & 6.129 & sdss j031545.69 - 002949.15 & 0.086943 & sdss j031545.45 - 002944.19 & 0.086960 + 405 & 03:16:03.13 & + 01:11:06.23 & 18.595 & 17.123 & 16.522 & 16.113 & 15.816 & 8.327 & sdss j031603.40 + 011105.78 & 0.049977 & sdss j031602.85 + 011106.68 & - + 406 & 03:16:06.24 & -00:26:18.85 & 17.776 & 17.389 & 17.477 & 17.484 & 17.382 & 2.399 & sdss j031606.31 - 002618.33 & 0.022917 & sdss j031606.16 - 002619.37 & - + 407 & 03:17:12.80 & + 00:06:46.17 & 19.432 & 17.428 & 16.289 & 15.785 & 15.420 & 2.414 & sdss j031712.86 + 000646.98 & - & sdss j031712.74 + 000645.37 & - + 408 & 03:17:14.77 & + 00:05:29.84 & 19.474 & 18.112 & 17.392 & 16.846 & 16.651 & 5.006 & sdss j031714.68 + 000532.00 & - & sdss j031714.85 + 000527.68 & - + 409 & 03:17:22.15 & + 00:48:01.33 & 19.954 & 18.306 & 17.284 & 16.770 & 16.433 & 3.015 & sdss j031722.24 + 004800.88 & 0.156132 & sdss j031722.05 + 004801.78 & - + 410 & 03:17:25.98 & + 00:28:03.97 & 19.430 & 18.350 & 18.015 & 17.736 & 17.595 & 5.358 & sdss j031725.82 + 002805.27 & - & sdss j031726.13 + 002802.66 & - + 411 & 03:18:03.01 & -00:32:25.98 & 17.705 & 15.984 & 15.222 & 14.640 & 14.165 & 13.034 & sdss j031802.78 - 003220.43 & 0.020884 & sdss j031803.24 - 003231.53 & - + 412 & 03:18:08.07 & + 00:05:15.54 & 21.442 & 18.991 & 17.934 & 17.480 & 17.168 & 2.717 & sdss j031808.08 + 000516.89 & - & sdss j031808.06 + 000514.19 & - + 413 & 03:18:09.68 & -00:48:53.15 & 20.823 & 19.547 & 18.882 & 18.441 & 18.151 & 4.787 & sdss j031809.57 - 004854.91 & - & sdss j031809.79 - 004851.39 & - + 414 & 03:20:18.94 & + 00:23:38.27 & 18.222 & 16.879 & 16.255 & 15.956 & 15.699 & 6.034 & sdss j032018.96 + 002341.28 & 0.066793 & sdss j032018.93 + 002335.26 & - + 415 & 03:21:23.98 & + 00:18:30.89 & 19.615 & 18.485 & 17.618 & 17.026 & 16.449 & 5.437 & sdss j032124.16 + 001831.20 & - & sdss j032123.80 + 001830.57 & - + 416 & 03:23:24.70 & + 00:39:02.24 & 20.702 & 18.806 & 17.522 & 16.974 & 16.669 & 5.039 & sdss j032324.60 + 003904.17 & - & sdss j032324.81 + 003900.31 & - + 417 & 03:24:03.96 & -00:02:03.48 & 19.855 & 17.752 & 16.665 & 16.172 & 15.686 & 9.396 & sdss j032403.64 - 000203.90 & 0.140839 & sdss j032404.27 - 000203.07 & - + 418 & 03:24:31.08 & -00:45:45.70 & 19.944 & 18.979 & 18.268 & 17.912 & 17.667 & 3.022 & sdss j032431.00 - 004546.75 & - & sdss j032431.15 - 004544.64 & - + 419 & 03:24:49.68 & -00:36:41.96 & 20.139 & 19.395 & 18.985 & 18.587 & 18.525 & 2.972 & sdss j032449.65 - 003643.40 & - & sdss j032449.70 - 003640.52 & - + 420 & 03:24:55.27 & + 00:36:18.17 & 18.537 & 16.381 & 15.312 & 14.834 & 14.432 & 11.858 & sdss j032454.93 + 003621.29 & - & sdss j032455.60 + 003615.05 & - + 421 & 03:25:39.07 & + 00:14:34.04 & 18.967 & 16.950 & 16.064 & 15.604 & 15.191 & 4.956 & sdss j032539.09 + 001431.59 & 0.051103 & sdss j032539.04 + 001436.49 & - + 422 & 03:26:45.91 & + 01:10:59.44 & 18.709 & 17.687 & 17.432 & 17.119 & 16.980 & 3.284 & sdss j032645.86 + 011057.97 & - & sdss j032645.96 + 011100.92 & - + 423 & 03:27:17.89 & -00:04:29.11 & 18.867 & 16.968 & 15.935 & 15.352 & 14.798 & 13.019 & sdss j032717.92 - 000435.60 & - & sdss j032717.85 - 000422.63 & 0.051527 + 424 & 03:27:18.66 & -00:28:32.06 & 19.141 & 17.810 & 17.028 & 16.462 & 16.038 & 3.628 & sdss j032718.60 - 002830.48 & 0.133798 & sdss j032718.72 - 002833.63 & - + 425 & 03:27:25.48 & + 00:13:08.17 & 19.588 & 18.411 & 17.517 & 17.072 & 16.672 & 8.704 & sdss j032725.77 + 001308.69 & 0.150742 & sdss j032725.20 + 001307.64 & - + 426 & 03:28:12.82 & -00:09:50.70 & 18.952 & 17.808 & 17.489 & 17.129 & 17.026 & 5.437 & sdss j032812.67 - 000949.31 & 0.150742 & sdss j032812.98 - 000952.08 & - + 427 & 03:28:17.55 & + 00:43:51.26 & 20.094 & 18.727 & 17.910 & 17.496 & 17.215 & 5.504 & sdss j032817.44 + 004349.04 & 0.100692 & sdss j032817.66 + 004353.49 & - + 428 & 03:28:31.92 & + 00:20:23.86 & 19.322 & 18.368 & 18.197 & 17.930 & 17.709 & 2.416 & sdss j032831.96 + 002024.83 & - & sdss j032831.87 + 002022.89 & - + 429 & 03:29:52.15 & -00:54:07.07 & 20.280 & 18.355 & 17.250 & 16.796 & 16.357 & 7.364 & sdss j032952.39 - 005407.85 & 0.145567 & sdss j032951.91 - 005406.30 & - + 430 & 03:33:28.75 & + 00:01:57.26 & 20.598 & 18.218 & 16.945 & 16.428 & 16.089 & 4.257 & sdss j033328.87 + 000156.13 & 0.176824 & sdss j033328.63 + 000158.40 & - + 431 & 03:35:36.85 & + 00:35:32.29 & 20.817 & 19.416 & 17.916 & 17.331 & 17.002 & 4.655 & sdss j033536.72 + 003533.51 & 0.317134 & sdss j033536.98 + 003531.07 & - + 432 & 03:35:37.70 & -00:41:31.63 & 20.463 & 18.234 & 16.991 & 16.399 & 15.961 & 8.085 & sdss j033537.82 - 004128.01 & 0.155444 & sdss j033537.58 - 004135.25 & - + 433 & 03:38:33.02 & + 00:48:24.39 & 19.434 & 18.411 & 17.826 & 17.415 & 17.099 & 6.257 & sdss j033833.12 + 004821.61 & - & sdss j033832.92 + 004827.16 & - + 434 & 03:39:40.81 & -00:50:01.68 & 17.902 & 16.937 & 16.442 & 16.330 & 16.371 & 2.528 & sdss j033940.75 - 005000.79 & 0.060929 & sdss j033940.87 - 005002.56 & - + 435 & 03:40:10.54 & + 00:07:56.06 & 20.094 & 19.384 & 18.838 & 18.518 & 18.336 & 4.755 & sdss j034010.56 + 000753.69 & - & sdss j034010.53 + 000758.43 & - + 436 & 03:40:19.14 & -01:10:50.80 & 19.817 & 18.408 & 17.407 & 16.959 & 16.649 & 5.578 & sdss j034019.17 - 011048.07 & 0.146324 & sdss j034019.10 - 011053.54 & - + 437 & 03:41:32.05 & + 00:23:55.05 & 17.375 & 16.138 & 15.757 & 15.609 & 15.480 & 2.520 & sdss j034131.96 + 002355.07 & - & sdss j034132.13 + 002355.02 & - + 438 & 03:42:36.66 & -00:28:01.28 & 19.828 & 18.350 & 17.334 & 16.865 & 16.506 & 5.886 & sdss j034236.55 - 002758.82 & - & sdss j034236.76 - 002803.74 & - + 439 & 03:42:42.76 & -00:17:09.31 & 21.061 & 18.795 & 17.063 & 16.377 & 16.117 & 4.066 & sdss j034242.64 - 001708.37 & - & sdss j034242.88 - 001710.26 & 0.312721 + 440 & 03:44:00.06 & + 00:40:44.90 & 18.940 & 17.042 & 16.180 & 15.723 & 15.415 & 8.908 & sdss j034400.26 + 004041.66 & 0.072268 & sdss j034359.85 + 004048.14 & - + 441 & 09:43:06.12 & + 00:19:12.20 & 18.161 & 17.089 & 17.161 & 17.210 & 17.081 & 3.833 & sdss j094306.00 + 001912.86 & 0.024996 & sdss j094306.24 + 001911.54 & - + 442 & 09:43:33.72 & -00:51:37.57 & 19.994 & 18.943 & 18.651 & 18.388 & 18.412 & 3.671 & sdss j094333.84 - 005137.21 & - & sdss j094333.60 - 005137.93 & - + 443 & 09:43:39.00 & -00:52:41.65 & 18.474 & 17.281 & 16.548 & 16.253 & 15.924 & 7.007 & sdss j094339.12 - 005238.64 & - & sdss j094338.88 - 005244.65 & - + 444 & 09:44:02.04 & -00:38:36.79 & 16.835 & 16.098 & 16.140 & 16.733 & 16.684 & 9.867 & sdss j094401.92 - 003832.19 & 0.004809 & sdss j094402.16 - 003841.38 & 0.004677 + 445 & 09:45:29.76 & -00:22:00.49 & 17.510 & 16.111 & 15.430 & 14.861 & 14.578 & 11.592 & sdss j094529.76 - 002154.70 & - & sdss j094529.76 - 002206.29 & 0.052903 + 446 & 09:47:44.28 & + 00:00:02.54 & 20.188 & 19.120 & 18.980 & 18.792 & 18.914 & 5.138 & sdss j094744.16 + 000000.71 & - & sdss j094744.40 + 000004.37 & - + 447 & 09:49:14.16 & + 00:20:41.37 & 18.331 & 17.112 & 16.759 & 16.406 & 16.375 & 3.931 & sdss j094914.16 + 002039.40 & 0.072901 & sdss j094914.16 + 002043.33 & - + 448 & 09:49:24.48 & -00:06:30.04 & 17.857 & 17.256 & 17.104 & 17.348 & 17.249 & 2.729 & sdss j094924.48 - 000628.67 & - & sdss j094924.48 - 000631.40 & - + 449 & 09:49:58.80 & -00:52:54.31 & 17.721 & 16.492 & 15.615 & 15.290 & 14.901 & 12.404 & sdss j094959.04 - 005249.26 & - & sdss j094958.56 - 005259.36 & 0.091560 + 450 & 09:49:59.88 & + 00:06:19.56 & 17.300 & 16.643 & 15.929 & 15.782 & 15.490 & 14.063 & sdss j094959.52 + 000615.06 & 0.084193 & sdss j095000.24 + 000624.06 & - + 451 & 09:50:29.04 & -00:54:51.17 & 19.023 & 17.096 & 16.260 & 15.871 & 15.539 & 4.579 & sdss j095029.04 - 005453.46 & 0.066402 & sdss j095029.04 - 005448.88 & - + 452 & 09:51:13.80 & -00:52:59.07 & 17.604 & 16.116 & 15.312 & 14.983 & 14.717 & 11.435 & sdss j095113.92 - 005304.50 & 0.091285 & sdss j095113.68 - 005253.65 & - + 453 & 09:51:39.60 & + 00:59:39.21 & 20.440 & 18.542 & 17.720 & 17.254 & 16.927 & 2.614 & sdss j095139.60 + 005937.91 & - & sdss j095139.60 + 005940.52 & - + 454 & 09:52:34.92 & + 00:14:58.17 & 18.157 & 16.828 & 16.215 & 15.709 & 15.525 & 4.838 & sdss j095234.80 + 001459.79 & 0.081409 & sdss j095235.04 + 001456.56 & 0.081953 + 455 & 09:52:41.52 & -00:03:56.34 & 19.157 & 17.388 & 16.398 & 15.923 & 15.576 & 6.762 & sdss j095241.52 - 000352.95 & 0.085599 & sdss j095241.52 - 000359.72 & - + 456 & 09:53:06.96 & + 00:37:58.08 & 19.214 & 18.040 & 17.325 & 16.943 & 16.740 & 3.211 & sdss j095306.96 + 003759.68 & - & sdss j095306.96 + 003756.47 & - + 457 & 09:53:14.88 & + 00:38:58.39 & 19.836 & 18.081 & 17.117 & 16.598 & 16.096 & 2.884 & sdss j095314.88 + 003859.84 & 0.093933 & sdss j095314.88 + 003856.95 & - + 458 & 09:53:16.20 & + 00:40:02.71 & 19.246 & 17.178 & 16.087 & 15.581 & 15.133 & 6.344 & sdss j095316.32 + 004000.10 & 0.093741 & sdss j095316.08 + 004005.32 & 0.094023 + 459 & 09:53:49.08 & + 00:12:13.21 & 19.859 & 18.302 & 17.429 & 16.938 & 16.549 & 14.188 & sdss j095348.72 + 001217.82 & 0.094100 & sdss j095349.44 + 001208.61 & - + 460 & 09:55:11.16 & + 00:19:53.71 & 19.696 & 18.485 & 17.829 & 17.453 & 17.198 & 3.686 & sdss j095511.04 + 001954.11 & - & sdss j095511.28 + 001953.32 & - + 461 & 09:55:34.68 & -00:53:49.48 & 20.025 & 18.764 & 18.269 & 17.988 & 17.969 & 4.891 & sdss j095534.56 - 005351.13 & - & sdss j095534.80 - 005347.82 & - + 462 & 09:55:39.60 & -00:05:49.50 & 20.411 & 18.505 & 17.137 & 16.487 & 16.141 & 2.646 & sdss j095539.60 - 000550.82 & - & sdss j095539.60 - 000548.18 & 0.216023 + 463 & 09:55:48.12 & + 00:33:23.15 & 17.953 & 16.097 & 15.157 & 14.710 & 14.354 & 11.338 & sdss j095548.48 + 003324.87 & 0.079948 & sdss j095547.76 + 003321.42 & 0.077780 + 464 & 09:55:52.44 & -00:10:45.95 & 19.310 & 17.584 & 16.765 & 16.360 & 16.090 & 4.390 & sdss j095552.56 - 001044.70 & 0.083202 & sdss j095552.32 - 001047.21 & - + 465 & 09:56:59.40 & + 00:14:00.34 & 20.195 & 18.496 & 17.504 & 17.023 & 16.757 & 4.221 & sdss j095659.52 + 001359.24 & - & sdss j095659.28 + 001401.44 & - + 466 & 09:57:05.28 & -00:05:07.26 & 17.006 & 16.543 & 15.595 & 14.764 & 14.797 & 9.231 & sdss j095705.28 - 000502.64 & - & sdss j095705.28 - 000511.87 & - + 467 & 09:57:38.52 & + 00:49:53.85 & 21.135 & 18.884 & 17.550 & 17.010 & 16.615 & 5.732 & sdss j095738.64 + 004956.08 & - & sdss j095738.40 + 004951.62 & - + 468 & 09:57:46.56 & + 00:40:26.11 & 17.221 & 16.059 & 15.527 & 15.405 & 15.313 & 10.842 & sdss j095746.80 + 004022.06 & 0.046601 & sdss j095746.32 + 004030.17 & - + 469 & 09:58:07.20 & + 00:03:26.09 & 20.290 & 18.638 & 17.402 & 16.916 & 16.567 & 3.213 & sdss j095807.20 + 000324.48 & - & sdss j095807.20 + 000327.70 & - + 470 & 09:58:53.88 & + 00:07:12.14 & 19.330 & 18.101 & 17.797 & 17.373 & 17.269 & 9.941 & sdss j095854.00 + 000707.51 & - & sdss j095853.76 + 000716.78 & - + 471 & 10:00:04.08 & -00:35:15.39 & 18.123 & 16.849 & 16.151 & 15.754 & 15.491 & 3.301 & sdss j100004.08 - 003517.04 & 0.046010 & sdss j100004.08 - 003513.74 & - + 472 & 10:00:54.36 & + 00:02:35.76 & 17.926 & 16.263 & 15.585 & 15.556 & 15.168 & 18.115 & sdss j100053.76 + 000234.74 & - & sdss j100054.96 + 000236.78 & 0.099593 + 473 & 10:00:54.72 & -00:18:41.53 & 18.426 & 16.604 & 15.704 & 15.273 & 14.951 & 6.905 & sdss j100054.72 - 001838.08 & 0.087918 & sdss j100054.72 - 001844.98 & - + 474 & 10:01:20.16 & + 00:24:01.50 & 21.437 & 19.559 & 18.318 & 17.883 & 17.522 & 2.851 & sdss j100120.16 + 002402.93 & - & sdss j100120.16 + 002400.08 & - + 475 & 10:01:32.28 & + 00:39:38.14 & 19.388 & 17.998 & 16.864 & 16.410 & 16.150 & 6.789 & sdss j100132.40 + 003935.26 & - & sdss j100132.16 + 003941.02 & - + 476 & 10:01:55.32 & + 00:40:58.67 & 18.758 & 17.024 & 16.173 & 15.704 & 15.385 & 7.784 & sdss j100155.44 + 004102.12 & 0.094373 & sdss j100155.20 + 004055.22 & - + 477 & 10:01:56.04 & -00:09:41.42 & 19.758 & 18.049 & 17.146 & 16.756 & 16.458 & 7.438 & sdss j100156.16 - 000944.67 & - & sdss j100155.92 - 000938.17 & - + 478 & 10:02:07.44 & -00:57:48.19 & 20.428 & 18.845 & 17.820 & 17.329 & 16.976 & 2.480 & sdss j100207.44 - 005749.43 & - & sdss j100207.44 - 005746.95 & - + 479 & 10:02:10.08 & -00:44:50.90 & 18.376 & 16.536 & 15.506 & 15.086 & 14.718 & 14.496 & sdss j100210.32 - 004444.61 & 0.086750 & sdss j100209.84 - 004457.19 & - + 480 & 10:02:11.28 & -00:37:41.92 & 19.621 & 18.446 & 17.703 & 17.313 & 17.055 & 6.685 & sdss j100211.28 - 003745.27 & - & sdss j100211.28 - 003738.58 & - + 481 & 10:02:14.28 & + 00:34:49.29 & 19.706 & 18.784 & 18.272 & 18.036 & 17.962 & 5.099 & sdss j100214.40 + 003447.48 & - & sdss j100214.16 + 003451.09 & - + 482 & 10:02:14.40 & -00:28:14.81 & 20.005 & 18.696 & 18.132 & 17.836 & 17.640 & 2.686 & sdss j100214.40 - 002816.16 & - & sdss j100214.40 - 002813.47 & - + 483 & 10:03:12.84 & + 00:18:59.72 & 20.119 & 19.391 & 19.138 & 20.770 & 18.679 & 3.858 & sdss j100312.96 + 001859.03 & - & sdss j100312.72 + 001900.41 & - + 484 & 10:03:13.80 & + 00:55:03.33 & 18.534 & 16.733 & 15.797 & 15.304 & 14.981 & 7.707 & sdss j100313.68 + 005459.92 & 0.096464 & sdss j100313.92 + 005506.74 & - + 485 & 10:05:59.04 & -00:01:38.30 & 19.515 & 17.840 & 16.848 & 16.361 & 16.035 & 8.779 & sdss j100558.80 - 000140.81 & 0.181579 & sdss j100559.28 - 000135.79 & - + 486 & 10:06:32.28 & -00:51:54.65 & 21.389 & 19.309 & 18.175 & 17.695 & 17.363 & 3.726 & sdss j100632.16 - 005155.13 & - & sdss j100632.40 - 005154.17 & - + 487 & 10:06:35.76 & -00:44:03.78 & 18.912 & 17.282 & 16.443 & 15.999 & 15.707 & 7.484 & sdss j100635.76 - 004407.52 & - & sdss j100635.76 - 004400.03 & 0.211010 + 488 & 10:06:44.76 & -00:59:16.15 & 20.581 & 18.962 & 17.895 & 17.387 & 16.965 & 6.869 & sdss j100644.64 - 005913.23 & - & sdss j100644.88 - 005919.08 & - + 489 & 10:06:45.36 & + 01:02:30.46 & 20.103 & 17.896 & 16.974 & 16.496 & 16.194 & 3.924 & sdss j100645.36 + 010228.50 & - & sdss j100645.36 + 010232.42 & - + 490 & 10:06:47.88 & -00:30:15.55 & 17.828 & 16.690 & 16.333 & 16.059 & 15.980 & 6.080 & sdss j100648.00 - 003013.10 & 0.044643 & sdss j100647.76 - 003018.00 & - + 491 & 10:07:09.24 & -00:34:53.39 & 18.830 & 17.648 & 16.787 & 16.378 & 16.061 & 3.601 & sdss j100709.12 - 003453.45 & 0.185142 & sdss j100709.36 - 003453.34 & - + 492 & 10:07:11.64 & + 00:48:23.81 & 18.625 & 17.293 & 16.721 & 16.330 & 15.989 & 18.000 & sdss j100711.76 + 004832.63 & 0.021274 & sdss j100711.52 + 004814.99 & - + 493 & 10:07:19.32 & -00:09:03.74 & 19.507 & 18.180 & 17.199 & 16.736 & 16.350 & 5.184 & sdss j100719.44 - 000905.60 & 0.190823 & sdss j100719.20 - 000901.87 & - + 494 & 10:07:33.00 & + 00:35:34.25 & 18.045 & 16.002 & 14.978 & 14.576 & 14.121 & 14.232 & sdss j100732.64 + 003538.89 & - & sdss j100733.36 + 003529.62 & - + 495 & 10:07:47.40 & + 00:34:03.97 & 19.491 & 17.643 & 16.687 & 16.224 & 15.800 & 4.791 & sdss j100747.28 + 003405.55 & - & sdss j100747.52 + 003402.39 & - + 496 & 10:08:28.44 & -00:34:17.99 & 19.977 & 18.774 & 17.726 & 17.197 & 16.826 & 3.750 & sdss j100828.32 - 003417.46 & - & sdss j100828.56 - 003418.51 & - + 497 & 10:08:29.16 & -00:44:08.36 & 18.462 & 17.118 & 16.486 & 16.129 & 15.944 & 5.280 & sdss j100829.28 - 004410.29 & 0.067471 & sdss j100829.04 - 004406.43 & - + 498 & 10:08:34.92 & -00:51:48.15 & 19.345 & 18.256 & 17.739 & 17.475 & 17.177 & 6.144 & sdss j100835.04 - 005145.66 & - & sdss j100834.80 - 005150.64 & 0.194000 + 499 & 10:08:39.00 & + 00:01:06.49 & 20.573 & 18.829 & 17.722 & 17.134 & 16.759 & 6.976 & sdss j100838.88 + 000109.47 & - & sdss j100839.12 + 000103.50 & - + 500 & 10:08:54.00 & -00:13:59.32 & 19.429 & 18.225 & 17.697 & 17.362 & 17.183 & 4.662 & sdss j100854.00 - 001401.65 & - & sdss j100854.00 - 001356.99 & - + 501 & 10:09:00.36 & + 00:48:01.37 & 19.562 & 18.635 & 18.050 & 17.689 & 17.454 & 4.407 & sdss j100900.24 + 004802.64 & 0.125200 & sdss j100900.48 + 004800.10 & - + 502 & 10:09:04.20 & + 00:21:43.97 & 20.255 & 18.416 & 17.312 & 16.836 & 16.542 & 3.600 & sdss j100904.08 + 002144.00 & - & sdss j100904.32 + 002143.94 & - + 503 & 10:09:13.92 & + 00:31:56.07 & 18.874 & 17.910 & 17.591 & 17.358 & 17.161 & 8.644 & sdss j100913.92 + 003200.39 & - & sdss j100913.92 + 003151.75 & - + 504 & 10:09:15.96 & -00:44:24.80 & 17.496 & 16.542 & 16.091 & 15.991 & 15.904 & 3.781 & sdss j100916.08 - 004425.38 & 0.067299 & sdss j100915.84 - 004424.22 & - + 505 & 10:09:17.04 & -00:30:51.57 & 20.148 & 18.281 & 17.110 & 16.636 & 16.370 & 2.891 & sdss j100917.04 - 003053.01 & - & sdss j100917.04 - 003050.12 & - + 506 & 10:09:26.88 & + 00:15:28.63 & 20.807 & 19.921 & 19.629 & 19.354 & 19.497 & 2.786 & sdss j100926.88 + 001527.23 & - & sdss j100926.88 + 001530.02 & - + 507 & 10:09:29.76 & -00:21:12.53 & 19.840 & 18.546 & 17.726 & 17.282 & 16.947 & 7.631 & sdss j100930.00 - 002111.26 & - & sdss j100929.52 - 002113.79 & - + 508 & 10:09:31.08 & -00:20:01.43 & 17.702 & 15.971 & 15.121 & 14.704 & 14.346 & 18.029 & sdss j100930.48 - 002001.95 & 0.045726 & sdss j100931.68 - 002000.92 & - + 509 & 10:11:05.04 & + 00:15:56.95 & 19.836 & 18.109 & 17.213 & 16.765 & 16.425 & 4.241 & sdss j101105.04 + 001559.07 & 0.088160 & sdss j101105.04 + 001554.83 & - + 510 & 10:11:14.40 & + 00:26:51.86 & 18.720 & 16.608 & 15.617 & 15.233 & 14.926 & 11.772 & sdss j101114.16 + 002647.21 & 0.099242 & sdss j101114.64 + 002656.52 & - + 511 & 10:11:35.64 & + 00:44:55.18 & 20.607 & 19.959 & 19.229 & 18.790 & 18.510 & 4.145 & sdss j101135.76 + 004454.16 & - & sdss j101135.52 + 004456.21 & - + 512 & 10:11:59.88 & -00:11:25.36 & 17.633 & 16.488 & 16.037 & 15.936 & 15.941 & 4.048 & sdss j101159.76 - 001124.43 & - & sdss j101200.00 - 001126.28 & - + 513 & 10:12:27.72 & -00:52:11.44 & 19.015 & 18.259 & 17.703 & 17.396 & 17.254 & 4.255 & sdss j101227.84 - 005210.31 & - & sdss j101227.60 - 005212.57 & - + 514 & 10:12:39.36 & -00:34:00.23 & 17.870 & 16.786 & 16.353 & 15.851 & 15.670 & 3.694 & sdss j101239.36 - 003358.38 & - & sdss j101239.36 - 003402.07 & - + 515 & 10:12:56.76 & -00:28:00.17 & 17.399 & 16.054 & 15.281 & 14.878 & 14.588 & 13.419 & sdss j101256.64 - 002753.70 & - & sdss j101256.88 - 002806.63 & - + 516 & 10:13:20.52 & + 00:06:54.82 & 17.997 & 16.432 & 15.896 & 15.540 & 15.176 & 3.832 & sdss j101320.64 + 000655.47 & 0.096028 & sdss j101320.40 + 000654.16 & - + 517 & 10:13:24.84 & -00:55:26.09 & 19.060 & 17.461 & 16.695 & 16.371 & 16.109 & 4.750 & sdss j101324.96 - 005524.54 & - & sdss j101324.72 - 005527.64 & - + 518 & 10:13:25.56 & -00:54:33.76 & 18.187 & 16.392 & 15.487 & 15.071 & 14.728 & 4.904 & sdss j101325.68 - 005435.43 & 0.041736 & sdss j101325.44 - 005432.10 & - + 519 & 10:13:30.84 & -00:25:52.91 & 20.316 & 19.419 & 18.532 & 18.044 & 17.538 & 5.278 & sdss j101330.72 - 002554.84 & - & sdss j101330.96 - 002550.98 & - + 520 & 10:13:45.48 & -00:06:37.71 & 21.277 & 19.337 & 18.334 & 17.848 & 17.502 & 3.632 & sdss j101345.60 - 000637.47 & - & sdss j101345.36 - 000637.95 & - + 521 & 10:13:45.96 & -00:08:03.13 & 19.612 & 17.870 & 16.889 & 16.441 & 16.119 & 5.682 & sdss j101346.08 - 000800.93 & 0.096323 & sdss j101345.84 - 000805.33 & - + 522 & 10:13:48.48 & -00:06:16.97 & 19.779 & 17.886 & 16.930 & 16.494 & 16.136 & 3.524 & sdss j101348.48 - 000618.74 & 0.091566 & sdss j101348.48 - 000615.21 & - + 523 & 10:14:23.64 & -00:03:15.70 & 21.151 & 19.018 & 17.673 & 17.135 & 16.780 & 4.991 & sdss j101423.76 - 000313.97 & - & sdss j101423.52 - 000317.42 & - + 524 & 10:14:28.44 & + 00:39:53.85 & 19.438 & 17.558 & 16.546 & 16.086 & 15.710 & 10.849 & sdss j101428.80 + 003954.37 & 0.101599 & sdss j101428.08 + 003953.33 & - + 525 & 10:15:04.80 & -01:03:05.49 & 20.349 & 17.967 & 16.597 & 16.080 & 15.767 & 3.060 & sdss j101504.80 - 010303.96 & 0.201200 & sdss j101504.80 - 010307.02 & - + 526 & 10:15:14.04 & + 00:05:06.20 & 19.571 & 18.292 & 17.533 & 17.155 & 16.939 & 3.769 & sdss j101513.92 + 000505.64 & - & sdss j101514.16 + 000506.76 & - + 527 & 10:15:35.76 & -00:04:57.85 & 20.793 & 19.348 & 18.037 & 17.557 & 17.332 & 2.835 & sdss j101535.76 - 000459.26 & - & sdss j101535.76 - 000456.43 & - + 528 & 10:15:52.92 & + 00:05:12.67 & 18.359 & 16.348 & 15.261 & 14.757 & 14.305 & 15.162 & sdss j101552.56 + 000518.00 & - & sdss j101553.28 + 000507.35 & - + 529 & 10:16:21.48 & -00:58:19.07 & 18.716 & 17.744 & 17.493 & 17.241 & 17.286 & 5.365 & sdss j101621.60 - 005817.08 & - & sdss j101621.36 - 005821.06 & - + 530 & 10:16:36.72 & -00:59:33.10 & 20.320 & 18.063 & 16.861 & 16.320 & 15.989 & 2.092 & sdss j101636.72 - 005934.14 & - & sdss j101636.72 - 005932.05 & - + 531 & 10:16:40.68 & + 00:28:01.71 & 18.283 & 16.376 & 15.239 & 14.851 & 14.514 & 6.741 & sdss j101640.56 + 002804.56 & - & sdss j101640.80 + 002758.86 & - + 532 & 10:16:52.56 & -00:46:34.25 & 17.898 & 16.483 & 15.629 & 15.291 & 15.021 & 8.453 & sdss j101652.56 - 004630.02 & - & sdss j101652.56 - 004638.47 & - + 533 & 10:16:53.64 & + 00:04:37.65 & 17.827 & 16.368 & 15.519 & 15.046 & 14.712 & 10.347 & sdss j101653.52 + 000442.50 & - & sdss j101653.76 + 000432.80 & - + 534 & 10:17:19.32 & + 00:20:34.37 & 20.249 & 18.591 & 17.700 & 17.263 & 16.898 & 5.486 & sdss j101719.44 + 002032.30 & - & sdss j101719.20 + 002036.44 & - + 535 & 10:17:27.48 & + 00:11:35.04 & 19.837 & 18.854 & 18.331 & 18.066 & 17.764 & 4.374 & sdss j101727.36 + 001133.80 & - & sdss j101727.60 + 001136.29 & - + 536 & 10:17:28.92 & + 00:20:12.66 & 19.530 & 18.385 & 17.819 & 17.475 & 17.274 & 6.511 & sdss j101728.80 + 002015.37 & - & sdss j101729.04 + 002009.95 & - + 537 & 10:17:42.72 & -00:11:37.68 & 18.040 & 16.482 & 15.584 & 15.232 & 14.909 & 7.588 & sdss j101742.48 - 001136.48 & - & sdss j101742.96 - 001138.87 & - + 538 & 10:17:53.88 & + 00:19:20.85 & 18.709 & 16.797 & 15.798 & 15.347 & 15.138 & 3.607 & sdss j101754.00 + 001920.74 & - & sdss j101753.76 + 001920.96 & - + 539 & 10:18:02.04 & -00:25:28.06 & 18.370 & 16.615 & 15.651 & 15.247 & 14.936 & 3.652 & sdss j101802.16 - 002527.76 & - & sdss j101801.92 - 002528.37 & - + 540 & 10:18:51.96 & -00:59:02.58 & 18.496 & 16.344 & 15.339 & 14.834 & 14.456 & 15.199 & sdss j101852.32 - 005857.24 & - & sdss j101851.60 - 005907.93 & - + 541 & 10:19:16.20 & -00:09:18.59 & 21.708 & 19.478 & 18.226 & 17.779 & 17.515 & 3.685 & sdss j101916.08 - 000918.20 & - & sdss j101916.32 - 000918.99 & - + 542 & 10:19:16.20 & -00:37:13.38 & 20.662 & 19.066 & 17.989 & 17.561 & 17.311 & 4.841 & sdss j101916.32 - 003715.00 & - & sdss j101916.08 - 003711.76 & - + 543 & 10:19:16.80 & -00:54:09.27 & 20.099 & 18.908 & 18.415 & 18.061 & 17.831 & 4.212 & sdss j101916.80 - 005407.16 & - & sdss j101916.80 - 005411.37 & - + 544 & 10:20:21.96 & -00:57:40.53 & 19.191 & 18.009 & 17.335 & 16.981 & 16.678 & 5.618 & sdss j102022.08 - 005738.37 & - & sdss j102021.84 - 005742.69 & - + 545 & 10:21:24.24 & + 00:02:46.56 & 18.956 & 17.795 & 17.336 & 16.999 & 16.904 & 7.263 & sdss j102124.48 + 000246.08 & - & sdss j102124.00 + 000247.04 & - + 546 & 10:23:31.80 & + 00:10:25.47 & 17.917 & 15.956 & 14.991 & 14.523 & 14.167 & 10.800 & sdss j102332.16 + 001025.46 & 0.095567 & sdss j102331.44 + 001025.48 & - + 547 & 10:25:05.88 & + 00:20:54.62 & 19.272 & 18.727 & 18.565 & 18.203 & 18.490 & 4.924 & sdss j102505.76 + 002056.30 & - & sdss j102506.00 + 002052.94 & - + 548 & 10:25:25.44 & -00:35:53.10 & 19.504 & 17.674 & 16.784 & 16.376 & 16.030 & 7.754 & sdss j102525.44 - 003556.97 & 0.074631 & sdss j102525.44 - 003549.22 & - + 549 & 10:25:38.76 & -00:16:22.99 & 17.596 & 15.988 & 15.025 & 14.556 & 14.245 & 10.744 & sdss j102538.64 - 001617.93 & 0.104435 & sdss j102538.88 - 001628.05 & - + 550 & 10:26:53.64 & + 00:33:27.77 & 19.597 & 18.121 & 17.076 & 16.596 & 16.267 & 4.333 & sdss j102653.52 + 003328.98 & 0.173649 & sdss j102653.76 + 003326.57 & - + 551 & 10:27:19.08 & + 00:10:54.30 & 20.292 & 19.269 & 17.999 & 17.185 & 16.649 & 4.165 & sdss j102718.96 + 001055.34 & - & sdss j102719.20 + 001053.25 & - + 552 & 10:27:26.28 & + 00:44:37.31 & 20.153 & 18.145 & 17.037 & 16.571 & 16.148 & 5.560 & sdss j102726.16 + 004439.42 & 0.129482 & sdss j102726.40 + 004435.19 & - + 553 & 10:28:10.20 & -00:49:18.59 & 20.560 & 19.800 & 19.723 & 19.259 & 19.171 & 4.511 & sdss j102810.32 - 004919.95 & - & sdss j102810.08 - 004917.23 & - + 554 & 10:28:36.96 & + 00:42:09.41 & 20.251 & 19.303 & 18.890 & 18.606 & 18.665 & 1.321 & sdss j102836.96 + 004208.75 & - & sdss j102836.96 + 004210.08 & - + 555 & 10:28:42.96 & -00:08:39.72 & 17.887 & 16.845 & 16.473 & 16.271 & 16.061 & 7.255 & sdss j102842.72 - 000840.17 & 0.034560 & sdss j102843.20 - 000839.28 & - + 556 & 10:30:12.48 & -00:50:36.63 & 19.102 & 17.371 & 16.095 & 15.650 & 15.325 & 7.234 & sdss j103012.24 - 005036.99 & 0.115187 & sdss j103012.72 - 005036.28 & - + 557 & 10:30:23.28 & -00:04:12.77 & 19.032 & 18.069 & 17.806 & 17.466 & 17.505 & 3.222 & sdss j103023.28 - 000411.16 & - & sdss j103023.28 - 000414.38 & - + 558 & 10:31:21.00 & -00:36:41.76 & 18.417 & 16.959 & 16.342 & 15.833 & 15.498 & 13.141 & sdss j103120.64 - 003638.01 & - & sdss j103121.36 - 003645.50 & - + 559 & 10:33:33.12 & + 01:06:36.52 & 18.514 & 16.854 & 16.071 & 15.497 & 15.239 & 2.844 & sdss j103333.12 + 010635.10 & 0.065745 & sdss j103333.12 + 010637.94 & - + 560 & 10:33:52.80 & + 00:44:04.32 & 18.778 & 17.295 & 16.431 & 15.427 & 15.201 & 7.503 & sdss j103352.56 + 004403.26 & 0.131258 & sdss j103353.04 + 004405.38 & - + 561 & 10:33:53.16 & -01:02:45.92 & 20.748 & 18.720 & 17.543 & 17.017 & 16.754 & 3.635 & sdss j103353.04 - 010246.17 & - & sdss j103353.28 - 010245.67 & - + 562 & 10:34:22.08 & -00:24:31.68 & 20.629 & 18.523 & 17.235 & 16.711 & 16.214 & 9.198 & sdss j103422.08 - 002436.28 & 0.184654 & sdss j103422.08 - 002427.08 & - + 563 & 10:35:29.64 & -00:00:52.75 & 17.601 & 16.649 & 16.422 & 16.326 & 16.178 & 12.113 & sdss j103530.00 - 000050.01 & - & sdss j103529.28 - 000055.49 & - + 564 & 10:35:48.12 & + 00:35:03.49 & 19.188 & 17.322 & 16.306 & 15.847 & 15.480 & 12.226 & sdss j103547.76 + 003506.36 & 0.108682 & sdss j103548.48 + 003500.63 & 0.109264 + 565 & 10:36:10.08 & + 00:57:35.67 & 20.431 & 18.865 & 17.645 & 17.067 & 16.777 & 8.965 & sdss j103609.84 + 005738.34 & 0.311351 & sdss j103610.32 + 005733.00 & - + 566 & 10:37:01.68 & + 00:29:09.75 & 18.343 & 17.339 & 17.162 & 16.967 & 16.929 & 3.992 & sdss j103701.68 + 002907.76 & 0.049760 & sdss j103701.68 + 002911.75 & - + 567 & 10:37:29.88 & -00:40:43.48 & 18.653 & 16.460 & 15.417 & 14.939 & 14.510 & 6.777 & sdss j103729.76 - 004040.60 & 0.095479 & sdss j103730.00 - 004046.35 & - + 568 & 10:38:22.08 & -00:48:26.92 & 19.278 & 17.500 & 16.612 & 16.208 & 15.893 & 2.315 & sdss j103822.08 - 004828.08 & 0.124975 & sdss j103822.08 - 004825.76 & - + 569 & 10:38:45.84 & + 00:59:21.43 & 19.573 & 17.608 & 16.582 & 16.102 & 15.679 & 15.518 & sdss j103846.32 + 005924.33 & - & sdss j103845.36 + 005918.54 & 0.131386 + 570 & 10:39:20.52 & + 01:00:59.56 & 21.238 & 19.473 & 18.536 & 18.064 & 17.799 & 3.608 & sdss j103920.64 + 010059.68 & - & sdss j103920.40 + 010059.43 & - + 571 & 10:39:47.28 & + 00:41:08.28 & 19.797 & 18.324 & 17.673 & 17.262 & 16.908 & 7.203 & sdss j103947.04 + 004108.39 & - & sdss j103947.52 + 004108.16 & - + 572 & 10:40:10.80 & -00:33:29.73 & 20.172 & 18.688 & 17.969 & 17.585 & 17.318 & 1.343 & sdss j104010.80 - 003330.40 & - & sdss j104010.80 - 003329.05 & - + 573 & 10:40:27.48 & -00:01:13.67 & 20.158 & 18.298 & 17.217 & 16.640 & 16.269 & 3.605 & sdss j104027.60 - 000113.77 & 0.140191 & sdss j104027.36 - 000113.57 & - + 574 & 10:40:29.76 & -00:02:53.08 & 19.693 & 17.972 & 16.939 & 16.419 & 16.007 & 7.460 & sdss j104029.52 - 000252.10 & 0.132908 & sdss j104030.00 - 000254.06 & - + 575 & 10:40:40.32 & + 00:22:31.99 & 18.523 & 17.622 & 17.371 & 17.190 & 17.056 & 7.444 & sdss j104040.08 + 002231.04 & - & sdss j104040.56 + 002232.93 & - + 576 & 10:41:15.24 & -01:07:24.88 & 19.907 & 17.735 & 16.604 & 16.070 & 15.681 & 3.625 & sdss j104115.36 - 010725.10 & - & sdss j104115.12 - 010724.67 & 0.135113 + 577 & 10:41:32.16 & + 01:03:52.38 & 20.584 & 19.045 & 18.096 & 17.620 & 17.326 & 2.232 & sdss j104132.16 + 010351.26 & - & sdss j104132.16 + 010353.49 & - + 578 & 10:41:44.04 & -00:39:58.86 & 20.287 & 18.336 & 17.231 & 16.766 & 16.415 & 6.182 & sdss j104144.16 - 003956.35 & 0.135058 & sdss j104143.92 - 004001.38 & - + 579 & 10:41:48.48 & + 01:06:20.03 & 18.737 & 17.790 & 17.047 & 16.605 & 16.211 & 2.700 & sdss j104148.48 + 010621.38 & 0.214942 & sdss j104148.48 + 010618.68 & - + 580 & 10:41:51.84 & + 00:24:02.62 & 17.976 & 16.999 & 16.598 & 16.307 & 16.130 & 7.954 & sdss j104152.08 + 002404.31 & 0.065739 & sdss j104151.60 + 002400.93 & - + 581 & 10:42:11.76 & -01:00:58.35 & 18.878 & 17.520 & 16.519 & 16.077 & 16.043 & 7.341 & sdss j104212.00 - 010059.07 & 0.192361 & sdss j104211.52 - 010057.63 & - + 582 & 10:42:22.20 & -00:48:22.87 & 19.871 & 17.899 & 16.816 & 16.359 & 15.965 & 5.947 & sdss j104222.08 - 004820.50 & 0.136223 & sdss j104222.32 - 004825.23 & - + 583 & 10:42:37.92 & + 00:52:15.69 & 19.990 & 17.881 & 16.862 & 16.336 & 15.995 & 5.803 & sdss j104237.92 + 005212.79 & 0.123984 & sdss j104237.92 + 005218.59 & - + 584 & 10:42:42.24 & + 00:40:50.59 & 19.437 & 17.406 & 16.466 & 16.014 & 15.643 & 4.288 & sdss j104242.24 + 004052.73 & 0.094943 & sdss j104242.24 + 004048.45 & 0.094463 + 585 & 10:43:07.92 & -00:05:40.58 & 17.656 & 16.728 & 16.462 & 16.284 & 16.213 & 7.282 & sdss j104308.16 - 000541.12 & - & sdss j104307.68 - 000540.03 & 0.061507 + 586 & 10:43:15.24 & + 00:13:12.05 & 17.732 & 16.800 & 16.604 & 16.400 & 16.250 & 5.446 & sdss j104315.12 + 001314.09 & 0.047006 & sdss j104315.36 + 001310.00 & - + 587 & 10:43:18.84 & + 00:57:05.82 & 19.473 & 18.279 & 17.654 & 17.241 & 17.250 & 5.093 & sdss j104318.72 + 005707.62 & - & sdss j104318.96 + 005704.02 & - + 588 & 10:43:28.92 & -00:20:35.35 & 19.320 & 18.331 & 17.915 & 17.620 & 17.596 & 3.624 & sdss j104328.80 - 002035.14 & - & sdss j104329.04 - 002035.56 & - + 589 & 10:43:29.04 & + 01:02:24.61 & 19.216 & 17.349 & 16.424 & 16.047 & 15.729 & 5.328 & sdss j104329.04 + 010221.94 & 0.117105 & sdss j104329.04 + 010227.27 & - + 590 & 10:43:37.08 & + 00:23:23.94 & 20.175 & 18.375 & 17.442 & 16.980 & 16.601 & 4.135 & sdss j104336.96 + 002324.96 & - & sdss j104337.20 + 002322.92 & - + 591 & 10:43:48.96 & + 00:33:24.43 & 19.079 & 17.705 & 16.844 & 16.322 & 15.929 & 8.772 & sdss j104348.72 + 003326.93 & 0.080354 & sdss j104349.20 + 003321.92 & - + 592 & 10:43:49.56 & + 00:57:48.04 & 20.342 & 19.297 & 18.821 & 18.565 & 18.128 & 5.462 & sdss j104349.68 + 005750.09 & - & sdss j104349.44 + 005745.99 & - + 593 & 10:43:51.96 & + 01:03:44.87 & 18.906 & 16.465 & 15.453 & 15.032 & 14.592 & 6.640 & sdss j104351.84 + 010342.08 & 0.115857 & sdss j104352.08 + 010347.66 & - + 594 & 10:44:01.44 & + 01:08:05.69 & 20.797 & 18.938 & 17.946 & 17.546 & 17.122 & 3.852 & sdss j104401.44 + 010807.62 & - & sdss j104401.44 + 010803.76 & - + 595 & 10:44:29.64 & -00:38:54.04 & 20.308 & 18.349 & 17.194 & 16.623 & 16.192 & 9.201 & sdss j104429.76 - 003858.27 & 0.192824 & sdss j104429.52 - 003849.80 & - + 596 & 10:44:58.44 & + 00:56:09.37 & 19.343 & 18.552 & 18.023 & 17.539 & 17.395 & 3.626 & sdss j104458.32 + 005609.15 & 0.149759 & sdss j104458.56 + 005609.58 & - + 597 & 10:45:03.12 & + 00:32:21.48 & 16.741 & 15.508 & 14.695 & 14.367 & 14.106 & 10.447 & sdss j104503.12 + 003216.26 & 0.072682 & sdss j104503.12 + 003226.71 & - + 598 & 10:45:09.00 & + 00:04:30.64 & 18.202 & 16.796 & 16.020 & 15.624 & 15.283 & 6.444 & sdss j104509.12 + 000433.31 & 0.094270 & sdss j104508.88 + 000427.97 & - + 599 & 10:45:24.36 & -00:58:56.49 & 18.056 & 17.146 & 16.529 & 16.286 & 16.069 & 7.605 & sdss j104524.48 - 005859.84 & - & sdss j104524.24 - 005853.14 & - + 600 & 10:45:54.72 & + 01:04:06.99 & 16.995 & 16.281 & 16.463 & 16.634 & 16.520 & 2.520 & sdss j104554.72 + 010405.73 & 0.026250 & sdss j104554.72 + 010408.25 & - + 601 & 10:46:34.32 & -00:00:12.49 & 20.698 & 18.802 & 17.600 & 17.041 & 16.711 & 1.748 & sdss j104634.32 - 000011.62 & 0.177618 & sdss j104634.32 - 000013.37 & - + 602 & 10:46:51.48 & -00:40:18.14 & 19.988 & 18.848 & 18.160 & 17.751 & 17.689 & 3.617 & sdss j104651.36 - 004018.32 & - & sdss j104651.60 - 004017.96 & - + 603 & 10:47:52.68 & + 00:12:57.50 & 17.583 & 16.445 & 15.866 & 15.631 & 15.444 & 3.600 & sdss j104752.80 + 001257.53 & 0.091849 & sdss j104752.56 + 001257.47 & - + 604 & 10:49:26.04 & + 01:00:41.25 & 18.609 & 16.625 & 15.598 & 15.134 & 14.763 & 10.845 & sdss j104925.68 + 010040.75 & 0.106467 & sdss j104926.40 + 010041.76 & 0.106951 + 605 & 10:49:43.08 & -00:11:45.46 & 19.561 & 18.395 & 18.150 & 17.906 & 17.751 & 3.736 & sdss j104942.96 - 001145.96 & 0.073100 & sdss j104943.20 - 001144.97 & - + 606 & 10:50:06.72 & -00:31:43.22 & 17.820 & 16.596 & 16.012 & 15.695 & 15.463 & 6.653 & sdss j105006.72 - 003139.90 & 0.071824 & sdss j105006.72 - 003146.55 & 0.073043 + 607 & 10:50:20.76 & -00:52:23.81 & 18.922 & 16.867 & 15.829 & 15.385 & 15.062 & 5.400 & sdss j105020.64 - 005225.82 & 0.107379 & sdss j105020.88 - 005221.80 & 0.107790 + 608 & 10:51:33.24 & -00:04:35.39 & 19.289 & 18.355 & 18.019 & 17.783 & 17.663 & 4.130 & sdss j105133.36 - 000434.38 & 0.088700 & sdss j105133.12 - 000436.40 & - + 609 & 10:52:21.96 & -00:05:54.62 & 17.285 & 16.421 & 15.997 & 15.912 & 15.869 & 5.754 & sdss j105221.84 - 000552.38 & 0.050233 & sdss j105222.08 - 000556.86 & - + 610 & 10:53:09.00 & + 00:54:59.93 & 19.328 & 17.582 & 16.681 & 16.228 & 15.919 & 5.788 & sdss j105309.12 + 005457.67 & 0.097155 & sdss j105308.88 + 005502.20 & - + 611 & 10:53:32.76 & -00:57:32.73 & 18.625 & 16.985 & 15.925 & 15.387 & 14.963 & 13.265 & sdss j105333.12 - 005728.87 & - & sdss j105332.40 - 005736.58 & 0.126604 + 612 & 10:54:47.64 & + 00:57:39.35 & 19.914 & 18.610 & 18.106 & 17.690 & 17.526 & 6.234 & sdss j105447.76 + 005736.81 & - & sdss j105447.52 + 005741.90 & - + 613 & 10:55:03.24 & + 00:58:58.64 & 20.201 & 18.277 & 17.116 & 16.598 & 16.274 & 5.025 & sdss j105503.12 + 005856.88 & 0.170780 & sdss j105503.36 + 005900.39 & - + 614 & 10:55:52.44 & + 00:23:40.36 & 19.952 & 18.390 & 17.273 & 16.799 & 16.385 & 3.753 & sdss j105552.32 + 002339.82 & 0.190351 & sdss j105552.56 + 002340.89 & - + 615 & 10:56:55.56 & + 00:45:56.50 & 18.872 & 17.047 & 16.142 & 15.690 & 15.302 & 8.130 & sdss j105655.44 + 004600.15 & 0.092905 & sdss j105655.68 + 004552.86 & - + 616 & 10:56:59.16 & + 00:22:24.61 & 18.013 & 16.912 & 16.459 & 16.263 & 16.046 & 7.973 & sdss j105659.04 + 002228.16 & 0.078899 & sdss j105659.28 + 002221.05 & - + 617 & 10:57:11.16 & + 00:46:10.40 & 18.897 & 17.663 & 16.958 & 16.574 & 16.295 & 4.033 & sdss j105711.28 + 004611.31 & 0.147044 & sdss j105711.04 + 004609.49 & - + 618 & 10:57:30.60 & + 00:11:08.71 & 19.485 & 18.388 & 17.711 & 17.311 & 17.100 & 4.779 & sdss j105730.48 + 001110.28 & 0.166500 & sdss j105730.72 + 001107.14 & - + 619 & 10:59:13.80 & -00:46:26.88 & 20.480 & 18.592 & 17.878 & 17.379 & 17.045 & 3.600 & sdss j105913.92 - 004626.91 & - & sdss j105913.68 - 004626.85 & - + 620 & 10:59:28.44 & -01:01:38.87 & 18.516 & 17.088 & 15.937 & 15.515 & 15.165 & 10.801 & sdss j105928.80 - 010138.74 & 0.185731 & sdss j105928.08 - 010139.00 & - + 621 & 10:59:52.44 & + 00:34:13.97 & 18.798 & 16.959 & 15.960 & 15.492 & 15.138 & 5.114 & sdss j105952.56 + 003415.79 & - & sdss j105952.32 + 003412.15 & 0.101746 + 622 & 11:00:35.64 & -00:01:18.26 & 18.980 & 17.770 & 18.572 & 18.624 & 18.698 & 3.682 & sdss j110035.52 - 000117.87 & 0.185731 & sdss j110035.76 - 000118.64 & - + 623 & 11:02:13.80 & + 00:33:32.65 & 18.955 & 17.703 & 17.154 & 16.914 & 16.774 & 3.601 & sdss j110213.92 + 003332.69 & 0.051700 & sdss j110213.68 + 003332.62 & - + 624 & 11:02:17.16 & + 00:57:59.61 & 18.091 & 16.899 & 16.310 & 15.913 & 15.701 & 4.855 & sdss j110217.28 + 005757.98 & 0.102300 & sdss j110217.04 + 005801.24 & - + 625 & 11:02:33.12 & -00:12:52.65 & 18.940 & 17.352 & 16.471 & 16.029 & 15.842 & 7.832 & sdss j110232.88 - 001251.10 & 0.113218 & sdss j110233.36 - 001254.19 & - + 626 & 11:02:38.40 & -01:09:50.70 & 17.979 & 17.579 & 17.371 & 17.499 & 17.651 & 7.412 & sdss j110238.16 - 010949.82 & 0.010900 & sdss j110238.64 - 010951.58 & - + 627 & 11:04:24.96 & -00:49:16.76 & 17.888 & 16.652 & 16.065 & 15.816 & 15.666 & 4.003 & sdss j110424.96 - 004914.76 & 0.101101 & sdss j110424.96 - 004918.76 & - + 628 & 11:05:11.52 & + 00:40:20.40 & 17.951 & 17.152 & 16.995 & 16.904 & 16.756 & 7.200 & sdss j110511.28 + 004020.42 & - & sdss j110511.76 + 004020.39 & - + 629 & 11:05:15.12 & + 00:59:23.52 & 17.109 & 15.748 & 15.318 & 15.148 & 15.031 & 8.708 & sdss j110515.36 + 005925.97 & 0.334842 & sdss j110514.88 + 005921.07 & - + 630 & 11:05:27.72 & + 00:49:16.13 & 18.982 & 17.116 & 16.159 & 15.775 & 15.383 & 3.606 & sdss j110527.84 + 004916.23 & - & sdss j110527.60 + 004916.02 & - + 631 & 11:05:33.12 & + 00:14:20.00 & 18.965 & 17.729 & 17.054 & 16.847 & 16.563 & 21.959 & sdss j110532.40 + 001421.98 & - & sdss j110533.84 + 001418.03 & - + 632 & 11:05:50.04 & + 00:14:31.02 & 19.232 & 18.255 & 17.718 & 17.299 & 17.067 & 5.587 & sdss j110549.92 + 001428.88 & - & sdss j110550.16 + 001433.15 & - + 633 & 11:06:07.68 & -00:31:03.46 & 19.735 & 18.732 & 18.067 & 17.717 & 17.643 & 2.387 & sdss j110607.68 - 003102.26 & 0.203200 & sdss j110607.68 - 003104.65 & - + 634 & 11:06:30.72 & -00:57:50.65 & 19.691 & 18.516 & 18.015 & 17.652 & 17.460 & 7.212 & sdss j110630.48 - 005750.43 & - & sdss j110630.96 - 005750.86 & - + 635 & 11:06:38.52 & -00:45:26.44 & 19.292 & 17.344 & 16.224 & 15.707 & 15.274 & 8.360 & sdss j110638.64 - 004530.22 & - & sdss j110638.40 - 004522.67 & 0.111972 + 636 & 11:07:15.84 & + 00:45:49.22 & 21.751 & 19.903 & 18.878 & 18.351 & 17.877 & 2.394 & sdss j110715.84 + 004550.42 & - & sdss j110715.84 + 004548.03 & - + 637 & 11:07:32.28 & -00:12:21.99 & 20.076 & 18.631 & 17.644 & 17.127 & 16.788 & 5.922 & sdss j110732.16 - 001219.64 & - & sdss j110732.40 - 001224.34 & - + 638 & 11:07:38.16 & + 00:03:38.26 & 18.417 & 17.022 & 16.271 & 15.842 & 15.494 & 7.503 & sdss j110738.40 + 000337.20 & - & sdss j110737.92 + 000339.31 & - + 639 & 11:07:48.96 & + 00:55:24.01 & 17.374 & 16.556 & 16.403 & 16.137 & 16.079 & 10.000 & sdss j110749.20 + 005520.54 & 0.061297 & sdss j110748.72 + 005527.48 & - + 640 & 11:08:10.32 & + 00:42:46.99 & 19.644 & 18.111 & 16.922 & 16.332 & 16.011 & 3.226 & sdss j110810.32 + 004248.60 & 0.200025 & sdss j110810.32 + 004245.38 & - + 641 & 11:08:16.56 & + 00:50:15.84 & 18.919 & 17.654 & 17.203 & 17.037 & 16.939 & 7.274 & sdss j110816.80 + 005016.36 & - & sdss j110816.32 + 005015.32 & - + 642 & 11:08:45.24 & + 01:08:35.59 & 20.791 & 19.246 & 18.683 & 18.586 & 18.479 & 3.611 & sdss j110845.12 + 010835.73 & - & sdss j110845.36 + 010835.44 & - + 643 & 11:09:11.88 & -00:53:10.85 & 21.485 & 19.984 & 19.152 & 18.743 & 18.468 & 3.709 & sdss j110912.00 - 005311.29 & - & sdss j110911.76 - 005310.40 & - + 644 & 11:09:13.80 & + 00:20:04.66 & 20.253 & 18.738 & 18.252 & 17.907 & 17.593 & 5.560 & sdss j110913.68 + 002006.78 & - & sdss j110913.92 + 002002.54 & - + 645 & 11:09:30.36 & + 00:37:49.22 & 20.047 & 19.247 & 18.293 & 17.892 & 17.493 & 5.690 & sdss j110930.24 + 003751.43 & - & sdss j110930.48 + 003747.02 & - + 646 & 11:09:47.64 & -00:23:30.69 & 19.566 & 18.244 & 17.542 & 17.208 & 17.051 & 4.432 & sdss j110947.76 - 002329.40 & - & sdss j110947.52 - 002331.98 & - + 647 & 11:09:58.08 & + 00:10:58.60 & 17.224 & 16.175 & 15.779 & 15.502 & 15.289 & 18.552 & sdss j110958.56 + 001052.75 & 0.018970 & sdss j110957.60 + 001104.45 & - + 648 & 11:10:21.72 & -00:49:18.82 & 19.495 & 18.300 & 17.496 & 17.017 & 16.736 & 4.960 & sdss j111021.60 - 004917.11 & - & sdss j111021.84 - 004920.52 & - + 649 & 11:10:22.32 & + 00:42:34.74 & 19.458 & 17.626 & 16.655 & 16.217 & 15.859 & 5.170 & sdss j111022.32 + 004232.15 & 0.084365 & sdss j111022.32 + 004237.32 & - + 650 & 11:11:07.08 & + 00:42:45.65 & 20.840 & 18.863 & 17.772 & 17.312 & 16.959 & 3.924 & sdss j111107.20 + 004246.43 & - & sdss j111106.96 + 004244.87 & - + 651 & 11:11:07.32 & + 01:05:51.10 & 19.980 & 17.931 & 16.834 & 16.384 & 16.127 & 4.436 & sdss j111107.44 + 010549.81 & 0.096497 & sdss j111107.20 + 010552.40 & - + 652 & 11:11:16.44 & + 00:30:34.20 & 18.703 & 17.597 & 17.038 & 16.728 & 16.440 & 4.739 & sdss j111116.56 + 003035.74 & 0.111231 & sdss j111116.32 + 003032.66 & - + 653 & 11:11:24.00 & + 01:03:02.88 & 19.238 & 17.589 & 16.708 & 16.354 & 16.052 & 4.608 & sdss j111124.00 + 010305.18 & 0.124068 & sdss j111124.00 + 010300.57 & - + 654 & 11:11:55.20 & -00:42:00.73 & 19.935 & 19.335 & 18.929 & 18.766 & 18.695 & 2.221 & sdss j111155.20 - 004159.62 & - & sdss j111155.20 - 004201.84 & - + 655 & 11:12:52.44 & -00:11:28.84 & 19.476 & 17.455 & 16.397 & 15.939 & 15.510 & 5.996 & sdss j111252.56 - 001131.24 & 0.124068 & sdss j111252.32 - 001126.45 & - + 656 & 11:13:49.08 & -00:37:00.42 & 16.897 & 15.988 & 15.658 & 15.458 & 15.410 & 6.454 & sdss j111348.96 - 003703.10 & - & sdss j111349.20 - 003657.74 & - + 657 & 11:14:09.72 & -00:08:09.16 & 18.164 & 16.848 & 16.094 & 15.601 & 15.279 & 3.688 & sdss j111409.60 - 000809.56 & - & sdss j111409.84 - 000808.76 & - + 658 & 11:14:35.04 & -00:14:32.62 & 17.503 & 16.282 & 16.024 & 15.986 & 15.617 & 7.232 & sdss j111434.80 - 001432.96 & - & sdss j111435.28 - 001432.28 & - + 659 & 11:15:36.96 & + 01:06:05.61 & 19.954 & 18.952 & 18.173 & 17.762 & 17.460 & 3.888 & sdss j111536.96 + 010607.56 & - & sdss j111536.96 + 010603.67 & - + 660 & 11:15:39.00 & + 01:11:19.73 & 20.362 & 19.085 & 18.230 & 17.755 & 17.404 & 3.947 & sdss j111538.88 + 011120.54 & - & sdss j111539.12 + 011118.92 & - + 661 & 11:17:52.20 & -00:57:59.16 & 20.621 & 19.725 & 19.097 & 18.925 & 18.631 & 3.767 & sdss j111752.32 - 005759.72 & - & sdss j111752.08 - 005758.61 & - + 662 & 11:18:27.48 & -00:50:23.15 & 19.400 & 18.191 & 17.807 & 17.610 & 17.515 & 4.870 & sdss j111827.60 - 005021.51 & - & sdss j111827.36 - 005024.79 & - + 663 & 11:18:28.32 & -00:33:05.32 & 18.378 & 16.755 & 15.813 & 15.410 & 15.088 & 5.018 & sdss j111828.32 - 003302.81 & - & sdss j111828.32 - 003307.83 & - + 664 & 11:19:51.84 & + 00:04:16.19 & 19.111 & 16.995 & 15.998 & 15.521 & 15.181 & 4.822 & sdss j111951.84 + 000418.60 & - & sdss j111951.84 + 000413.78 & - + 665 & 11:20:13.68 & + 00:17:36.07 & 19.692 & 17.735 & 16.812 & 16.401 & 16.099 & 6.476 & sdss j112013.68 + 001739.31 & - & sdss j112013.68 + 001732.83 & - + 666 & 11:20:13.92 & + 00:32:16.55 & 19.886 & 18.344 & 17.424 & 16.997 & 16.599 & 5.119 & sdss j112013.92 + 003213.99 & - & sdss j112013.92 + 003219.11 & - + 667 & 11:21:21.36 & + 00:07:48.82 & 19.314 & 18.298 & 17.843 & 17.482 & 17.305 & 7.588 & sdss j112121.12 + 000747.63 & - & sdss j112121.60 + 000750.02 & - + 668 & 11:21:41.04 & + 00:57:15.24 & 19.324 & 17.720 & 16.772 & 16.339 & 15.972 & 8.931 & sdss j112140.80 + 005717.89 & - & sdss j112141.28 + 005712.60 & - + 669 & 11:21:45.48 & + 00:59:14.53 & 19.007 & 17.207 & 16.094 & 15.603 & 15.204 & 10.764 & sdss j112145.60 + 005919.61 & - & sdss j112145.36 + 005909.46 & - + 670 & 11:22:44.64 & + 00:27:40.29 & 18.260 & 16.206 & 15.229 & 14.789 & 14.437 & 10.492 & sdss j112244.88 + 002744.11 & 0.100528 & sdss j112244.40 + 002736.47 & - + 671 & 11:23:15.60 & -00:08:01.04 & 19.615 & 18.573 & 17.994 & 17.618 & 17.503 & 3.172 & sdss j112315.60 - 000759.45 & - & sdss j112315.60 - 000802.62 & - + 672 & 11:23:18.24 & + 00:57:56.31 & 18.990 & 18.110 & 17.774 & 17.533 & 17.274 & 6.566 & sdss j112318.24 + 005753.03 & - & sdss j112318.24 + 005759.60 & - + 673 & 11:24:40.68 & -00:49:20.81 & 19.973 & 18.838 & 18.290 & 17.891 & 17.743 & 3.603 & sdss j112440.56 - 004920.74 & - & sdss j112440.80 - 004920.88 & - + 674 & 11:25:00.96 & + 00:14:41.08 & 19.416 & 18.164 & 16.960 & 16.617 & 16.300 & 7.208 & sdss j112501.20 + 001440.90 & - & sdss j112500.72 + 001441.25 & - + 675 & 11:25:09.24 & + 00:51:24.31 & 19.552 & 17.189 & 16.602 & 16.358 & 16.059 & 5.810 & sdss j112509.36 + 005126.59 & - & sdss j112509.12 + 005122.03 & - + 676 & 11:25:12.72 & + 00:08:55.03 & 18.641 & 17.503 & 17.059 & 16.754 & 16.510 & 11.175 & sdss j112512.48 + 000859.30 & - & sdss j112512.96 + 000850.76 & - + 677 & 11:26:29.16 & + 00:59:00.73 & 18.625 & 17.622 & 17.249 & 16.852 & 16.839 & 4.840 & sdss j112629.04 + 005859.12 & 0.116429 & sdss j112629.28 + 005902.35 & - + 678 & 11:27:14.28 & + 00:09:02.04 & 20.866 & 18.948 & 17.983 & 17.572 & 17.046 & 4.151 & sdss j112714.16 + 000903.08 & - & sdss j112714.40 + 000901.01 & - + 679 & 11:27:59.40 & + 00:10:11.06 & 18.759 & 17.188 & 16.423 & 16.075 & 15.747 & 6.179 & sdss j112759.28 + 001008.55 & 0.049190 & sdss j112759.52 + 001013.57 & - + 680 & 11:28:24.60 & -00:39:11.22 & 20.147 & 18.434 & 17.405 & 16.962 & 16.584 & 3.659 & sdss j112824.72 - 003910.89 & 0.148800 & sdss j112824.48 - 003911.55 & - + 681 & 11:28:44.16 & -00:17:33.85 & 19.062 & 16.288 & 15.871 & 15.804 & 15.862 & 9.771 & sdss j112844.40 - 001730.55 & 0.049927 & sdss j112843.92 - 001737.15 & - + 682 & 11:29:45.72 & + 00:14:37.48 & 18.542 & 17.653 & 17.383 & 17.008 & 17.161 & 8.101 & sdss j112945.84 + 001433.86 & - & sdss j112945.60 + 001441.11 & - + 683 & 11:29:50.16 & + 00:12:03.50 & 18.382 & 16.565 & 15.671 & 15.228 & 14.903 & 6.570 & sdss j112950.16 + 001200.21 & 0.064724 & sdss j112950.16 + 001206.78 & - + 684 & 11:31:07.08 & + 00:26:20.06 & 18.637 & 17.839 & 18.032 & 17.529 & 17.882 & 4.419 & sdss j113107.20 + 002621.34 & 0.070700 & sdss j113106.96 + 002618.78 & - + 685 & 11:31:32.52 & -00:49:39.70 & 20.667 & 18.446 & 17.279 & 16.811 & 16.371 & 5.844 & sdss j113132.40 - 004937.39 & - & sdss j113132.64 - 004942.00 & - + 686 & 11:31:47.28 & + 00:55:54.11 & 18.581 & 16.854 & 16.062 & 15.589 & 15.267 & 4.795 & sdss j113147.28 + 005556.51 & 0.104175 & sdss j113147.28 + 005551.71 & 0.103597 + 687 & 11:33:14.04 & + 00:12:13.19 & 19.214 & 18.371 & 17.542 & 17.190 & 16.971 & 5.593 & sdss j113313.92 + 001215.33 & - & sdss j113314.16 + 001211.05 & - + 688 & 11:33:27.36 & -00:26:38.46 & 21.270 & 19.862 & 19.204 & 18.875 & 18.627 & 2.779 & sdss j113327.36 - 002637.07 & - & sdss j113327.36 - 002639.85 & - + 689 & 11:34:56.40 & -00:45:12.55 & 17.353 & 16.260 & 15.830 & 15.784 & 15.677 & 21.984 & sdss j113457.12 - 004514.60 & 0.019647 & sdss j113455.68 - 004510.50 & - + 690 & 11:35:57.00 & -00:16:17.71 & 16.540 & 15.676 & 15.393 & 15.054 & 14.960 & 15.870 & sdss j113557.36 - 001623.52 & - & sdss j113556.64 - 001611.89 & - + 691 & 11:36:30.48 & + 01:02:18.94 & 20.247 & 18.526 & 17.503 & 17.055 & 16.746 & 3.924 & sdss j113630.48 + 010220.90 & - & sdss j113630.48 + 010216.98 & - + 692 & 11:37:57.24 & + 00:24:24.96 & 19.866 & 18.742 & 18.099 & 17.764 & 17.614 & 3.625 & sdss j113757.12 + 002424.74 & - & sdss j113757.36 + 002425.17 & - + 693 & 11:40:14.04 & -00:52:14.21 & 19.432 & 18.620 & 18.353 & 18.106 & 18.183 & 4.524 & sdss j114014.16 - 005215.58 & 0.106400 & sdss j114013.92 - 005212.84 & - + 694 & 11:40:15.72 & -00:10:02.09 & 18.561 & 17.509 & 16.977 & 16.777 & 16.669 & 6.235 & sdss j114015.84 - 000959.55 & - & sdss j114015.60 - 001004.64 & - + 695 & 11:40:15.96 & + 01:08:50.24 & 19.405 & 17.942 & 17.274 & 16.916 & 16.648 & 6.853 & sdss j114015.84 + 010847.32 & 0.075654 & sdss j114016.08 + 010853.16 & - + 696 & 11:40:31.32 & + 01:05:57.06 & 20.294 & 18.726 & 17.663 & 17.162 & 16.877 & 4.293 & sdss j114031.44 + 010555.89 & - & sdss j114031.20 + 010558.23 & - + 697 & 11:41:08.04 & -00:27:23.61 & 19.798 & 18.364 & 17.207 & 16.762 & 16.389 & 4.449 & sdss j114108.16 - 002724.92 & - & sdss j114107.92 - 002722.30 & - + 698 & 11:41:11.64 & -01:04:48.66 & 19.372 & 17.786 & 16.644 & 16.253 & 15.982 & 4.771 & sdss j114111.52 - 010447.10 & - & sdss j114111.76 - 010450.23 & 0.091700 + 699 & 11:41:37.32 & -00:10:52.73 & 18.432 & 17.276 & 16.532 & 16.225 & 15.869 & 13.828 & sdss j114136.96 - 001057.05 & 0.191148 & sdss j114137.68 - 001048.42 & - + 700 & 11:41:49.68 & + 00:12:59.41 & 18.678 & 16.775 & 15.848 & 15.401 & 15.114 & 3.704 & sdss j114149.68 + 001257.56 & 0.092151 & sdss j114149.68 + 001301.26 & - + 701 & 11:42:16.56 & + 00:07:06.31 & 20.414 & 18.760 & 17.862 & 17.413 & 17.160 & 3.060 & sdss j114216.56 + 000707.84 & - & sdss j114216.56 + 000704.78 & - + 702 & 11:42:47.76 & + 00:24:30.44 & 18.902 & 17.705 & 17.120 & 16.806 & 16.630 & 7.517 & sdss j114247.52 + 002429.36 & 0.125013 & sdss j114248.00 + 002431.52 & - + 703 & 11:42:48.36 & -01:10:56.67 & 18.284 & 18.209 & 17.775 & 17.314 & 17.342 & 3.625 & sdss j114248.24 - 011056.46 & 0.222574 & sdss j114248.48 - 011056.89 & - + 704 & 11:42:50.64 & -01:11:03.76 & 20.778 & 19.267 & 18.386 & 17.937 & 17.722 & 2.880 & sdss j114250.64 - 011105.20 & - & sdss j114250.64 - 011102.32 & - + 705 & 11:43:09.12 & + 00:43:59.66 & 19.071 & 18.160 & 17.750 & 17.459 & 17.402 & 7.208 & sdss j114308.88 + 004359.48 & - & sdss j114309.36 + 004359.84 & - + 706 & 11:43:44.88 & -00:10:20.01 & 20.110 & 18.383 & 17.327 & 16.930 & 16.539 & 7.378 & sdss j114344.64 - 001020.82 & - & sdss j114345.12 - 001019.20 & - + 707 & 11:44:50.40 & + 01:01:33.76 & 18.510 & 17.285 & 16.834 & 16.622 & 16.518 & 9.021 & sdss j114450.64 + 010136.48 & - & sdss j114450.16 + 010131.04 & 0.090576 + 708 & 11:45:43.20 & -00:49:39.72 & 20.397 & 19.297 & 18.641 & 18.262 & 18.094 & 4.122 & sdss j114543.20 - 004937.66 & - & sdss j114543.20 - 004941.78 & - + 709 & 11:45:48.72 & -00:28:43.56 & 20.813 & 19.608 & 18.603 & 18.133 & 17.744 & 3.647 & sdss j114548.72 - 002841.73 & - & sdss j114548.72 - 002845.38 & - + 710 & 11:45:56.76 & -00:55:12.62 & 20.536 & 19.629 & 19.209 & 18.871 & 18.718 & 3.797 & sdss j114556.88 - 005512.01 & - & sdss j114556.64 - 005513.22 & - + 711 & 11:46:04.92 & -00:31:39.66 & 19.844 & 17.865 & 16.692 & 16.225 & 15.843 & 6.039 & sdss j114605.04 - 003137.23 & 0.156487 & sdss j114604.80 - 003142.08 & - + 712 & 11:46:24.36 & + 00:24:05.26 & 19.746 & 18.133 & 17.035 & 16.603 & 16.258 & 3.748 & sdss j114624.48 + 002404.74 & 0.122811 & sdss j114624.24 + 002405.78 & - + 713 & 11:47:59.64 & -01:06:28.58 & 18.343 & 16.396 & 15.459 & 14.975 & 14.661 & 15.332 & sdss j114759.52 - 010636.03 & 0.094973 & sdss j114759.76 - 010621.13 & - + 714 & 11:49:27.72 & -00:48:04.48 & 18.639 & 17.442 & 16.742 & 16.304 & 16.137 & 3.602 & sdss j114927.60 - 004804.41 & - & sdss j114927.84 - 004804.55 & - + 715 & 11:49:40.68 & + 00:07:32.60 & 20.520 & 18.759 & 17.716 & 17.259 & 16.927 & 3.635 & sdss j114940.56 + 000732.35 & - & sdss j114940.80 + 000732.85 & - + 716 & 11:49:42.48 & -00:39:36.92 & 19.178 & 17.716 & 16.779 & 16.348 & 16.090 & 4.910 & sdss j114942.48 - 003939.37 & - & sdss j114942.48 - 003934.46 & 0.121686 + 717 & 11:49:53.04 & + 01:09:58.26 & 18.479 & 17.594 & 17.181 & 16.906 & 16.759 & 8.460 & sdss j114953.04 + 010954.03 & 0.106315 & sdss j114953.04 + 011002.49 & - + 718 & 11:50:02.64 & -00:18:08.65 & 19.336 & 18.060 & 17.211 & 16.784 & 16.525 & 4.853 & sdss j115002.64 - 001811.08 & - & sdss j115002.64 - 001806.23 & - + 719 & 11:50:43.32 & -01:04:23.50 & 19.456 & 17.765 & 16.838 & 16.406 & 16.166 & 9.526 & sdss j115043.20 - 010419.09 & 0.166988 & sdss j115043.44 - 010427.91 & - + 720 & 11:50:52.68 & -00:05:58.79 & 20.611 & 19.018 & 17.698 & 17.216 & 16.820 & 7.342 & sdss j115052.80 - 000601.99 & - & sdss j115052.56 - 000555.59 & - + 721 & 11:51:14.88 & -00:54:54.53 & 18.695 & 17.031 & 16.138 & 15.683 & 15.325 & 8.626 & sdss j115114.64 - 005456.90 & 0.105016 & sdss j115115.12 - 005452.15 & - + 722 & 11:51:20.88 & + 01:04:20.19 & 18.445 & 17.023 & 16.219 & 15.756 & 15.398 & 10.891 & sdss j115121.12 + 010424.27 & 0.105743 & sdss j115120.64 + 010416.10 & - + 723 & 11:51:49.32 & -00:42:41.85 & 18.614 & 17.946 & 17.716 & 17.388 & 17.429 & 4.337 & sdss j115149.44 - 004240.64 & 0.108344 & sdss j115149.20 - 004243.05 & - + 724 & 11:51:54.36 & -01:09:43.00 & 19.283 & 18.773 & 18.271 & 17.953 & 17.849 & 4.587 & sdss j115154.48 - 010941.58 & 0.226455 & sdss j115154.24 - 010944.42 & - + 725 & 11:52:26.16 & + 00:17:46.78 & 19.660 & 17.764 & 16.725 & 16.254 & 15.854 & 6.761 & sdss j115226.16 + 001743.40 & 0.127837 & sdss j115226.16 + 001750.16 & - + 726 & 11:52:26.40 & -00:06:33.12 & 19.046 & 17.311 & 16.269 & 15.715 & 15.268 & 9.078 & sdss j115226.64 - 000630.35 & - & sdss j115226.16 - 000635.88 & 0.128328 + 727 & 11:52:32.16 & -00:03:47.86 & 20.192 & 18.410 & 17.447 & 16.999 & 16.663 & 3.706 & sdss j115232.16 - 000346.01 & 0.127516 & sdss j115232.16 - 000349.71 & 0.128328 + 728 & 11:53:18.00 & -00:39:46.52 & 20.117 & 18.730 & 18.113 & 17.829 & 17.571 & 3.312 & sdss j115318.00 - 003948.17 & - & sdss j115318.00 - 003944.86 & - + 729 & 11:53:46.20 & + 01:11:28.75 & 16.789 & 15.879 & 15.428 & 15.225 & 14.953 & 15.842 & sdss j115346.56 + 011134.54 & - & sdss j115345.84 + 011122.95 & - + 730 & 11:53:51.84 & -01:03:05.50 & 19.702 & 17.754 & 16.712 & 16.169 & 15.821 & 9.720 & sdss j115351.84 - 010300.64 & 0.169023 & sdss j115351.84 - 010310.36 & - + 731 & 11:54:09.96 & + 00:08:18.04 & 17.412 & 17.011 & 16.310 & 16.308 & 16.032 & 3.631 & sdss j115410.08 + 000818.28 & - & sdss j115409.84 + 000817.81 & - + 732 & 11:55:41.76 & -01:00:29.88 & 20.852 & 18.960 & 17.503 & 16.998 & 16.702 & 4.104 & sdss j115541.76 - 010027.82 & 0.226700 & sdss j115541.76 - 010031.93 & - + 733 & 11:56:14.52 & -00:11:52.45 & 20.377 & 18.369 & 17.339 & 16.852 & 16.454 & 3.633 & sdss j115614.64 - 001152.21 & - & sdss j115614.40 - 001152.70 & - + 734 & 11:57:15.96 & + 00:44:41.17 & 19.062 & 18.409 & 18.207 & 17.915 & 17.924 & 3.680 & sdss j115716.08 + 004440.79 & - & sdss j115715.84 + 004441.55 & - + 735 & 11:57:37.68 & -00:55:27.67 & 19.399 & 18.582 & 18.308 & 18.141 & 18.312 & 3.308 & sdss j115737.68 - 005526.02 & - & sdss j115737.68 - 005529.33 & - + 736 & 11:57:40.68 & + 01:04:17.90 & 20.001 & 18.488 & 17.472 & 17.005 & 16.600 & 4.057 & sdss j115740.56 + 010416.96 & - & sdss j115740.80 + 010418.84 & - + 737 & 11:58:04.92 & + 01:07:49.62 & 19.736 & 18.608 & 17.711 & 17.339 & 17.115 & 3.779 & sdss j115805.04 + 010749.04 & - & sdss j115804.80 + 010750.19 & - + 738 & 11:58:15.48 & + 00:18:31.22 & 20.055 & 18.747 & 17.923 & 17.468 & 17.304 & 4.208 & sdss j115815.36 + 001830.13 & - & sdss j115815.60 + 001832.31 & - + 739 & 11:58:25.20 & + 00:16:25.42 & 19.825 & 18.827 & 18.298 & 17.948 & 17.738 & 5.893 & sdss j115825.20 + 001622.48 & - & sdss j115825.20 + 001628.37 & - + 740 & 11:58:27.24 & -00:39:34.75 & 18.518 & 16.983 & 16.112 & 15.653 & 15.376 & 11.260 & sdss j115827.60 - 003936.34 & 0.124834 & sdss j115826.88 - 003933.15 & - + 741 & 11:58:41.76 & -00:12:49.43 & 17.382 & 15.993 & 15.295 & 14.916 & 14.668 & 7.952 & sdss j115842.00 - 001251.12 & 0.094750 & sdss j115841.52 - 001247.75 & - + 742 & 11:59:15.12 & -00:03:23.14 & 21.385 & 19.294 & 17.928 & 17.379 & 16.939 & 2.807 & sdss j115915.12 - 000321.74 & - & sdss j115915.12 - 000324.54 & - + 743 & 11:59:19.92 & -00:12:00.27 & 20.981 & 19.528 & 18.554 & 18.085 & 17.685 & 3.694 & sdss j115919.92 - 001202.12 & - & sdss j115919.92 - 001158.43 & - + 744 & 11:59:21.12 & -00:09:23.29 & 19.847 & 18.998 & 18.238 & 18.019 & 17.801 & 2.902 & sdss j115921.12 - 000924.75 & - & sdss j115921.12 - 000921.84 & - + 745 & 11:59:35.52 & + 00:11:11.25 & 19.660 & 17.839 & 16.862 & 16.421 & 16.153 & 6.318 & sdss j115935.52 + 001108.09 & 0.178555 & sdss j115935.52 + 001114.40 & - + 746 & 12:00:02.76 & -00:46:21.30 & 18.568 & 17.214 & 16.558 & 16.212 & 16.075 & 6.418 & sdss j120002.64 - 004618.65 & - & sdss j120002.88 - 004623.96 & - + 747 & 12:00:16.80 & -00:28:40.76 & 20.612 & 18.820 & 17.762 & 17.312 & 16.968 & 2.286 & sdss j120016.80 - 002839.62 & - & sdss j120016.80 - 002841.90 & 0.153500 + 748 & 12:00:50.04 & + 00:27:24.18 & 18.960 & 17.518 & 16.662 & 16.240 & 16.043 & 10.839 & sdss j120049.68 + 002724.64 & 0.124598 & sdss j120050.40 + 002723.72 & 0.227958 + 749 & 12:00:52.80 & -00:55:14.75 & 19.758 & 17.827 & 16.740 & 16.256 & 15.998 & 8.480 & sdss j120053.04 - 005517.00 & 0.108832 & sdss j120052.56 - 005512.51 & 0.108600 + 750 & 12:01:04.68 & -00:47:14.40 & 19.496 & 17.476 & 17.089 & 16.151 & 15.694 & 4.226 & sdss j120104.80 - 004715.51 & - & sdss j120104.56 - 004713.29 & 0.140827 + 751 & 12:01:25.08 & + 00:48:33.90 & 17.730 & 16.053 & 15.457 & 15.277 & 15.151 & 3.600 & sdss j120124.96 + 004833.88 & - & sdss j120125.20 + 004833.92 & - + 752 & 12:01:46.32 & -00:12:18.54 & 19.738 & 17.852 & 16.783 & 16.368 & 16.085 & 7.980 & sdss j120146.56 - 001220.26 & - & sdss j120146.08 - 001216.82 & - + 753 & 12:02:02.52 & -00:25:37.94 & 20.795 & 19.437 & 18.666 & 18.355 & 17.921 & 5.272 & sdss j120202.64 - 002536.01 & - & sdss j120202.40 - 002539.87 & - + 754 & 12:02:06.60 & -00:05:58.22 & 19.530 & 18.407 & 17.537 & 17.108 & 16.757 & 6.852 & sdss j120206.48 - 000555.31 & - & sdss j120206.72 - 000601.14 & - + 755 & 12:02:34.56 & -00:08:05.13 & 19.074 & 18.028 & 17.562 & 17.151 & 17.074 & 2.243 & sdss j120234.56 - 000806.25 & 0.130000 & sdss j120234.56 - 000804.01 & - + 756 & 12:02:41.52 & + 00:41:55.85 & 19.601 & 18.667 & 17.860 & 17.514 & 17.227 & 7.296 & sdss j120241.76 + 004156.44 & - & sdss j120241.28 + 004155.26 & - + 757 & 12:02:57.96 & + 00:08:28.19 & 18.004 & 16.530 & 15.686 & 15.434 & 15.177 & 3.719 & sdss j120258.08 + 000828.65 & 0.078826 & sdss j120257.84 + 000827.72 & - + 758 & 12:03:07.68 & + 00:41:13.36 & 18.154 & 17.136 & 16.749 & 16.581 & 16.548 & 1.962 & sdss j120307.68 + 004112.38 & - & sdss j120307.68 + 004114.34 & 0.102666 + 759 & 12:03:49.44 & + 01:03:26.91 & 19.593 & 18.116 & 17.241 & 16.821 & 16.458 & 5.868 & sdss j120349.44 + 010329.84 & - & sdss j120349.44 + 010323.97 & - + 760 & 12:03:51.12 & + 01:10:25.35 & 19.977 & 18.354 & 17.560 & 17.160 & 16.809 & 2.304 & sdss j120351.12 + 011026.50 & - & sdss j120351.12 + 011024.20 & - + 761 & 12:03:52.44 & + 00:31:47.11 & 18.648 & 17.211 & 16.498 & 16.148 & 15.879 & 3.632 & sdss j120352.32 + 003147.35 & - & sdss j120352.56 + 003146.86 & 0.102666 + 762 & 12:03:56.64 & + 00:19:58.66 & 18.935 & 17.135 & 16.170 & 15.682 & 15.323 & 15.942 & sdss j120357.12 + 001955.24 & 0.081623 & sdss j120356.16 + 002002.08 & - + 763 & 12:04:26.76 & -00:07:28.32 & 20.499 & 18.563 & 17.566 & 17.125 & 16.809 & 3.712 & sdss j120426.64 - 000728.77 & - & sdss j120426.88 - 000727.87 & 0.118300 + 764 & 12:05:19.68 & + 00:16:07.50 & 19.960 & 17.994 & 16.824 & 16.347 & 15.962 & 7.211 & sdss j120519.44 + 001607.30 & 0.159304 & sdss j120519.92 + 001607.70 & - + 765 & 12:05:50.16 & + 01:03:19.40 & 18.742 & 17.436 & 16.983 & 16.616 & 16.459 & 3.312 & sdss j120550.16 + 010317.74 & 0.077126 & sdss j120550.16 + 010321.06 & - + 766 & 12:06:05.88 & + 00:27:53.60 & 18.514 & 16.500 & 15.477 & 15.105 & 14.791 & 8.218 & sdss j120606.00 + 002749.91 & 0.060736 & sdss j120605.76 + 002757.29 & - + 767 & 12:06:09.48 & + 00:55:27.49 & 19.708 & 18.251 & 17.372 & 16.873 & 16.582 & 7.234 & sdss j120609.60 + 005524.35 & - & sdss j120609.36 + 005530.63 & - + 768 & 12:07:01.08 & + 00:22:22.39 & 19.859 & 18.358 & 17.226 & 16.773 & 16.396 & 4.718 & sdss j120701.20 + 002220.87 & 0.160380 & sdss j120700.96 + 002223.92 & - + 769 & 12:07:15.60 & -00:23:07.56 & 19.633 & 18.188 & 17.454 & 17.016 & 16.670 & 7.460 & sdss j120715.36 - 002308.53 & 0.113190 & sdss j120715.84 - 002306.58 & - + 770 & 12:07:22.32 & + 01:08:14.22 & 19.417 & 17.503 & 16.428 & 15.952 & 15.658 & 3.852 & sdss j120722.32 + 010816.15 & 0.121184 & sdss j120722.32 + 010812.30 & - + 771 & 12:07:53.40 & -01:04:17.31 & 20.222 & 18.566 & 18.034 & 17.684 & 17.392 & 6.106 & sdss j120753.28 - 010419.77 & - & sdss j120753.52 - 010414.84 & - + 772 & 12:07:55.08 & -01:00:04.98 & 19.413 & 17.522 & 16.553 & 16.145 & 15.816 & 5.933 & sdss j120754.96 - 010002.62 & 0.111589 & sdss j120755.20 - 010007.34 & - + 773 & 12:08:24.72 & + 00:05:27.80 & 17.216 & 16.095 & 15.340 & 15.151 & 15.252 & 10.393 & sdss j120824.96 + 000531.54 & 0.100744 & sdss j120824.48 + 000524.05 & - + 774 & 12:08:54.12 & + 00:40:19.06 & 19.270 & 18.309 & 17.982 & 17.756 & 17.631 & 3.810 & sdss j120854.24 + 004018.44 & - & sdss j120854.00 + 004019.68 & - + 775 & 12:08:58.44 & -00:36:09.87 & 19.184 & 17.551 & 16.721 & 16.259 & 15.878 & 3.610 & sdss j120858.32 - 003609.74 & 0.100110 & sdss j120858.56 - 003610.00 & - + 776 & 12:09:29.16 & -00:10:54.04 & 20.003 & 18.961 & 18.491 & 18.295 & 18.168 & 3.628 & sdss j120929.04 - 001053.82 & - & sdss j120929.28 - 001054.27 & - + 777 & 12:09:41.40 & + 01:10:21.45 & 18.116 & 16.136 & 15.206 & 14.692 & 14.283 & 18.063 & sdss j120940.80 + 011022.22 & 0.077605 & sdss j120942.00 + 011020.67 & - + 778 & 12:09:49.56 & + 00:11:17.61 & 20.361 & 18.844 & 18.038 & 17.639 & 17.352 & 6.126 & sdss j120949.68 + 001115.13 & - & sdss j120949.44 + 001120.09 & - + 779 & 12:10:06.00 & + 00:26:38.05 & 19.361 & 17.354 & 16.365 & 15.779 & 15.452 & 4.514 & sdss j121006.00 + 002640.31 & 0.127886 & sdss j121006.00 + 002635.79 & - + 780 & 12:10:06.84 & -00:02:44.47 & 18.362 & 17.212 & 16.584 & 16.379 & 16.166 & 3.968 & sdss j121006.72 - 000245.30 & - & sdss j121006.96 - 000243.63 & 0.116151 + 781 & 12:11:08.76 & -00:43:09.39 & 18.336 & 16.806 & 15.908 & 15.467 & 15.125 & 7.564 & sdss j121108.88 - 004306.07 & 0.079022 & sdss j121108.64 - 004312.72 & - + 782 & 12:11:21.24 & + 01:03:52.97 & 17.173 & 15.967 & 15.692 & 15.347 & 15.179 & 8.798 & sdss j121121.12 + 010356.98 & - & sdss j121121.36 + 010348.96 & 0.047019 + 783 & 12:11:29.16 & + 00:25:41.13 & 19.443 & 18.545 & 18.114 & 17.760 & 17.581 & 5.859 & sdss j121129.04 + 002543.44 & 0.127525 & sdss j121129.28 + 002538.82 & - + 784 & 12:11:51.96 & + 00:57:37.84 & 19.817 & 18.833 & 18.176 & 17.855 & 17.755 & 4.122 & sdss j121151.84 + 005736.84 & - & sdss j121152.08 + 005738.85 & - + 785 & 12:12:00.72 & -00:46:06.60 & 19.719 & 17.659 & 16.922 & 16.300 & 16.018 & 6.952 & sdss j121200.72 - 004610.08 & 0.127525 & sdss j121200.72 - 004603.12 & - + 786 & 12:12:12.60 & + 00:13:01.83 & 20.035 & 18.941 & 18.621 & 18.369 & 18.424 & 3.602 & sdss j121212.72 + 001301.77 & - & sdss j121212.48 + 001301.89 & - + 787 & 12:12:44.40 & -00:22:04.94 & 17.736 & 16.220 & 15.348 & 14.870 & 14.578 & 8.050 & sdss j121244.64 - 002203.14 & 0.073947 & sdss j121244.16 - 002206.74 & - + 788 & 12:13:41.04 & -00:34:50.61 & 18.932 & 18.782 & 18.324 & 18.072 & 17.657 & 3.434 & sdss j121341.04 - 003448.89 & 0.253264 & sdss j121341.04 - 003452.32 & - + 789 & 12:13:41.04 & -00:53:05.06 & 19.653 & 18.024 & 16.807 & 16.343 & 16.015 & 7.713 & sdss j121341.28 - 005303.68 & - & sdss j121340.80 - 005306.45 & - + 790 & 12:13:45.36 & -00:50:08.65 & 18.115 & 16.953 & 16.459 & 16.115 & 16.056 & 8.323 & sdss j121345.36 - 005004.49 & 0.050793 & sdss j121345.36 - 005012.81 & - + 791 & 12:13:54.48 & -01:05:12.76 & 18.650 & 17.189 & 16.395 & 16.005 & 15.720 & 17.925 & sdss j121354.72 - 010504.56 & 0.100031 & sdss j121354.24 - 010520.97 & - + 792 & 12:14:03.48 & -01:00:31.89 & 21.838 & 19.366 & 18.155 & 17.643 & 17.322 & 5.298 & sdss j121403.36 - 010033.84 & - & sdss j121403.60 - 010029.95 & - + 793 & 12:14:45.12 & -00:07:46.18 & 20.438 & 19.302 & 18.233 & 17.741 & 17.412 & 4.187 & sdss j121445.12 - 000748.27 & - & sdss j121445.12 - 000744.08 & - + 794 & 12:14:58.08 & -00:29:52.16 & 18.254 & 17.264 & 16.771 & 16.555 & 16.402 & 7.206 & sdss j121457.84 - 002952.31 & - & sdss j121458.32 - 002952.01 & - + 795 & 12:15:18.60 & + 00:20:47.95 & 20.787 & 18.692 & 17.359 & 16.800 & 16.558 & 4.173 & sdss j121518.72 + 002046.89 & - & sdss j121518.48 + 002049.00 & - + 796 & 12:15:30.36 & -01:12:12.52 & 19.889 & 18.804 & 18.179 & 17.877 & 17.732 & 4.610 & sdss j121530.24 - 011211.08 & - & sdss j121530.48 - 011213.96 & - + 797 & 12:15:33.12 & + 00:41:45.20 & 19.377 & 18.238 & 17.408 & 16.947 & 16.660 & 7.354 & sdss j121533.36 + 004144.45 & 0.184714 & sdss j121532.88 + 004145.95 & - + 798 & 12:15:47.64 & + 01:09:14.07 & 21.216 & 19.497 & 18.099 & 17.580 & 17.295 & 3.738 & sdss j121547.52 + 010913.57 & - & sdss j121547.76 + 010914.58 & - + 799 & 12:15:54.84 & -00:57:05.90 & 19.213 & 17.935 & 17.159 & 16.747 & 16.404 & 7.542 & sdss j121554.72 - 005702.58 & - & sdss j121554.96 - 005709.21 & - + 800 & 12:16:30.96 & + 00:44:34.32 & 18.702 & 17.627 & 16.966 & 16.545 & 16.221 & 5.065 & sdss j121630.96 + 004431.79 & 0.120768 & sdss j121630.96 + 004436.85 & - + 801 & 12:16:37.32 & -00:02:54.19 & 18.680 & 18.022 & 17.840 & 17.506 & 17.961 & 4.741 & sdss j121637.44 - 000255.74 & - & sdss j121637.20 - 000252.65 & - + 802 & 12:16:58.56 & -00:13:22.60 & 19.112 & 17.292 & 16.372 & 16.030 & 15.696 & 7.762 & sdss j121658.56 - 001318.72 & 0.071795 & sdss j121658.56 - 001326.48 & 0.071118 + 803 & 12:17:02.40 & -00:30:52.16 & 20.485 & 19.261 & 18.433 & 18.042 & 17.877 & 2.624 & sdss j121702.40 - 003050.85 & - & sdss j121702.40 - 003053.47 & - + 804 & 12:17:35.52 & + 00:41:46.13 & 20.710 & 19.443 & 18.125 & 17.534 & 17.144 & 2.549 & sdss j121735.52 + 004144.85 & - & sdss j121735.52 + 004147.40 & - + 805 & 12:17:41.40 & + 00:41:22.23 & 19.465 & 18.268 & 17.673 & 17.389 & 17.109 & 6.580 & sdss j121741.52 + 004124.98 & - & sdss j121741.28 + 004119.47 & - + 806 & 12:17:51.96 & -00:54:22.46 & 17.469 & 16.175 & 15.533 & 15.209 & 14.954 & 9.287 & sdss j121752.08 - 005426.74 & 0.021131 & sdss j121751.84 - 005418.18 & - + 807 & 12:18:17.88 & + 01:07:40.87 & 20.373 & 19.538 & 18.515 & 18.094 & 17.774 & 3.600 & sdss j121817.76 + 010740.83 & - & sdss j121818.00 + 010740.90 & - + 808 & 12:18:18.84 & -00:49:54.33 & 20.530 & 18.998 & 17.835 & 17.389 & 16.996 & 5.101 & sdss j121818.72 - 004956.13 & - & sdss j121818.96 - 004952.52 & - + 809 & 12:18:23.40 & + 01:08:28.01 & 20.514 & 19.650 & 19.045 & 18.681 & 18.534 & 3.614 & sdss j121823.28 + 010828.17 & - & sdss j121823.52 + 010827.85 & - + 810 & 12:18:26.88 & + 01:06:16.12 & 20.595 & 19.408 & 18.511 & 18.106 & 17.850 & 3.600 & sdss j121826.88 + 010614.32 & - & sdss j121826.88 + 010617.92 & - + 811 & 12:18:36.84 & -01:02:18.92 & 20.535 & 18.589 & 17.516 & 17.029 & 16.657 & 7.162 & sdss j121836.72 - 010215.82 & - & sdss j121836.96 - 010222.02 & - + 812 & 12:18:42.60 & + 00:42:13.58 & 19.312 & 17.955 & 16.830 & 16.386 & 16.015 & 5.552 & sdss j121842.48 + 004211.47 & 0.175847 & sdss j121842.72 + 004215.69 & - + 813 & 12:18:49.80 & -01:02:51.46 & 18.132 & 16.299 & 15.259 & 14.845 & 14.497 & 5.961 & sdss j121849.68 - 010249.09 & - & sdss j121849.92 - 010253.84 & 0.115697 + 814 & 12:18:58.80 & -00:02:34.91 & 19.956 & 17.819 & 16.552 & 16.037 & 15.692 & 9.502 & sdss j121858.56 - 000231.81 & 0.185560 & sdss j121859.04 - 000238.01 & - + 815 & 12:19:06.60 & -01:00:43.63 & 20.303 & 19.146 & 18.180 & 17.708 & 17.471 & 3.738 & sdss j121906.48 - 010044.13 & - & sdss j121906.72 - 010043.12 & - + 816 & 12:19:06.84 & + 00:05:33.41 & 20.845 & 19.849 & 19.160 & 18.856 & 18.466 & 3.636 & sdss j121906.72 + 000533.16 & - & sdss j121906.96 + 000533.67 & - + 817 & 12:19:44.64 & + 00:21:18.75 & 20.326 & 18.429 & 17.273 & 16.770 & 16.439 & 7.406 & sdss j121944.88 + 002119.62 & 0.173100 & sdss j121944.40 + 002117.89 & - + 818 & 12:19:48.36 & + 00:43:56.94 & 17.240 & 16.082 & 15.533 & 15.471 & 15.348 & 5.448 & sdss j121948.24 + 004358.99 & 0.041788 & sdss j121948.48 + 004354.90 & - + 819 & 12:20:30.24 & -00:26:59.52 & 17.568 & 16.975 & 16.914 & 17.164 & 17.262 & 6.098 & sdss j122030.24 - 002702.57 & - & sdss j122030.24 - 002656.47 & - + 820 & 12:21:19.32 & -00:36:03.15 & 21.014 & 19.597 & 18.667 & 18.268 & 17.898 & 3.749 & sdss j122119.44 - 003602.62 & - & sdss j122119.20 - 003603.67 & - + 821 & 12:21:21.24 & + 00:37:16.24 & 18.198 & 16.558 & 15.731 & 15.271 & 14.939 & 8.608 & sdss j122121.36 + 003712.33 & 0.078595 & sdss j122121.12 + 003720.15 & - + 822 & 12:21:23.64 & + 01:01:51.74 & 20.952 & 19.109 & 17.837 & 17.329 & 17.022 & 5.459 & sdss j122123.52 + 010149.69 & - & sdss j122123.76 + 010153.79 & - + 823 & 12:21:32.52 & + 00:12:56.69 & 19.505 & 17.160 & 15.970 & 15.480 & 15.065 & 4.855 & sdss j122132.64 + 001255.06 & 0.169255 & sdss j122132.40 + 001258.32 & 0.173081 + 824 & 12:21:47.16 & -00:53:48.47 & 18.532 & 17.686 & 17.532 & 17.534 & 17.442 & 7.047 & sdss j122147.04 - 005351.50 & - & sdss j122147.28 - 005345.44 & - + 825 & 12:21:48.72 & + 00:21:52.80 & 19.594 & 17.818 & 16.497 & 16.066 & 15.673 & 7.303 & sdss j122148.96 + 002152.19 & 0.156411 & sdss j122148.48 + 002153.41 & - + 826 & 12:22:22.20 & -00:43:41.75 & 20.493 & 19.483 & 18.587 & 18.330 & 17.989 & 3.606 & sdss j122222.32 - 004341.64 & - & sdss j122222.08 - 004341.86 & - + 827 & 12:22:39.24 & -00:58:49.85 & 18.810 & 17.018 & 15.786 & 15.338 & 15.184 & 4.517 & sdss j122239.12 - 005848.48 & 0.175300 & sdss j122239.36 - 005851.21 & 0.175300 + 828 & 12:22:46.92 & -01:02:41.13 & 19.890 & 19.133 & 18.333 & 17.987 & 17.634 & 3.702 & sdss j122246.80 - 010240.70 & - & sdss j122247.04 - 010241.56 & - + 829 & 12:22:53.16 & -00:53:58.50 & 19.961 & 18.732 & 18.051 & 17.705 & 17.389 & 4.909 & sdss j122253.04 - 005400.17 & 0.157700 & sdss j122253.28 - 005356.83 & - + 830 & 12:23:00.60 & -00:51:17.87 & 20.857 & 19.950 & 19.448 & 19.359 & 18.944 & 5.808 & sdss j122300.48 - 005115.59 & - & sdss j122300.72 - 005120.15 & - + 831 & 12:23:19.20 & + 01:03:54.79 & 18.113 & 16.410 & 15.619 & 15.220 & 14.900 & 7.701 & sdss j122318.96 + 010356.16 & 0.089106 & sdss j122319.44 + 010353.42 & - + 832 & 12:23:24.36 & -00:22:18.84 & 19.411 & 18.020 & 16.985 & 16.585 & 16.334 & 6.650 & sdss j122324.24 - 002216.05 & 0.125717 & sdss j122324.48 - 002221.64 & - + 833 & 12:23:37.80 & + 00:20:06.76 & 18.497 & 17.271 & 16.482 & 16.023 & 15.711 & 5.443 & sdss j122337.68 + 002004.72 & 0.159076 & sdss j122337.92 + 002008.80 & - + 834 & 12:23:58.92 & + 00:56:22.81 & 19.963 & 18.395 & 17.445 & 16.937 & 16.715 & 3.623 & sdss j122359.04 + 005623.02 & - & sdss j122358.80 + 005622.60 & - + 835 & 12:24:33.96 & -00:03:05.76 & 19.132 & 18.068 & 17.595 & 17.252 & 17.070 & 8.544 & sdss j122433.84 - 000301.89 & - & sdss j122434.08 - 000309.64 & - + 836 & 12:25:14.76 & + 00:15:48.73 & 18.707 & 17.567 & 16.569 & 16.373 & 16.007 & 3.658 & sdss j122514.64 + 001548.40 & - & sdss j122514.88 + 001549.05 & - + 837 & 12:26:07.08 & -00:11:19.68 & 20.885 & 19.613 & 18.796 & 18.466 & 18.132 & 4.147 & sdss j122606.96 - 001120.70 & - & sdss j122607.20 - 001118.65 & - + 838 & 12:26:55.68 & -00:38:00.00 & 22.047 & 19.539 & 18.314 & 17.903 & 17.600 & 5.281 & sdss j122655.68 - 003757.36 & - & sdss j122655.68 - 003802.64 & - + 839 & 12:27:04.56 & -00:54:23.22 & 16.628 & 15.752 & 15.668 & 15.513 & 15.811 & 5.094 & sdss j122704.56 - 005420.67 & 0.007354 & sdss j122704.56 - 005425.77 & - + 840 & 12:27:27.24 & -01:05:16.17 & 20.145 & 19.326 & 18.958 & 18.919 & 18.670 & 4.179 & sdss j122727.36 - 010515.10 & - & sdss j122727.12 - 010517.23 & - + 841 & 12:27:36.60 & -00:25:36.94 & 19.780 & 16.616 & 15.637 & 15.204 & 14.808 & 11.790 & sdss j122736.24 - 002534.57 & 0.061914 & sdss j122736.96 - 002539.30 & - + 842 & 12:27:36.84 & -00:23:06.68 & 17.919 & 16.043 & 14.953 & 14.534 & 14.210 & 9.002 & sdss j122736.96 - 002302.55 & 0.115369 & sdss j122736.72 - 002310.80 & - + 843 & 12:27:50.76 & + 00:02:42.48 & 19.826 & 18.053 & 17.067 & 16.638 & 16.348 & 5.288 & sdss j122750.88 + 000244.42 & 0.112809 & sdss j122750.64 + 000240.55 & - + 844 & 12:27:52.44 & -00:37:54.26 & 19.181 & 17.639 & 16.745 & 16.374 & 16.081 & 8.172 & sdss j122752.32 - 003750.59 & - & sdss j122752.56 - 003757.93 & - + 845 & 12:28:33.00 & -00:37:30.71 & 20.299 & 19.467 & 18.906 & 18.643 & 18.351 & 4.914 & sdss j122833.12 - 003732.39 & - & sdss j122832.88 - 003729.04 & - + 846 & 12:28:35.88 & -00:55:56.70 & 19.787 & 18.239 & 17.180 & 16.762 & 16.434 & 5.579 & sdss j122835.76 - 005558.83 & 0.157358 & sdss j122836.00 - 005554.57 & - + 847 & 12:28:41.76 & -00:20:14.95 & 20.166 & 17.933 & 16.707 & 16.216 & 15.869 & 4.817 & sdss j122841.76 - 002017.36 & 0.154617 & sdss j122841.76 - 002012.54 & - + 848 & 12:28:42.84 & + 00:11:51.45 & 21.077 & 19.148 & 17.765 & 17.343 & 16.983 & 4.601 & sdss j122842.72 + 001150.02 & - & sdss j122842.96 + 001152.89 & - + 849 & 12:28:44.28 & -00:53:51.23 & 18.891 & 17.283 & 16.172 & 15.738 & 15.436 & 3.644 & sdss j122844.16 - 005351.51 & 0.161359 & sdss j122844.40 - 005350.94 & - + 850 & 12:29:37.44 & -00:51:21.70 & 19.394 & 18.195 & 17.628 & 17.397 & 17.310 & 2.524 & sdss j122937.44 - 005122.97 & 0.133500 & sdss j122937.44 - 005120.44 & - + 851 & 12:29:48.00 & -00:20:03.84 & 19.341 & 16.860 & 15.786 & 15.460 & 15.096 & 7.271 & sdss j122947.76 - 002004.34 & 0.153293 & sdss j122948.24 - 002003.33 & - + 852 & 12:29:55.80 & + 00:25:43.30 & 19.893 & 17.904 & 16.758 & 16.357 & 15.926 & 6.008 & sdss j122955.92 + 002540.90 & 0.152136 & sdss j122955.68 + 002545.71 & - + 853 & 12:30:06.60 & -00:57:26.04 & 19.735 & 18.146 & 17.303 & 16.937 & 16.646 & 3.720 & sdss j123006.48 - 005725.57 & - & sdss j123006.72 - 005726.51 & - + 854 & 12:30:15.00 & -00:06:26.96 & 19.267 & 18.416 & 17.875 & 17.510 & 17.549 & 3.621 & sdss j123014.88 - 000626.76 & - & sdss j123015.12 - 000627.15 & - + 855 & 12:30:27.36 & -00:43:14.49 & 19.570 & 17.828 & 16.711 & 16.222 & 15.874 & 8.283 & sdss j123027.12 - 004316.54 & - & sdss j123027.60 - 004312.44 & - + 856 & 12:30:32.40 & -00:11:02.73 & 20.159 & 18.481 & 17.050 & 16.501 & 16.123 & 7.553 & sdss j123032.40 - 001058.96 & - & sdss j123032.40 - 001106.51 & - + 857 & 12:30:42.12 & -01:07:13.26 & 21.752 & 18.894 & 17.717 & 17.208 & 16.984 & 4.198 & sdss j123042.24 - 010714.34 & - & sdss j123042.00 - 010712.18 & - + 858 & 12:31:00.36 & + 00:15:55.43 & 19.383 & 18.226 & 17.811 & 17.579 & 17.348 & 3.875 & sdss j123100.24 + 001554.71 & - & sdss j123100.48 + 001556.14 & - + 859 & 12:31:26.40 & -00:56:04.37 & 17.849 & 16.489 & 15.670 & 15.393 & 15.137 & 5.238 & sdss j123126.40 - 005606.99 & 0.112353 & sdss j123126.40 - 005601.75 & - + 860 & 12:31:59.16 & + 00:17:58.47 & 18.200 & 16.967 & 16.340 & 16.064 & 15.812 & 6.406 & sdss j123159.28 + 001755.82 & - & sdss j123159.04 + 001801.11 & - + 861 & 12:32:22.32 & + 00:00:40.20 & 17.471 & 16.077 & 15.321 & 14.965 & 14.725 & 4.379 & sdss j123222.32 + 000042.39 & 0.044157 & sdss j123222.32 + 000038.02 & 0.043701 + 862 & 12:33:27.84 & -00:04:58.72 & 19.962 & 18.301 & 17.405 & 16.959 & 16.635 & 7.152 & sdss j123327.84 - 000455.15 & - & sdss j123327.84 - 000502.30 & - + 863 & 12:33:37.08 & -00:25:07.02 & 20.051 & 18.176 & 17.044 & 16.607 & 16.170 & 5.707 & sdss j123337.20 - 002509.23 & 0.151592 & sdss j123336.96 - 002504.81 & - + 864 & 12:35:43.68 & + 01:12:09.45 & 20.008 & 19.239 & 19.035 & 18.819 & 19.080 & 2.484 & sdss j123543.68 + 011208.20 & - & sdss j123543.68 + 011210.69 & - + 865 & 12:36:05.76 & -00:56:33.07 & 18.850 & 17.917 & 17.420 & 17.048 & 16.951 & 2.243 & sdss j123605.76 - 005634.19 & - & sdss j123605.76 - 005631.94 & - + 866 & 12:37:45.60 & -00:17:30.34 & 20.002 & 18.096 & 17.009 & 16.550 & 16.095 & 8.240 & sdss j123745.36 - 001728.34 & 0.134053 & sdss j123745.84 - 001732.34 & - + 867 & 12:38:17.52 & -00:55:53.79 & 18.479 & 17.227 & 16.402 & 16.043 & 15.740 & 7.200 & sdss j123817.76 - 005553.72 & 0.153234 & sdss j123817.28 - 005553.87 & - + 868 & 12:38:22.20 & -00:49:55.48 & 18.294 & 17.067 & 16.472 & 16.010 & 15.789 & 5.328 & sdss j123822.32 - 004953.51 & 0.076065 & sdss j123822.08 - 004957.44 & - + 869 & 12:38:48.84 & -00:44:28.21 & 18.268 & 17.085 & 16.268 & 15.900 & 15.534 & 13.255 & sdss j123848.48 - 004424.37 & - & sdss j123849.20 - 004432.06 & 0.135984 + 870 & 12:39:00.84 & + 00:00:31.90 & 19.349 & 18.013 & 17.436 & 16.985 & 16.840 & 4.972 & sdss j123900.96 + 000030.18 & - & sdss j123900.72 + 000033.61 & - + 871 & 12:39:45.12 & -00:31:43.00 & 20.687 & 18.497 & 17.255 & 16.785 & 16.457 & 2.372 & sdss j123945.12 - 003144.18 & - & sdss j123945.12 - 003141.81 & - + 872 & 12:39:55.20 & + 00:32:33.93 & 18.661 & 18.066 & 17.295 & 16.828 & 16.659 & 7.683 & sdss j123954.96 + 003232.59 & 0.137270 & sdss j123955.44 + 003235.27 & - + 873 & 12:40:06.96 & + 00:48:58.42 & 19.169 & 17.252 & 16.110 & 15.666 & 15.269 & 3.974 & sdss j124006.96 + 004900.41 & 0.146787 & sdss j124006.96 + 004856.43 & - + 874 & 12:40:10.56 & + 00:41:58.11 & 18.546 & 17.364 & 16.826 & 16.487 & 16.360 & 2.398 & sdss j124010.56 + 004159.30 & 0.079641 & sdss j124010.56 + 004156.91 & - + 875 & 12:43:26.88 & -00:51:12.81 & 20.164 & 18.588 & 17.652 & 17.316 & 17.029 & 3.949 & sdss j124326.88 - 005110.83 & - & sdss j124326.88 - 005114.78 & - + 876 & 12:43:34.44 & -00:43:26.62 & 19.557 & 18.382 & 17.284 & 16.881 & 16.519 & 3.742 & sdss j124334.32 - 004326.11 & - & sdss j124334.56 - 004327.13 & - + 877 & 12:43:46.08 & + 00:53:21.03 & 18.758 & 17.343 & 16.746 & 16.441 & 16.235 & 3.902 & sdss j124346.08 + 005319.07 & 0.089667 & sdss j124346.08 + 005322.98 & - + 878 & 12:44:25.56 & + 01:08:20.18 & 16.725 & 15.693 & 15.128 & 14.821 & 14.659 & 3.993 & sdss j124425.44 + 010819.32 & - & sdss j124425.68 + 010821.04 & 0.090127 + 879 & 12:44:40.20 & + 01:08:46.53 & 17.789 & 16.373 & 15.647 & 15.452 & 15.346 & 3.657 & sdss j124440.32 + 010846.21 & 0.090182 & sdss j124440.08 + 010846.86 & - + 880 & 12:44:46.92 & -00:58:21.76 & 18.213 & 16.727 & 15.772 & 15.441 & 15.175 & 3.617 & sdss j124446.80 - 005821.94 & 0.149002 & sdss j124447.04 - 005821.59 & - + 881 & 12:44:50.76 & + 00:59:36.39 & 17.958 & 16.832 & 16.432 & 16.245 & 16.099 & 11.053 & sdss j124450.88 + 005931.17 & 0.064219 & sdss j124450.64 + 005941.62 & - + 882 & 12:44:54.48 & -00:26:37.64 & 19.893 & 18.137 & 16.811 & 16.332 & 15.956 & 5.227 & sdss j124454.48 - 002640.25 & 0.230911 & sdss j124454.48 - 002635.02 & - + 883 & 12:45:52.92 & + 00:08:07.06 & 19.638 & 18.297 & 17.346 & 16.948 & 16.609 & 4.213 & sdss j124552.80 + 000808.16 & - & sdss j124553.04 + 000805.97 & - + 884 & 12:46:10.56 & -00:19:38.59 & 19.239 & 17.255 & 16.154 & 15.738 & 15.364 & 8.629 & sdss j124610.32 - 001936.21 & 0.145822 & sdss j124610.80 - 001940.97 & 0.146639 + 885 & 12:46:19.20 & -00:34:03.79 & 21.337 & 19.304 & 17.777 & 17.268 & 16.829 & 1.998 & sdss j124619.20 - 003404.78 & - & sdss j124619.20 - 003402.79 & - + 886 & 12:46:26.16 & + 00:31:25.72 & 18.417 & 16.555 & 15.557 & 15.126 & 14.719 & 11.296 & sdss j124626.40 + 003121.37 & 0.047469 & sdss j124625.92 + 003130.07 & 0.088321 + 887 & 12:46:30.12 & + 00:30:12.18 & 18.286 & 17.289 & 16.877 & 16.791 & 16.765 & 5.030 & sdss j124630.24 + 003010.42 & - & sdss j124630.00 + 003013.93 & - + 888 & 12:46:31.08 & -00:22:53.72 & 18.175 & 17.040 & 16.366 & 15.955 & 15.709 & 10.922 & sdss j124631.44 - 002252.91 & 0.082653 & sdss j124630.72 - 002254.54 & 0.082309 + 889 & 12:47:06.96 & -00:37:28.54 & 19.928 & 18.259 & 17.344 & 16.959 & 16.715 & 3.280 & sdss j124706.96 - 003726.90 & - & sdss j124706.96 - 003730.18 & - + 890 & 12:47:12.72 & -00:51:22.04 & 19.263 & 17.618 & 16.573 & 16.090 & 15.774 & 2.927 & sdss j124712.72 - 005123.50 & 0.082460 & sdss j124712.72 - 005120.58 & - + 891 & 12:47:23.76 & -00:14:51.71 & 20.564 & 18.820 & 18.155 & 17.731 & 17.480 & 3.020 & sdss j124723.76 - 001450.20 & - & sdss j124723.76 - 001453.22 & - + 892 & 12:47:53.88 & + 00:04:25.93 & 19.148 & 17.530 & 16.695 & 16.263 & 15.985 & 3.606 & sdss j124754.00 + 000426.03 & 0.088715 & sdss j124753.76 + 000425.82 & - + 893 & 12:48:13.20 & -00:31:56.07 & 19.544 & 18.358 & 17.806 & 17.642 & 17.553 & 3.888 & sdss j124813.20 - 003154.12 & - & sdss j124813.20 - 003158.01 & 0.290300 + 894 & 12:48:24.48 & -00:56:09.44 & 19.412 & 17.976 & 16.946 & 16.492 & 16.267 & 4.331 & sdss j124824.48 - 005607.28 & 0.193984 & sdss j124824.48 - 005611.61 & - + 895 & 12:49:07.92 & + 00:23:12.93 & 20.720 & 18.934 & 17.871 & 17.378 & 17.125 & 2.642 & sdss j124907.92 + 002311.61 & - & sdss j124907.92 + 002314.25 & - + 896 & 12:49:59.40 & + 00:48:05.83 & 19.516 & 18.371 & 17.441 & 17.037 & 16.756 & 5.497 & sdss j124959.28 + 004807.90 & 0.195700 & sdss j124959.52 + 004803.75 & - + 897 & 12:50:01.32 & -00:24:35.20 & 18.461 & 17.487 & 17.130 & 16.748 & 16.613 & 6.683 & sdss j125001.44 - 002438.02 & - & sdss j125001.20 - 002432.39 & - + 898 & 12:50:17.04 & + 00:26:26.05 & 19.384 & 18.404 & 18.118 & 17.904 & 17.895 & 4.568 & sdss j125017.04 + 002623.77 & - & sdss j125017.04 + 002628.34 & - + 899 & 12:51:47.52 & -01:00:50.29 & 19.510 & 17.661 & 16.705 & 16.283 & 15.972 & 4.320 & sdss j125147.52 - 010052.45 & - & sdss j125147.52 - 010048.13 & 0.093762 + 900 & 12:52:19.56 & + 00:07:03.75 & 19.185 & 18.175 & 17.919 & 17.700 & 17.722 & 4.036 & sdss j125219.68 + 000702.83 & - & sdss j125219.44 + 000704.66 & - + 901 & 12:52:37.20 & + 00:15:37.77 & 20.766 & 19.315 & 18.777 & 18.653 & 18.237 & 7.207 & sdss j125237.20 + 001541.37 & 0.083400 & sdss j125237.20 + 001534.16 & - + 902 & 12:53:14.04 & + 00:39:55.64 & 19.335 & 17.930 & 17.352 & 17.041 & 16.872 & 6.028 & sdss j125314.16 + 003958.06 & 0.105218 & sdss j125313.92 + 003953.22 & 0.104900 + 903 & 12:54:01.80 & + 01:08:01.78 & 19.416 & 18.098 & 17.219 & 16.722 & 16.481 & 3.802 & sdss j125401.68 + 010801.17 & - & sdss j125401.92 + 010802.40 & - + 904 & 12:54:35.28 & -00:10:57.03 & 19.379 & 17.569 & 16.651 & 16.229 & 15.901 & 7.809 & sdss j125435.04 - 001055.52 & - & sdss j125435.52 - 001058.54 & 0.081850 + 905 & 12:54:47.28 & -00:31:49.17 & 20.120 & 19.216 & 18.761 & 18.472 & 18.387 & 7.636 & sdss j125447.52 - 003150.44 & - & sdss j125447.04 - 003147.89 & - + 906 & 12:55:09.48 & -01:05:28.78 & 20.012 & 17.970 & 16.965 & 16.592 & 16.330 & 3.993 & sdss j125509.36 - 010529.65 & - & sdss j125509.60 - 010527.92 & 0.122923 + 907 & 12:55:20.40 & -00:20:38.15 & 20.982 & 19.946 & 19.494 & 19.223 & 19.312 & 1.912 & sdss j125520.40 - 002037.20 & - & sdss j125520.40 - 002039.11 & - + 908 & 12:55:28.68 & -00:59:32.67 & 19.936 & 18.800 & 18.077 & 17.732 & 17.587 & 3.930 & sdss j125528.80 - 005933.46 & - & sdss j125528.56 - 005931.88 & - + 909 & 12:56:26.16 & -00:38:22.63 & 20.716 & 19.299 & 18.191 & 17.710 & 17.340 & 4.417 & sdss j125626.16 - 003820.42 & - & sdss j125626.16 - 003824.83 & - + 910 & 12:56:43.20 & + 00:18:19.85 & 19.511 & 18.106 & 17.218 & 16.792 & 16.441 & 4.637 & sdss j125643.20 + 001822.17 & - & sdss j125643.20 + 001817.53 & - + 911 & 12:57:25.32 & -00:34:16.77 & 17.665 & 16.557 & 16.075 & 15.891 & 15.784 & 14.205 & sdss j125725.44 - 003423.64 & 0.046930 & sdss j125725.20 - 003409.90 & - + 912 & 12:58:07.80 & -01:04:35.59 & 21.267 & 20.056 & 18.923 & 18.477 & 18.289 & 4.216 & sdss j125807.68 - 010436.69 & - & sdss j125807.92 - 010434.50 & - + 913 & 12:58:27.72 & -00:24:21.62 & 19.834 & 19.206 & 18.890 & 18.696 & 18.714 & 5.884 & sdss j125827.60 - 002419.29 & - & sdss j125827.84 - 002423.95 & - + 914 & 12:58:57.60 & -00:59:41.38 & 19.933 & 18.589 & 17.580 & 17.138 & 16.818 & 6.710 & sdss j125857.60 - 005944.73 & - & sdss j125857.60 - 005938.02 & - + 915 & 12:59:49.08 & + 00:13:44.90 & 19.371 & 17.485 & 16.458 & 16.034 & 15.714 & 3.611 & sdss j125948.96 + 001345.04 & 0.126977 & sdss j125949.20 + 001344.76 & - + 916 & 13:01:13.68 & -00:53:29.30 & 19.219 & 18.145 & 17.706 & 17.407 & 17.324 & 7.292 & sdss j130113.44 - 005329.88 & - & sdss j130113.92 - 005328.72 & - + 917 & 13:01:46.68 & -00:11:29.50 & 20.246 & 19.076 & 18.355 & 17.920 & 17.651 & 4.223 & sdss j130146.80 - 001130.60 & 0.145200 & sdss j130146.56 - 001128.39 & - + 918 & 13:01:50.16 & -00:37:10.18 & 19.216 & 18.464 & 18.501 & 18.376 & 18.286 & 3.103 & sdss j130150.16 - 003708.63 & - & sdss j130150.16 - 003711.74 & - + 919 & 13:02:00.36 & -00:18:40.93 & 19.227 & 18.561 & 18.095 & 17.867 & 17.710 & 4.748 & sdss j130200.24 - 001842.48 & - & sdss j130200.48 - 001839.38 & - + 920 & 13:02:06.24 & -00:11:55.53 & 19.822 & 18.417 & 17.627 & 17.189 & 16.870 & 7.567 & sdss j130206.24 - 001159.31 & - & sdss j130206.24 - 001151.74 & - + 921 & 13:02:57.72 & + 00:28:05.85 & 18.156 & 16.544 & 15.740 & 15.251 & 14.894 & 4.590 & sdss j130257.60 + 002807.28 & 0.082151 & sdss j130257.84 + 002804.43 & - + 922 & 13:02:57.72 & + 00:28:05.85 & 18.156 & 16.544 & 15.740 & 15.251 & 14.894 & 4.590 & sdss j130257.60 + 002807.28 & 0.082151 & sdss j130257.84 + 002804.43 & - + 923 & 13:03:53.04 & + 00:03:08.79 & 20.432 & 18.520 & 17.231 & 16.740 & 16.377 & 2.238 & sdss j130353.04 + 000309.91 & - & sdss j130353.04 + 000307.67 & 0.185700 + 924 & 13:04:34.08 & + 00:39:48.63 & 19.248 & 18.263 & 17.760 & 17.322 & 17.404 & 2.138 & sdss j130434.08 + 003947.56 & - & sdss j130434.08 + 003949.70 & - + 925 & 13:04:35.40 & -00:03:15.45 & 18.957 & 17.773 & 17.284 & 17.183 & 17.314 & 3.885 & sdss j130435.28 - 000316.18 & 0.084771 & sdss j130435.52 - 000314.72 & - + 926 & 13:04:51.84 & + 01:12:18.46 & 19.724 & 18.231 & 17.445 & 17.003 & 16.794 & 7.808 & sdss j130452.08 + 011219.98 & - & sdss j130451.60 + 011216.95 & - + 927 & 13:04:52.44 & -00:05:44.49 & 20.152 & 18.159 & 17.036 & 16.619 & 16.246 & 3.675 & sdss j130452.56 - 000544.86 & 0.143974 & sdss j130452.32 - 000544.12 & - + 928 & 13:06:21.84 & -00:49:39.28 & 20.173 & 18.001 & 16.734 & 16.222 & 15.885 & 2.804 & sdss j130621.84 - 004940.68 & 0.190131 & sdss j130621.84 - 004937.88 & - + 929 & 13:06:21.84 & + 00:02:17.64 & 18.648 & 17.548 & 16.766 & 16.420 & 16.241 & 3.453 & sdss j130621.84 + 000215.91 & 0.174784 & sdss j130621.84 + 000219.36 & - + 930 & 13:06:51.60 & + 01:12:19.18 & 19.178 & 17.743 & 16.934 & 16.561 & 16.104 & 8.625 & sdss j130651.36 + 011216.81 & - & sdss j130651.84 + 011221.56 & - + 931 & 13:07:28.08 & + 00:29:17.01 & 18.780 & 17.090 & 16.153 & 15.743 & 15.466 & 8.074 & sdss j130727.84 + 002915.19 & 0.123675 & sdss j130728.32 + 002918.84 & - + 932 & 13:08:06.72 & + 00:28:18.42 & 21.105 & 18.848 & 17.518 & 17.067 & 16.695 & 2.416 & sdss j130806.72 + 002817.21 & - & sdss j130806.72 + 002819.63 & - + 933 & 13:08:34.32 & -00:09:44.92 & 18.896 & 17.965 & 17.258 & 17.118 & 16.615 & 8.198 & sdss j130834.56 - 000946.88 & - & sdss j130834.08 - 000942.96 & - + 934 & 13:08:38.40 & -00:11:31.93 & 20.108 & 18.970 & 18.404 & 18.149 & 17.959 & 2.473 & sdss j130838.40 - 001133.17 & - & sdss j130838.40 - 001130.69 & - + 935 & 13:08:45.60 & -00:14:17.21 & 20.173 & 18.998 & 18.301 & 17.926 & 17.666 & 2.365 & sdss j130845.60 - 001418.39 & - & sdss j130845.60 - 001416.03 & - + 936 & 13:08:45.96 & -00:47:19.59 & 19.541 & 17.403 & 16.112 & 15.621 & 15.222 & 11.160 & sdss j130845.60 - 004718.18 & 0.188305 & sdss j130846.32 - 004721.00 & - + 937 & 13:08:52.92 & -00:18:33.00 & 19.206 & 18.436 & 18.143 & 17.963 & 17.775 & 6.179 & sdss j130852.80 - 001835.51 & - & sdss j130853.04 - 001830.49 & - + 938 & 13:08:56.16 & -01:04:06.09 & 20.264 & 19.437 & 18.693 & 18.370 & 18.066 & 7.199 & sdss j130855.92 - 010406.13 & - & sdss j130856.40 - 010406.06 & - + 939 & 13:09:15.36 & + 00:56:38.86 & 18.627 & 17.307 & 16.699 & 16.372 & 16.136 & 8.075 & sdss j130915.12 + 005637.03 & - & sdss j130915.60 + 005640.68 & 0.098898 + 940 & 13:09:55.56 & + 00:26:00.47 & 20.017 & 18.946 & 18.236 & 17.949 & 17.520 & 6.350 & sdss j130955.68 + 002557.86 & - & sdss j130955.44 + 002603.09 & - + 941 & 13:10:27.24 & + 01:04:35.72 & 20.054 & 18.778 & 18.159 & 17.803 & 17.695 & 4.235 & sdss j131027.12 + 010434.60 & - & sdss j131027.36 + 010436.84 & - + 942 & 13:10:41.64 & + 00:39:30.14 & 18.467 & 16.765 & 15.920 & 15.500 & 15.137 & 11.676 & sdss j131042.00 + 003927.92 & 0.053299 & sdss j131041.28 + 003932.36 & - + 943 & 13:10:59.52 & -00:59:33.66 & 19.030 & 17.909 & 16.970 & 16.538 & 16.286 & 9.384 & sdss j131059.28 - 005936.67 & 0.181549 & sdss j131059.76 - 005930.65 & - + 944 & 13:12:06.72 & -00:49:52.64 & 18.838 & 16.840 & 15.818 & 15.344 & 14.957 & 8.098 & sdss j131206.48 - 004950.79 & 0.084362 & sdss j131206.96 - 004954.50 & - + 945 & 13:12:10.68 & + 00:50:18.17 & 19.725 & 17.540 & 16.714 & 16.296 & 16.006 & 4.812 & sdss j131210.56 + 005016.58 & 0.071973 & sdss j131210.80 + 005019.77 & - + 946 & 13:13:04.32 & + 00:31:50.24 & 19.863 & 18.610 & 17.364 & 16.857 & 16.483 & 6.793 & sdss j131304.32 + 003146.84 & - & sdss j131304.32 + 003153.63 & - + 947 & 13:13:15.24 & + 00:05:42.03 & 19.718 & 18.669 & 17.921 & 17.568 & 17.281 & 4.413 & sdss j131315.36 + 000543.31 & - & sdss j131315.12 + 000540.75 & - + 948 & 13:13:28.20 & -01:12:40.39 & 18.700 & 17.157 & 16.322 & 15.904 & 15.658 & 3.600 & sdss j131328.32 - 011240.35 & - & sdss j131328.08 - 011240.42 & 0.109016 + 949 & 13:13:43.08 & + 00:33:31.51 & 19.427 & 17.702 & 16.770 & 16.321 & 15.925 & 5.018 & sdss j131343.20 + 003333.26 & 0.081697 & sdss j131342.96 + 003329.77 & - + 950 & 13:14:17.28 & + 00:18:48.98 & 18.066 & 16.102 & 15.164 & 14.762 & 14.381 & 10.175 & sdss j131417.04 + 001852.58 & - & sdss j131417.52 + 001845.39 & 0.081383 + 951 & 13:14:25.08 & -00:17:24.36 & 19.994 & 18.682 & 17.643 & 17.202 & 16.845 & 4.088 & sdss j131424.96 - 001725.32 & - & sdss j131425.20 - 001723.39 & - + 952 & 13:14:46.92 & + 01:03:24.42 & 20.301 & 19.397 & 18.969 & 18.739 & 18.678 & 3.890 & sdss j131447.04 + 010323.68 & - & sdss j131446.80 + 010325.16 & - + 953 & 13:15:04.32 & -00:08:48.14 & 19.625 & 18.498 & 17.886 & 17.581 & 17.357 & 5.407 & sdss j131504.32 - 000845.43 & - & sdss j131504.32 - 000850.84 & - + 954 & 13:15:17.04 & -00:36:30.03 & 18.722 & 17.562 & 17.027 & 16.684 & 16.470 & 5.256 & sdss j131517.04 - 003627.40 & 0.085819 & sdss j131517.04 - 003632.66 & - + 955 & 13:15:30.48 & -00:34:40.98 & 21.584 & 19.152 & 17.877 & 17.392 & 17.064 & 3.204 & sdss j131530.48 - 003439.37 & - & sdss j131530.48 - 003442.58 & - + 956 & 13:16:14.64 & + 00:14:03.16 & 20.467 & 19.067 & 18.163 & 17.802 & 17.578 & 2.484 & sdss j131614.64 + 001404.40 & - & sdss j131614.64 + 001401.92 & - + 957 & 13:16:19.08 & -00:56:51.28 & 17.332 & 16.246 & 15.654 & 15.263 & 15.052 & 12.098 & sdss j131619.44 - 005648.55 & 0.087904 & sdss j131618.72 - 005654.00 & - + 958 & 13:16:40.80 & + 00:35:18.79 & 17.528 & 16.462 & 16.067 & 15.730 & 15.534 & 8.174 & sdss j131641.04 + 003520.73 & 0.081291 & sdss j131640.56 + 003516.86 & - + 959 & 13:16:58.92 & + 00:32:23.14 & 17.168 & 16.013 & 15.470 & 15.185 & 14.977 & 9.234 & sdss j131659.04 + 003218.89 & 0.081262 & sdss j131658.80 + 003227.39 & - + 960 & 13:17:00.84 & -00:47:11.56 & 21.268 & 19.688 & 18.696 & 18.218 & 17.964 & 3.604 & sdss j131700.72 - 004711.65 & 0.081262 & sdss j131700.96 - 004711.47 & - + 961 & 13:17:06.72 & -00:23:56.74 & 19.523 & 18.459 & 18.023 & 17.707 & 17.559 & 5.011 & sdss j131706.72 - 002359.25 & - & sdss j131706.72 - 002354.24 & - + 962 & 13:17:07.08 & + 00:54:51.24 & 19.540 & 18.008 & 17.425 & 17.128 & 16.968 & 3.607 & sdss j131706.96 + 005451.12 & 0.080530 & sdss j131707.20 + 005451.35 & - + 963 & 13:17:11.88 & + 00:59:09.77 & 19.597 & 18.048 & 17.089 & 16.662 & 16.374 & 5.139 & sdss j131712.00 + 005907.93 & 0.157678 & sdss j131711.76 + 005911.60 & - + 964 & 13:17:14.16 & -00:46:09.94 & 19.150 & 18.202 & 17.982 & 17.775 & 17.836 & 3.445 & sdss j131714.16 - 004611.67 & - & sdss j131714.16 - 004608.22 & - + 965 & 13:18:20.28 & -01:05:27.22 & 18.783 & 17.171 & 16.333 & 15.904 & 15.628 & 12.221 & sdss j131819.92 - 010530.08 & 0.085790 & sdss j131820.64 - 010524.36 & - + 966 & 13:18:21.00 & + 00:24:40.71 & 19.632 & 17.774 & 16.958 & 16.553 & 16.198 & 10.801 & sdss j131821.36 + 002440.64 & 0.076912 & sdss j131820.64 + 002440.78 & - + 967 & 13:18:33.36 & + 00:43:52.03 & 19.298 & 17.985 & 17.200 & 16.803 & 16.501 & 4.558 & sdss j131833.36 + 004349.75 & 0.137853 & sdss j131833.36 + 004354.31 & - + 968 & 13:18:40.56 & -01:02:08.66 & 21.374 & 19.367 & 18.111 & 17.674 & 17.283 & 4.752 & sdss j131840.56 - 010211.04 & - & sdss j131840.56 - 010206.28 & - + 969 & 13:18:41.76 & -00:02:53.06 & 19.871 & 18.628 & 18.185 & 17.932 & 17.643 & 5.008 & sdss j131841.76 - 000250.55 & - & sdss j131841.76 - 000255.56 & - + 970 & 13:18:42.60 & + 00:52:37.73 & 19.921 & 18.933 & 18.331 & 18.126 & 17.930 & 10.170 & sdss j131842.72 + 005232.97 & - & sdss j131842.48 + 005242.48 & - + 971 & 13:18:52.44 & -00:34:30.59 & 20.075 & 18.826 & 18.192 & 17.871 & 17.537 & 5.155 & sdss j131852.32 - 003432.43 & - & sdss j131852.56 - 003428.74 & - + 972 & 13:18:58.92 & + 01:09:47.88 & 20.356 & 18.757 & 17.537 & 16.998 & 16.760 & 4.843 & sdss j131859.04 + 010949.50 & - & sdss j131858.80 + 010946.26 & - + 973 & 13:19:11.04 & -00:58:56.77 & 19.342 & 17.498 & 16.504 & 16.076 & 15.728 & 6.138 & sdss j131911.04 - 005859.84 & - & sdss j131911.04 - 005853.70 & - + 974 & 13:19:14.28 & -00:39:38.65 & 19.642 & 18.695 & 18.161 & 17.829 & 17.612 & 4.572 & sdss j131914.40 - 003937.24 & - & sdss j131914.16 - 003940.06 & - + 975 & 13:19:30.48 & + 01:02:20.25 & 18.697 & 17.080 & 16.339 & 15.878 & 15.655 & 4.392 & sdss j131930.48 + 010222.45 & 0.081367 & sdss j131930.48 + 010218.06 & - + 976 & 13:19:36.12 & + 00:29:15.40 & 19.519 & 18.550 & 18.039 & 17.722 & 17.628 & 3.818 & sdss j131936.00 + 002914.77 & - & sdss j131936.24 + 002916.04 & - + 977 & 13:19:38.76 & + 00:25:09.64 & 18.777 & 17.224 & 16.440 & 16.017 & 15.793 & 10.800 & sdss j131939.12 + 002509.68 & 0.074681 & sdss j131938.40 + 002509.60 & - + 978 & 13:19:39.96 & + 00:07:37.90 & 19.307 & 18.225 & 17.550 & 17.126 & 16.887 & 6.707 & sdss j131940.08 + 000735.07 & - & sdss j131939.84 + 000740.73 & - + 979 & 13:19:46.44 & -00:24:16.64 & 19.624 & 18.502 & 17.847 & 17.467 & 17.225 & 4.568 & sdss j131946.56 - 002418.05 & - & sdss j131946.32 - 002415.24 & - + 980 & 13:19:49.32 & -00:43:34.37 & 19.715 & 17.598 & 16.429 & 15.964 & 15.674 & 3.600 & sdss j131949.44 - 004334.37 & - & sdss j131949.20 - 004334.38 & - + 981 & 13:20:10.08 & + 01:11:14.01 & 20.719 & 19.525 & 18.401 & 17.994 & 17.723 & 3.564 & sdss j132010.08 + 011112.22 & - & sdss j132010.08 + 011115.79 & - + 982 & 13:20:24.36 & -00:16:12.80 & 19.974 & 18.646 & 17.789 & 17.317 & 17.012 & 5.582 & sdss j132024.48 - 001614.93 & - & sdss j132024.24 - 001610.66 & - + 983 & 13:20:47.04 & -00:46:26.34 & 21.170 & 19.054 & 17.632 & 17.140 & 16.749 & 4.576 & sdss j132047.04 - 004624.06 & - & sdss j132047.04 - 004628.63 & - + 984 & 13:20:53.16 & -00:54:01.24 & 19.413 & 18.357 & 17.876 & 17.592 & 17.536 & 5.370 & sdss j132053.04 - 005403.23 & - & sdss j132053.28 - 005359.24 & - + 985 & 13:21:01.44 & -00:53:12.73 & 18.644 & 16.990 & 15.988 & 15.559 & 15.250 & 8.672 & sdss j132101.44 - 005308.39 & 0.115599 & sdss j132101.44 - 005317.07 & - + 986 & 13:21:03.36 & -00:07:26.42 & 19.657 & 17.707 & 16.656 & 16.208 & 15.913 & 2.059 & sdss j132103.36 - 000727.45 & 0.136147 & sdss j132103.36 - 000725.39 & 0.135223 + 987 & 13:21:12.72 & -00:42:25.26 & 20.881 & 19.586 & 18.907 & 18.627 & 18.311 & 7.210 & sdss j132112.48 - 004225.06 & - & sdss j132112.96 - 004225.45 & - + 988 & 13:22:37.68 & + 00:37:00.88 & 19.115 & 18.140 & 17.861 & 17.598 & 17.526 & 7.200 & sdss j132237.44 + 003700.82 & - & sdss j132237.92 + 003700.93 & - + 989 & 13:23:11.28 & + 00:49:11.18 & 18.923 & 17.373 & 16.465 & 16.056 & 15.653 & 7.237 & sdss j132311.52 + 004911.55 & 0.111999 & sdss j132311.04 + 004910.81 & - + 990 & 13:23:15.48 & -00:09:47.73 & 20.028 & 17.918 & 16.768 & 16.336 & 15.987 & 9.560 & sdss j132315.36 - 000952.16 & 0.174249 & sdss j132315.60 - 000943.31 & - + 991 & 13:23:21.36 & + 00:42:18.79 & 21.087 & 18.692 & 17.443 & 17.053 & 16.743 & 7.711 & sdss j132321.12 + 004217.41 & - & sdss j132321.60 + 004220.17 & - + 992 & 13:23:51.12 & + 00:30:14.00 & 19.185 & 18.255 & 17.855 & 17.662 & 17.586 & 7.997 & sdss j132351.36 + 003015.74 & - & sdss j132350.88 + 003012.26 & - + 993 & 13:24:02.76 & + 00:37:56.69 & 19.489 & 18.840 & 18.382 & 18.140 & 18.105 & 4.211 & sdss j132402.88 + 003757.79 & - & sdss j132402.64 + 003755.60 & - + 994 & 13:24:16.68 & + 00:48:28.07 & 18.350 & 16.394 & 15.402 & 14.998 & 14.600 & 11.538 & sdss j132416.32 + 004830.10 & 0.107977 & sdss j132417.04 + 004826.03 & 0.110003 + 995 & 13:24:33.24 & + 00:58:18.20 & 19.838 & 18.701 & 17.469 & 16.997 & 16.651 & 6.208 & sdss j132433.12 + 005820.73 & - & sdss j132433.36 + 005815.67 & - + 996 & 13:24:42.12 & + 00:37:48.59 & 18.458 & 17.349 & 16.751 & 16.329 & 16.216 & 3.897 & sdss j132442.00 + 003747.84 & 0.083786 & sdss j132442.24 + 003749.33 & - + 997 & 13:25:59.40 & + 00:26:48.22 & 21.194 & 19.634 & 18.401 & 17.985 & 17.659 & 3.613 & sdss j132559.28 + 002648.06 & - & sdss j132559.52 + 002648.37 & - + 998 & 13:26:15.36 & + 00:24:07.06 & 20.132 & 18.306 & 17.340 & 16.849 & 16.477 & 7.483 & sdss j132615.60 + 002408.08 & 0.083648 & sdss j132615.12 + 002406.04 & - + 999 & 13:26:28.44 & -00:28:51.20 & 19.517 & 18.723 & 18.044 & 17.809 & 17.585 & 4.030 & sdss j132628.56 - 002852.11 & - & sdss j132628.32 - 002850.30 & - + 1000 & 13:26:32.76 & + 00:19:36.44 & 19.744 & 17.805 & 16.946 & 16.522 & 16.201 & 6.270 & sdss j132632.88 + 001933.88 & 0.083707 & sdss j132632.64 + 001939.01 & - + 1001 & 13:26:43.68 & + 00:19:51.26 & 19.400 & 17.857 & 16.988 & 16.595 & 16.302 & 4.655 & sdss j132643.68 + 001948.93 & 0.081967 & sdss j132643.68 + 001953.59 & - + 1002 & 13:26:50.76 & -00:48:58.66 & 20.357 & 18.838 & 17.700 & 17.247 & 16.930 & 4.365 & sdss j132650.64 - 004857.43 & - & sdss j132650.88 - 004859.90 & - + 1003 & 13:26:55.80 & + 00:41:52.11 & 17.562 & 16.415 & 15.777 & 15.227 & 15.078 & 5.099 & sdss j132655.92 + 004153.92 & - & sdss j132655.68 + 004150.31 & 0.081574 + 1004 & 13:27:40.32 & + 00:41:15.84 & 17.037 & 16.086 & 15.809 & 15.806 & 15.760 & 7.418 & sdss j132740.56 + 004116.74 & 0.018310 & sdss j132740.08 + 004114.95 & - + 1005 & 13:27:51.00 & + 00:58:42.99 & 20.194 & 18.819 & 18.106 & 17.721 & 17.603 & 3.612 & sdss j132751.12 + 005842.84 & 0.079400 & sdss j132750.88 + 005843.14 & - + 1006 & 13:27:52.44 & + 00:09:09.57 & 20.089 & 18.371 & 17.581 & 17.142 & 16.943 & 3.635 & sdss j132752.56 + 000909.83 & - & sdss j132752.32 + 000909.32 & - + 1007 & 13:28:17.52 & + 00:17:19.81 & 18.071 & 16.150 & 15.098 & 14.735 & 14.381 & 7.236 & sdss j132817.28 + 001719.45 & - & sdss j132817.76 + 001720.17 & 0.109956 + 1008 & 13:28:18.24 & -00:58:38.89 & 19.499 & 18.653 & 17.843 & 17.528 & 17.407 & 4.968 & sdss j132818.24 - 005841.37 & - & sdss j132818.24 - 005836.41 & - + 1009 & 13:28:21.72 & + 00:09:04.66 & 19.386 & 18.444 & 17.967 & 17.693 & 17.551 & 3.829 & sdss j132821.60 + 000905.31 & 0.047700 & sdss j132821.84 + 000904.01 & - + 1010 & 13:28:32.28 & + 00:15:46.34 & 20.583 & 19.723 & 18.790 & 18.419 & 18.075 & 3.660 & sdss j132832.40 + 001546.01 & - & sdss j132832.16 + 001546.67 & - + 1011 & 13:28:56.88 & + 01:07:58.99 & 19.491 & 17.616 & 16.596 & 16.231 & 15.917 & 7.199 & sdss j132856.64 + 010759.05 & 0.116950 & sdss j132857.12 + 010758.94 & - + 1012 & 13:29:06.60 & + 00:25:32.66 & 19.197 & 17.960 & 17.176 & 16.796 & 16.532 & 7.992 & sdss j132906.72 + 002536.23 & - & sdss j132906.48 + 002529.09 & - + 1013 & 13:30:42.60 & + 01:05:16.72 & 20.380 & 19.110 & 18.370 & 17.942 & 17.530 & 4.394 & sdss j133042.72 + 010515.46 & - & sdss j133042.48 + 010517.98 & - + 1014 & 13:30:55.32 & -01:04:06.24 & 20.968 & 19.063 & 18.182 & 17.690 & 17.368 & 5.194 & sdss j133055.20 - 010408.11 & - & sdss j133055.44 - 010404.36 & - + 1015 & 13:31:51.36 & -00:34:57.23 & 20.781 & 19.699 & 18.711 & 18.442 & 17.985 & 2.282 & sdss j133151.36 - 003456.09 & - & sdss j133151.36 - 003458.37 & - + 1016 & 13:31:58.32 & + 00:11:05.40 & 20.220 & 18.987 & 19.488 & 18.985 & 19.280 & 4.043 & sdss j133158.32 + 001107.42 & 0.178200 & sdss j133158.32 + 001103.37 & - + 1017 & 13:33:31.92 & + 00:30:28.96 & 20.300 & 19.263 & 18.519 & 18.073 & 17.890 & 3.542 & sdss j133331.92 + 003027.19 & - & sdss j133331.92 + 003030.73 & - + 1018 & 13:34:06.00 & + 00:44:26.89 & 17.751 & 16.123 & 15.350 & 14.932 & 14.569 & 23.855 & sdss j133406.48 + 004436.40 & - & sdss j133405.52 + 004417.39 & - + 1019 & 13:34:06.48 & -00:06:58.97 & 19.714 & 17.894 & 16.878 & 16.434 & 15.955 & 9.438 & sdss j133406.24 - 000702.02 & - & sdss j133406.72 - 000655.92 & - + 1020 & 13:34:42.24 & -00:08:41.56 & 18.445 & 17.454 & 16.787 & 16.587 & 16.385 & 8.421 & sdss j133442.48 - 000843.74 & - & sdss j133442.00 - 000839.38 & - + 1021 & 13:36:04.80 & -00:53:22.93 & 18.728 & 17.506 & 16.673 & 16.339 & 15.985 & 9.510 & sdss j133605.04 - 005319.82 & - & sdss j133604.56 - 005326.03 & - + 1022 & 13:36:16.20 & + 00:00:45.13 & 19.166 & 17.863 & 17.264 & 17.102 & 17.007 & 4.207 & sdss j133616.32 + 000044.05 & - & sdss j133616.08 + 000046.22 & - + 1023 & 13:36:17.16 & + 01:04:57.99 & 19.942 & 18.631 & 17.855 & 17.393 & 17.052 & 3.947 & sdss j133617.28 + 010458.80 & - & sdss j133617.04 + 010457.18 & - + 1024 & 13:38:21.96 & -01:02:14.71 & 18.611 & 17.657 & 17.186 & 16.888 & 16.897 & 3.702 & sdss j133822.08 - 010214.28 & 0.086221 & sdss j133821.84 - 010215.14 & - + 1025 & 13:39:04.44 & + 00:55:42.59 & 18.916 & 18.050 & 17.903 & 17.654 & 17.875 & 4.120 & sdss j133904.32 + 005543.60 & - & sdss j133904.56 + 005541.59 & - + 1026 & 13:39:23.76 & -01:06:23.63 & 17.847 & 16.262 & 15.501 & 15.142 & 14.896 & 7.767 & sdss j133924.00 - 010622.17 & 0.070756 & sdss j133923.52 - 010625.09 & - + 1027 & 13:39:33.96 & + 00:06:54.97 & 20.255 & 18.933 & 17.702 & 17.142 & 16.757 & 5.484 & sdss j133934.08 + 000652.90 & - & sdss j133933.84 + 000657.04 & - + 1028 & 13:39:39.24 & -00:19:38.92 & 20.786 & 18.764 & 17.662 & 17.186 & 16.842 & 3.916 & sdss j133939.36 - 001939.69 & - & sdss j133939.12 - 001938.15 & - + 1029 & 13:40:28.56 & + 00:49:22.97 & 19.224 & 17.964 & 17.182 & 16.848 & 16.633 & 8.236 & sdss j134028.80 + 004920.97 & - & sdss j134028.32 + 004924.97 & 0.124800 + 1030 & 13:40:33.72 & -00:42:59.48 & 18.981 & 17.579 & 16.746 & 16.255 & 15.962 & 10.877 & sdss j134033.36 - 004258.83 & 0.113700 & sdss j134034.08 - 004300.13 & - + 1031 & 13:40:45.24 & -00:27:51.62 & 19.810 & 17.814 & 16.685 & 16.229 & 15.806 & 8.487 & sdss j134045.36 - 002755.47 & 0.143132 & sdss j134045.12 - 002747.78 & - + 1032 & 13:42:15.12 & -01:00:50.25 & 18.708 & 17.895 & 17.254 & 17.046 & 16.870 & 7.328 & sdss j134214.88 - 010049.57 & - & sdss j134215.36 - 010050.94 & 0.236523 + 1033 & 13:42:25.20 & -00:57:31.09 & 17.887 & 17.006 & 16.617 & 16.462 & 16.461 & 5.227 & sdss j134225.20 - 005728.47 & 0.101686 & sdss j134225.20 - 005733.70 & - + 1034 & 13:42:56.76 & -00:52:53.84 & 18.962 & 18.021 & 17.411 & 17.024 & 16.882 & 4.724 & sdss j134256.88 - 005252.31 & 0.178000 & sdss j134256.64 - 005255.37 & - + 1035 & 13:43:10.20 & -00:04:19.05 & 20.132 & 18.506 & 17.480 & 17.012 & 16.715 & 4.564 & sdss j134310.08 - 000417.65 & - & sdss j134310.32 - 000420.45 & - + 1036 & 13:43:17.16 & -01:09:30.42 & 20.595 & 19.565 & 19.125 & 18.886 & 18.805 & 3.932 & sdss j134317.04 - 010931.21 & - & sdss j134317.28 - 010929.62 & - + 1037 & 13:44:21.36 & -00:26:16.13 & 19.312 & 17.593 & 16.673 & 16.286 & 15.979 & 7.209 & sdss j134421.60 - 002616.31 & 0.088791 & sdss j134421.12 - 002615.95 & - + 1038 & 13:45:14.40 & -01:06:34.50 & 20.268 & 18.689 & 17.610 & 17.143 & 16.777 & 6.588 & sdss j134514.40 - 010637.80 & - & sdss j134514.40 - 010631.21 & - + 1039 & 13:45:18.84 & -00:56:04.89 & 18.789 & 17.308 & 16.429 & 16.164 & 15.803 & 9.029 & sdss j134518.96 - 005600.75 & 0.077236 & sdss j134518.72 - 005609.03 & - + 1040 & 13:45:43.56 & + 00:20:57.69 & 18.993 & 17.885 & 17.426 & 17.157 & 16.966 & 7.265 & sdss j134543.68 + 002054.53 & - & sdss j134543.44 + 002100.84 & - + 1041 & 13:45:53.04 & + 00:18:16.02 & 19.696 & 18.441 & 17.371 & 16.887 & 16.548 & 8.137 & sdss j134553.28 + 001814.12 & - & sdss j134552.80 + 001817.91 & - + 1042 & 13:46:31.80 & -00:18:18.10 & 19.783 & 17.826 & 16.652 & 16.182 & 15.817 & 4.546 & sdss j134631.68 - 001816.71 & 0.148754 & sdss j134631.92 - 001819.49 & - + 1043 & 13:46:33.00 & + 00:39:06.66 & 18.044 & 16.388 & 15.581 & 15.344 & 14.950 & 11.797 & sdss j134632.64 + 003909.04 & 0.111607 & sdss j134633.36 + 003904.29 & - + 1044 & 13:47:18.84 & -00:53:54.05 & 19.466 & 17.332 & 16.295 & 15.852 & 15.487 & 4.051 & sdss j134718.72 - 005353.12 & - & sdss j134718.96 - 005354.98 & 0.132691 + 1045 & 13:47:21.48 & + 00:28:17.68 & 19.693 & 17.927 & 16.968 & 16.466 & 16.192 & 8.053 & sdss j134721.60 + 002814.08 & 0.166264 & sdss j134721.36 + 002821.28 & - + 1046 & 13:47:54.60 & + 00:54:34.15 & 19.340 & 18.655 & 18.034 & 17.652 & 17.396 & 4.708 & sdss j134754.48 + 005435.66 & 0.259069 & sdss j134754.72 + 005432.63 & - + 1047 & 13:48:40.32 & + 00:47:21.56 & 20.962 & 19.294 & 18.071 & 17.551 & 17.171 & 2.660 & sdss j134840.32 + 004722.89 & - & sdss j134840.32 + 004720.23 & - + 1048 & 13:49:01.08 & + 00:41:20.41 & 19.005 & 17.264 & 16.273 & 15.818 & 15.433 & 5.043 & sdss j134900.96 + 004118.65 & 0.090257 & sdss j134901.20 + 004122.18 & - + 1049 & 13:50:59.28 & -00:57:55.60 & 20.088 & 18.758 & 17.980 & 17.572 & 17.324 & 2.531 & sdss j135059.28 - 005756.86 & - & sdss j135059.28 - 005754.33 & - + 1050 & 13:51:07.44 & -00:20:51.21 & 20.555 & 18.857 & 17.990 & 17.581 & 17.282 & 3.809 & sdss j135107.44 - 002053.12 & - & sdss j135107.44 - 002049.31 & - + 1051 & 13:51:56.16 & + 00:33:01.79 & 17.954 & 16.277 & 15.643 & 15.230 & 15.168 & 8.352 & sdss j135156.40 + 003303.90 & 0.048180 & sdss j135155.92 + 003259.67 & - + 1052 & 13:52:17.88 & + 01:03:00.57 & 19.408 & 17.438 & 16.362 & 15.903 & 15.550 & 11.088 & sdss j135218.24 + 010301.83 & 0.137588 & sdss j135217.52 + 010259.31 & - + 1053 & 13:52:34.44 & -00:48:50.77 & 18.995 & 18.012 & 17.560 & 17.117 & 17.042 & 4.311 & sdss j135234.56 - 004849.59 & 0.150391 & sdss j135234.32 - 004851.96 & - + 1054 & 13:52:42.36 & -00:57:07.57 & 18.575 & 17.299 & 16.240 & 15.820 & 15.462 & 10.880 & sdss j135242.72 - 005708.23 & 0.147386 & sdss j135242.00 - 005706.90 & - + 1055 & 13:52:59.40 & -00:43:22.18 & 20.357 & 18.693 & 17.773 & 17.417 & 17.089 & 3.624 & sdss j135259.52 - 004321.97 & - & sdss j135259.28 - 004322.39 & - + 1056 & 13:53:17.88 & + 00:50:07.95 & 20.624 & 18.451 & 17.332 & 16.878 & 16.478 & 3.606 & sdss j135317.76 + 005008.06 & 0.116065 & sdss j135318.00 + 005007.85 & - + 1057 & 13:53:18.48 & -00:10:16.20 & 20.238 & 18.553 & 17.417 & 16.919 & 16.540 & 7.202 & sdss j135318.72 - 001016.29 & - & sdss j135318.24 - 001016.11 & 0.188526 + 1058 & 13:54:08.64 & + 00:37:28.30 & 19.757 & 18.940 & 18.569 & 18.236 & 18.355 & 1.166 & sdss j135408.64 + 003727.72 & - & sdss j135408.64 + 003728.88 & - + 1059 & 13:54:21.24 & + 00:29:28.98 & 20.470 & 18.906 & 17.770 & 17.251 & 16.915 & 3.771 & sdss j135421.12 + 002929.55 & - & sdss j135421.36 + 002928.42 & - + 1060 & 13:55:57.96 & + 00:15:28.45 & 19.037 & 17.620 & 16.824 & 16.411 & 16.179 & 5.637 & sdss j135557.84 + 001526.28 & - & sdss j135558.08 + 001530.62 & 0.133310 + 1061 & 13:57:03.36 & + 01:05:34.33 & 18.917 & 17.392 & 16.486 & 16.035 & 15.671 & 11.191 & sdss j135703.12 + 010530.04 & - & sdss j135703.60 + 010538.61 & 0.103872 + 1062 & 13:57:35.52 & -00:08:36.09 & 18.241 & 17.217 & 16.958 & 16.810 & 16.654 & 7.253 & sdss j135735.76 - 000835.66 & 0.029418 & sdss j135735.28 - 000836.53 & - + 1063 & 13:57:51.60 & -01:00:27.18 & 20.176 & 18.206 & 16.932 & 16.409 & 16.069 & 4.320 & sdss j135751.60 - 010029.34 & 0.191559 & sdss j135751.60 - 010025.02 & - + 1064 & 13:58:22.68 & + 00:05:42.48 & 21.029 & 19.432 & 18.170 & 17.709 & 17.415 & 3.759 & sdss j135822.80 + 000543.02 & - & sdss j135822.56 + 000541.94 & - + 1065 & 13:58:25.08 & + 00:02:27.08 & 20.459 & 19.180 & 18.513 & 18.018 & 17.965 & 5.379 & sdss j135825.20 + 000225.08 & - & sdss j135824.96 + 000229.08 & - + 1066 & 13:58:27.12 & -00:35:00.53 & 20.244 & 18.292 & 17.239 & 16.774 & 16.341 & 6.055 & sdss j135827.12 - 003457.50 & 0.131371 & sdss j135827.12 - 003503.55 & - + 1067 & 13:58:41.64 & + 00:14:58.96 & 18.098 & 16.899 & 16.384 & 16.142 & 15.985 & 16.738 & sdss j135841.28 + 001505.36 & 0.032489 & sdss j135842.00 + 001452.57 & - + 1068 & 14:00:19.44 & -00:09:43.63 & 20.773 & 19.580 & 19.215 & 19.065 & 18.789 & 3.362 & sdss j140019.44 - 000941.95 & - & sdss j140019.44 - 000945.32 & - + 1069 & 14:00:44.64 & + 00:41:40.51 & 18.526 & 16.712 & 15.906 & 15.495 & 15.208 & 5.238 & sdss j140044.64 + 004143.13 & 0.043029 & sdss j140044.64 + 004137.89 & - + 1070 & 14:00:47.64 & -00:02:19.07 & 19.715 & 18.305 & 17.825 & 17.604 & 17.489 & 5.145 & sdss j140047.76 - 000217.23 & - & sdss j140047.52 - 000220.90 & - + 1071 & 14:01:07.68 & -00:40:51.51 & 19.093 & 18.316 & 18.306 & 18.597 & 18.639 & 2.365 & sdss j140107.68 - 004050.33 & - & sdss j140107.68 - 004052.70 & - + 1072 & 14:04:21.96 & + 00:25:19.00 & 20.399 & 19.456 & 18.652 & 18.253 & 18.028 & 4.245 & sdss j140421.84 + 002520.12 & - & sdss j140422.08 + 002517.87 & - + 1073 & 14:04:24.84 & -00:02:19.13 & 20.118 & 18.721 & 18.147 & 17.767 & 17.649 & 3.600 & sdss j140424.96 - 000219.16 & - & sdss j140424.72 - 000219.11 & - + 1074 & 14:05:00.12 & + 00:50:51.47 & 17.893 & 16.696 & 16.458 & 16.221 & 16.210 & 6.622 & sdss j140500.24 + 005054.25 & 0.069518 & sdss j140500.00 + 005048.69 & - + 1075 & 14:05:18.72 & -00:34:15.64 & 18.778 & 17.889 & 17.580 & 17.373 & 17.132 & 7.972 & sdss j140518.48 - 003413.93 & - & sdss j140518.96 - 003417.36 & - + 1076 & 14:05:30.60 & -00:21:33.39 & 21.014 & 18.345 & 17.103 & 16.613 & 16.233 & 7.060 & sdss j140530.72 - 002136.43 & - & sdss j140530.48 - 002130.35 & - + 1077 & 14:07:18.48 & -00:00:12.47 & 20.145 & 19.133 & 18.678 & 18.409 & 18.412 & 6.165 & sdss j140718.48 - 000009.39 & - & sdss j140718.48 - 000015.55 & - + 1078 & 14:07:34.44 & -00:24:32.16 & 20.403 & 19.023 & 17.973 & 17.453 & 17.159 & 5.241 & sdss j140734.32 - 002434.07 & - & sdss j140734.56 - 002430.26 & - + 1079 & 14:08:19.32 & + 00:37:18.22 & 18.050 & 17.327 & 17.193 & 17.180 & 17.084 & 6.750 & sdss j140819.20 + 003721.07 & - & sdss j140819.44 + 003715.36 & - + 1080 & 14:10:27.00 & -00:26:51.80 & 20.313 & 18.713 & 17.790 & 17.323 & 17.031 & 5.165 & sdss j141027.12 - 002653.65 & - & sdss j141026.88 - 002649.94 & - + 1081 & 14:10:34.92 & -00:48:02.28 & 20.248 & 19.148 & 18.595 & 18.274 & 18.213 & 4.748 & sdss j141034.80 - 004803.83 & - & sdss j141035.04 - 004800.73 & - + 1082 & 14:10:55.80 & + 00:36:49.14 & 19.633 & 17.770 & 16.566 & 16.092 & 15.721 & 5.643 & sdss j141055.92 + 003646.97 & 0.178255 & sdss j141055.68 + 003651.31 & - + 1083 & 14:11:32.28 & + 00:27:57.21 & 19.400 & 17.465 & 16.292 & 15.870 & 15.506 & 3.675 & sdss j141132.40 + 002756.84 & 0.144597 & sdss j141132.16 + 002757.58 & 0.255106 + 1084 & 14:12:09.36 & -00:50:05.12 & 19.532 & 18.283 & 17.187 & 16.744 & 16.478 & 4.910 & sdss j141209.36 - 005007.58 & - & sdss j141209.36 - 005002.67 & - + 1085 & 14:12:12.36 & + 00:00:17.10 & 20.244 & 18.509 & 17.516 & 17.028 & 16.724 & 4.054 & sdss j141212.24 + 000016.17 & - & sdss j141212.48 + 000018.03 & - + 1086 & 14:12:24.96 & -00:37:35.50 & 19.806 & 17.468 & 16.522 & 16.040 & 15.741 & 7.974 & sdss j141224.96 - 003739.49 & 0.135613 & sdss j141224.96 - 003731.51 & - + 1087 & 14:12:35.40 & + 00:44:32.66 & 20.392 & 18.799 & 17.572 & 17.115 & 16.670 & 5.723 & sdss j141235.28 + 004430.43 & - & sdss j141235.52 + 004434.88 & - + 1088 & 14:12:51.96 & -01:02:29.47 & 18.178 & 16.520 & 15.743 & 15.444 & 15.341 & 12.344 & sdss j141251.84 - 010235.37 & - & sdss j141252.08 - 010223.56 & - + 1089 & 14:13:00.36 & + 00:01:10.04 & 19.887 & 18.693 & 18.073 & 17.714 & 17.540 & 4.843 & sdss j141300.24 + 000108.42 & - & sdss j141300.48 + 000111.66 & - + 1090 & 14:13:14.04 & -00:49:41.49 & 19.483 & 18.435 & 17.631 & 17.472 & 17.314 & 4.660 & sdss j141314.16 - 004940.01 & - & sdss j141313.92 - 004942.97 & - + 1091 & 14:13:55.80 & -01:00:00.70 & 20.128 & 18.138 & 16.772 & 16.256 & 15.989 & 4.172 & sdss j141355.68 - 010001.76 & 0.226098 & sdss j141355.92 - 005959.65 & - + 1092 & 14:14:29.16 & -00:22:29.72 & 19.308 & 17.145 & 15.991 & 15.572 & 15.121 & 3.831 & sdss j141429.28 - 002229.06 & 0.136033 & sdss j141429.04 - 002230.37 & - + 1093 & 14:14:34.20 & -00:21:39.14 & 20.158 & 18.484 & 17.687 & 17.363 & 17.042 & 3.600 & sdss j141434.32 - 002139.11 & - & sdss j141434.08 - 002139.17 & - + 1094 & 14:14:47.28 & -00:00:12.28 & 17.678 & 16.210 & 15.412 & 14.988 & 14.652 & 7.471 & sdss j141447.04 - 000013.28 & 0.047497 & sdss j141447.52 - 000011.29 & 0.047335 + 1095 & 14:14:58.80 & -00:12:48.82 & 19.075 & 18.082 & 17.901 & 17.733 & 17.775 & 7.798 & sdss j141459.04 - 001250.32 & - & sdss j141458.56 - 001247.32 & - + 1096 & 14:15:45.72 & + 00:57:26.91 & 19.958 & 18.425 & 17.521 & 16.996 & 16.611 & 5.259 & sdss j141545.84 + 005728.83 & - & sdss j141545.60 + 005725.00 & - + 1097 & 14:16:01.80 & + 00:16:26.72 & 18.924 & 16.832 & 15.695 & 15.317 & 14.899 & 18.781 & sdss j141602.16 + 001634.41 & - & sdss j141601.44 + 001619.04 & - + 1098 & 14:16:18.12 & + 00:42:20.67 & 19.057 & 18.003 & 17.319 & 16.936 & 16.737 & 5.732 & sdss j141618.24 + 004222.90 & - & sdss j141618.00 + 004218.44 & - + 1099 & 14:16:37.08 & -00:30:19.76 & 20.706 & 18.511 & 17.285 & 16.784 & 16.418 & 4.158 & sdss j141636.96 - 003020.80 & - & sdss j141637.20 - 003018.72 & - + 1100 & 14:16:44.88 & -00:01:17.12 & 19.779 & 17.616 & 16.545 & 16.103 & 15.733 & 9.173 & sdss j141644.64 - 000119.96 & 0.124650 & sdss j141645.12 - 000114.28 & - + 1101 & 14:17:13.08 & + 00:32:03.05 & 18.363 & 16.495 & 15.671 & 15.246 & 14.933 & 7.545 & sdss j141712.96 + 003159.73 & 0.077200 & sdss j141713.20 + 003206.37 & 0.077097 + 1102 & 14:17:33.00 & -00:35:06.50 & 20.542 & 18.502 & 17.370 & 16.905 & 16.499 & 6.921 & sdss j141733.12 - 003509.45 & 0.147796 & sdss j141732.88 - 003503.54 & - + 1103 & 14:17:51.48 & -00:18:34.21 & 18.847 & 17.276 & 16.392 & 15.984 & 15.637 & 6.161 & sdss j141751.36 - 001836.71 & 0.123036 & sdss j141751.60 - 001831.71 & - + 1104 & 14:18:01.92 & + 00:29:01.23 & 18.519 & 16.730 & 15.851 & 15.424 & 15.102 & 8.236 & sdss j141802.16 + 002903.23 & 0.052777 & sdss j141801.68 + 002859.23 & 0.052611 + 1105 & 14:19:08.52 & -00:13:51.15 & 19.697 & 17.994 & 16.840 & 16.474 & 16.025 & 7.905 & sdss j141908.64 - 001347.63 & 0.185066 & sdss j141908.40 - 001354.67 & - + 1106 & 14:19:18.48 & + 00:03:31.62 & 18.321 & 17.205 & 16.656 & 16.278 & 16.032 & 7.561 & sdss j141918.48 + 000327.84 & 0.096980 & sdss j141918.48 + 000335.40 & - + 1107 & 14:19:57.36 & -00:28:53.83 & 19.014 & 17.173 & 16.052 & 15.594 & 15.213 & 11.992 & sdss j141957.12 - 002858.62 & - & sdss j141957.60 - 002849.03 & 0.138488 + 1108 & 14:20:56.64 & -00:04:27.69 & 17.950 & 16.424 & 15.649 & 15.207 & 14.896 & 7.648 & sdss j142056.64 - 000423.87 & 0.102018 & sdss j142056.64 - 000431.52 & - + 1109 & 14:21:06.60 & + 00:57:12.95 & 20.161 & 17.971 & 16.727 & 16.222 & 15.934 & 3.843 & sdss j142106.48 + 005712.28 & - & sdss j142106.72 + 005713.62 & 0.168777 + 1110 & 14:21:58.92 & -00:35:22.63 & 19.260 & 17.419 & 16.508 & 16.060 & 15.685 & 6.430 & sdss j142159.04 - 003525.29 & 0.050993 & sdss j142158.80 - 003519.97 & - + 1111 & 14:22:10.68 & + 00:23:07.00 & 20.260 & 19.077 & 18.204 & 17.791 & 17.527 & 3.752 & sdss j142210.56 + 002306.47 & - & sdss j142210.80 + 002307.53 & - + 1112 & 14:22:33.12 & + 01:04:10.93 & 20.883 & 18.463 & 17.399 & 17.012 & 16.589 & 15.575 & sdss j142233.60 + 010407.96 & 0.117348 & sdss j142232.64 + 010413.90 & - + 1113 & 14:23:58.80 & + 00:43:53.02 & 19.611 & 18.755 & 18.272 & 18.063 & 17.955 & 3.661 & sdss j142358.80 + 004354.85 & - & sdss j142358.80 + 004351.18 & - + 1114 & 14:24:10.80 & + 00:37:10.79 & 18.595 & 17.372 & 16.707 & 16.350 & 16.113 & 7.305 & sdss j142411.04 + 003711.41 & 0.102991 & sdss j142410.56 + 003710.17 & - + 1115 & 14:24:17.40 & -00:12:16.87 & 19.297 & 18.205 & 17.650 & 17.271 & 17.050 & 4.619 & sdss j142417.28 - 001215.42 & 0.084204 & sdss j142417.52 - 001218.32 & - + 1116 & 14:24:17.76 & -00:17:04.25 & 19.903 & 18.603 & 17.744 & 17.364 & 17.228 & 4.619 & sdss j142417.76 - 001706.56 & - & sdss j142417.76 - 001701.94 & - + 1117 & 14:24:34.32 & -00:43:38.34 & 20.343 & 19.191 & 18.135 & 17.692 & 17.306 & 3.028 & sdss j142434.32 - 004336.82 & - & sdss j142434.32 - 004339.85 & - + 1118 & 14:25:03.12 & + 00:50:24.82 & 20.263 & 18.428 & 17.279 & 16.758 & 16.504 & 3.672 & sdss j142503.12 + 005026.66 & 0.157975 & sdss j142503.12 + 005022.99 & - + 1119 & 14:25:27.48 & + 00:20:17.96 & 19.084 & 17.063 & 15.956 & 15.541 & 15.218 & 5.228 & sdss j142527.60 + 002016.06 & 0.134251 & sdss j142527.36 + 002019.85 & - + 1120 & 14:25:28.68 & -00:01:22.54 & 17.730 & 16.353 & 15.677 & 15.287 & 15.111 & 3.604 & sdss j142528.80 - 000122.63 & 0.054873 & sdss j142528.56 - 000122.45 & - + 1121 & 14:25:33.48 & -00:33:00.58 & 19.292 & 18.243 & 17.888 & 17.722 & 17.640 & 4.822 & sdss j142533.60 - 003258.98 & - & sdss j142533.36 - 003302.19 & - + 1122 & 14:25:41.28 & + 00:20:48.42 & 18.807 & 17.417 & 16.552 & 16.228 & 15.961 & 3.413 & sdss j142541.28 + 002046.71 & 0.131009 & sdss j142541.28 + 002050.13 & - + 1123 & 14:25:53.40 & + 00:34:51.32 & 17.976 & 16.136 & 14.750 & 14.350 & 13.887 & 5.825 & sdss j142553.52 + 003449.03 & 0.128967 & sdss j142553.28 + 003453.61 & - + 1124 & 14:27:21.36 & + 00:11:05.78 & 19.364 & 18.418 & 18.107 & 17.834 & 17.835 & 8.374 & sdss j142721.12 + 001103.64 & - & sdss j142721.60 + 001107.92 & - + 1125 & 14:27:27.12 & -00:58:45.67 & 18.481 & 17.537 & 16.979 & 17.211 & 17.044 & 3.092 & sdss j142727.12 - 005844.13 & - & sdss j142727.12 - 005847.22 & - + 1126 & 14:27:55.20 & -00:33:43.47 & 17.695 & 16.304 & 15.676 & 15.187 & 14.896 & 7.900 & sdss j142754.96 - 003345.09 & 0.079141 & sdss j142755.44 - 003341.84 & 0.079464 + 1127 & 14:28:28.44 & + 00:56:08.00 & 18.075 & 16.772 & 15.962 & 15.679 & 15.371 & 6.649 & sdss j142828.32 + 005605.21 & 0.114831 & sdss j142828.56 + 005610.80 & 0.136004 + 1128 & 14:28:46.20 & -00:02:43.54 & 18.180 & 17.244 & 16.544 & 16.212 & 15.983 & 5.491 & sdss j142846.32 - 000245.61 & 0.184273 & sdss j142846.08 - 000241.47 & - + 1129 & 14:28:54.12 & -00:55:02.92 & 20.041 & 18.826 & 18.098 & 17.747 & 17.450 & 5.053 & sdss j142854.24 - 005501.14 & - & sdss j142854.00 - 005504.69 & - + 1130 & 14:29:28.68 & + 00:44:56.32 & 20.617 & 19.115 & 18.226 & 17.845 & 17.486 & 4.098 & sdss j142928.56 + 004455.34 & - & sdss j142928.80 + 004457.30 & - + 1131 & 14:29:57.72 & -00:00:58.86 & 20.322 & 18.808 & 17.915 & 17.525 & 17.219 & 3.606 & sdss j142957.60 - 000058.75 & - & sdss j142957.84 - 000058.96 & - + 1132 & 14:29:57.96 & + 00:55:10.49 & 20.887 & 18.887 & 17.799 & 17.284 & 16.949 & 4.305 & sdss j142957.84 + 005509.31 & - & sdss j142958.08 + 005511.67 & - + 1133 & 14:30:02.04 & + 00:39:27.40 & 19.255 & 18.123 & 17.626 & 17.229 & 17.031 & 4.950 & sdss j143002.16 + 003925.70 & - & sdss j143001.92 + 003929.10 & - + 1134 & 14:30:09.36 & + 00:34:49.27 & 18.429 & 17.054 & 16.138 & 15.758 & 15.440 & 8.884 & sdss j143009.60 + 003451.87 & 0.135817 & sdss j143009.12 + 003446.67 & - + 1135 & 14:30:11.40 & -01:02:29.07 & 18.721 & 17.893 & 17.530 & 17.432 & 17.444 & 3.962 & sdss j143011.52 - 010229.90 & - & sdss j143011.28 - 010228.24 & 0.029840 + 1136 & 14:30:18.84 & + 00:43:37.27 & 20.255 & 18.584 & 17.662 & 17.201 & 16.958 & 3.600 & sdss j143018.72 + 004337.25 & - & sdss j143018.96 + 004337.28 & - + 1137 & 14:30:19.80 & + 00:22:22.30 & 19.475 & 18.180 & 17.490 & 17.185 & 17.071 & 3.713 & sdss j143019.68 + 002221.84 & 0.132168 & sdss j143019.92 + 002222.76 & - + 1138 & 14:30:30.36 & + 00:30:27.77 & 19.773 & 18.439 & 17.793 & 17.400 & 17.173 & 5.111 & sdss j143030.24 + 003025.96 & - & sdss j143030.48 + 003029.59 & - + 1139 & 14:30:34.20 & -00:18:12.24 & 19.659 & 17.893 & 16.855 & 16.390 & 16.018 & 6.397 & sdss j143034.08 - 001809.60 & 0.131204 & sdss j143034.32 - 001814.89 & - + 1140 & 14:30:44.76 & -00:02:21.65 & 19.760 & 18.276 & 17.537 & 17.114 & 16.800 & 12.187 & sdss j143044.88 - 000215.83 & 0.087590 & sdss j143044.64 - 000227.48 & - + 1141 & 14:30:45.72 & + 00:29:07.01 & 20.366 & 18.711 & 17.687 & 17.173 & 16.782 & 4.081 & sdss j143045.60 + 002906.05 & - & sdss j143045.84 + 002907.97 & - + 1142 & 14:30:48.12 & -00:10:34.33 & 18.833 & 17.557 & 16.917 & 16.561 & 16.179 & 6.863 & sdss j143048.00 - 001031.41 & - & sdss j143048.24 - 001037.26 & - + 1143 & 14:30:48.12 & + 00:42:27.26 & 19.833 & 18.038 & 17.106 & 16.676 & 16.389 & 5.930 & sdss j143048.00 + 004224.91 & 0.130450 & sdss j143048.24 + 004229.62 & - + 1144 & 14:30:51.72 & -00:19:56.60 & 20.570 & 19.199 & 18.138 & 17.733 & 17.340 & 5.272 & sdss j143051.60 - 001958.53 & - & sdss j143051.84 - 001954.67 & - + 1145 & 14:30:56.64 & + 00:44:40.76 & 20.169 & 18.128 & 16.982 & 16.504 & 16.160 & 3.380 & sdss j143056.64 + 004439.07 & 0.135620 & sdss j143056.64 + 004442.45 & - + 1146 & 14:31:02.76 & + 00:47:35.54 & 18.685 & 17.061 & 16.071 & 15.590 & 15.256 & 5.996 & sdss j143102.64 + 004737.93 & 0.136035 & sdss j143102.88 + 004733.14 & - + 1147 & 14:31:07.08 & -00:28:39.99 & 20.655 & 19.263 & 18.389 & 17.952 & 17.694 & 4.444 & sdss j143107.20 - 002838.69 & - & sdss j143106.96 - 002841.29 & - + 1148 & 14:31:51.48 & + 00:48:43.69 & 19.319 & 18.241 & 17.599 & 17.208 & 16.972 & 5.134 & sdss j143151.36 + 004841.86 & - & sdss j143151.60 + 004845.52 & - + 1149 & 14:31:53.16 & + 00:22:29.75 & 19.686 & 18.864 & 18.236 & 17.943 & 17.612 & 5.473 & sdss j143153.28 + 002231.81 & - & sdss j143153.04 + 002227.69 & - + 1150 & 14:32:16.20 & + 00:22:46.67 & 17.975 & 16.830 & 16.336 & 16.082 & 16.094 & 3.664 & sdss j143216.08 + 002246.33 & - & sdss j143216.32 + 002247.01 & 0.035096 + 1151 & 14:33:10.68 & -00:34:34.14 & 19.248 & 18.089 & 17.749 & 17.573 & 18.201 & 3.635 & sdss j143310.56 - 003433.89 & - & sdss j143310.80 - 003434.40 & - + 1152 & 14:33:10.80 & -00:08:07.59 & 19.276 & 17.269 & 16.134 & 15.656 & 15.285 & 7.213 & sdss j143310.56 - 000807.37 & - & sdss j143311.04 - 000807.81 & 0.136818 + 1153 & 14:33:11.64 & -00:26:43.89 & 19.336 & 17.408 & 16.398 & 15.986 & 15.611 & 16.103 & sdss j143312.00 - 002649.86 & 0.106039 & sdss j143311.28 - 002637.91 & - + 1154 & 14:33:33.60 & + 00:49:47.11 & 20.177 & 18.724 & 17.708 & 17.353 & 17.085 & 4.453 & sdss j143333.60 + 004949.34 & - & sdss j143333.60 + 004944.88 & - + 1155 & 14:33:44.76 & + 00:47:42.17 & 18.913 & 16.678 & 15.586 & 15.136 & 14.763 & 3.682 & sdss j143344.88 + 004741.79 & 0.128086 & sdss j143344.64 + 004742.56 & 0.128096 + 1156 & 14:33:51.36 & + 00:46:25.31 & 18.477 & 16.959 & 15.894 & 15.586 & 15.256 & 8.658 & sdss j143351.36 + 004620.98 & 0.132673 & sdss j143351.36 + 004629.64 & - + 1157 & 14:34:16.92 & + 00:53:02.17 & 17.885 & 16.642 & 15.959 & 15.672 & 15.424 & 4.550 & sdss j143417.04 + 005300.78 & 0.126609 & sdss j143416.80 + 005303.56 & - + 1158 & 14:35:33.36 & -00:11:38.16 & 19.805 & 17.874 & 16.774 & 16.331 & 15.954 & 9.268 & sdss j143533.60 - 001135.25 & 0.138918 & sdss j143533.12 - 001141.08 & - + 1159 & 14:35:43.32 & + 00:02:23.79 & 21.011 & 19.098 & 18.001 & 17.499 & 17.158 & 3.689 & sdss j143543.44 + 000223.39 & 0.132200 & sdss j143543.20 + 000224.20 & - + 1160 & 14:36:12.24 & -00:14:59.15 & 19.334 & 17.954 & 16.811 & 16.348 & 16.131 & 1.818 & sdss j143612.24 - 001458.24 & - & sdss j143612.24 - 001500.06 & - + 1161 & 14:36:23.04 & -00:35:02.23 & 18.019 & 16.853 & 16.311 & 15.897 & 15.622 & 6.077 & sdss j143623.04 - 003505.27 & 0.081981 & sdss j143623.04 - 003459.19 & - + 1162 & 14:36:47.04 & + 00:43:07.26 & 18.290 & 16.196 & 15.295 & 14.859 & 14.440 & 10.818 & sdss j143646.80 + 004311.30 & - & sdss j143647.28 + 004303.23 & - + 1163 & 14:36:53.88 & + 00:20:34.77 & 19.375 & 18.533 & 18.202 & 17.951 & 17.893 & 4.612 & sdss j143653.76 + 002033.33 & - & sdss j143654.00 + 002036.21 & - + 1164 & 14:37:29.52 & -00:52:45.45 & 18.184 & 16.447 & 15.487 & 15.027 & 14.733 & 7.254 & sdss j143729.52 - 005249.08 & 0.121140 & sdss j143729.52 - 005241.82 & - + 1165 & 14:37:57.60 & -00:33:59.40 & 19.818 & 18.716 & 18.206 & 17.868 & 17.833 & 4.396 & sdss j143757.60 - 003401.60 & - & sdss j143757.60 - 003357.21 & - + 1166 & 14:38:34.68 & -00:36:32.53 & 20.958 & 20.228 & 19.498 & 19.123 & 18.902 & 4.219 & sdss j143834.80 - 003631.43 & - & sdss j143834.56 - 003633.63 & - + 1167 & 14:39:02.76 & -00:38:07.36 & 19.624 & 17.216 & 16.024 & 15.524 & 15.334 & 3.714 & sdss j143902.88 - 003806.90 & - & sdss j143902.64 - 003807.81 & 0.137116 + 1168 & 14:39:27.72 & + 00:32:54.80 & 20.097 & 18.002 & 16.908 & 16.409 & 15.981 & 4.349 & sdss j143927.84 + 003256.02 & 0.149700 & sdss j143927.60 + 003253.58 & - + 1169 & 14:39:41.52 & + 00:30:28.84 & 20.085 & 18.516 & 17.591 & 17.177 & 16.847 & 5.116 & sdss j143941.52 + 003026.29 & 0.137489 & sdss j143941.52 + 003031.40 & - + 1170 & 14:39:44.64 & + 00:24:51.17 & 20.239 & 18.490 & 17.410 & 16.904 & 16.677 & 1.973 & sdss j143944.64 + 002450.18 & - & sdss j143944.64 + 002452.16 & - + 1171 & 14:40:11.76 & -00:45:10.18 & 18.726 & 17.515 & 16.746 & 16.257 & 16.038 & 3.294 & sdss j144011.76 - 004511.82 & 0.178927 & sdss j144011.76 - 004508.53 & - + 1172 & 14:40:14.88 & + 00:12:23.30 & 18.175 & 16.395 & 16.006 & 15.861 & 15.885 & 14.518 & sdss j144015.36 + 001224.22 & 0.006198 & sdss j144014.40 + 001222.38 & - + 1173 & 14:42:41.88 & -00:38:07.21 & 19.508 & 17.950 & 17.121 & 16.641 & 16.389 & 4.683 & sdss j144241.76 - 003805.71 & 0.150468 & sdss j144242.00 - 003808.71 & - + 1174 & 14:42:41.88 & -00:38:07.78 & 19.483 & 18.075 & 17.215 & 16.753 & 16.479 & 5.478 & sdss j144241.76 - 003805.71 & 0.150468 & sdss j144242.00 - 003809.84 & - + 1175 & 14:42:45.72 & -00:05:11.29 & 17.773 & 16.434 & 15.557 & 15.317 & 15.088 & 4.884 & sdss j144245.60 - 000509.64 & 0.103216 & sdss j144245.84 - 000512.94 & - + 1176 & 14:43:04.68 & -00:39:06.75 & 18.688 & 17.192 & 16.230 & 15.779 & 15.682 & 4.323 & sdss j144304.56 - 003905.56 & 0.152385 & sdss j144304.80 - 003907.95 & - + 1177 & 14:43:58.68 & + 00:51:31.61 & 20.576 & 19.079 & 18.034 & 17.602 & 17.262 & 4.181 & sdss j144358.80 + 005130.55 & - & sdss j144358.56 + 005132.68 & - + 1178 & 14:44:49.32 & + 00:00:57.83 & 19.272 & 18.236 & 17.696 & 17.331 & 17.159 & 4.442 & sdss j144449.44 + 000056.53 & 0.198234 & sdss j144449.20 + 000059.13 & - + 1179 & 14:44:55.44 & + 00:00:31.93 & 20.691 & 19.613 & 18.772 & 18.827 & 18.022 & 3.341 & sdss j144455.44 + 000033.60 & - & sdss j144455.44 + 000030.26 & - + 1180 & 14:46:08.88 & + 00:51:53.67 & 17.209 & 16.238 & 15.651 & 15.245 & 15.264 & 8.361 & sdss j144608.64 + 005151.54 & - & sdss j144609.12 + 005155.80 & - + 1181 & 14:47:47.64 & -00:32:24.27 & 19.822 & 18.915 & 18.168 & 17.784 & 17.503 & 4.690 & sdss j144747.76 - 003225.78 & 0.255500 & sdss j144747.52 - 003222.77 & - + 1182 & 14:48:28.44 & -00:22:05.91 & 20.742 & 18.862 & 17.356 & 16.840 & 16.481 & 3.806 & sdss j144828.56 - 002205.29 & 0.217700 & sdss j144828.32 - 002206.52 & - + 1183 & 14:50:59.16 & -00:02:05.73 & 17.858 & 15.739 & 14.934 & 14.482 & 14.194 & 23.325 & sdss j145059.76 - 000213.15 & 0.042884 & sdss j145058.56 - 000158.32 & 0.044600 + 1184 & 14:51:46.92 & -00:56:42.62 & 17.935 & 17.266 & 17.557 & 17.398 & 17.530 & 4.152 & sdss j145147.04 - 005643.65 & 0.043278 & sdss j145146.80 - 005641.58 & - + 1185 & 14:51:48.96 & + 00:46:33.26 & 20.457 & 19.710 & 19.243 & 18.901 & 18.863 & 3.366 & sdss j145148.96 + 004634.95 & - & sdss j145148.96 + 004631.58 & - + 1186 & 14:51:55.80 & -00:44:19.89 & 19.649 & 18.979 & 18.441 & 18.006 & 17.827 & 4.867 & sdss j145155.92 - 004421.53 & - & sdss j145155.68 - 004418.26 & - + 1187 & 14:53:13.56 & + 00:42:45.89 & 20.563 & 18.330 & 17.106 & 16.580 & 16.194 & 3.622 & sdss j145313.44 + 004245.69 & 0.171204 & sdss j145313.68 + 004246.09 & - + 1188 & 14:53:22.80 & -00:16:44.21 & 18.775 & 17.508 & 16.831 & 16.364 & 16.096 & 3.791 & sdss j145322.80 - 001642.32 & 0.075784 & sdss j145322.80 - 001646.11 & - + 1189 & 14:54:52.92 & + 00:41:38.39 & 18.515 & 17.576 & 16.835 & 16.693 & 16.558 & 5.999 & sdss j145453.04 + 004140.79 & - & sdss j145452.80 + 004135.99 & - + 1190 & 14:55:03.96 & + 00:11:14.69 & 21.420 & 19.601 & 18.640 & 18.155 & 17.945 & 4.149 & sdss j145504.08 + 001113.66 & - & sdss j145503.84 + 001115.72 & - + 1191 & 14:55:21.12 & + 00:11:25.69 & 20.428 & 18.532 & 17.298 & 16.755 & 16.399 & 7.879 & sdss j145520.88 + 001124.09 & 0.185717 & sdss j145521.36 + 001127.29 & - + 1192 & 14:55:27.36 & + 00:03:16.28 & 19.005 & 17.096 & 16.006 & 15.513 & 15.152 & 7.777 & sdss j145527.36 + 000312.39 & - & sdss j145527.36 + 000320.17 & - + 1193 & 14:56:05.88 & -00:13:32.24 & 20.842 & 19.361 & 18.776 & 18.588 & 18.385 & 3.605 & sdss j145606.00 - 001332.14 & - & sdss j145605.76 - 001332.33 & - + 1194 & 14:57:15.00 & + 00:25:30.25 & 21.010 & 19.034 & 17.894 & 17.317 & 16.991 & 5.811 & sdss j145714.88 + 002527.97 & - & sdss j145715.12 + 002532.53 & - + 1195 & 14:57:52.20 & + 00:34:05.72 & 18.624 & 17.905 & 17.774 & 17.590 & 17.528 & 4.313 & sdss j145752.32 + 003406.91 & - & sdss j145752.08 + 003404.54 & - + 1196 & 14:58:20.76 & + 00:23:19.88 & 19.507 & 17.735 & 16.547 & 16.094 & 15.856 & 4.941 & sdss j145820.64 + 002321.57 & - & sdss j145820.88 + 002318.18 & - + 1197 & 14:59:11.04 & -00:05:18.31 & 18.057 & 16.888 & 16.468 & 16.233 & 16.165 & 4.511 & sdss j145911.04 - 000520.57 & - & sdss j145911.04 - 000516.05 & 0.076137 + 1198 & 14:59:45.48 & -00:37:36.05 & 19.094 & 18.088 & 17.855 & 17.694 & 17.670 & 5.448 & sdss j145945.36 - 003738.10 & - & sdss j145945.60 - 003734.01 & - + 1199 & 14:59:53.28 & -00:37:09.59 & 17.459 & 16.479 & 15.584 & 16.023 & 15.768 & 17.422 & sdss j145953.04 - 003701.66 & - & sdss j145953.52 - 003717.52 & - + 1200 & 15:00:15.12 & -00:53:49.37 & 20.673 & 18.561 & 17.464 & 17.016 & 16.694 & 1.944 & sdss j150015.12 - 005350.34 & 0.133954 & sdss j150015.12 - 005348.40 & - + 1201 & 15:00:35.04 & + 00:48:52.35 & 19.634 & 18.504 & 17.780 & 17.375 & 17.126 & 2.016 & sdss j150035.04 + 004851.34 & - & sdss j150035.04 + 004853.35 & - + 1202 & 15:00:58.68 & + 00:49:34.68 & 20.120 & 18.524 & 17.481 & 17.024 & 16.679 & 4.623 & sdss j150058.56 + 004936.13 & - & sdss j150058.80 + 004933.22 & - + 1203 & 15:02:29.88 & + 00:07:40.05 & 18.235 & 16.703 & 16.122 & 15.669 & 15.439 & 4.776 & sdss j150229.76 + 000741.62 & - & sdss j150230.00 + 000738.48 & 0.086077 + 1204 & 15:03:07.44 & -00:25:43.59 & 20.976 & 19.265 & 17.846 & 17.301 & 16.880 & 6.408 & sdss j150307.44 - 002546.80 & - & sdss j150307.44 - 002540.39 & - + 1205 & 15:03:55.92 & + 00:25:51.11 & 16.228 & 15.761 & 15.781 & 15.889 & 15.778 & 11.599 & sdss j150355.68 + 002555.65 & 0.005273 & sdss j150356.16 + 002546.56 & 0.005242 + 1206 & 15:05:15.24 & -00:37:21.88 & 20.500 & 19.056 & 18.203 & 17.679 & 17.443 & 5.111 & sdss j150515.36 - 003723.70 & - & sdss j150515.12 - 003720.07 & - + 1207 & 15:05:37.68 & + 00:37:11.42 & 21.183 & 19.547 & 18.400 & 17.834 & 17.467 & 2.437 & sdss j150537.68 + 003712.64 & - & sdss j150537.68 + 003710.21 & - + 1208 & 15:05:45.36 & + 00:49:37.71 & 20.007 & 18.286 & 17.265 & 16.843 & 16.420 & 4.414 & sdss j150545.36 + 004939.91 & 0.114892 & sdss j150545.36 + 004935.50 & - + 1209 & 15:06:32.76 & -00:51:00.78 & 19.545 & 18.165 & 17.487 & 17.109 & 16.881 & 7.397 & sdss j150632.64 - 005104.01 & - & sdss j150632.88 - 005057.55 & - + 1210 & 15:06:46.68 & + 00:14:48.50 & 19.870 & 18.757 & 18.279 & 18.010 & 17.949 & 3.721 & sdss j150646.56 + 001448.03 & - & sdss j150646.80 + 001448.98 & - + 1211 & 15:07:57.36 & + 00:29:36.40 & 20.036 & 18.410 & 17.333 & 16.819 & 16.417 & 7.255 & sdss j150757.60 + 002935.95 & - & sdss j150757.12 + 002936.85 & - + 1212 & 15:08:12.84 & -00:21:45.27 & 18.933 & 17.253 & 16.241 & 15.667 & 15.259 & 10.778 & sdss j150812.96 - 002150.34 & 0.092863 & sdss j150812.72 - 002140.19 & - + 1213 & 15:08:33.00 & + 00:54:48.78 & 19.637 & 18.154 & 17.301 & 16.855 & 16.659 & 4.508 & sdss j150833.12 + 005450.13 & 0.126304 & sdss j150832.88 + 005447.42 & - + 1214 & 15:08:50.40 & -00:23:53.44 & 18.411 & 16.569 & 15.651 & 15.163 & 14.823 & 12.050 & sdss j150850.16 - 002348.60 & 0.093499 & sdss j150850.64 - 002358.27 & - + 1215 & 15:09:05.16 & + 00:23:40.11 & 18.845 & 16.794 & 15.824 & 15.356 & 14.953 & 4.800 & sdss j150905.04 + 002338.52 & 0.095726 & sdss j150905.28 + 002341.70 & - + 1216 & 15:09:08.76 & + 00:15:14.63 & 18.078 & 16.834 & 16.480 & 16.242 & 16.101 & 5.604 & sdss j150908.88 + 001512.48 & 0.053995 & sdss j150908.64 + 001516.77 & - + 1217 & 15:09:27.96 & + 00:53:52.20 & 21.695 & 19.123 & 17.597 & 17.045 & 16.729 & 6.463 & sdss j150928.08 + 005354.89 & - & sdss j150927.84 + 005349.52 & - + 1218 & 15:10:21.00 & + 00:45:27.26 & 19.983 & 18.903 & 18.626 & 18.461 & 18.523 & 4.062 & sdss j151021.12 + 004526.31 & - & sdss j151020.88 + 004528.20 & - + 1219 & 15:10:51.84 & -00:11:40.41 & 18.368 & 16.536 & 15.645 & 15.206 & 14.850 & 10.472 & sdss j151051.84 - 001135.18 & 0.091227 & sdss j151051.84 - 001145.65 & - + 1220 & 15:11:16.92 & -00:07:47.00 & 18.912 & 16.915 & 15.875 & 15.426 & 15.027 & 5.797 & sdss j151117.04 - 000749.27 & 0.092037 & sdss j151116.80 - 000744.73 & - + 1221 & 15:11:21.12 & + 00:03:34.87 & 20.654 & 19.469 & 18.671 & 18.168 & 18.093 & 2.678 & sdss j151121.12 + 000333.53 & - & sdss j151121.12 + 000336.21 & - + 1222 & 15:11:24.84 & + 00:09:05.87 & 17.776 & 16.091 & 15.226 & 14.891 & 14.554 & 11.442 & sdss j151125.20 + 000903.98 & 0.050240 & sdss j151124.48 + 000907.76 & - + 1223 & 15:11:28.32 & -00:08:57.65 & 19.828 & 18.977 & 18.337 & 18.089 & 18.043 & 2.426 & sdss j151128.32 - 000856.43 & - & sdss j151128.32 - 000858.86 & - + 1224 & 15:11:38.52 & + 00:15:00.36 & 19.980 & 18.848 & 18.244 & 17.882 & 17.669 & 3.626 & sdss j151138.64 + 001500.57 & - & sdss j151138.40 + 001500.14 & - + 1225 & 15:11:48.36 & + 00:26:25.12 & 20.354 & 19.089 & 17.956 & 17.562 & 17.095 & 3.682 & sdss j151148.24 + 002624.73 & - & sdss j151148.48 + 002625.51 & - + 1226 & 15:11:51.36 & + 00:35:01.88 & 17.871 & 16.693 & 15.743 & 15.440 & 15.103 & 7.573 & sdss j151151.60 + 003503.06 & 0.153784 & sdss j151151.12 + 003500.71 & - + 1227 & 15:12:52.32 & + 00:39:31.70 & 20.081 & 17.965 & 16.781 & 16.281 & 15.948 & 2.592 & sdss j151252.32 + 003930.40 & - & sdss j151252.32 + 003933.00 & 0.124369 + 1228 & 15:13:10.44 & + 00:02:06.99 & 20.237 & 19.442 & 18.577 & 18.113 & 17.832 & 4.359 & sdss j151310.32 + 000205.76 & - & sdss j151310.56 + 000208.22 & - + 1229 & 15:13:32.04 & + 00:44:07.38 & 20.412 & 19.096 & 18.005 & 17.523 & 17.062 & 3.633 & sdss j151332.16 + 004407.14 & - & sdss j151331.92 + 004407.63 & - + 1230 & 15:13:35.16 & -00:26:39.53 & 20.612 & 19.273 & 18.374 & 17.938 & 17.826 & 4.341 & sdss j151335.04 - 002640.74 & - & sdss j151335.28 - 002638.32 & - + 1231 & 15:14:16.80 & -00:36:15.18 & 20.731 & 19.808 & 19.201 & 19.022 & 18.814 & 2.538 & sdss j151416.80 - 003616.45 & - & sdss j151416.80 - 003613.91 & - + 1232 & 15:15:27.72 & -00:25:24.30 & 19.247 & 17.697 & 16.981 & 16.563 & 16.300 & 5.225 & sdss j151527.60 - 002526.20 & 0.091363 & sdss j151527.84 - 002522.41 & - + 1233 & 15:16:31.08 & -00:23:19.90 & 20.108 & 18.804 & 18.218 & 17.885 & 17.662 & 4.524 & sdss j151631.20 - 002318.53 & - & sdss j151630.96 - 002321.27 & - + 1234 & 15:16:38.40 & -00:28:05.58 & 19.972 & 18.698 & 17.564 & 17.050 & 16.675 & 4.640 & sdss j151638.40 - 002803.26 & - & sdss j151638.40 - 002807.90 & - + 1235 & 15:17:02.28 & -00:37:51.16 & 19.752 & 17.914 & 16.889 & 16.419 & 16.055 & 4.938 & sdss j151702.16 - 003749.47 & - & sdss j151702.40 - 003752.85 & - + 1236 & 15:17:27.72 & -00:39:04.76 & 19.451 & 17.772 & 16.696 & 16.233 & 15.832 & 3.646 & sdss j151727.60 - 003905.05 & - & sdss j151727.84 - 003904.47 & - + 1237 & 15:17:27.96 & -00:01:42.19 & 20.613 & 18.494 & 17.403 & 16.934 & 16.526 & 4.457 & sdss j151727.84 - 000140.88 & - & sdss j151728.08 - 000143.51 & - + 1238 & 15:17:32.52 & -00:37:15.00 & 19.338 & 18.354 & 17.876 & 17.572 & 17.303 & 5.648 & sdss j151732.64 - 003712.82 & - & sdss j151732.40 - 003717.17 & - + 1239 & 15:17:33.84 & -00:21:54.90 & 19.748 & 18.349 & 17.187 & 16.695 & 16.343 & 7.720 & sdss j151734.08 - 002156.29 & 0.169287 & sdss j151733.60 - 002153.51 & - + 1240 & 15:17:49.44 & + 00:15:50.38 & 19.639 & 18.128 & 17.349 & 16.854 & 16.493 & 10.192 & sdss j151749.20 + 001546.77 & - & sdss j151749.68 + 001553.99 & - + 1241 & 15:18:26.16 & + 00:12:02.74 & 19.204 & 17.123 & 16.050 & 15.557 & 15.190 & 7.997 & sdss j151826.40 + 001204.48 & 0.115317 & sdss j151825.92 + 001201.00 & 0.117205 + 1242 & 15:18:44.52 & + 00:23:39.75 & 20.013 & 18.008 & 16.854 & 16.359 & 15.983 & 3.637 & sdss j151844.40 + 002340.00 & 0.152263 & sdss j151844.64 + 002339.49 & - + 1243 & 15:18:56.76 & + 00:52:47.40 & 19.017 & 17.111 & 16.088 & 15.606 & 15.247 & 4.465 & sdss j151856.64 + 005248.72 & 0.115843 & sdss j151856.88 + 005246.08 & - + 1244 & 15:21:24.36 & + 00:06:56.27 & 18.307 & 16.371 & 15.343 & 14.824 & 14.454 & 11.282 & sdss j152124.24 + 000650.92 & 0.076074 & sdss j152124.48 + 000701.62 & 0.075992 + 1245 & 15:21:43.68 & -00:18:09.79 & 20.293 & 18.093 & 16.986 & 16.512 & 16.131 & 3.247 & sdss j152143.68 - 001808.17 & 0.130500 & sdss j152143.68 - 001811.42 & - + 1246 & 15:22:26.40 & -00:13:14.21 & 20.128 & 18.750 & 17.675 & 17.144 & 16.709 & 4.115 & sdss j152226.40 - 001316.27 & - & sdss j152226.40 - 001312.16 & - + 1247 & 15:23:20.52 & + 00:22:20.19 & 20.556 & 19.385 & 18.836 & 18.460 & 18.284 & 4.349 & sdss j152320.64 + 002221.41 & - & sdss j152320.40 + 002218.96 & - + 1248 & 15:23:44.40 & -00:49:54.00 & 18.997 & 16.926 & 15.703 & 15.095 & 14.617 & 7.213 & sdss j152344.16 - 004954.22 & 0.132095 & sdss j152344.64 - 004953.78 & - + 1249 & 15:23:48.60 & -00:31:05.35 & 18.013 & 16.903 & 16.306 & 16.128 & 15.925 & 4.681 & sdss j152348.72 - 003103.86 & - & sdss j152348.48 - 003106.85 & - + 1250 & 15:24:21.84 & + 00:01:45.63 & 19.135 & 18.009 & 17.396 & 16.971 & 16.762 & 7.241 & sdss j152422.08 + 000145.25 & 0.129138 & sdss j152421.60 + 000146.02 & - + 1251 & 15:25:17.52 & -00:47:55.66 & 21.717 & 19.916 & 18.937 & 18.406 & 18.075 & 3.607 & sdss j152517.52 - 004753.85 & - & sdss j152517.52 - 004757.46 & - + 1252 & 15:25:43.08 & + 00:17:49.28 & 18.594 & 17.323 & 16.719 & 16.287 & 16.013 & 7.960 & sdss j152542.96 + 001752.83 & 0.084539 & sdss j152543.20 + 001745.73 & - + 1253 & 15:27:35.04 & -00:03:31.76 & 18.466 & 17.114 & 16.356 & 15.951 & 15.589 & 4.776 & sdss j152735.04 - 000334.15 & 0.044273 & sdss j152735.04 - 000329.38 & - + 1254 & 15:28:54.12 & -00:11:23.71 & 19.059 & 17.572 & 16.860 & 16.365 & 16.024 & 7.523 & sdss j152854.00 - 001127.01 & 0.084047 & sdss j152854.24 - 001120.40 & - + 1255 & 15:29:13.80 & -00:22:23.84 & 18.194 & 16.598 & 15.726 & 15.364 & 15.091 & 4.030 & sdss j152913.92 - 002224.75 & - & sdss j152913.68 - 002222.94 & - + 1256 & 15:29:15.60 & + 00:12:26.19 & 19.438 & 17.534 & 16.601 & 16.180 & 15.830 & 3.730 & sdss j152915.60 + 001224.33 & 0.093443 & sdss j152915.60 + 001228.06 & - + 1257 & 15:29:20.04 & -00:08:35.97 & 20.537 & 18.861 & 17.879 & 17.526 & 17.083 & 5.278 & sdss j152919.92 - 000834.04 & - & sdss j152920.16 - 000837.90 & - + 1258 & 15:30:37.32 & + 00:05:30.15 & 18.762 & 16.870 & 15.944 & 15.419 & 15.036 & 10.976 & sdss j153037.68 + 000529.17 & 0.071174 & sdss j153036.96 + 000531.13 & - + 1259 & 15:30:39.72 & -00:15:25.74 & 20.298 & 18.643 & 17.630 & 17.059 & 16.591 & 7.707 & sdss j153039.60 - 001522.33 & 0.086519 & sdss j153039.84 - 001529.15 & - + 1260 & 15:30:42.96 & -00:10:45.41 & 19.954 & 18.106 & 17.216 & 16.833 & 16.508 & 3.218 & sdss j153042.96 - 001047.02 & 0.085894 & sdss j153042.96 - 001043.80 & - + 1261 & 15:30:48.12 & + 00:18:45.73 & 20.636 & 18.822 & 17.607 & 17.052 & 16.724 & 4.268 & sdss j153048.00 + 001844.59 & - & sdss j153048.24 + 001846.88 & - + 1262 & 15:31:33.00 & -00:31:31.74 & 18.106 & 16.127 & 15.172 & 14.735 & 14.366 & 6.900 & sdss j153132.88 - 003134.69 & - & sdss j153133.12 - 003128.80 & 0.059224 + 1263 & 15:31:49.68 & -00:38:03.24 & 19.694 & 17.753 & 16.569 & 16.058 & 15.629 & 8.370 & sdss j153149.44 - 003805.38 & 0.085310 & sdss j153149.92 - 003801.11 & - + 1264 & 15:31:53.40 & + 00:01:10.26 & 18.239 & 16.986 & 16.420 & 16.333 & 16.724 & 10.803 & sdss j153153.76 + 000110.12 & - & sdss j153153.04 + 000110.39 & - + 1265 & 15:33:38.64 & + 00:22:11.85 & 19.493 & 17.397 & 16.348 & 15.874 & 15.490 & 1.958 & sdss j153338.64 + 002212.83 & 0.113226 & sdss j153338.64 + 002210.88 & 0.113669 + 1266 & 15:34:30.60 & -00:22:01.56 & 17.784 & 16.619 & 15.887 & 15.779 & 15.825 & 9.118 & sdss j153430.72 - 002205.75 & 0.095774 & sdss j153430.48 - 002157.37 & - + 1267 & 15:34:35.28 & -00:28:41.00 & 17.953 & 16.555 & 15.925 & 15.513 & 15.246 & 10.126 & sdss j153435.52 - 002844.56 & 0.067210 & sdss j153435.04 - 002837.44 & 0.065739 + 1268 & 15:34:50.16 & + 00:16:56.12 & 20.468 & 18.556 & 17.397 & 16.862 & 16.468 & 9.257 & sdss j153449.92 + 001659.03 & - & sdss j153450.40 + 001653.21 & - + 1269 & 15:35:06.36 & + 00:43:20.67 & 19.447 & 17.744 & 16.684 & 16.222 & 15.888 & 3.907 & sdss j153506.48 + 004321.43 & 0.123146 & sdss j153506.24 + 004319.91 & - + 1270 & 15:35:29.88 & -00:43:35.13 & 20.375 & 19.032 & 18.007 & 17.492 & 17.112 & 4.333 & sdss j153530.00 - 004333.93 & - & sdss j153529.76 - 004336.34 & - + 1271 & 15:35:55.08 & + 00:35:00.61 & 20.374 & 19.269 & 18.396 & 18.019 & 17.671 & 4.597 & sdss j153555.20 + 003459.18 & - & sdss j153554.96 + 003502.04 & - + 1272 & 15:35:57.00 & + 00:31:51.75 & 19.568 & 18.311 & 17.572 & 17.107 & 16.853 & 3.613 & sdss j153557.12 + 003151.90 & - & sdss j153556.88 + 003151.59 & - + 1273 & 15:36:30.12 & + 00:41:46.12 & 17.957 & 16.696 & 15.804 & 15.423 & 15.074 & 11.496 & sdss j153630.48 + 004148.09 & 0.137945 & sdss j153629.76 + 004144.14 & - + 1274 & 15:37:30.72 & -00:02:31.10 & 18.831 & 17.264 & 16.150 & 15.783 & 15.369 & 9.721 & sdss j153730.48 - 000234.36 & 0.147701 & sdss j153730.96 - 000227.83 & - + 1275 & 15:38:29.52 & + 00:36:38.51 & 19.347 & 17.728 & 16.821 & 16.414 & 16.056 & 5.900 & sdss j153829.52 + 003635.56 & 0.072477 & sdss j153829.52 + 003641.46 & - + 1276 & 15:42:03.72 & + 00:05:37.17 & 19.938 & 18.527 & 17.303 & 16.812 & 16.526 & 3.730 & sdss j154203.84 + 000536.68 & - & sdss j154203.60 + 000537.65 & - + 1277 & 15:42:58.20 & + 00:32:30.81 & 18.075 & 15.955 & 14.887 & 14.414 & 14.012 & 16.350 & sdss j154257.84 + 003224.67 & - & sdss j154258.56 + 003236.94 & 0.092777 + 1278 & 16:45:41.28 & + 64:12:43.74 & 17.299 & 16.073 & 15.347 & 14.881 & 14.632 & 9.729 & sdss j164540.56 + 641245.00 & 0.068500 & sdss j164542.00 + 641242.48 & - + 1279 & 16:46:05.76 & + 63:36:53.28 & 19.865 & 18.819 & 18.896 & 18.818 & 18.768 & 6.754 & sdss j164606.24 + 633652.20 & - & sdss j164605.28 + 633654.36 & - + 1280 & 16:50:34.32 & + 62:24:08.64 & 18.954 & 17.978 & 17.361 & 16.849 & 16.641 & 6.044 & sdss j165034.56 + 622406.12 & - & sdss j165034.08 + 622411.16 & - + 1281 & 16:51:27.00 & + 62:48:04.68 & 19.952 & 18.210 & 17.007 & 16.603 & 16.242 & 3.317 & sdss j165127.12 + 624803.24 & - & sdss j165126.88 + 624806.12 & - + 1282 & 16:53:18.24 & + 62:22:59.70 & 21.140 & 19.270 & 18.011 & 17.432 & 17.040 & 4.182 & sdss j165318.00 + 622258.44 & - & sdss j165318.48 + 622300.96 & - + 1283 & 16:55:37.08 & + 64:01:11.28 & 17.962 & 16.960 & 16.720 & 16.549 & 16.372 & 4.786 & sdss j165537.44 + 640111.64 & - & sdss j165536.72 + 640110.92 & 0.023474 + 1284 & 16:55:39.24 & + 63:37:03.90 & 19.899 & 19.377 & 19.486 & 20.106 & 20.382 & 1.930 & sdss j165539.12 + 633703.36 & - & sdss j165539.36 + 633704.44 & - + 1285 & 16:57:21.12 & + 62:51:42.66 & 18.087 & 15.964 & 14.975 & 14.464 & 14.110 & 16.519 & sdss j165722.32 + 625141.76 & - & sdss j165719.92 + 625143.56 & 0.105194 + 1286 & 16:58:34.92 & + 63:35:19.14 & 19.804 & 18.712 & 18.079 & 17.808 & 17.596 & 5.425 & sdss j165834.56 + 633520.40 & - & sdss j165835.28 + 633517.88 & - + 1287 & 16:58:51.96 & + 63:10:40.80 & 18.051 & 16.143 & 15.151 & 14.719 & 14.368 & 10.921 & sdss j165852.08 + 631046.20 & - & sdss j165851.84 + 631035.40 & 0.099920 + 1288 & 16:59:41.52 & + 64:37:03.18 & 18.490 & 16.475 & 15.580 & 15.135 & 14.798 & 3.270 & sdss j165941.76 + 643703.72 & - & sdss j165941.28 + 643702.64 & 0.060477 + 1289 & 16:59:51.00 & + 60:18:39.06 & 18.856 & 18.076 & 17.790 & 17.480 & 17.461 & 1.819 & sdss j165951.12 + 601839.24 & - & sdss j165950.88 + 601838.88 & - + 1290 & 16:59:55.68 & + 63:03:40.50 & 18.576 & 17.142 & 16.905 & 16.832 & 17.363 & 5.130 & sdss j165955.44 + 630338.52 & - & sdss j165955.92 + 630342.48 & - + 1291 & 17:00:08.52 & + 64:04:22.08 & 19.253 & 17.875 & 17.123 & 16.710 & 16.440 & 8.075 & sdss j170008.64 + 640418.12 & 0.084626 & sdss j170008.40 + 640426.04 & - + 1292 & 17:00:24.12 & + 62:11:31.02 & 19.323 & 17.815 & 16.717 & 16.237 & 15.900 & 30.654 & sdss j170022.08 + 621136.60 & - & sdss j170026.16 + 621125.44 & - + 1293 & 17:00:50.04 & + 60:11:10.14 & 19.351 & 18.034 & 17.199 & 16.748 & 16.458 & 6.376 & sdss j170049.92 + 601107.08 & 0.159335 & sdss j170050.16 + 601113.20 & - + 1294 & 17:02:27.00 & + 60:43:15.60 & 16.811 & 15.916 & 15.523 & 15.290 & 15.034 & 14.664 & sdss j170226.64 + 604322.44 & 0.028502 & sdss j170227.36 + 604308.76 & - + 1295 & 17:02:50.64 & + 64:19:52.32 & 20.586 & 18.682 & 17.409 & 16.897 & 16.583 & 5.927 & sdss j170250.40 + 641949.80 & - & sdss j170250.88 + 641954.84 & - + 1296 & 17:02:51.36 & + 59:53:26.70 & 19.825 & 17.894 & 17.056 & 16.645 & 16.294 & 4.036 & sdss j170251.60 + 595325.80 & - & sdss j170251.12 + 595327.60 & - + 1297 & 17:02:59.04 & + 59:09:17.64 & 20.422 & 18.791 & 17.502 & 16.950 & 16.611 & 2.880 & sdss j170259.04 + 590916.20 & 0.230828 & sdss j170259.04 + 590919.08 & - + 1298 & 17:03:39.36 & + 60:21:50.22 & 20.131 & 18.913 & 18.091 & 17.625 & 17.379 & 3.721 & sdss j170339.12 + 602150.76 & - & sdss j170339.60 + 602149.68 & - + 1299 & 17:03:39.60 & + 61:36:04.86 & 19.492 & 18.656 & 18.213 & 18.009 & 17.883 & 3.591 & sdss j170339.36 + 613604.32 & - & sdss j170339.84 + 613605.40 & - + 1300 & 17:03:42.60 & + 60:21:31.68 & 19.509 & 18.279 & 17.377 & 16.976 & 16.634 & 5.532 & sdss j170342.96 + 602130.96 & - & sdss j170342.24 + 602132.40 & - + 1301 & 17:03:53.88 & + 61:53:37.32 & 19.915 & 17.938 & 16.919 & 16.504 & 16.183 & 5.847 & sdss j170353.52 + 615338.76 & 0.109330 & sdss j170354.24 + 615335.88 & - + 1302 & 17:03:55.68 & + 61:31:59.16 & 18.316 & 17.137 & 16.562 & 16.179 & 15.985 & 7.444 & sdss j170356.16 + 613157.72 & 0.081684 & sdss j170355.20 + 613200.60 & - + 1303 & 17:03:58.80 & + 62:52:45.30 & 21.419 & 19.740 & 18.625 & 18.193 & 17.873 & 3.455 & sdss j170358.56 + 625244.76 & - & sdss j170359.04 + 625245.84 & - + 1304 & 17:04:13.08 & + 59:56:54.42 & 18.493 & 17.635 & 17.498 & 17.386 & 17.299 & 6.305 & sdss j170412.72 + 595652.80 & 0.030617 & sdss j170413.44 + 595656.04 & - + 1305 & 17:04:38.28 & + 59:54:23.76 & 18.078 & 16.262 & 15.386 & 14.981 & 14.670 & 5.830 & sdss j170438.64 + 595422.68 & - & sdss j170437.92 + 595424.84 & - + 1306 & 17:05:06.72 & + 62:51:37.62 & 18.195 & 16.678 & 16.018 & 15.525 & 15.416 & 10.440 & sdss j170506.72 + 625142.84 & 0.088094 & sdss j170506.72 + 625132.40 & 0.087541 + 1307 & 17:05:46.08 & + 59:15:42.12 & 18.405 & 16.720 & 15.813 & 15.338 & 14.977 & 7.670 & sdss j170545.60 + 591541.04 & 0.077852 & sdss j170546.56 + 591543.20 & - + 1308 & 17:06:27.36 & + 58:52:29.28 & 20.943 & 18.896 & 17.423 & 16.874 & 16.507 & 6.858 & sdss j170627.12 + 585226.40 & 0.250680 & sdss j170627.60 + 585232.16 & - + 1309 & 17:06:38.52 & + 59:51:35.28 & 19.074 & 17.636 & 16.727 & 16.165 & 15.866 & 6.727 & sdss j170638.40 + 595138.52 & 0.096665 & sdss j170638.64 + 595132.04 & - + 1310 & 17:07:09.12 & + 62:46:01.56 & 19.380 & 18.080 & 17.205 & 16.792 & 16.572 & 3.295 & sdss j170708.88 + 624601.56 & - & sdss j170709.36 + 624601.56 & - + 1311 & 17:08:05.28 & + 63:56:44.16 & 19.626 & 18.818 & 18.303 & 18.045 & 18.071 & 3.243 & sdss j170805.04 + 635643.80 & - & sdss j170805.52 + 635644.52 & - + 1312 & 17:08:25.32 & + 58:25:39.54 & 20.454 & 18.328 & 17.387 & 16.923 & 16.556 & 5.666 & sdss j170825.68 + 582539.36 & - & sdss j170824.96 + 582539.72 & - + 1313 & 17:08:41.40 & + 57:40:23.34 & 19.612 & 18.825 & 18.041 & 17.775 & 17.465 & 2.636 & sdss j170841.52 + 574022.44 & - & sdss j170841.28 + 574024.24 & - + 1314 & 17:08:41.64 & + 61:06:29.88 & 17.427 & 16.363 & 16.076 & 15.960 & 15.907 & 3.364 & sdss j170841.52 + 610631.32 & 0.020106 & sdss j170841.76 + 610628.44 & - + 1315 & 17:09:25.56 & + 57:40:11.64 & 20.388 & 18.966 & 18.173 & 17.749 & 17.411 & 5.953 & sdss j170925.20 + 574010.92 & - & sdss j170925.92 + 574012.36 & - + 1316 & 17:09:29.52 & + 57:55:09.66 & 19.441 & 18.475 & 18.079 & 17.905 & 17.857 & 6.617 & sdss j170929.76 + 575512.36 & - & sdss j170929.28 + 575506.96 & - + 1317 & 17:09:45.24 & + 64:56:33.54 & 20.177 & 19.289 & 18.622 & 18.286 & 18.117 & 3.581 & sdss j170945.36 + 645635.16 & - & sdss j170945.12 + 645631.92 & - + 1318 & 17:09:56.52 & + 60:10:41.52 & 20.042 & 18.143 & 16.944 & 16.403 & 15.994 & 9.648 & sdss j170957.12 + 601039.72 & 0.123328 & sdss j170955.92 + 601043.32 & - + 1319 & 17:10:01.68 & + 57:46:26.04 & 18.860 & 16.973 & 16.036 & 15.583 & 15.166 & 5.263 & sdss j171001.44 + 574627.84 & 0.082035 & sdss j171001.92 + 574624.24 & - + 1320 & 17:10:27.84 & + 56:52:51.42 & 19.583 & 17.641 & 16.603 & 16.146 & 15.777 & 4.079 & sdss j171027.60 + 565250.88 & 0.126313 & sdss j171028.08 + 565251.96 & - + 1321 & 17:10:55.08 & + 56:58:02.82 & 18.873 & 18.304 & 18.032 & 18.034 & 18.222 & 6.720 & sdss j171054.72 + 565801.20 & - & sdss j171055.44 + 565804.44 & - + 1322 & 17:10:55.68 & + 64:05:35.70 & 21.005 & 19.232 & 18.473 & 18.162 & 17.969 & 4.031 & sdss j171055.44 + 640536.96 & - & sdss j171055.92 + 640534.44 & - + 1323 & 17:11:02.52 & + 59:33:44.10 & 20.067 & 19.052 & 18.147 & 17.844 & 17.533 & 2.562 & sdss j171102.64 + 593345.00 & - & sdss j171102.40 + 593343.20 & - + 1324 & 17:11:04.44 & + 56:07:24.78 & 21.236 & 19.602 & 18.362 & 17.853 & 17.416 & 4.439 & sdss j171104.32 + 560722.80 & - & sdss j171104.56 + 560726.76 & - + 1325 & 17:11:20.40 & + 58:19:47.46 & 18.923 & 17.600 & 16.757 & 16.360 & 16.189 & 8.452 & sdss j171120.64 + 581943.68 & - & sdss j171120.16 + 581951.24 & - + 1326 & 17:11:20.40 & + 62:44:47.76 & 19.609 & 17.683 & 16.736 & 16.262 & 15.966 & 3.375 & sdss j171120.64 + 624448.12 & 0.070129 & sdss j171120.16 + 624447.40 & - + 1327 & 17:11:32.64 & + 58:02:52.80 & 19.739 & 18.067 & 17.058 & 16.525 & 16.201 & 3.810 & sdss j171132.40 + 580252.80 & - & sdss j171132.88 + 580252.80 & - + 1328 & 17:11:33.48 & + 58:40:55.92 & 19.100 & 17.980 & 17.450 & 17.101 & 16.803 & 2.005 & sdss j171133.36 + 584055.56 & - & sdss j171133.60 + 584056.28 & - + 1329 & 17:11:52.32 & + 56:16:09.30 & 19.341 & 17.375 & 16.360 & 15.934 & 15.583 & 4.141 & sdss j171152.56 + 561608.76 & 0.112448 & sdss j171152.08 + 561609.84 & - + 1330 & 17:12:02.52 & + 59:58:37.74 & 17.840 & 17.012 & 15.861 & 15.484 & 15.210 & 5.962 & sdss j171202.88 + 595836.48 & 0.106960 & sdss j171202.16 + 595839.00 & - + 1331 & 17:12:06.60 & + 64:03:16.92 & 18.991 & 17.159 & 16.220 & 15.799 & 15.434 & 7.450 & sdss j171206.96 + 640319.80 & 0.082651 & sdss j171206.24 + 640314.04 & - + 1332 & 17:12:13.08 & + 64:01:56.28 & 20.403 & 18.691 & 17.772 & 17.418 & 17.119 & 3.283 & sdss j171213.20 + 640157.72 & - & sdss j171212.96 + 640154.84 & - + 1333 & 17:12:39.36 & + 58:41:46.68 & 19.028 & 18.039 & 17.473 & 17.056 & 16.938 & 4.721 & sdss j171239.60 + 584148.12 & 0.165357 & sdss j171239.12 + 584145.24 & - + 1334 & 17:12:58.68 & + 61:51:58.50 & 22.281 & 19.183 & 17.855 & 17.377 & 17.068 & 2.012 & sdss j171258.80 + 615157.96 & - & sdss j171258.56 + 615159.04 & - + 1335 & 17:13:09.24 & + 58:28:16.50 & 19.205 & 18.364 & 18.516 & 18.085 & 18.399 & 2.170 & sdss j171309.36 + 582817.04 & - & sdss j171309.12 + 582815.96 & - + 1336 & 17:13:12.72 & + 59:20:36.78 & 19.124 & 18.022 & 17.110 & 16.592 & 16.337 & 3.689 & sdss j171312.48 + 592036.60 & - & sdss j171312.96 + 592036.96 & - + 1337 & 17:13:17.64 & + 62:04:07.14 & 20.347 & 18.724 & 17.412 & 16.907 & 16.659 & 5.657 & sdss j171317.76 + 620404.44 & - & sdss j171317.52 + 620409.84 & 0.087541 + 1338 & 17:13:21.36 & + 57:57:21.60 & 20.152 & 17.847 & 16.659 & 16.141 & 15.744 & 4.388 & sdss j171321.60 + 575720.52 & 0.145573 & sdss j171321.12 + 575722.68 & - + 1339 & 17:13:39.36 & + 61:41:42.90 & 18.436 & 17.579 & 17.522 & 17.496 & 17.618 & 4.707 & sdss j171339.12 + 614141.28 & - & sdss j171339.60 + 614144.52 & - + 1340 & 17:14:00.48 & + 64:05:43.62 & 19.971 & 18.136 & 17.235 & 16.889 & 16.540 & 4.516 & sdss j171400.24 + 640542.00 & - & sdss j171400.72 + 640545.24 & - + 1341 & 17:14:03.48 & + 61:36:10.80 & 20.400 & 19.073 & 18.041 & 17.469 & 17.137 & 8.844 & sdss j171403.84 + 613614.40 & - & sdss j171403.12 + 613607.20 & - + 1342 & 17:14:26.40 & + 56:48:38.16 & 19.294 & 18.286 & 17.570 & 17.315 & 16.905 & 5.338 & sdss j171426.16 + 564836.36 & - & sdss j171426.64 + 564839.96 & - + 1343 & 17:14:47.64 & + 59:35:07.80 & 18.847 & 18.070 & 17.552 & 17.156 & 17.146 & 4.035 & sdss j171447.76 + 593509.60 & - & sdss j171447.52 + 593506.00 & - + 1344 & 17:15:03.60 & + 54:52:26.94 & 20.637 & 18.986 & 17.812 & 17.377 & 16.861 & 5.400 & sdss j171503.60 + 545229.64 & - & sdss j171503.60 + 545224.24 & - + 1345 & 17:15:03.96 & + 56:47:16.98 & 18.242 & 17.975 & 17.391 & 16.912 & 16.709 & 6.183 & sdss j171504.32 + 564716.08 & 0.190947 & sdss j171503.60 + 564717.88 & - + 1346 & 17:15:04.08 & + 61:03:41.40 & 19.567 & 17.972 & 17.230 & 16.742 & 16.437 & 7.843 & sdss j171503.60 + 610339.60 & 0.079373 & sdss j171504.56 + 610343.20 & - + 1347 & 17:15:23.76 & + 62:26:28.50 & 18.675 & 17.327 & 16.682 & 16.250 & 15.955 & 7.608 & sdss j171524.00 + 622625.08 & 0.080099 & sdss j171523.52 + 622631.92 & - + 1348 & 17:15:28.44 & + 65:35:32.64 & 18.929 & 17.246 & 16.327 & 15.908 & 15.555 & 7.745 & sdss j171529.04 + 653531.56 & 0.103914 & sdss j171527.84 + 653533.72 & - + 1349 & 17:15:54.00 & + 61:21:34.38 & 16.452 & 15.819 & 15.687 & 15.593 & 15.653 & 10.996 & sdss j171553.76 + 612129.16 & - & sdss j171554.24 + 612139.60 & 0.013004 + 1350 & 17:15:58.20 & + 62:23:27.96 & 19.921 & 18.154 & 17.410 & 17.073 & 16.917 & 10.217 & sdss j171558.32 + 622322.92 & - & sdss j171558.08 + 622333.00 & - + 1351 & 17:16:16.20 & + 54:18:17.82 & 20.007 & 18.607 & 17.451 & 16.956 & 16.684 & 6.312 & sdss j171615.84 + 541818.00 & - & sdss j171616.56 + 541817.64 & - + 1352 & 17:16:30.72 & + 58:07:48.18 & 19.418 & 18.029 & 17.312 & 16.969 & 16.783 & 3.240 & sdss j171630.72 + 580749.80 & - & sdss j171630.72 + 580746.56 & - + 1353 & 17:16:33.48 & + 61:15:39.06 & 20.141 & 18.531 & 17.492 & 17.020 & 16.710 & 3.673 & sdss j171633.60 + 611540.68 & - & sdss j171633.36 + 611537.44 & - + 1354 & 17:16:36.60 & + 55:31:23.88 & 19.211 & 17.995 & 17.357 & 16.946 & 16.632 & 8.400 & sdss j171636.96 + 553126.76 & - & sdss j171636.24 + 553121.00 & - + 1355 & 17:16:40.32 & + 57:22:58.80 & 19.842 & 18.758 & 18.273 & 18.127 & 17.990 & 7.894 & sdss j171639.84 + 572258.08 & - & sdss j171640.80 + 572259.52 & - + 1356 & 17:16:51.84 & + 58:31:28.74 & 19.156 & 18.004 & 17.379 & 17.158 & 16.946 & 6.580 & sdss j171651.60 + 583131.44 & - & sdss j171652.08 + 583126.04 & - + 1357 & 17:17:14.28 & + 59:15:01.80 & 18.951 & 17.093 & 16.019 & 15.628 & 15.269 & 9.643 & sdss j171713.68 + 591503.24 & - & sdss j171714.88 + 591500.36 & 0.140652 + 1358 & 17:17:20.76 & + 53:58:47.82 & 20.425 & 19.284 & 18.144 & 17.728 & 17.490 & 6.361 & sdss j171720.40 + 535847.64 & - & sdss j171721.12 + 535848.00 & - + 1359 & 17:17:21.36 & + 62:38:09.06 & 17.926 & 16.825 & 16.270 & 16.063 & 16.065 & 6.120 & sdss j171721.36 + 623806.00 & - & sdss j171721.36 + 623812.12 & - + 1360 & 17:17:22.68 & + 64:37:24.06 & 18.819 & 17.903 & 17.719 & 17.464 & 17.517 & 3.589 & sdss j171722.56 + 643722.44 & - & sdss j171722.80 + 643725.68 & - + 1361 & 17:17:34.68 & + 61:59:06.54 & 19.871 & 18.253 & 17.243 & 16.792 & 16.521 & 8.462 & sdss j171735.28 + 615906.72 & - & sdss j171734.08 + 615906.36 & - + 1362 & 17:17:48.24 & + 54:31:03.00 & 20.288 & 18.838 & 17.479 & 17.053 & 16.735 & 2.160 & sdss j171748.24 + 543101.92 & - & sdss j171748.24 + 543104.08 & - + 1363 & 17:17:49.56 & + 64:25:46.92 & 18.561 & 17.104 & 16.642 & 16.653 & 17.152 & 4.879 & sdss j171749.92 + 642546.20 & - & sdss j171749.20 + 642547.64 & - + 1364 & 17:17:57.36 & + 64:45:42.66 & 19.279 & 18.230 & 17.702 & 17.347 & 17.169 & 6.212 & sdss j171757.60 + 644545.36 & - & sdss j171757.12 + 644539.96 & - + 1365 & 17:18:22.44 & + 54:31:04.44 & 20.103 & 18.325 & 16.989 & 16.453 & 15.960 & 6.899 & sdss j171822.80 + 543105.88 & 0.209749 & sdss j171822.08 + 543103.00 & - + 1366 & 17:18:27.00 & + 55:25:49.26 & 17.274 & 16.093 & 15.702 & 15.387 & 15.212 & 17.290 & sdss j171826.16 + 552544.40 & 0.028819 & sdss j171827.84 + 552554.12 & - + 1367 & 17:18:39.96 & + 55:57:01.98 & 20.244 & 18.443 & 17.305 & 16.717 & 16.369 & 7.824 & sdss j171840.08 + 555658.20 & - & sdss j171839.84 + 555705.76 & - + 1368 & 17:18:50.52 & + 56:32:39.66 & 19.827 & 17.867 & 16.872 & 16.435 & 16.076 & 6.778 & sdss j171850.88 + 563238.04 & 0.112260 & sdss j171850.16 + 563241.28 & - + 1369 & 17:18:52.68 & + 55:08:34.98 & 18.963 & 17.819 & 17.168 & 17.023 & 16.849 & 8.692 & sdss j171853.04 + 550838.04 & - & sdss j171852.32 + 550831.92 & - + 1370 & 17:19:26.40 & + 65:52:57.18 & 18.620 & 17.314 & 16.468 & 16.001 & 15.672 & 9.402 & sdss j171927.12 + 655255.56 & 0.103483 & sdss j171925.68 + 655258.80 & - + 1371 & 17:19:29.64 & + 55:25:59.34 & 18.768 & 16.649 & 15.650 & 15.168 & 14.819 & 6.222 & sdss j171930.00 + 552558.80 & 0.072397 & sdss j171929.28 + 552559.88 & - + 1372 & 17:19:36.72 & + 56:11:38.76 & 18.269 & 17.338 & 16.937 & 16.679 & 16.528 & 7.200 & sdss j171936.72 + 561135.16 & - & sdss j171936.72 + 561142.36 & - + 1373 & 17:19:46.92 & + 54:10:16.14 & 19.724 & 18.483 & 17.765 & 17.444 & 17.168 & 4.486 & sdss j171946.80 + 541014.16 & - & sdss j171947.04 + 541018.12 & - + 1374 & 17:19:50.88 & + 53:41:00.42 & 18.860 & 17.848 & 17.518 & 17.493 & 17.541 & 6.881 & sdss j171951.12 + 534057.72 & - & sdss j171950.64 + 534103.12 & - + 1375 & 17:19:53.16 & + 59:11:15.36 & 20.087 & 18.520 & 17.639 & 17.200 & 17.011 & 5.716 & sdss j171952.80 + 591114.64 & - & sdss j171953.52 + 591116.08 & - + 1376 & 17:20:06.24 & + 56:34:47.10 & 20.003 & 18.929 & 18.435 & 18.046 & 17.891 & 4.355 & sdss j172006.48 + 563446.20 & - & sdss j172006.00 + 563448.00 & - + 1377 & 17:20:08.16 & + 65:45:54.90 & 18.620 & 17.106 & 16.365 & 16.047 & 15.761 & 7.539 & sdss j172008.64 + 654552.56 & 0.035700 & sdss j172007.68 + 654557.24 & - + 1378 & 17:20:22.92 & + 61:18:49.14 & 20.079 & 18.338 & 17.057 & 16.599 & 16.250 & 5.670 & sdss j172022.80 + 611846.44 & 0.171234 & sdss j172023.04 + 611851.84 & - + 1379 & 17:21:00.12 & + 59:53:17.34 & 19.506 & 17.870 & 16.864 & 16.408 & 16.046 & 9.038 & sdss j172100.72 + 595317.16 & 0.157109 & sdss j172059.52 + 595317.52 & - + 1380 & 17:21:07.32 & + 65:55:34.32 & 18.500 & 16.576 & 15.591 & 15.142 & 14.824 & 10.284 & sdss j172107.92 + 655530.72 & 0.078251 & sdss j172106.72 + 655537.92 & - + 1381 & 17:21:09.00 & + 65:35:23.28 & 19.869 & 17.639 & 16.492 & 16.004 & 15.704 & 6.732 & sdss j172108.64 + 653520.76 & 0.148353 & sdss j172109.36 + 653525.80 & - + 1382 & 17:21:35.40 & + 59:51:51.12 & 20.530 & 18.841 & 17.851 & 17.455 & 17.132 & 5.470 & sdss j172135.76 + 595150.76 & - & sdss j172135.04 + 595151.48 & - + 1383 & 17:21:57.60 & + 56:52:18.30 & 20.462 & 19.624 & 19.081 & 18.835 & 18.764 & 5.583 & sdss j172157.84 + 565216.32 & - & sdss j172157.36 + 565220.28 & - + 1384 & 17:22:19.44 & + 59:57:41.40 & 20.349 & 18.673 & 17.412 & 16.875 & 16.502 & 5.760 & sdss j172219.44 + 595744.28 & - & sdss j172219.44 + 595738.52 & - + 1385 & 17:22:28.32 & + 54:02:09.60 & 19.587 & 17.942 & 16.720 & 16.201 & 16.298 & 7.738 & sdss j172228.56 + 540212.84 & 0.191094 & sdss j172228.08 + 540206.36 & - + 1386 & 17:22:48.36 & + 65:34:31.44 & 20.151 & 18.215 & 17.259 & 16.776 & 16.527 & 4.523 & sdss j172248.00 + 653431.08 & 0.080460 & sdss j172248.72 + 653431.80 & - + 1387 & 17:22:49.08 & + 53:23:08.34 & 18.457 & 16.572 & 15.696 & 15.268 & 14.930 & 10.742 & sdss j172248.48 + 532308.52 & 0.060749 & sdss j172249.68 + 532308.16 & - + 1388 & 17:22:49.56 & + 57:02:32.82 & 19.715 & 17.810 & 16.883 & 16.490 & 16.124 & 8.508 & sdss j172249.68 + 570228.68 & - & sdss j172249.44 + 570236.96 & - + 1389 & 17:22:51.00 & + 60:07:44.58 & 16.946 & 15.534 & 15.108 & 15.097 & 14.433 & 23.643 & sdss j172252.56 + 600746.56 & 0.027635 & sdss j172249.44 + 600742.60 & - + 1390 & 17:23:04.32 & + 58:13:17.40 & 20.628 & 19.212 & 18.108 & 17.611 & 17.407 & 3.792 & sdss j172304.08 + 581317.40 & - & sdss j172304.56 + 581317.40 & - + 1391 & 17:23:07.92 & + 54:36:12.24 & 19.722 & 18.151 & 16.880 & 16.331 & 15.959 & 4.232 & sdss j172308.16 + 543611.88 & - & sdss j172307.68 + 543612.60 & - + 1392 & 17:23:09.12 & + 64:27:36.00 & 18.889 & 17.386 & 16.346 & 15.796 & 15.522 & 8.507 & sdss j172309.36 + 642732.04 & 0.103218 & sdss j172308.88 + 642739.96 & - + 1393 & 17:23:40.80 & + 55:29:51.18 & 20.652 & 19.390 & 18.287 & 17.812 & 17.659 & 3.240 & sdss j172340.80 + 552949.56 & - & sdss j172340.80 + 552952.80 & - + 1394 & 17:23:52.20 & + 62:13:58.62 & 19.112 & 17.397 & 16.517 & 16.052 & 15.858 & 4.301 & sdss j172352.08 + 621400.60 & 0.086631 & sdss j172352.32 + 621356.64 & - + 1395 & 17:24:13.80 & + 64:18:51.84 & 18.406 & 16.748 & 15.754 & 15.274 & 14.868 & 8.918 & sdss j172413.20 + 641854.00 & 0.081462 & sdss j172414.40 + 641849.68 & - + 1396 & 17:24:32.88 & + 53:58:57.54 & 19.249 & 17.222 & 16.144 & 15.618 & 15.189 & 10.043 & sdss j172432.40 + 535854.84 & - & sdss j172433.36 + 535900.24 & 0.100612 + 1397 & 17:25:21.12 & + 60:10:19.02 & 17.870 & 16.616 & 15.801 & 15.446 & 15.168 & 7.593 & sdss j172521.60 + 601017.76 & 0.132559 & sdss j172520.64 + 601020.28 & - + 1398 & 17:25:33.48 & + 52:54:41.58 & 17.512 & 16.326 & 15.637 & 15.207 & 14.993 & 7.176 & sdss j172533.36 + 525438.16 & 0.098868 & sdss j172533.60 + 525445.00 & - + 1399 & 17:25:34.80 & + 54:06:28.44 & 19.686 & 18.259 & 17.322 & 16.887 & 16.524 & 5.110 & sdss j172534.56 + 540629.88 & - & sdss j172535.04 + 540627.00 & - + 1400 & 17:25:47.52 & + 58:10:05.88 & 20.360 & 19.165 & 18.391 & 18.026 & 17.927 & 3.600 & sdss j172547.52 + 581007.68 & - & sdss j172547.52 + 581004.08 & - + 1401 & 17:26:33.00 & + 61:36:01.44 & 18.442 & 17.071 & 16.469 & 16.123 & 15.969 & 4.647 & sdss j172632.88 + 613559.28 & 0.082622 & sdss j172633.12 + 613603.60 & - + 1402 & 17:26:39.60 & + 60:13:59.88 & 18.001 & 16.987 & 16.602 & 16.375 & 16.169 & 15.415 & sdss j172638.64 + 601357.00 & - & sdss j172640.56 + 601402.76 & - + 1403 & 17:26:47.76 & + 60:26:22.92 & 20.900 & 19.689 & 18.582 & 18.098 & 17.598 & 3.833 & sdss j172647.52 + 602623.64 & - & sdss j172648.00 + 602622.20 & - + 1404 & 17:29:02.28 & + 57:03:00.00 & 19.298 & 17.758 & 16.882 & 16.486 & 16.202 & 5.407 & sdss j172902.40 + 570302.52 & 0.039443 & sdss j172902.16 + 570257.48 & - + 1405 & 17:29:07.08 & + 57:08:18.24 & 19.876 & 18.325 & 17.397 & 17.000 & 16.728 & 4.096 & sdss j172906.96 + 570816.44 & - & sdss j172907.20 + 570820.04 & - + 1406 & 17:29:59.76 & + 53:57:25.20 & 20.682 & 18.355 & 17.353 & 16.849 & 16.459 & 2.880 & sdss j172959.76 + 535723.76 & - & sdss j172959.76 + 535726.64 & - + 1407 & 17:30:11.88 & + 61:21:26.46 & 20.420 & 18.311 & 17.240 & 16.784 & 16.450 & 5.189 & sdss j173011.52 + 612126.28 & 0.137577 & sdss j173012.24 + 612126.64 & - + 1408 & 17:30:32.64 & + 60:01:00.12 & 20.482 & 19.261 & 18.784 & 18.451 & 18.425 & 2.880 & sdss j173032.64 + 600101.56 & - & sdss j173032.64 + 600058.68 & - + 1409 & 17:30:55.80 & + 56:49:35.04 & 18.725 & 17.383 & 16.669 & 16.284 & 15.953 & 14.902 & sdss j173056.16 + 564928.20 & - & sdss j173055.44 + 564941.88 & 0.030125 + 1410 & 17:31:27.36 & + 60:41:32.28 & 18.802 & 17.433 & 16.589 & 16.318 & 16.185 & 2.880 & sdss j173127.36 + 604133.72 & - & sdss j173127.36 + 604130.84 & - + 1411 & 17:33:17.52 & + 56:54:32.94 & 21.321 & 19.525 & 18.364 & 17.927 & 17.917 & 4.680 & sdss j173317.52 + 565435.28 & - & sdss j173317.52 + 565430.60 & - + 1412 & 17:33:26.64 & + 58:47:49.56 & 18.296 & 17.568 & 17.429 & 17.252 & 17.119 & 3.998 & sdss j173326.88 + 584748.84 & - & sdss j173326.40 + 584750.28 & - + 1413 & 17:34:53.04 & + 53:45:39.96 & 18.957 & 17.800 & 17.263 & 16.957 & 16.836 & 8.364 & sdss j173453.28 + 534543.56 & - & sdss j173452.80 + 534536.36 & - + 1414 & 17:34:53.64 & + 53:46:29.82 & 19.194 & 17.245 & 16.190 & 15.716 & 15.360 & 3.876 & sdss j173453.52 + 534628.20 & 0.110026 & sdss j173453.76 + 534631.44 & - + 1415 & 17:35:00.72 & + 52:58:05.52 & 17.148 & 15.854 & 14.960 & 14.703 & 14.548 & 7.920 & sdss j173500.72 + 525801.56 & - & sdss j173500.72 + 525809.48 & - + 1416 & 17:35:02.40 & + 54:45:46.80 & 20.306 & 18.070 & 17.003 & 16.498 & 16.187 & 4.397 & sdss j173502.64 + 544546.08 & - & sdss j173502.16 + 544547.52 & - + 1417 & 17:36:05.16 & + 54:45:40.50 & 19.044 & 18.216 & 17.502 & 17.087 & 16.894 & 6.463 & sdss j173605.04 + 544543.56 & 0.179904 & sdss j173605.28 + 544537.44 & - + 1418 & 17:36:15.60 & + 56:57:56.88 & 18.029 & 17.226 & 17.068 & 16.985 & 16.923 & 6.480 & sdss j173615.60 + 565800.12 & 0.025041 & sdss j173615.60 + 565753.64 & - + 1419 & 17:36:21.24 & + 52:25:27.66 & 17.848 & 17.035 & 16.929 & 16.981 & 17.533 & 4.528 & sdss j173621.12 + 522525.68 & - & sdss j173621.36 + 522529.64 & - + 1420 & 17:36:21.48 & + 54:19:21.00 & 20.364 & 18.949 & 17.815 & 17.281 & 17.102 & 5.460 & sdss j173621.36 + 541918.48 & - & sdss j173621.60 + 541923.52 & - + 1421 & 17:36:59.52 & + 58:48:53.10 & 19.865 & 19.112 & 18.424 & 18.125 & 17.873 & 3.881 & sdss j173659.28 + 584852.56 & - & sdss j173659.76 + 584853.64 & - + 1422 & 17:37:33.00 & + 57:52:39.18 & 18.459 & 17.252 & 16.643 & 16.327 & 16.163 & 7.799 & sdss j173733.12 + 575235.40 & 0.053056 & sdss j173732.88 + 575242.96 & - + 1423 & 17:37:33.24 & + 52:42:47.70 & 18.569 & 17.180 & 16.592 & 16.195 & 15.893 & 19.789 & sdss j173734.32 + 524246.44 & - & sdss j173732.16 + 524248.96 & - + 1424 & 17:37:46.32 & + 58:57:45.00 & 19.353 & 17.574 & 16.489 & 16.047 & 15.694 & 6.853 & sdss j173746.08 + 585742.12 & - & sdss j173746.56 + 585747.88 & 0.131639 + 1425 & 17:38:17.88 & + 57:51:05.40 & 21.831 & 19.804 & 18.613 & 18.121 & 18.086 & 2.396 & sdss j173818.00 + 575104.68 & - & sdss j173817.76 + 575106.12 & - + 1426 & 17:38:18.60 & + 58:01:57.90 & 20.161 & 19.003 & 17.992 & 17.483 & 17.217 & 6.572 & sdss j173818.24 + 580156.28 & - & sdss j173818.96 + 580159.52 & - + 1427 & 17:38:32.52 & + 52:41:25.98 & 20.054 & 18.245 & 17.089 & 16.573 & 16.180 & 2.212 & sdss j173832.40 + 524126.16 & - & sdss j173832.64 + 524125.80 & - + 1428 & 17:38:38.64 & + 54:32:10.50 & 20.559 & 19.228 & 18.292 & 17.893 & 17.636 & 2.520 & sdss j173838.64 + 543211.76 & - & sdss j173838.64 + 543209.24 & - + 1429 & 17:38:48.96 & + 52:53:23.82 & 18.399 & 17.219 & 16.581 & 16.313 & 16.291 & 3.960 & sdss j173848.96 + 525321.84 & - & sdss j173848.96 + 525325.80 & - + 1430 & 17:38:56.76 & + 52:42:13.50 & 20.243 & 19.354 & 18.638 & 18.320 & 18.153 & 4.521 & sdss j173856.88 + 524211.52 & - & sdss j173856.64 + 524215.48 & - + 1431 & 17:39:17.40 & + 56:42:19.26 & 17.820 & 16.846 & 16.365 & 15.963 & 15.791 & 8.521 & sdss j173917.04 + 564216.20 & 0.083582 & sdss j173917.76 + 564222.32 & - + 1432 & 17:39:37.92 & + 52:55:21.90 & 19.540 & 18.358 & 17.559 & 17.128 & 16.922 & 4.699 & sdss j173937.68 + 525522.80 & - & sdss j173938.16 + 525521.00 & - + 1433 & 17:39:40.56 & + 56:58:17.76 & 19.589 & 18.186 & 17.599 & 17.243 & 17.086 & 3.600 & sdss j173940.56 + 565819.56 & - & sdss j173940.56 + 565815.96 & - + 1434 & 17:40:50.40 & + 54:05:50.46 & 19.909 & 18.641 & 17.803 & 17.369 & 17.113 & 4.237 & sdss j174050.64 + 540550.64 & - & sdss j174050.16 + 540550.28 & - + 1435 & 17:41:49.44 & + 53:24:15.12 & 18.443 & 17.319 & 16.367 & 16.044 & 15.839 & 8.705 & sdss j174149.92 + 532414.40 & - & sdss j174148.96 + 532415.84 & - + 1436 & 23:22:23.28 & + 01:06:33.17 & 18.561 & 16.257 & 15.109 & 14.705 & 14.270 & 9.519 & sdss j232223.52 + 010630.06 & - & sdss j232223.04 + 010636.28 & - + 1437 & 23:25:01.44 & -00:00:05.23 & 17.242 & 16.051 & 15.746 & 15.697 & 15.422 & 16.378 & sdss j232501.92 - 000001.33 & - & sdss j232500.96 - 000009.13 & - + 1438 & 23:27:07.92 & -00:45:57.80 & 19.488 & 18.475 & 18.066 & 17.739 & 17.455 & 4.961 & sdss j232707.92 - 004555.32 & - & sdss j232707.92 - 004600.28 & - + 1439 & 23:28:03.84 & + 00:50:43.43 & 21.526 & 19.512 & 18.068 & 16.933 & 16.212 & 1.688 & sdss j232803.84 + 005042.59 & - & sdss j232803.84 + 005044.28 & - + 1440 & 23:28:25.68 & -00:05:08.67 & 20.463 & 19.474 & 18.794 & 18.544 & 18.252 & 5.125 & sdss j232825.68 - 000506.11 & - & sdss j232825.68 - 000511.23 & - + 1441 & 23:29:05.52 & -00:51:37.69 & 19.552 & 18.224 & 17.353 & 17.011 & 16.611 & 7.324 & sdss j232905.28 - 005137.02 & - & sdss j232905.76 - 005138.37 & - + 1442 & 23:29:17.40 & -00:40:22.86 & 18.151 & 16.868 & 16.090 & 15.693 & 15.472 & 4.630 & sdss j232917.52 - 004021.41 & 0.119347 & sdss j232917.28 - 004024.32 & 0.119831 + 1443 & 23:29:31.08 & -00:27:54.58 & 19.601 & 17.809 & 16.556 & 16.000 & 15.558 & 10.956 & sdss j232930.72 - 002755.51 & 0.177502 & sdss j232931.44 - 002753.66 & - + 1444 & 23:31:07.08 & + 00:40:22.51 & 19.395 & 18.115 & 17.599 & 17.288 & 17.102 & 10.456 & sdss j233107.20 + 004017.60 & - & sdss j233106.96 + 004027.42 & - + 1445 & 23:31:55.20 & -01:08:04.66 & 20.274 & 19.019 & 18.024 & 17.578 & 17.186 & 6.480 & sdss j233155.20 - 010801.42 & - & sdss j233155.20 - 010807.90 & 0.335598 + 1446 & 23:32:21.60 & -00:08:23.89 & 18.797 & 17.545 & 17.116 & 16.793 & 16.573 & 7.597 & sdss j233221.84 - 000825.10 & 0.069814 & sdss j233221.36 - 000822.68 & - + 1447 & 23:33:05.88 & + 01:10:40.38 & 19.234 & 18.350 & 17.979 & 17.764 & 17.692 & 7.507 & sdss j233306.00 + 011037.09 & - & sdss j233305.76 + 011043.68 & - + 1448 & 23:33:15.84 & + 01:05:13.16 & 19.521 & 18.495 & 17.706 & 17.367 & 17.034 & 4.608 & sdss j233315.84 + 010510.86 & - & sdss j233315.84 + 010515.46 & - + 1449 & 23:33:34.44 & -00:02:48.92 & 19.495 & 18.424 & 17.678 & 17.433 & 17.215 & 5.495 & sdss j233334.56 - 000246.84 & - & sdss j233334.32 - 000251.00 & - + 1450 & 23:34:49.92 & -01:04:07.68 & 19.070 & 18.003 & 17.468 & 17.190 & 17.322 & 5.184 & sdss j233449.92 - 010410.27 & - & sdss j233449.92 - 010405.08 & - + 1451 & 23:34:54.84 & + 01:01:37.29 & 19.132 & 17.431 & 16.516 & 16.106 & 15.750 & 6.164 & sdss j233454.72 + 010134.78 & 0.084666 & sdss j233454.96 + 010139.79 & - + 1452 & 23:34:58.44 & + 01:01:24.43 & 19.399 & 17.261 & 16.179 & 15.712 & 15.349 & 8.146 & sdss j233458.56 + 010120.78 & 0.131471 & sdss j233458.32 + 010128.09 & - + 1453 & 23:35:24.72 & + 00:34:32.99 & 19.281 & 17.705 & 16.619 & 16.170 & 15.830 & 10.076 & sdss j233524.96 + 003429.47 & - & sdss j233524.48 + 003436.52 & 0.152887 + 1454 & 23:35:38.28 & + 00:20:44.15 & 18.988 & 17.819 & 17.136 & 16.695 & 16.434 & 8.185 & sdss j233538.16 + 002040.47 & 0.193928 & sdss j233538.40 + 002047.82 & - + 1455 & 23:35:38.52 & + 00:21:50.82 & 18.099 & 16.947 & 15.959 & 15.595 & 15.321 & 10.886 & sdss j233538.88 + 002151.50 & 0.194217 & sdss j233538.16 + 002150.14 & - + 1456 & 23:38:18.36 & + 00:38:57.52 & 19.882 & 17.868 & 16.748 & 16.235 & 15.893 & 11.620 & sdss j233818.24 + 003903.05 & - & sdss j233818.48 + 003852.00 & - + 1457 & 23:38:21.00 & -00:36:27.56 & 19.413 & 17.880 & 17.113 & 16.640 & 16.361 & 3.681 & sdss j233821.12 - 003627.17 & 0.075113 & sdss j233820.88 - 003627.94 & - + 1458 & 23:38:38.76 & + 00:31:26.37 & 19.659 & 18.094 & 17.164 & 16.745 & 16.474 & 4.149 & sdss j233838.64 + 003125.34 & 0.148767 & sdss j233838.88 + 003127.40 & - + 1459 & 23:39:32.88 & -00:30:34.29 & 19.279 & 18.395 & 18.262 & 17.888 & 18.152 & 1.958 & sdss j233932.88 - 003035.27 & - & sdss j233932.88 - 003033.31 & - + 1460 & 23:40:44.28 & -00:53:09.08 & 18.496 & 17.881 & 17.792 & 17.772 & 17.507 & 12.252 & sdss j234044.40 - 005314.94 & 0.019188 & sdss j234044.16 - 005303.23 & - + 1461 & 23:41:49.08 & -01:02:11.36 & 20.616 & 19.338 & 18.575 & 18.026 & 17.845 & 5.791 & sdss j234149.20 - 010209.09 & - & sdss j234148.96 - 010213.63 & - + 1462 & 23:44:00.96 & + 00:34:34.60 & 20.163 & 18.900 & 17.791 & 17.308 & 17.051 & 3.730 & sdss j234400.96 + 003436.46 & - & sdss j234400.96 + 003432.73 & - + 1463 & 23:44:19.80 & + 00:51:08.52 & 18.618 & 17.661 & 17.406 & 17.365 & 17.242 & 6.689 & sdss j234419.68 + 005105.70 & - & sdss j234419.92 + 005111.34 & - + 1464 & 23:45:06.48 & + 01:15:53.20 & 17.595 & 16.469 & 16.091 & 15.738 & 15.698 & 7.780 & sdss j234506.24 + 011551.73 & - & sdss j234506.72 + 011554.68 & - + 1465 & 23:46:22.08 & + 00:10:18.08 & 19.610 & 17.895 & 16.890 & 16.424 & 16.188 & 4.432 & sdss j234622.08 + 001020.29 & 0.132678 & sdss j234622.08 + 001015.86 & - + 1466 & 23:47:48.48 & -01:00:06.35 & 20.026 & 18.751 & 17.804 & 17.337 & 16.949 & 4.356 & sdss j234748.48 - 010008.53 & - & sdss j234748.48 - 010004.17 & - + 1467 & 23:50:10.32 & -00:51:14.73 & 19.690 & 18.452 & 17.981 & 17.690 & 17.508 & 2.689 & sdss j235010.32 - 005116.07 & - & sdss j235010.32 - 005113.38 & - + 1468 & 23:50:30.84 & -00:58:45.58 & 18.317 & 17.322 & 16.535 & 16.353 & 16.115 & 4.213 & sdss j235030.72 - 005844.48 & - & sdss j235030.96 - 005846.67 & - + 1469 & 23:51:11.40 & + 00:35:32.70 & 20.445 & 19.390 & 18.308 & 17.837 & 17.558 & 3.674 & sdss j235111.52 + 003532.33 & - & sdss j235111.28 + 003533.06 & - + 1470 & 23:51:36.36 & -00:58:58.21 & 19.231 & 18.409 & 18.120 & 17.923 & 17.808 & 5.196 & sdss j235136.24 - 005856.33 & - & sdss j235136.48 - 005900.08 & - + 1471 & 23:52:49.68 & + 00:29:44.41 & 19.588 & 18.443 & 17.480 & 17.002 & 16.647 & 9.102 & sdss j235249.44 + 002947.19 & - & sdss j235249.92 + 002941.62 & - + 1472 & 23:54:10.68 & -00:56:35.08 & 20.223 & 18.779 & 18.202 & 17.772 & 17.489 & 5.916 & sdss j235410.80 - 005632.73 & - & sdss j235410.56 - 005637.42 & - + 1473 & 23:54:49.80 & -01:00:06.08 & 19.835 & 18.596 & 17.852 & 17.458 & 17.223 & 4.394 & sdss j235449.92 - 010007.34 & - & sdss j235449.68 - 010004.82 & - + 1474 & 23:55:04.68 & -00:53:48.04 & 22.626 & 19.471 & 17.990 & 17.514 & 17.288 & 3.600 & sdss j235504.56 - 005348.06 & - & sdss j235504.80 - 005348.03 & - + 1475 & 23:55:59.40 & -01:05:00.45 & 20.271 & 18.205 & 17.247 & 16.785 & 16.422 & 11.194 & sdss j235559.04 - 010501.93 & 0.141098 & sdss j235559.76 - 010458.98 & - + 1476 & 23:56:17.04 & -00:32:07.22 & 19.813 & 18.207 & 17.006 & 16.541 & 16.153 & 7.242 & sdss j235617.28 - 003207.61 & 0.187244 & sdss j235616.80 - 003206.82 & - + 1477 & 23:57:44.40 & + 00:01:10.84 & 20.196 & 19.118 & 18.755 & 18.487 & 18.273 & 4.439 & sdss j235744.40 + 000108.62 & - & sdss j235744.40 + 000113.06 & - + 1478 & 23:59:04.56 & + 00:48:54.49 & 18.852 & 17.147 & 16.263 & 15.753 & 15.365 & 10.703 & sdss j235904.32 + 004850.53 & 0.061097 & sdss j235904.80 + 004858.45 & - + 1479 & 23:59:52.68 & -01:13:02.82 & 19.827 & 17.942 & 16.942 & 16.480 & 16.090 & 11.194 & sdss j235953.04 - 011304.29 & 0.162889 & sdss j235952.32 - 011301.34 & - + lrrrrr @xmath50 & 19.37@xmath440.027 & 19.43 & 19.18@xmath440.027 & 19.25 & + @xmath28 & 17.91@xmath440.026 & 18.00 & 17.77@xmath440.026 & 17.86 & + @xmath51 & 17.11@xmath440.026 & 17.18 & 17.01@xmath440.026 & 17.07 & + @xmath52 & 16.73@xmath440.026 & 16.77 & 16.65@xmath440.026 & 16.69 & + @xmath53 & 16.47@xmath440.028 & 16.46 & 16.41@xmath440.028 & 16.41 & + projected separation [ arcsec ] & 6.12@xmath440.086 & 5.24 & & & + @xmath91-@xmath92 & 1.18@xmath440.031 & 1.01 & 1.17@xmath440.031 & 1.01 & + @xmath93-@xmath94 & 1.29@xmath440.026 & 1.06 & 1.28@xmath440.026 & 1.06 + @xmath95-@xmath96 & 1.32@xmath440.029 & 1.12 & 1.32@xmath440.029 & 1.12 & + @xmath97-@xmath98 & 1.32@xmath440.030 & 1.14 & 1.31@xmath440.030 & 1.13 & + @xmath99-@xmath100 & 1.36@xmath440.033 & 1.19 & 1.35@xmath440.033 & 1.19 & + lrrrr @xmath101 & 0.1107@xmath440.0019 & 0.104 & 0.1107@xmath440.0006 & 0.104 + @xmath102 & -20.134@xmath440.048 & -20.337 & -20.243@xmath440.015 & -20.367 + @xmath103 & -20.767@xmath440.052 & -20.986 & -20.898@xmath440.016 & -21.047 + @xmath104 & 1.406@xmath440.015 & 1.534 & 1.444@xmath440.004 & 1.534 + @xmath105 & 0.632@xmath440.008 & 0.714 & 0.658@xmath440.002 & 0.709 + @xmath106 & 0.315@xmath440.007 & 0.368 & 0.343@xmath440.001 & 0.370 + @xmath107 & 0.246@xmath440.010 & 0.264 & 0.262@xmath440.002 & 0.271 + lcc @xmath101 & 0.0019 & 1.00000 + @xmath102 & 0.0409 & 0.20879 + @xmath103 & 0.0472 & 0.09850 + @xmath104 & 0.0812 & 0.00027 + @xmath105 & 0.0796 & 0.00038 + @xmath106 & 0.0933 & 0.00002 + @xmath107 & 0.0659 & 0.00566 + lcc @xmath101 vs. @xmath108 & 0.081 & 0.00520 + & & + @xmath109 vs. @xmath110 & 0.090 & 0.00051 + @xmath108 vs. @xmath110 & 0.094 & 0.00020 + @xmath111 vs. @xmath110 & 0.095 & 0.00034 + @xmath112 vs. @xmath110 & 0.083 & 0.00412 + & & + @xmath109 vs. @xmath113 & 0.097 & 0.00039 + @xmath108 vs. @xmath113 & 0.100 & 0.00017 + @xmath111 vs. @xmath113 & 0.093 & 0.00064 + @xmath112 vs. @xmath113 & 0.088 & 0.00019 + & & + @xmath108 vs. @xmath109 & 0.118 & @xmath114 + @xmath111 vs. @xmath108 & 0.147 & @xmath115 + @xmath112 vs. @xmath111 & 0.114 & @xmath116 +

the selection algorithm , implementing a variation on the original @xcite criteria , proved to be very efficient and fast . merging galaxies were selected such that the inter - galaxy separations were less than the sum of the component galaxies radii . the atlas images also include the relevant data for each pair member

we present a new catalog of merging galaxies obtained through an automated systematic search routine . the 1479 new pairs of merging galaxies were found in @xmath0 462 sq deg of the sloan digital sky survey early data release ( sdss edr ; @xcite ) photometric data , and the pair catalog is complete for galaxies in the magnitude range @xmath1 . the selection algorithm , implementing a variation on the original @xcite criteria , proved to be very efficient and fast . merging galaxies were selected such that the inter - galaxy separations were less than the sum of the component galaxies radii . we discuss the characteristics of the sample in terms of completeness , pair separation , and the holmberg effect . we also present an online atlas of images for the sdss edr pairs obtained using the corrected frames from the sdss edr database . the atlas images also include the relevant data for each pair member . this catalog will be useful for conducting studies of the general characteristics of merging galaxies , their environments , and their component galaxies . the redshifts for a subset of the interacting and merging galaxies and the distribution of angular sizes for these systems indicate the sdss provides a much deeper sample than almost any other wide - area catalog to date .

0805.0162

i

given two isometric poses of the same non - rigid object as triangular meshes @xmath3 and @xmath4 with known point - to - point correspondences , we aim to find a smooth isometric deformation between the poses . interpolating smoothly between two given poses is called _ morphing_. we achieve this by finding shortest paths in an appropriate shape space similar to the approach by kilian et al . we propose a novel shape space . a deformation of a shape represented by a triangular mesh is isometric if and only if all edge lengths are preserved during the deformation @xcite . this property holds because each face of the mesh is a triangle . a deformation of a shape is called _ most isometric _ if the sum of the squared differences between the corresponding edge lengths of the two shapes is minimized . in this paper , we examine isometric deformations of general _ triangular meshes _ in @xmath1 and of _ triangulated @xmath1 polygons _ , which are triangular meshes with no interior vertices . we introduce a new shape space @xmath0 for triangulated @xmath1 polygons that has the property that interpolating linearly in shape space corresponds to the most isometric morph in @xmath2 . we then extend this shape space to arbitrary triangulations in @xmath1 using a heuristic approach . furthermore , we discuss a modification of the shape space that is useful for isometric skeleton morphing .

we present a novel approach to morph between two isometric poses of the same non - rigid object given as triangular meshes . , we prove that interpolating linearly in this shape space corresponds to the most isometric morph in @xmath2 . we then extend this shape space to arbitrary triangulations in @xmath1 using a heuristic approach and show the practical use of the approach using experiments . furthermore , we discuss a modified shape space that is useful for isometric skeleton morphing .

we present a novel approach to morph between two isometric poses of the same non - rigid object given as triangular meshes . we model the morphs as linear interpolations in a suitable shape space @xmath0 . for triangulated @xmath1 polygons , we prove that interpolating linearly in this shape space corresponds to the most isometric morph in @xmath2 . we then extend this shape space to arbitrary triangulations in @xmath1 using a heuristic approach and show the practical use of the approach using experiments . furthermore , we discuss a modified shape space that is useful for isometric skeleton morphing . all of the newly presented approaches solve the morphing problem without the need to solve a minimization problem .

1305.7178

i

the study of extreme and rare events is a highly active and interdisciplinary research field @xcite . extreme events can have catastrophic consequences in fields such as climatology , population dynamics or economy @xcite . in lasers , for example , extreme and rare pulses have been observed in mode - locked lasers @xcite and in semiconductor lasers with continuous - wave optical injection @xcite or with phase conjugated feedback @xcite . we present a numerical study of the intensity pulses displayed by a semiconductor laser with optical feedback in the short cavity regime @xcite , such that the external cavity round trip time is smaller than the laser relaxation oscillation period . we use as a framework the well - known lang - kobayashi ( lk ) model @xcite . previous numerical work based on the lk model has found high intensity pulses in the laser chaotic output , that correspond to transitions between external cavity modes ( ecms ) @xcite . we characterize these pulses and show that in specific parameter regions they are high enough to be considered extreme events . in extreme value analysis the definition of an extreme event is arbitrary as is associated to an event that is rare and that has an extreme deviation from the average . qualitatively , extreme values are those in the tail of a long - tailed distribution ; quantitatively , there are two main approaches to define extreme values : 1 ) values that exceed ( or fall below ) a certain threshold are considered extreme @xcite , and 2 ) maxima ( or minima ) in `` blocks '' of the time series are considered extreme @xcite . in this work we use the first criterion and define extreme intensity pulses as those above a certain threshold . one should notice that both approaches involve a certain degree of arbitrariness , either in the selection of the threshold or in the selection of the length of the block . an example of the use of the first criterium is in oceanography , where extreme waves ( referred to as freak or rogue waves ) are those whose height is larger than the mean value plus four to eight times the standard deviation of the height distribution , or as waves with abnormality index larger than 2 @xcite . an example of the use of the second criterium is in climate data analysis , where extreme values can be annual , biannual , etc . using the point - over - threshold criterium to define extreme intensity pulses , we study how they develop and how they are affected by noise . we demonstrate that an abrupt expansion in phase space of an attractor developed from an ecm creates an expanded attractor that sustains extreme pulses . for certain parameters this attractor coexists with a smaller attractor that develops from a different ecm . we identify two phenomena involved in the appearance and in the destruction of the attractor that sustains extreme pulses : deterministic intermittency when the attractor abruptly expands , and hysteresis when the attractor is destroyed . we also show that this scenario is robust under the inclusion of noise . this paper is organized as follows . section ii briefly describes the model employed , which is the well - known delay - differential lang - kobayashi model @xcite . section iii presents the numerical results ; we first focus on deterministic simulations and then discuss the influence of noise . section iv presents a summary of the results and the conclusions .

we present a numerical study of the pulses displayed by a semiconductor laser with optical feedback in the short cavity regime , such that the external cavity round trip time is smaller than the laser relaxation oscillation period . for certain parameters there are occasional pulses , which are high enough to be considered extreme events . we characterize the bifurcation scenario that gives rise to such extreme pulses and study the influence of noise . we demonstrate intermittency when the extreme pulses appear and hysteresis when the attractor that sustains these pulses is destroyed . we also show that this scenario is robust under the inclusion of noise .

we present a numerical study of the pulses displayed by a semiconductor laser with optical feedback in the short cavity regime , such that the external cavity round trip time is smaller than the laser relaxation oscillation period . for certain parameters there are occasional pulses , which are high enough to be considered extreme events . we characterize the bifurcation scenario that gives rise to such extreme pulses and study the influence of noise . we demonstrate intermittency when the extreme pulses appear and hysteresis when the attractor that sustains these pulses is destroyed . we also show that this scenario is robust under the inclusion of noise .

astro-ph0007429

i

the circular polarization ( cp ) of radio emission observed from pulsars ( manchester , taylor & huguenin 1975 ; radhakrishnan & rankin 1990 ; han et al 1999 ) and from some quasars ( roberts et al 1975 , weiler & de pater 1983 ; saikia & salter 1988 ) is not understood . in both cases , simple theory suggests that any polarization should be linear , determined by the direction of the projection of the magnetic field in the source region on the plane of the sky . in both cases , intrinsic cp is expected as a correction to first order in an expansion in the inverse of the lorentz factor of the radiating particles , but it does not seem possible to account for the observations in terms of cp intrinsic to the emission process ( radhakrishnan & rankin 1990 ; radhakrishnan 1992 ; saikia & salter 1988 ) . another possibility is that the cp is imposed as a propagation effect due to the partial conversion of linear polarization into cp resulting from the ellipticity of the natural modes of the medium ( sazonov 1969 ; pacholczyk 1973 ; jones & odell 1977a , b ) . however , this also fails to provide a satisfactory explanation for the properties of the observed cp . in this paper we describe a different propagation effect that can lead to cp for a source , independent of its degree of linear polarization . we refer to this as scintillation - induced cp . although the observed cps from pulsars and quasars are quite different , we suggest that both might be due to scintillation - induced cp , with the most obvious differences being due to pulsars scintillating in the diffractive regime and quasars scintillating in the refractive regime . in the formal theory of scattering in a turbulent , magnetized plasma ( melrose 1993a , b ) there are differences in the scattering in the two oppositely circularly polarized wave modes of the medium due to their different refractive indices . most of the terms contributing to the cp are too small to be of interest for scattering in the interstellar medium ( ism ) . however , we have recently shown ( macquart and melrose 2000 ; hereinafter paper i ) that there is one much larger contribution to the cp that is a possible candidate for explaining the cp in pulsars and quasars . the cp identified in paper i is due to a nonzero variance in stokes @xmath0 , and the formal theory implies that the dominant contribution is of the form @xmath1 , where @xmath2 is a phase structure function associated with the relative phase , @xmath3 , between the components in the opposite cps . the distance @xmath4 is the refractive scale , which is defined in terms of the fresnel scale @xmath5 , where @xmath6 is the distance between the scattering screen and the observer s plane and @xmath7 is the wavelength , and the diffractive scale @xmath8 , which is defined by writing the phase structure function in the forms @xmath9 for a power - law spectrum of turbulence . our purposes in this paper are threefold : first , to provide a physical explanation for the mechanism that leads to this term , second , to use this interpretation to relax some of the restrictive assumptions made in paper i to obtain a more general semiquantitative expression for the predicted cp , and , third , to explore the suggested application to the observed cp in pulsars and extragalactic sources . we start ( section 2 ) by including birefringence in a simple model for strong scattering in which scattering is attributed to a large number of coherent patches of size @xmath10 within an envelope of size @xmath11 on the scattering screen ( e.g. , goodman & narayan 1989 , narayan 1992 , gwinn et al 1998 ) . when the birefringence is included , this model reproduces the result @xmath1 derived from the formal theory of scattering in a magnetized plasma in paper i. this simple model corresponds to strong diffractive scintillation , suggesting that our expression for @xmath12 applies only to a source that exhibits strong diffractive scintillations ( which is the case for pulsars but not for quasars ) . further physical interpretation of scintillation - induced cp is developed in section 3 , where it is argued that it arises from a combination of two processes : a rippling of the wavefront , as in the conventional theory for scattering in a turbulent medium , combined with random refractions in the birefringent medium that cause a separation in the rays associated with the opposite cps . this leads to the following interpretation : the ripples in the wavefront for the two cps become spatially separated due to the random birefringent refractions , so that they do not overlap in the observer s plane . this leads to alternate patches in which one cp and then the other dominates , leading to a nonzero @xmath12 . this interpretation is the basis for two important generalizations that we propose here . first , an essential requirement in this interpretation is that the images in the two cps be displaced relative to each other by @xmath13 in the observer s plane . our interpretation of the formal theory is that this is due to random birefringent scatterings at the putative scattering screen . however , any mechanism that causes such a displacement of the rays corresponding to the two opposite cps leads to a nonzero @xmath13 and hence to a nonzero @xmath12 . in particular , an alternative to random birefringent refractions is birefringent refraction at a single structure , which we refer to as a faraday wedge , cf . section 4 . second , although the result derived from the formal theory applies for strong diffractive scintillations , our interpretation implies that a nonzero @xmath12 results for any source that exhibits scintillations . consider a source with a scintillation index @xmath14 on a spatial scale @xmath15 in the observer s plane ; it should exhibit fluctuations in the degree of cp , @xmath16 , that is of order @xmath17 times @xmath14 . in particular , a source that exhibits refractive scintillations should exhibit fluctuations in cp on a similar timescale with an amplitude smaller by the factor @xmath17 . for scintillation - induced cp to account for the observed cp in quasars and pulsars , two conditions need to be satisfied . first , the predicted degree of cp , @xmath16 , must be in the observed range , which appears to be @xmath18 for a few pulsars and is @xmath19 for relevant extragalactic sources . second , the predicted timescale for the fluctuations in cp must be consistent with the observed variations in the cp . for pulsars this is the diffractive timescale , and for quasars it is the refractive timescale . these requirements are discussed for pulsars in section 5 , and for extragalactic sources in section 6 .

we present a physical interpretation for the generation of circular polarization resulting from the propagation of radiation through a magnetized plasma in terms of a rotation measure gradient , or ` faraday wedges ' . application of the theory to the circular polarization in pulsars and compact extragalactic sources is discussed .

we present a physical interpretation for the generation of circular polarization resulting from the propagation of radiation through a magnetized plasma in terms of a rotation measure gradient , or ` faraday wedges ' . criteria for the observability of scintillation - induced circular polarization are identified . application of the theory to the circular polarization in pulsars and compact extragalactic sources is discussed . # 1

1101.4610

i

the characterization of laser beams is traditionally a basic task in optical science and performed for decades now . however , the existence of different archaic approaches like the variable aperture or moving knife - edge method , which are known to produce deviant results , has shown the need for a standardization of the definition . especially the question how to reproducibly and reliably measure beam quality , which is very important from an user - oriented point of view , stimulated a lot of discussions @xcite . the iso standard 11146 - 1/2/3 has brought a great unification by defining all relevant quantities of laser beams including instructions how to perform the measurements conform to the iso standard @xcite . in the general case of so - called general astigmatic beams this approach relies on the determination of ten independent parameters , which are the second order moments of the wigner distribution function . from these , three quantities can easily be derived according to iso 11146 - 2 : the beam propagation ratio simply called @xmath0 parameter , the intrinsic astigmatism , and the twist parameter @xcite . especially the @xmath0 factor has become a well accepted measure for beam quality in the laser community by now although it has to be used with care . siegman pointed out that the use of measurements not conform to the iso standard will result in values for @xmath0 , which are not comparable to each other @xcite . this is an important fact since other techniques as the aforementioned knife - edge method are still in use for one reason : their simplicity . as stated above , a measurement of a general astigmatic beam , which is fully conform to the iso standard , requires the measurement of ten second order moments of the wigner distribution function and , thus , is experimentally cumbersome and slow . fortunately , due to their high symmetry most laser beams of practical interest require less than these ten independent parameters to be measured for a complete characterization : most lasers emit beams that are simple astigmatic or even stigmatic because of their resonator design . in this case the @xmath0 determination is based on a caustic measurement that includes the determination of beam width as a function of propagation distance . to do this , the beam width has to be determined at least at 10 positions along the propagation axis , completed by a hyperbolic fit . according to iso 11146 - 1 , the beam width determination has to be carried out using the three spatial second order moments of the intensity distribution @xcite . despite its experimental simplicity , the caustic measurement still is quite time - consuming and requires a careful treatment of background intensity , measuring area , and noise , which makes high demands on the temporal stability of a cw laser or the pulse - to - pulse stability of a pulsed source . caustic measurements are therefore unsuitable to characterize the fast dynamics of a laser system . to react on the need for a faster and more detailed analysis , several other methods for laser beam characterization were presented such as shack - hartmann wavefront analysis @xcite , measurement of the complete 4d wigner distribution function @xcite , or the use of diffraction gratings @xcite . in this paper , we investigate the possibility to monitor the beam quality based on a decomposition of the laser beam into its constituent eigenmodes . many laser resonators possess rectangular or circular symmetry . in this case , the laser beam emerging from the resonator can completely be described as a superposition of the well - known hermite - gaussian or laguerre - gaussian modes @xcite . from the point of view of beam quality , they represent a natural choice of description since the fundamental gaussian mode has the lowest possible value of @xmath1 . any deviation from the ideal diffraction - limited gaussian beam profile can be attributed to the contribution of higher order modes , leading to @xmath2 . here , any excited higher order mode contributes with a certain value to the beam propagation parameter . this value can be readily calculated for every mode in a way which is conform to the iso standard @xcite . therefore , performing a modal decomposition of a given beam enables us to determine a value for @xmath0 which is compatible to the one resulting from a caustic measurement . to determine the modal weights necessary for the decomposition , various methods have been suggested such as coherence measurements @xcite , intensity recordings [ 911 ] , or the use of a ring resonator @xcite . again , one has to see the required experimental or numerical effort that makes those methods unsuitable for the intended task of real - time characterization . hence , we suggest to use the correlation filter technique based on computer - generated holograms ( cghs ) @xcite . recently we successfully applied this method to characterize the field produced by multimode optical fibers and to determine the polarization states of different modes @xcite . here we will show that the correlation filter method yields @xmath0 values conform to the iso standard but with diverse advantages . the experimental realization is simple and yields information about the beam quality in real - time in contrast to other approaches . it relies on a decomposition of the electromagnetic field into the spatial modes of the resonator generating the laser beam . since our investigated laser cavity possesses rectangular symmetry , hermite - gaussian modes are used in this work , but represent no restriction of the method . any complete set of suitable modes may be used in other cases . from the measured modal weights , we calculate the beam propagation factor @xmath0 and compare our results to values obtained from traditional caustic measurements as defined by the iso standard . moreover , we demonstrate the on - line monitoring of the modal spectrum as well as the @xmath0 factor while realigning the resonator in real - time .

the all - optical measurement of modal amplitudes yields @xmath0 parameters conform to the iso standard method . the experimental technique is simple and fast , which allows to investigate laser beams under conditions inaccessible to other methods . + 99 a. e. siegman , `` how to ( maybe ) measure laser beam quality , '' in _ dpss ( diode pumped solid state ) lasers : applications and issues _ , m. dowley , ed . , vol . 17 of osa trends in optics and photonics ( optical society of america , 1998 ) , paper mq1 . , _ iso 11146 - 1/2/3 test methods for laser beam widths , divergence angles and beam propagation ratios part 1 : stigmatic and simple astigmatic beams / part 2 : general astigmatic beams / part 3 : intrinsic and geometrical laser beam classification , propagation and details of test methods _ ( iso , geneva , 2005 ) . b. schfer and k. mann , `` determination of beam parameters and coherence properties of laser radiation by use of an extended hartmann - shack wave - front sensor , '' appl . opt . * 41 * , 28092817 ( 2002 ) . b. eppich , g. mann , and h. weber , `` measurement of the four - dimensional wigner distribution of paraxial light sources , '' in _ optical design and engineering ii _ , l. mazuray and r. wartmann , eds . , proc . spie * 5962 * , 59622d ( 2005 ) . r. w. lambert , r. corts - martnez , a. j. waddie , j. d. shephard , m. r. taghizadeh , a. h. greenaway , and d. p. hand , `` compact optical system for pulse - to - pulse laser beam quality measurement and applications in laser machining , '' appl . opt . * 43 * , 50375046 ( 2004 ) . a. e. siegman , _ lasers _ ( university science books , sausalito , 1986 ) . s. saghafi and c. j. r. sheppard , `` the beam propagation factor for higher order gaussian beams , '' opt . commun . * 153 * , 207210 ( 1998 ) . e. tervonen , j. turunen , and a. friberg , `` transverse laser mode structure determination from spatial coherence measurements : experimental results , '' appl . phys . a. cutolo , t. isernia , i. izzo , r. pierri , and l. zeni , `` transverse mode analysis of a laser beam by near - and far - field intensity measurements , '' appl . opt . * 34 * , 79747978 ( 1995 ) . soc . am . a * 17 * , 10861091 ( 2000 ) . n. andermahr , t. theeg , and c. fallnich , `` novel approach for polarization - sensitive measurements of transverse modes in few - mode optical fibers , '' appl . phys . b * 91 * , 353357 ( 2008 ) . v. a. soifer and m. golub , _ laser beam mode selection by computer generated holograms _ ( crc press , boca raton , 1994 ) . proc . spie * 5962 * , 59622 g ( 2005 ) . d. flamm , o. a. schmidt , c. schulze , j. borchardt , t. kaiser , s. schrter , and m. duparr , `` measuring the spatial polarization distribution of multimode beams emerging from passive step - index large - mode - area fibers , '' opt . lett . * 35 * , 34293431 ( 2010 ) . h. kogelnik and t. li , `` laser beams and resonators , '' appl . opt . * 5 * , 15501567 ( 1966 ) . h. laabs and b. ozygus , `` excitation of hermite - gaussian modes in end - pumped solid - state lasers via off - axis pumping , '' optics & laser technology * 28 * , 213214 ( 1996 ) . ( amer . math . soc . ,

we present a real - time method to determine the beam propagation ratio @xmath0 of laser beams . the all - optical measurement of modal amplitudes yields @xmath0 parameters conform to the iso standard method . the experimental technique is simple and fast , which allows to investigate laser beams under conditions inaccessible to other methods . + 99 a. e. siegman , `` how to ( maybe ) measure laser beam quality , '' in _ dpss ( diode pumped solid state ) lasers : applications and issues _ , m. dowley , ed . , vol . 17 of osa trends in optics and photonics ( optical society of america , 1998 ) , paper mq1 . , _ iso 11146 - 1/2/3 test methods for laser beam widths , divergence angles and beam propagation ratios part 1 : stigmatic and simple astigmatic beams / part 2 : general astigmatic beams / part 3 : intrinsic and geometrical laser beam classification , propagation and details of test methods _ ( iso , geneva , 2005 ) . b. schfer and k. mann , `` determination of beam parameters and coherence properties of laser radiation by use of an extended hartmann - shack wave - front sensor , '' appl . opt . * 41 * , 28092817 ( 2002 ) . b. eppich , g. mann , and h. weber , `` measurement of the four - dimensional wigner distribution of paraxial light sources , '' in _ optical design and engineering ii _ , l. mazuray and r. wartmann , eds . , proc . spie * 5962 * , 59622d ( 2005 ) . r. w. lambert , r. corts - martnez , a. j. waddie , j. d. shephard , m. r. taghizadeh , a. h. greenaway , and d. p. hand , `` compact optical system for pulse - to - pulse laser beam quality measurement and applications in laser machining , '' appl . opt . * 43 * , 50375046 ( 2004 ) . a. e. siegman , _ lasers _ ( university science books , sausalito , 1986 ) . s. saghafi and c. j. r. sheppard , `` the beam propagation factor for higher order gaussian beams , '' opt . commun . * 153 * , 207210 ( 1998 ) . e. tervonen , j. turunen , and a. friberg , `` transverse laser mode structure determination from spatial coherence measurements : experimental results , '' appl . phys . b * 49 * , 409414 ( 1989 ) . a. cutolo , t. isernia , i. izzo , r. pierri , and l. zeni , `` transverse mode analysis of a laser beam by near - and far - field intensity measurements , '' appl . opt . * 34 * , 79747978 ( 1995 ) . m. santarsiero , f. gori , r. borghi , and g. guattari , `` evaluation of the modal structure of light beams composed of incoherent mixtures of hermite - gaussian modes , '' appl . opt . * 38 * , 52725281 ( 1999 ) . x. xue , h. wei , and a. g. kirk , `` intensity - based modal decomposition of optical beams in terms of hermite - gaussian functions , '' j. opt . soc . am . a * 17 * , 10861091 ( 2000 ) . n. andermahr , t. theeg , and c. fallnich , `` novel approach for polarization - sensitive measurements of transverse modes in few - mode optical fibers , '' appl . phys . b * 91 * , 353357 ( 2008 ) . v. a. soifer and m. golub , _ laser beam mode selection by computer generated holograms _ ( crc press , boca raton , 1994 ) . m. duparr , b. ldge , and s. schrter , `` on - line characterization of nd : yag laser beams by means of modal decomposition using diffractive optical correlation filters , '' in _ optical design and engineering ii _ , l. mazuray and r. wartmann , eds . , proc . spie * 5962 * , 59622 g ( 2005 ) . t. kaiser , d. flamm , s. schrter , and m. duparr , `` complete modal decomposition for optical fibers using cgh - based correlation filters , '' opt . express * 17 * , 93479356 ( 2009 ) . d. flamm , o. a. schmidt , c. schulze , j. borchardt , t. kaiser , s. schrter , and m. duparr , `` measuring the spatial polarization distribution of multimode beams emerging from passive step - index large - mode - area fibers , '' opt . lett . * 35 * , 34293431 ( 2010 ) . h. kogelnik and t. li , `` laser beams and resonators , '' appl . opt . * 5 * , 15501567 ( 1966 ) . h. laabs and b. ozygus , `` excitation of hermite - gaussian modes in end - pumped solid - state lasers via off - axis pumping , '' optics & laser technology * 28 * , 213214 ( 1996 ) . g. szeg , _ orthogonal polynomials _ ( amer . math . soc . , providence , 1975 ) .

1101.4610

r

the optical setup in fig . [ fig : setup ] consists of a laser source and two branches that enable two simultaneous but independent measurements of the @xmath0 parameter of the emerging beam . the nd : yag laser can produce different hg@xmath39 modes at @xmath40 nm . the excited hg@xmath39 modes are restricted to @xmath41 since the pump light ( @xmath42 nm ) is coupled into the plane - concave resonator by a horizontally movable fiber @xcite . a beam splitter divides the beam and guides the replicas into the two branches for analysis . determination using a cgh . lower branch : @xmath0 determination by a caustic measurement conform to the iso standard.,scaledwidth=90.0% ] in the first branch a lens images the laser beam waist onto an adapted cgh , which is an amplitude hologram consisting of @xmath43 lee cells with cell widths of 16@xmath44 m . the far field intensity behind the cgh realized by a subsequent @xmath45-setup is recorded by a ccd camera . this intensity pattern contains the information about the weights @xmath14 of the hg modes since the complex conjugated modes are implemented in the cgh called _ correlation filter _ @xcite . hence , the correlation filter technique enables the determination of the @xmath0 factor in real - time using a computer - aided calculation of eq . ( [ eq : m2 ] ) . the cgh for this experiment is designed to simultaneously analyze the amplitudes of 21 hg modes , i.e. , all hg@xmath39 modes with @xmath46 are implemented taking into account a possible rotation of the resonator coordinate system . this correlation filter configuration corresponds to a truncation of all sums in the equations of section [ sec : fund ] . in the second branch of the setup in fig . [ fig : setup ] , an additional lens is used to analyze the caustic of the beam conform to the iso standard @xcite , which serves as a reference measurement . to investigate the reliability of the cgh - based measurement procedure , a modal spectrum of an arbitrarily chosen beam consisting mainly of @xmath47 and @xmath48 is depicted in fig . [ fig : beams ] . using eq . ( [ eq : intens ] ) the intensity distribution in the plane of the cgh can be reconstructed . since the method will only be as good as it is able to reconstruct the investigated beam , the measured intensity distribution is compared to the reconstructed one by calculating their two - dimensional cross - correlation coefficient . a value of 1.0 denotes perfect match . cross - correlation coefficients greater than 0.9 in all investigated cases indicate the excellent functionality of the method . in particular , the cross - correlation coefficient for the beam investigated in fig . [ fig : beams ] is 0.98 . for the determination of @xmath0 , the reconstruction of the intensity profile is not necessary as a matter of course and just shown here to illustrate the functionality of the method . the results for the measurement of the beam propagation ratio using the correlation filter technique and the iso standard method are compared in fig . [ fig : resultx ] . seven different mode mixtures are selected and analyzed to test the accordance of the results of both techniques for beams with different @xmath0 factors . for instance , the beam in fig . [ fig : beams ] is denoted as mix6 . as the bar charts in fig . [ fig : resultx ] show , the results of both measurement techniques are in very good agreement . the @xmath37 parameters confirm the characteristic of the laser to emit only mixtures of @xmath49 modes consistent with the theory . the slight deviations in the @xmath37 factors are caused by several reasons : first , the hologram needs to be placed accurately at the waist position and on the optical axis . furthermore , the waist diameter has to match the beam diameter the correlation filter is designed for . any deviance from the ideal alignment as well as ccd noise affect the measured modal weights resulting in slight inaccuracies of the cgh - based beam quality determination . and @xmath50 factors determined by the cgh technique and the iso standard method , respectively.,title="fig:",scaledwidth=49.0% ] and @xmath50 factors determined by the cgh technique and the iso standard method , respectively.,title="fig:",scaledwidth=49.0% ] the deviation between the differently determined @xmath37 factors behaves statistically , whereas a tendency in the deviation of the @xmath51 values is recognizable : for mixtures with low @xmath51 factors such as mix1 to mix4 , the @xmath51 values determined with the cgh are larger than the ones of the iso conformable measurement . here slight errors of the modal weights occur for higher order modes due to ccd noise producing an offset of the implemented higher order mode amplitudes , which enlarge the cgh - based @xmath51 factors . on the other hand , mix6 and 7 mainly consist of modes from mode groups with @xmath52 near the truncation limit . due to the finite number of implemented modes in the cgh , modal weights of hg@xmath39 modes with @xmath53 , which would increase the beam quality @xmath51 , are set to zero in the experiment . hence , the missing amplitudes cause reduced @xmath51 factors . for mix5 these two effects nearly compensate one another . in all analyzed cases , the maximum measured deviation is 13% for @xmath51 and 5% for @xmath37 . this result demonstrates the functionality of the method , especially when beams with high beam quality are considered . to demonstrate the real - time capability of the all - optical cgh technique , we continuously varied the alignment of the laser cavity and monitored the output . figure [ fig : m2 t ] illustrates an @xmath0 measurement on a time scale of 30s , where the cavity was initially aligned to produce the fundamental hg@xmath54 mode . then we changed the transverse position of the end - pumping fiber @xcite and the @xmath0 factor increased . after 15s we reversed the process to return to the fundamental gaussian mode after 30s . the reachable speed of the method is only limited by the used hardware .

b * 49 * , 409414 ( 1989 ) . x. xue , h. wei , and a. g. kirk , `` intensity - based modal decomposition of optical beams in terms of hermite - gaussian functions , '' j. opt .

we present a real - time method to determine the beam propagation ratio @xmath0 of laser beams . the all - optical measurement of modal amplitudes yields @xmath0 parameters conform to the iso standard method . the experimental technique is simple and fast , which allows to investigate laser beams under conditions inaccessible to other methods . + 99 a. e. siegman , `` how to ( maybe ) measure laser beam quality , '' in _ dpss ( diode pumped solid state ) lasers : applications and issues _ , m. dowley , ed . , vol . 17 of osa trends in optics and photonics ( optical society of america , 1998 ) , paper mq1 . , _ iso 11146 - 1/2/3 test methods for laser beam widths , divergence angles and beam propagation ratios part 1 : stigmatic and simple astigmatic beams / part 2 : general astigmatic beams / part 3 : intrinsic and geometrical laser beam classification , propagation and details of test methods _ ( iso , geneva , 2005 ) . b. schfer and k. mann , `` determination of beam parameters and coherence properties of laser radiation by use of an extended hartmann - shack wave - front sensor , '' appl . opt . * 41 * , 28092817 ( 2002 ) . b. eppich , g. mann , and h. weber , `` measurement of the four - dimensional wigner distribution of paraxial light sources , '' in _ optical design and engineering ii _ , l. mazuray and r. wartmann , eds . , proc . spie * 5962 * , 59622d ( 2005 ) . r. w. lambert , r. corts - martnez , a. j. waddie , j. d. shephard , m. r. taghizadeh , a. h. greenaway , and d. p. hand , `` compact optical system for pulse - to - pulse laser beam quality measurement and applications in laser machining , '' appl . opt . * 43 * , 50375046 ( 2004 ) . a. e. siegman , _ lasers _ ( university science books , sausalito , 1986 ) . s. saghafi and c. j. r. sheppard , `` the beam propagation factor for higher order gaussian beams , '' opt . commun . * 153 * , 207210 ( 1998 ) . e. tervonen , j. turunen , and a. friberg , `` transverse laser mode structure determination from spatial coherence measurements : experimental results , '' appl . phys . b * 49 * , 409414 ( 1989 ) . a. cutolo , t. isernia , i. izzo , r. pierri , and l. zeni , `` transverse mode analysis of a laser beam by near - and far - field intensity measurements , '' appl . opt . * 34 * , 79747978 ( 1995 ) . m. santarsiero , f. gori , r. borghi , and g. guattari , `` evaluation of the modal structure of light beams composed of incoherent mixtures of hermite - gaussian modes , '' appl . opt . * 38 * , 52725281 ( 1999 ) . x. xue , h. wei , and a. g. kirk , `` intensity - based modal decomposition of optical beams in terms of hermite - gaussian functions , '' j. opt . soc . am . a * 17 * , 10861091 ( 2000 ) . n. andermahr , t. theeg , and c. fallnich , `` novel approach for polarization - sensitive measurements of transverse modes in few - mode optical fibers , '' appl . phys . b * 91 * , 353357 ( 2008 ) . v. a. soifer and m. golub , _ laser beam mode selection by computer generated holograms _ ( crc press , boca raton , 1994 ) . m. duparr , b. ldge , and s. schrter , `` on - line characterization of nd : yag laser beams by means of modal decomposition using diffractive optical correlation filters , '' in _ optical design and engineering ii _ , l. mazuray and r. wartmann , eds . , proc . spie * 5962 * , 59622 g ( 2005 ) . t. kaiser , d. flamm , s. schrter , and m. duparr , `` complete modal decomposition for optical fibers using cgh - based correlation filters , '' opt . express * 17 * , 93479356 ( 2009 ) . d. flamm , o. a. schmidt , c. schulze , j. borchardt , t. kaiser , s. schrter , and m. duparr , `` measuring the spatial polarization distribution of multimode beams emerging from passive step - index large - mode - area fibers , '' opt . lett . * 35 * , 34293431 ( 2010 ) . h. kogelnik and t. li , `` laser beams and resonators , '' appl . opt . * 5 * , 15501567 ( 1966 ) . h. laabs and b. ozygus , `` excitation of hermite - gaussian modes in end - pumped solid - state lasers via off - axis pumping , '' optics & laser technology * 28 * , 213214 ( 1996 ) . g. szeg , _ orthogonal polynomials _ ( amer . math . soc . , providence , 1975 ) .

1101.4610

c

we have shown that a modal decomposition of an investigated laser beam allows not only the quantitative determination of its transverse modal content but also of its beam quality factor @xmath0 . using the correlation filter technique , it is possible to determine the modal spectrum in real - time . we demonstrated the working capabilities by analyzing the beam emerging from an end - pumped nd : yag laser . by changing the alignment of its cavity , several hermite - gaussian modes of higher order could be excited . we showed that a correlation analysis involving the first 21 hermite - gaussian modes yields values for a derived @xmath0 parameter , which are in good agreement with the caustic measurements proposed by the iso standard . the advantage of the method is the ability for real - time analysis of the beam that was demonstrated by continuously changing the alignment of the laser cavity and monitoring the beam propagation ratio @xmath0 as a function of time . we conclude that this method provides an experimentally simple possibility to measure the beam propagation ratio @xmath0 , which is compatible to the iso standard in cases where caustic measurements are too time - consuming or even impossible to perform . the additional information about the modal spectrum of the beam is highly advantageous for diverse laser applications .

we present a real - time method to determine the beam propagation ratio @xmath0 of laser beams . m. duparr , b. ldge , and s. schrter , `` on - line characterization of nd : yag laser beams by means of modal decomposition using diffractive optical correlation filters , '' in _ optical design and engineering ii _ , l. mazuray and r. wartmann , eds . , t. kaiser , d. flamm , s. schrter , and m. duparr , `` complete modal decomposition for optical fibers using cgh - based correlation filters , '' opt . providence , 1975 ) .

we present a real - time method to determine the beam propagation ratio @xmath0 of laser beams . the all - optical measurement of modal amplitudes yields @xmath0 parameters conform to the iso standard method . the experimental technique is simple and fast , which allows to investigate laser beams under conditions inaccessible to other methods . + 99 a. e. siegman , `` how to ( maybe ) measure laser beam quality , '' in _ dpss ( diode pumped solid state ) lasers : applications and issues _ , m. dowley , ed . , vol . 17 of osa trends in optics and photonics ( optical society of america , 1998 ) , paper mq1 . , _ iso 11146 - 1/2/3 test methods for laser beam widths , divergence angles and beam propagation ratios part 1 : stigmatic and simple astigmatic beams / part 2 : general astigmatic beams / part 3 : intrinsic and geometrical laser beam classification , propagation and details of test methods _ ( iso , geneva , 2005 ) . b. schfer and k. mann , `` determination of beam parameters and coherence properties of laser radiation by use of an extended hartmann - shack wave - front sensor , '' appl . opt . * 41 * , 28092817 ( 2002 ) . b. eppich , g. mann , and h. weber , `` measurement of the four - dimensional wigner distribution of paraxial light sources , '' in _ optical design and engineering ii _ , l. mazuray and r. wartmann , eds . , proc . spie * 5962 * , 59622d ( 2005 ) . r. w. lambert , r. corts - martnez , a. j. waddie , j. d. shephard , m. r. taghizadeh , a. h. greenaway , and d. p. hand , `` compact optical system for pulse - to - pulse laser beam quality measurement and applications in laser machining , '' appl . opt . * 43 * , 50375046 ( 2004 ) . a. e. siegman , _ lasers _ ( university science books , sausalito , 1986 ) . s. saghafi and c. j. r. sheppard , `` the beam propagation factor for higher order gaussian beams , '' opt . commun . * 153 * , 207210 ( 1998 ) . e. tervonen , j. turunen , and a. friberg , `` transverse laser mode structure determination from spatial coherence measurements : experimental results , '' appl . phys . b * 49 * , 409414 ( 1989 ) . a. cutolo , t. isernia , i. izzo , r. pierri , and l. zeni , `` transverse mode analysis of a laser beam by near - and far - field intensity measurements , '' appl . opt . * 34 * , 79747978 ( 1995 ) . m. santarsiero , f. gori , r. borghi , and g. guattari , `` evaluation of the modal structure of light beams composed of incoherent mixtures of hermite - gaussian modes , '' appl . opt . * 38 * , 52725281 ( 1999 ) . x. xue , h. wei , and a. g. kirk , `` intensity - based modal decomposition of optical beams in terms of hermite - gaussian functions , '' j. opt . soc . am . a * 17 * , 10861091 ( 2000 ) . n. andermahr , t. theeg , and c. fallnich , `` novel approach for polarization - sensitive measurements of transverse modes in few - mode optical fibers , '' appl . phys . b * 91 * , 353357 ( 2008 ) . v. a. soifer and m. golub , _ laser beam mode selection by computer generated holograms _ ( crc press , boca raton , 1994 ) . m. duparr , b. ldge , and s. schrter , `` on - line characterization of nd : yag laser beams by means of modal decomposition using diffractive optical correlation filters , '' in _ optical design and engineering ii _ , l. mazuray and r. wartmann , eds . , proc . spie * 5962 * , 59622 g ( 2005 ) . t. kaiser , d. flamm , s. schrter , and m. duparr , `` complete modal decomposition for optical fibers using cgh - based correlation filters , '' opt . express * 17 * , 93479356 ( 2009 ) . d. flamm , o. a. schmidt , c. schulze , j. borchardt , t. kaiser , s. schrter , and m. duparr , `` measuring the spatial polarization distribution of multimode beams emerging from passive step - index large - mode - area fibers , '' opt . lett . * 35 * , 34293431 ( 2010 ) . h. kogelnik and t. li , `` laser beams and resonators , '' appl . opt . * 5 * , 15501567 ( 1966 ) . h. laabs and b. ozygus , `` excitation of hermite - gaussian modes in end - pumped solid - state lasers via off - axis pumping , '' optics & laser technology * 28 * , 213214 ( 1996 ) . g. szeg , _ orthogonal polynomials _ ( amer . math . soc . , providence , 1975 ) .

1005.0630

c

in the present study we have used observations from the mid - infrared to the submillimeter to properly characterize the ir luminosities for a diverse sample of 22 galaxies spanning a redshift range of @xmath23 . in addition , we have used the mid - infrared spectra of these sources to estimate the fractions of their ir luminosities which arise from an agn . our conclusions can be summarized as follows : 1 . ir ( @xmath6 ) luminosities derived by sed fitting observed 24 @xmath0 flux densities alone are well matched to those when additional mid - infrared spectroscopy and 16 , 70 , and 850 @xmath0 photometry are included in the fits for galaxies having @xmath24 and @xmath25 values typically @xmath26@xmath27 . in contrast , for galaxies lying in a redshift range between 1.4 and 2.6 with @xmath25 values typically @xmath21@xmath27 , ir luminosities derived by sed template fitting using observed 24 @xmath0 flux densities alone overestimate the true ir luminosity by a factor of @xmath35 , on average , compared to fitting all available data . a comparison between the observed mid - infrared spectra with that of the seds chosen from fitting 24 @xmath0 photometry alone and from fitting all available photometric data demonstrates that local high luminosity sed templates show weaker pah emission by an average factor of @xmath35 in this redshift range and do not properly characterize the contribution from pah emission . 2 . after decomposing the ir luminosity into star forming and agn components , we find the agn luminosity to be increasing with increasing difference between the 24 @xmath0-derived and our best - fit ir luminosities . such a trend suggests that the agn power increases with mid - infrared luminosity . however , we also find that the median fraction of the agn to the difference between the 24 @xmath0-derived and best - fit ir luminosities is only 16% suggesting the agn power is almost negligible compared to the bolometric correction necessary to properly calibrate the 24 @xmath0-derived ir luminosities . allamandola , l. j. , tielens , a. g. g. m. , and barker , j. r. 1985 , , 290 , l25 armus , l. , et al . 2007 , , 656 , 148 chary , r .- r . and elbaz , d. 2001 , , 556 , 562 daddi et al . 2007 , , 670 , 156 dale , d. a. , et al . 2005 , , 633 , 857 desai , v. , et al . 2007 , , 669 , 810 elbaz , d. , et al . 2002 , , 384 , 848 engelbracht , c. w. , et al . 2006 , , 642 , l127 leger , a. , and puget , j. l. 1984 , , 137 , l5 madden , s. c. , galliano , f. , jones , a. p. , and sauvage , m. 2006 , , 446 , 877 magnelli , b. , et al . 2009 , , 496 , 57 murphy e. j. , et al . 2009 , , 698 , 1380 pope et al . 2008 , , 675 1171 rigby , j. r. , et al . 2008 , , 675 , 262 smith , j. d. t. , et al . 2007 , , 656 , 770

mid - infrared spectroscopy , along with 16 , 24 , 70 , and 850@xmath0 photometry , for 22 galaxies located in the great observatories origins deep survey - north ( goods - n ) field . we find that infrared ( ir ; @xmath6 ) luminosities derived by fitting local spectral energy distributions ( seds ) with 24 @xmath0 photometry alone are well matched to those when additional mid - infrared spectroscopic and longer wavelength photometric data is used for galaxies having @xmath7 and 24 @xmath0-derived ir luminosities typically @xmath8 .

we present deep _ spitzer _ mid - infrared spectroscopy , along with 16 , 24 , 70 , and 850@xmath0 photometry , for 22 galaxies located in the great observatories origins deep survey - north ( goods - n ) field . the sample spans a redshift range of @xmath1 , 24 @xmath2 m flux densities between @xmath30.2@xmath41.2 mjy , and consists of submillimeter galaxies ( smgs ) , x - ray or optically selected active galactic nuclei ( agn ) , and optically faint ( @xmath5mag ) sources . we find that infrared ( ir ; @xmath6 ) luminosities derived by fitting local spectral energy distributions ( seds ) with 24 @xmath0 photometry alone are well matched to those when additional mid - infrared spectroscopic and longer wavelength photometric data is used for galaxies having @xmath7 and 24 @xmath0-derived ir luminosities typically @xmath8 . however , for galaxies in the redshift range between @xmath9 , typically having 24 @xmath0-derived ir luminosities @xmath10 , ir luminosities are overestimated by an average factor of @xmath35 when sed fitting with 24 @xmath0 photometry alone . this result arises partly due to the fact that high redshift galaxies exhibit aromatic feature equivalent widths that are large compared to local galaxies of similar luminosities . through a spectral decomposition of mid - infrared spectroscopic data , we are able to isolate the fraction of ir luminosity arising from an agn as opposed to star formation activity . this fraction is only able to account for @xmath330% of the total ir luminosity among the entire sample .

0912.5435

i

the launch of @xmath0 satellite in late 2004 has brought about a new era in the field of gamma - ray bursts ( grbs ) . more than 95% of the @xmath3 @xmath0 grbs reported each year had their afterglows detected in x - rays and about 60% detected in the optical , which in turn led to a large fraction of @xmath0 grbs having redshift determination and detailed studies @xcite . new questions have also arisen as the cases of well - observed afterglows keep accumulating , which pose new challenges to the standard grb afterglow model ( for recent reviews see @xcite ) . one of these puzzles is the occasional lack of an optical light curve ( lc ) behavior synchronous to a lc break of the x - ray afterglow that usually indicates the end of a shallow decay phase ( e.g. , @xcite ; but see @xcite ) . the incredible brightness of grbs makes them excellent probes of the distant universe , e.g. , to explore the dust extinction properties of their host environments . typical attempts involve fitting the afterglow spectral energy distributions ( seds ) with template extinction laws , although a more sophisticated approach based on a parameterized model has been proposed @xcite . most studies favor a small magellanic cloud ( smc ) extinction law @xcite . however , the broad 2175- bump characteristic of the milky way ( mw ) extinction law ( also marginally appearing in that of the large magellanic cloud ( lmc ) ) , whose physical carrier remains a long - standing mystery @xcite , was recently identified in a small number of grbs @xcite . in this paper , we present the observations of the @xmath0 grb 060912a optical afterglow , which shows a lc behavior inconsistent with that of the x - ray one , and possible evidence of a 2175- host dust extinction feature in the sed . the gamma - ray and x - ray properties of the grb are summarized in [ sec - he ] . our ground - based observations and the telescopes used , as well as the @xmath0 ultra - violet and optical telescope ( uvot ) data that are extracted from the official online catalogue , are described in [ sec - oa ] . combined analysis of the optical and x - ray data are detailed in [ sec - pla ] , within the context of the standard afterglow model and energy injection hypothesis while also revealing discrepancies to the models . an optical - to - x - ray sed is built in [ sec - sed ] , and the presence of the 2175- feature is argued for through extinction template fitting after an simplified correction for h lyman absorption . a discussion on the implications of our results is given in [ sec - dis ] .

we present optical photometry of the grb 060912a afterglow obtained with ground - based telescopes , from about 100 sec after the grb trigger till about 0.3 day later , supplemented with the @xmath0 optical afterglow data released in its official website . it is shown by our combined x - ray and optical data analysis that this asynchronous behavior is difficult to be reconciled with the standard afterglow theory and energy injection hypothesis .

we present optical photometry of the grb 060912a afterglow obtained with ground - based telescopes , from about 100 sec after the grb trigger till about 0.3 day later , supplemented with the @xmath0 optical afterglow data released in its official website . the optical light curve ( lc ) displays a smooth single power - law decay throughout the observed epochs , with a power - law index of about -1 and no significant color evolution . this is in contrast to the x - ray lc which has a plateau phase between two normal power - law decays of a respective index of about -1 and -1.2 . it is shown by our combined x - ray and optical data analysis that this asynchronous behavior is difficult to be reconciled with the standard afterglow theory and energy injection hypothesis . we also construct an optical - to - x - ray spectral energy distribution at about 700 sec after the grb trigger . it displays a significant flux depression in the @xmath1-band , reminding us of the possibility of a host - galaxy ( at @xmath2 ) 2175- dust absorption similar to the one that characterizes the milky way extinction law . such an identification , although being tentative , may be confirmed by our detailed analysis using both template extinction laws and the afterglow theory . so far the feature is reported in very few grb afterglows . most seem to have a host galaxy either unusually bright for a grb , just like this one , or of an early type , supporting the general suggestion of an anti - correlation between the feature and star - forming activities .

astro-ph9910249

i

the formation epoch of early - type galaxies provides a strong test for galaxy formation models . traditional models assume early - type galaxies formed in a `` monolithic '' collapse at very high redshift , followed by a smooth and regular dimming of the stellar light ( e.g. , searle et al . 1973 ) . in contrast , currently popular models for galaxy formation in cdm cosmologies predict that early - type galaxies were formed in many generations of mergers , and many ellipticals experienced their last major merger at @xmath3 ( e.g. , baugh , cole , & frenk 1996 ) . early - type galaxies are easily studied in clusters , and most of what we have learned about the formation and evolution of early - types has come from studies of rich clusters at @xmath4 ( e.g. , dressler et al . strong constraints on the ages of the stars in early - type galaxies have come from studies of the evolution of the color - magnitude relation ( e.g. , ellis et al . 1997 , stanford et al . 1998 ) and the fundamental plane ( e.g. , van dokkum et al . 1998 ) . these studies are all in remarkable agreement : most of the stars in early - type galaxies appear to have formed at high redshift ( @xmath5 ) , and there is very little cluster - to - cluster scatter in their properties . however , as pointed out by , e.g. , kauffmann ( 1996 ) the time of assembly of massive galaxies may be much more recent than the mean age of their stars . the fp and the cm relation do not provide constraints on the assembly time of early - type galaxies , unless some assumption is made regarding the amount of star formation during and prior to the mergers . the relevance of merging can be constrained by other means . in particular , by studying large samples of distant galaxies the fraction of the galaxy population which is ( at a given epoch ) involved in a merger can be determined ( e.g. , le fevre et al . 1999 ) . here , we report on the merger fraction in the cluster ms105403 at @xmath0 . we have obtained a large hst wfpc2 mosaic of the cluster , and combined this with extensive spectroscopy with the keck telescope . the sample consists of 81 confirmed cluster members observed with hst . the results of this study are presented in full in van dokkum et al .

we present results from a morphological study of the distant x - ray cluster ms105403 at @xmath0 . we have obtained a large , two color hst wfpc2 mosaic of this cluster , and measured redshifts of 186 galaxies in the ms105403 field with the 10 m keck telescope . of 81 spectroscopically confirmed cluster galaxies observerd with hst , 13 are merger systems .

we present results from a morphological study of the distant x - ray cluster ms105403 at @xmath0 . we have obtained a large , two color hst wfpc2 mosaic of this cluster , and measured redshifts of 186 galaxies in the ms105403 field with the 10 m keck telescope . of 81 spectroscopically confirmed cluster galaxies observerd with hst , 13 are merger systems . most of these mergers will likely evolve into luminous elliptical galaxies , and some may evolve into s0 galaxies . if the galaxy population in ms105403 is typical for its redshift up to @xmath1% of ellipticals may have formed in mergers at @xmath2 . the mergers are generally red and have no detected [ oii]3727 emission . this result is consistent with the old stellar ages of ellipticals inferred from other studies . the mergers are preferentially found towards the outskirts of the cluster , indicating they probably occur in infalling clumps . a significant overabundance of close pairs of red galaxies detected in the outskirts of ms105403 confirms the large number of interacting galaxies in this cluster .

1002.3324

r

imaging the target source at the full resolution of the vlbi array , which is @xmath11 mas ( @xmath12 pc , pa=@xmath42 ) , achieved an rms noise level of @xmath43jy beam@xmath5 , but it did not reveal any continuum component in the field of goods 8503 . this indicates the absence of any compact radio continuum emission with flux densities of @xmath44 or @xmath45jy beam@xmath5 , which in turn implies an upper limit to the intrinsic brightness temperature ( corresponding to a rest frequency of @xmath46 ghz ) of @xmath15 k for any compact radio source in goods 8503 . our coherence tests during these observations using two vlbi calibrators show that the lack of a strong point source in goods 8503 at the full resolution of the array can not be due to the phase referencing procedure . the vlbi flux limit reported above is almost an order of magnitude lower than the flux measured by the vla+merlin ( @xmath47jy ) at 1.4 ghz @xcite . this immediately implies that more than 90% of the radio continuum emission in goods 8503 is extended and not confined to a central agn . in the following , we assess whether our hsa observations can recover the flux seen by the vla and merlin . to do so , we applied two dimensional gaussian tapers on the visibility data with various values . however , the only image with a reliable @xmath48 , detection was obtained by applying a gaussian taper falling to 30% at 0.5 m@xmath49 in both the u- and v- directions . this gave a beam size of @xmath50 ( @xmath3 kpc@xmath9 , p.a.=@xmath51 ) . the resulting image is shown in figure 2 . this image is practically made from the shortest baseline in our data set ( phased vla @xmath52 pie town ) , but only after calibrating its visibilities using all the antennas in the array as described in 2 . the rms noise level in this naturally weighted image is 38 @xmath14jy beam@xmath5 . at this resolution , a gaussian model fitting reveals a marginally resolved continuum source with a peak flux density of @xmath4jy beam@xmath5 and a total flux density of @xmath6jy , which agrees well with the flux density measured with the vla+merlin at 1.4 ghz @xcite . deconvolving the synthesized beam from the gaussian fitting model of the source results in @xmath53 for the size of the major axis , and an upper limit of @xmath54 for the size of the minor axis , i.e. , @xmath7 , or @xmath8 kpc@xmath9 . the derived intrinsic brightness temperature limit is @xmath55 k.

our sensitive tapered vlbi image of goods 8503 at 0.47@xmath1 @xmath2 0.34@xmath1 ( @xmath3 kpc ) resolution shows a marginally resolved continuum structure with a peak flux density of @xmath4jy beam@xmath5 , and a total flux density of @xmath6jy , consistent with previous vla and merlin measurements . the deconvolved size of the source is @xmath7 , or @xmath8 no continuum emission is detected at the full vlbi resolution ( @xmath11 mas , @xmath12 pc ) , with a @xmath13 point source upper limit of 26 @xmath14jy beam@xmath5 , or an upper limit to the intrinsic brightness temperature of @xmath15 k. the extent of the observed continuum source at 1.4 ghz and the derived brightness temperature limits are consistent with the radio emission ( and thus presumably the far - infrared emission ) being powered by a major starburst in goods 8503 , with a star formation rate of @xmath162500 @xmath17 . moreover , the absence of any continuum emission at the full resolution of the vlbi observations indicates the lack of a compact radio agn source in this @xmath0 smg .

we present sensitive phase - referenced vlbi results on the radio continuum emission from the @xmath0 luminous submillimeter galaxy ( smg ) goods 8503 . the observations were carried out at 1.4 ghz using the high sensitivity array ( hsa ) . our sensitive tapered vlbi image of goods 8503 at 0.47@xmath1 @xmath2 0.34@xmath1 ( @xmath3 kpc ) resolution shows a marginally resolved continuum structure with a peak flux density of @xmath4jy beam@xmath5 , and a total flux density of @xmath6jy , consistent with previous vla and merlin measurements . the deconvolved size of the source is @xmath7 , or @xmath8 kpc@xmath9 , and the derived intrinsic brightness temperature is @xmath10 k. the radio continuum position of this galaxy coincides with a bright and extended near - infrared source that nearly disappears in the deep hst optical image , indicating a dusty source of nearly 9 kpc in diameter . no continuum emission is detected at the full vlbi resolution ( @xmath11 mas , @xmath12 pc ) , with a @xmath13 point source upper limit of 26 @xmath14jy beam@xmath5 , or an upper limit to the intrinsic brightness temperature of @xmath15 k. the extent of the observed continuum source at 1.4 ghz and the derived brightness temperature limits are consistent with the radio emission ( and thus presumably the far - infrared emission ) being powered by a major starburst in goods 8503 , with a star formation rate of @xmath162500 @xmath17 . moreover , the absence of any continuum emission at the full resolution of the vlbi observations indicates the lack of a compact radio agn source in this @xmath0 smg .

1002.3324

c

we have detected 1.4 ghz emission from goods 8503 ( corresponding to a rest - frame frequency of @xmath164 ghz ) using the hsa . at a relatively low spatial resolution ( @xmath50 ; figure 2 ) the limit on the intrinsic brightness temperature value of the detected continuum source is @xmath10 k. its flux density at this resolution is consistent with that measured with the vla+merlin @xcite . this implies that the radio continuum emission at 1.4 ghz is confined to the extent of the structure seen in the vla+merlin image at @xmath56 resolution @xcite , or to the extent of the deconvolved size scale reported in this paper , which is @xmath7 , or @xmath8 kpc@xmath9 . at the full resolution of our array ( @xmath11 mas ) , the radio emission from goods 8503 is resolved out and does not show any single dominant source of very high brightness temperature ( @xmath57 k ) . this is in contrast to the results obtained by @xcite on a sample of three high-@xmath28 radio - loud quasars imaged with the vlba , namely j1053 - 0016 ( @xmath58 ) , j1235 - 0003 ( @xmath59 ) , and j0913 + 5919 ( @xmath60 ) . in each of these @xmath61 quasars , a radio - loud agn dominates the emission at 1.4 ghz on a few mas size scale , with intrinsic brightness temperatures in excess of @xmath62 k. @xcite have derived an empirical upper limit to the brightness temperature for nuclear starbursts . for a frequency value of 4 ghz ( our rest frequency ) , the resulting limit on the intrinsic brightness temperature is @xmath63 k , while typical radio - loud agns have brightness temperatures exceeding this value by at least two orders of magnitude . these authors also present a possible physical model for this limit involving a mixed non - thermal and thermal radio emitting ( and absorbing ) plasma , constrained by the radio - to - fir correlation for star - forming galaxies . the measured intrinsic brightness temperature limit for the radio source in goods 8503 is consistent with the empirical upper limit value for nuclear starbursts . for goods 8503 , the derived intrinsic brightness temperatures from our vlbi observations are typical of starburst galaxies . however , when compared to local starburst powered ultra - luminous ir galaxies ( ulirgs ; sanders & mirabel 1996 ) , such as arp 220 , mrk 273 , and iras 172080014 @xcite , the radio continuum emission from goods 8503 is an order of magnitude greater in luminosity , but also an order of magnitude larger in extent . in starburst dominated galaxies , the radio continuum is the sum of supernovae ( sne ) , supernova remnants , and residual relativistic electrons in the interstellar medium , as shown in the model presented by @xcite . however , detecting individual sne in goods 8503 at @xmath64 is unlikely . @xcite reported the detection of 49 luminous radio sne in the prototype ulirg arp 220 with flux densities between 0.053 and 1.228 mjy and typical upper limits on their linear extent of less then 1 pc . at the distance of goods 8503 , the flux densities of such luminous radio sne would be between @xmath65jy . these values are two to three orders of magnitude lower that the rms noise levels achieved in our vlbi observations . our radio continuum results with the hsa clearly rule out a compact radio - loud agn in goods 8503 and show physical characteristics consistent with an extreme starburst . however , we can not completely rule out that the radio emission in this source is from a kpc scale radio - jet structure with a very faint compact agn component that contributes to less than 10% of the total radio continuum emission , and hence falls below our detection threshold at the full resolution of the array . therefore , we further extend the discussion regarding the nature of the power source(s ) in this smg , and whether it hosts a radio - quiet agn , by looking into the optical and ir properties of goods 8503 at various bands , as described in the following section . evidence for an intensive starburst in goods 8503 is also seen at various other wavelengths . first , @xcite presented a method of using the local radio fir correlation and the radio and submillimeter flux densities to estimate redshifts of smgs . @xcite derived a simple redshift formula for arp 220-like spectral energy distribution ( seds ) : @xmath66 . with this formula , the measured redshift @xmath67 , and the radio and submillimeter fluxes of goods 8503 , we find its radio and submillimeter sed to be consistent with arp 220 within 20% . this implies that this smg excellently follows the same radio fir correlation as arp 220 , and suggests that its fir emission is powered by a starburst . goods 8503 is among the first smgs with an x - ray detection @xcite . it is detected at soft x - rays in the 2ms _ chandra _ image of the chandra deep field - north ( cdfn ) , but it is not detected at hard x - rays . it has an x - ray luminosity of @xmath68 erg s@xmath5 . these authors suggested that this source is powered by star formation , but they did not rule out a highly obscured agn with low x - ray luminosity . @xcite obtained a mir spectrum on goods 8503 ( gn06 in their paper ) and decomposed the spectrum into pah and `` continuum '' components . the continuum component contributes @xmath69 to its mir luminosity , and such a component can be powered by a dusty agn . the mir spectral decomposition method was further refined by @xcite , who noted that such mir continuum fraction is a strict upper limit on the agn contribution at this wavelength band . however , agn dust components are warmer than those powered by starbursts and contribute mainly to the mir . we therefore expect the agn fraction in the total ir luminosity of goods 8503 to be negligible . none of the above observational evidence , including our hsa observations , absolutely rule out the existence of an obscured agn in goods 8503 . however , a kpc - scale starburst is consistent with all observations from the x - ray to the radio . the last piece of evidence comes from the optical and nir morphologies . for the optical , we combined the latest version of the four ( f435w , f606w , f775w , and f850lp ) _ hst _ acs images from the great observatories origins deep survey ( goods ; @xcite ) to form a deep `` white '' optical image for goods 8503 . for the nir , we used three sets of data . first , lihwai lin et al . ( in preparation ) obtained nearly 30 hr of goods - n imaging data at @xmath70-band with the wide - field infrared camera ( wircam ) on the 3.6 m canada - france - hawaii telescope ( cfht ) . we downloaded these @xmath70-band data from the public archive and reduced them . we also used the wircam on cfht to obtain a deep @xmath71-band image with nearly 50 hr of integration . lastly , we obtained a deep @xmath71-band image of the goods - n with the multi - object infrared camera and spectrograph ( moircs ) on the 8.2 m subaru telescope . this moircs imaging is described in @xcite . in this imaging , goods 8503 received approximately 4 hr of integration . all the above @xmath70- and @xmath71-band images are still being deepened by various groups . all the data reduction was carried out by our group using simple imaging and mosaicking pipeline ( simple , @xcite ) . more details about the @xmath71-band observations and data reduction can be found in @xcite and @xcite . the reduction of the @xmath70-band data is identical to that of the @xmath71-band . here we adopt the moircs @xmath71-band image for morphological analyses because of its high angular resolution ( fwhm @xmath72 ) , and the wircam @xmath71-band image for photometry because of its greater depth . we present the ultradeep acs white , wircam @xmath70 , and moircs @xmath71 images of goods 8503 in figure 3 , and the f435w to 8.0 @xmath14 m photometry in table 2 . the acs fluxes were measured with @xmath73 apertures at the location of the @xmath71 source . this is the maximum possible aperture size for the acs fluxes to be free of contamination from nearby objects . the @xmath70-band image does not have sufficient resolution to separate goods 8503 from nearby objects , and therefore we did not attempt to measure its @xmath70-band flux . the @xmath71-band flux is measured with sextractor @xcite `` auto '' aperture , which approximates its total flux . in addition , @xcite used a clean - like method to construct _ spitzer _ irac source catalogs based on the wircam @xmath71 image . we include their irac fluxes for goods 8503 in table 2 . we present the observed optical to irac sed in figure 4 . goods 8503 is extremely faint in the optical , undetected by even the combination of the four acs images ( also see @xcite ) . it shows some hint of flux at f850lp ( see table 2 ) but nothing appears visually in the f850lp image and the white image . it clearly shows up at @xmath70-band , however it is blended with a nearby galaxy . in the @xmath71-band and _ spitzer _ images , goods 8503 is the brightest galaxy in its neighborhood . with the excellent , @xmath74 , resolution of subaru at @xmath71-band , the stellar component of goods 8503 is resolved . a simple gaussian fit to the source in this @xmath71-band image gives a fwhm of @xmath75 , corresponding to @xmath76 kpc@xmath77 at its redshift . the image shows an elongated morphology , which may be indicative of an edge on rotating disk , and a pronounced central region that coincides with the radio position , but does not dominate the total @xmath71 luminosity . these are consistent with a nuclear starburst hosted by a massive galaxy . the above optical and near - ir observations imply a large galaxy of roughly 9 kpc in size that is entirely hidden by dust . this shows that dense molecular clouds are widely distributed in this galaxy , despite the fact that only its nucleus is actively forming stars . the results obtained from various bands in the electromagnetic spectrum ( radio to the x - ray ) suggest that the dominant power source in the smg goods 8503 is a startburst . therefore , in the following , we derive an estimate of its star formation rate and star formation surface density . the 850 @xmath14 m flux density of goods 8503 implies a total ir luminosity of @xmath78 ( @xmath79 mjy@xmath5 ; @xcite ) . assuming that this ir luminosity is entirely powered by a starburst , then the associated star formation rate ( sfr ) is @xmath80 yr@xmath5 for a salpeter initial mass function ( @xmath81 yr@xmath82 ; @xcite ) . an estimate of the sfr can also be calculated using the conversion factor between radio luminosity and sfr ( @xmath81 yr@xmath83 ; @xcite ) , which is derived using the local radio fir correlation . the radio luminosity of goods 8503 is @xmath84 w hz@xmath5 , and the resulting sfr is @xmath85 yr@xmath5 . the consistency in the sfr values derived from the radio and the ir luminosities simply confirms that this smg follows the local radio - fir correlation . moreover , this suggests that the star formation activity is well confined within the radio source detected in our hsa observations . the size of the source seen in our 1.4 ghz image ( figure 2 ) compares well with other smgs , but is considerably smaller than optically selected starbursting galaxies at high redshift ( see , e.g. , * ? ? ? from the size and the sfr of this smg , we derive a star formation rate surface density of @xmath86 yr@xmath5 kpc@xmath87 . this surface density is extremely high even after including the @xmath88 uncertainty in its size . for instance , the derived @xmath89 in goods 8503 is a few times larger than that seen in a sample of smgs imaged at millimeter wavelengths @xcite . such a high value is at the very high end of smgs ( see figure 3 of @xcite ) , and is comparable to that measured in the two extremely luminous smgs resolved by high resolution submillimeter observations @xcite . furthermore , the @xmath89 in goods 8503 is comparable to that measured in the host galaxy of the @xmath90 qso sdss j114816.64 + 525150.3 @xcite . such high @xmath89 values are consistent with recent theoretical descriptions of ( dust opacity ) eddington limited star formation of a radiation pressure - supperted starbursts on kpc scales @xcite . using the population synthesis model of @xcite , the hyperz package @xcite package , and the acs , @xmath71 , and irac photometry in table 2 , we find a stellar mass of @xmath91 @xmath26 in goods 8503 . the best - fit sed is shown in figure 4 . with a star formation rate of @xmath92 @xmath26 yr@xmath5 , the stellar mass can be doubled in just 56 myr , roughly 1.6% of its hubble time . the model also requires an extinction of @xmath93 to explain the nondetections in the optical bands . we expect the extinction in the nuclear starburst component to be even larger . furthermore , we derive a value of 18 gyr@xmath5 for the star - formation rate per unit stellar mass ( i.e. , specific star - formation rate ; ssfr ) in goods 8503 . this is an order of magnitude higher than that seen in normal star forming galaxies at @xmath94 , which have ssfr values of about @xmath95 gyr@xmath5 @xcite . in summary , goods 8503 has a kpc - scale nuclear starburst with a star formation rate of @xmath92 @xmath26 yr@xmath5 . no evidence of an agn is seen at any wavelength . an upper limit on its mir agn contribution of 50% is estimated by @xcite , but the agn contribution to its total ir luminosity should be much lower . moreover , our hsa observations reveal that more than 90% of the radio continuum emission in this source is extended and not confined to a central compact agn . goods 8503 has a stellar component of @xmath91 @xmath26 with a spatial extent of roughly 9 kpc . this huge and massive stellar component is entirely hidden by dust , suggesting an extremely rich molecular gas reservoir fueling the nuclear starburst .

kpc@xmath9 , and the derived intrinsic brightness temperature is @xmath10 k. the radio continuum position of this galaxy coincides with a bright and extended near - infrared source that nearly disappears in the deep hst optical image , indicating a dusty source of nearly 9 kpc in diameter .

we present sensitive phase - referenced vlbi results on the radio continuum emission from the @xmath0 luminous submillimeter galaxy ( smg ) goods 8503 . the observations were carried out at 1.4 ghz using the high sensitivity array ( hsa ) . our sensitive tapered vlbi image of goods 8503 at 0.47@xmath1 @xmath2 0.34@xmath1 ( @xmath3 kpc ) resolution shows a marginally resolved continuum structure with a peak flux density of @xmath4jy beam@xmath5 , and a total flux density of @xmath6jy , consistent with previous vla and merlin measurements . the deconvolved size of the source is @xmath7 , or @xmath8 kpc@xmath9 , and the derived intrinsic brightness temperature is @xmath10 k. the radio continuum position of this galaxy coincides with a bright and extended near - infrared source that nearly disappears in the deep hst optical image , indicating a dusty source of nearly 9 kpc in diameter . no continuum emission is detected at the full vlbi resolution ( @xmath11 mas , @xmath12 pc ) , with a @xmath13 point source upper limit of 26 @xmath14jy beam@xmath5 , or an upper limit to the intrinsic brightness temperature of @xmath15 k. the extent of the observed continuum source at 1.4 ghz and the derived brightness temperature limits are consistent with the radio emission ( and thus presumably the far - infrared emission ) being powered by a major starburst in goods 8503 , with a star formation rate of @xmath162500 @xmath17 . moreover , the absence of any continuum emission at the full resolution of the vlbi observations indicates the lack of a compact radio agn source in this @xmath0 smg .

1305.5004

r

at about 00:30 ut on 2012 july 29 , a surge occurred in noaa ar 11530 ( s19w00 ) and plenty of material was ejected northward ( see figure 1__b _ _ and animation 1 in the online journal ) . by examining the _ sdo_/hmi line - of - sight magnetograms , we found that the magnetic flux cancellation took place several hours prior to the surge ( figure 1__d _ _ ) . the obvious brightening was observed at 171 at the location of the cancelled flux . this cancellation could be what led to the occurrence of the surge . when the surge first appears and starts to ascend , there is evidence of interaction between it and a loop - shaped filament in the east side of the erupting surge ( see figure 1__e _ _ and animation 2 in the online journal ) . this interaction seems to peel off " the filament and to add mass into the flux rope body . simultaneously , brightenings at the interaction location and the footpoint of the surge at 304 are also observed ( see figure 1__e _ _ and animation 2 in the online journal ) . at about 00:52 ut , the erupting material seemed to be confined and moved toward the west ( see animation 1 in the online journal ) . meanwhile , the bright fine - scale structures are clearly observed . about 52 min later ( 01:44 ut ) , the erupting material arrived at the west end of the flux rope and the entire flux rope was tracked out by the ejected material ( see figure 1__c _ _ ) . it seems that the surge occurs within the flux rope and the footpoint of the surge is located at one end of the flux rope , and thus the material from the surge flows along the flux rope . the approximate length of the flux rope is 596 mm , and the apparent flow speed of the material along the flux rope body is about 150 km s@xmath8 . the flux ropes observed at 304 , 193 , 335 and 131 are roughly the same on the whole . however , they are different in some details . taking the area denoted by white rectangles in figure 1 for example , the 193 observations are similar to those of 171 , and the 304 , 335 and 131 observations are different from 171 observations as the fine - scale structures ( pointed by white arrows ) are not clearly identified in these three channels . on 2012 august 04 , the second flux rope was observed in noaa ar 11539 ( s23e32 ) . before the flux rope was tracked , there existed a filament at the east part of the flux rope ( see figure 2__a _ _ ) . at 11:04 ut , a c2.9 flare occurred at the east of the filament ( see figure 2__e _ _ and animation 4 in the online journal ) , which peaked at 11:47 ut and ended at 12:49 ut . at about 11:14 ut , the filament started to turn over and brighten ( figure 2__b _ _ ) . at about 11:40 ut , the ejected material from the filament successively moved toward the southwest ( see animation 3 in the online journal ) . then the arch - shaped flux rope with helical fine - scale structures was observed clearly ( figure 2__c _ _ ) . the observed length of the flux rope is about 546 mm , and it takes the filament material about 51 min to flow from the east to the west end . the apparent flow velocity along the flux rope body is approximately 180 km s@xmath8 . similar to the first flux rope on 2012 july 29 , the fine - scale structures denoted by the white arrow in white rectangles of figure 2 are identified clearly at 171 and 193 and seems obscure at 304 , 335 and 131 . at about 16:00 ut on august 6 , the east part of the second flux rope erupted , and this eruption resulted in a faint cme with a speed of about 260 km s@xmath8 . the whole flux rope erupted at about 03:00 ut on august 8 , associated with a halo cme with a speed of about 230 km s@xmath8 . as the erupting material arrived at the west extreme end of the first flux rope on 2012 july 29 , the west end showed obvious brightening ( figures 1__c _ _ and 3__a _ _ ) . then partial material went back toward the east and brightened the east end at about 03:02 ut ( see figure 3__d _ _ and animation 1 in the online journal ) . the brightening at the ends makes it possible to determine the ends location . thus we select two areas ( denoted by red and blue rectangles in figure 1__c _ _ ) to investigate the ends and fine - scale structures . by counting the number of fine - scale structures one by one , we notice that the first flux rope is composed of 85@xmath012 fine - scale structures , and 15 well identified fine - scale structures are selected to measure their widths . two examples are shown in figures 3__c _ _ , _ f _ and _ g_. firstly , the intensity - location profiles ( black curves in figures 3__f _ _ and _ g _ ) along slices perpendicular to the fine - scale structures ( slices s1 " and s2 " in figure 3__c _ _ ) are obtained . secondly , we use gaussian function to fit the intensity - location profiles and two gaussian fitting profiles ( blue and red ones ) are shown in figures 3__f _ _ and _ g_. the full width at half maximum ( fwhw ) of the gaussian fitting profile is thought to be the width of fine - scale structure . the average width of these fine - scale structures is 1@xmath1.8 , with the maximum value of 2@xmath1.0 and the minimum value of 1@xmath1.4 . for the first flux rope , there are 12 western footpoints ( fps ) of the fine - scale structures that form the west end of the flux rope ( white circles in figure 3__a _ _ ) . by comparing the 171 observations with line - of - sight magnetograms , we find that all the western fps are rooted in negative polarity fields ( figure 3__b _ _ ) . the net magnetic fluxes of these fps are in the range of 8.6@xmath210@xmath3@xmath68.6@xmath210@xmath4 mx . the magnetic flux of the west end of the flux rope is @xmath64.3@xmath210@xmath5 mx . this is the lower limit of the magnetic flux since some fps are not identified and calculated for they are not accompanied by brightening . the 8 eastern fps are rooted in positive polarity fields ( figures 3__d _ _ and _ e _ ) . the net magnetic fluxes of eastern fps are from 5.6@xmath210@xmath3 to 2.8@xmath210@xmath4 mx . the magnetic flux of the east end of the flux rope is 1.3@xmath210@xmath5 mx , which is less than that of the western end . not all the eastern fps of the fine - scale structures are identified and thus there exists the discrepancy between the two sides . for the second flux rope on 2012 august 04 , we similarly select two areas where the brightening occurs at the ends ( figures 2__c _ _ and 4 ) . this arch - shaped flux rope seems more complex than the first one and has two main western ends ( one in figure 4__a _ _ and the other one in figure 4__d _ _ ) which are separated apart . the flux rope is composed of 102@xmath015 fine - scale structures . the average width of 20 clearly identified fine - scale structures is 1@xmath1.5 . the thickest one has a width of 1@xmath1.7 , and the thinnest one has that of 1@xmath1.1 ( figures 4__c _ _ , _ f _ and _ g _ ) . the line - of - sight magnetograms show that 22 western fps ( 15 ones in figures 4__a__@xmath6__b _ _ and 7 ones in figures 4__d__@xmath6__e _ _ ) of the fine - scale structures are anchored at positive polarity fields ( figures 4__a__@xmath6__b _ _ , _ _ d__@xmath6_e _ ) . the net magnetic fluxes of these western fps are in the range of 1.1@xmath68.1@xmath210@xmath4 mx . the total magnetic flux of western ends of the flux rope is 7.6@xmath210@xmath5 mx . the eastern end of the flux rope is close to the solar limb and not accompanied by euv enhancements , thus it could not be identified . by examining the magnetic field evolution at the fps of the fine - scale structures over 10 hr before the appearance of the flux rope , we find almost half of these fps show converging motion of smaller magnetic structures for both the flux ropes . figure 5 presents one example of the eastern fps of the first flux rope . as seen in the stack plot along slice a@xmath6b " , the west magnetic structure obviously moved toward the east one with a velocity of 0.2 km s@xmath8 and the motion of the east one was slower than the west one , with a velocity of 0.1 km s@xmath8 ( figure 5__e _ _ ) .

for the first event , the interaction between the erupting surge and a loop - shaped filament in the east seems to peel off " the filament and add bright mass into the flux rope body . the second event is associated with a c - class flare that occurs several minutes before the filament activation .

we present the _ solar dynamics observatory _ observations of two flux ropes respectively tracked out by material from a surge and a failed filament eruption on 2012 july 29 and august 04 . for the first event , the interaction between the erupting surge and a loop - shaped filament in the east seems to peel off " the filament and add bright mass into the flux rope body . the second event is associated with a c - class flare that occurs several minutes before the filament activation . the two flux ropes are respectively composed of 85@xmath012 and 102@xmath015 fine - scale structures , with an average width of about 1@xmath1.6 . our observations show that two extreme ends of the flux rope are rooted in the opposite polarity fields and each end is composed of multiple footpoints ( fps ) of the fine - scale structures . the fps of the fine - scale structures are located at network magnetic fields , with magnetic fluxes from 5.6@xmath210@xmath3 mx to 8.6@xmath210@xmath4 mx . moreover , almost half of the fps show converging motion of smaller magnetic structures over 10 hr before the appearance of the flux rope . by calculating the magnetic fields of the fps , we deduce that the two flux ropes occupy at least 4.3@xmath210@xmath5 mx and 7.6@xmath210@xmath5 mx magnetic fluxes , respectively .

1305.5004

i

we present the _ sdo_/aia observations of two flux ropes on 2012 july 29 and august 04 which are tracked out by material from a surge and a failed filament eruption . for the two flux ropes , the apparent speeds of filling of the flux rope structure with chromospheric and coronal plasma are respectively 150 and 180 km s@xmath8 , which are comparable to the typical sound speed for the corona of about 100@xmath6200 km s@xmath8 . for the first flux rope , the approximate length of the flux rope is 596 mm . by examining the fine - scale structures which are observed more clearly , we roughly estimate the twist is about @xmath9 . for event 2 , the observed length of the flux rope is about 546 mm , and the average twist is about 2@xmath9 . seen from the _ solar - terrestrial relations observatory _ ( _ stereo _ ; kaiser et al . 2008 ) b viewpoint , the two flux ropes are both located at the west limb . by using three - dimensional reconstructions , we obtain the heights of the two flux ropes , which are respectively 90 and 140 mm above the solar surface . the two flux ropes analyzed here are respectively composed of 85@xmath012 and 102@xmath015 fine - scale structures , which probably outline the magnetic field structures of flux ropes ( martin et al . 2008 ; lin 2011 ) . the width of the fine - scale structures ranges from 1@xmath1.1 to 2@xmath1.0 , with an average of about 1@xmath1.6 . it is comparable to the resolution limit of the aia telescope of about 1@xmath1.2 , which suggests that even thinner structures may exist . moreover , the width of the fine - scale structures is an order of magnitude larger than the ultrafine magnetic loop structures observed by ji et al . ( 2012 ) . before the flux ropes are tracked out by erupting material , part of magnetic flux rope structures may exist in the space filled in by the flux ropes . for event 1 , there are several similar events in two days before the appearance of the first flux rope on 2012 july 29 . moreover , the 304 images shortly before the surge injection and flux rope appearance reveal the presence of long and thin absorbing threads along the first flux rope . for event 2 , the filament at the east location of the flux rope may indicate part of the pre - existing flux rope structures . when the surge in event 1 appears and the filament in event 2 is activated , the obvious brightenings and flare activities are observed simultaneously at the east of the two flux ropes . this implies that heating takes place and may illuminate the flux rope body by filling it with hot and dense plasma emitting in the euv channels . this is similar to the observations of raouafi ( 2009 ) , who suggested that a c - class flare near one footpoint of the flux rope led to the brightening of the magnetic structure showing its fine structure . while the material arrives at the fps of the fine - scale structures , the fps are consequently brightened . the brightening at the fps may be caused by the conversion from the kinetic energy to the thermal energy . our observations show that there exist 7@xmath615 fps of the fine - scale structures for each end of the flux rope . by comparing the euv observations with the hmi magnetograms , we find that the fps at one end of the flux rope on july 29 are rooted in the same polarity fields and the fps at the other end are anchored at the opposite polarity fields ( figure 3 ) . for the flux rope on august 04 , the eastern end could not be identified and only the western end is analyzed here . the fps of the fine - scale structures are located at network magnetic fields and their magnetic fluxes are in the range of 5.6@xmath210@xmath3@xmath68.6@xmath210@xmath4 mx . the magnetic fluxes of the two flux ropes are at least 4.3@xmath210@xmath5 and 7.6@xmath210@xmath5 mx . according to the statistical study of sung et al . ( 2009 ) , the magnetic flux of 34 magnetic clouds ( mc ) for in - situ observations varies from 1.25@xmath210@xmath3 to 4.69@xmath210@xmath10 mx with the average of 1.1@xmath210@xmath10mx . the magnetic flux of the flux ropes in our observations is comparable to that of the mc . moreover , almost half of the fps of the fine - scale structures show converging motion of smaller magnetic structures over 10 hr before the appearance of the flux rope . the network magnetic field is often thought to be the converging center ( zhang et al . 1998 ) , which is consistent with our observations . as small - scale magnetic fields located at the converging centers always exist tens of hours ( liu et al . 1994 ) , implying that the flux ropes have a relatively long lifetime . the flux ropes are observed in all the 7 euv channels ( 304 , 171 , 193 , 211 , 335 , 94 and 131 ) of the _ sdo_/aia that cover the temperature from 0.05 mk to 11 mk . this is consistent with recent observations of patsourakos et al . ( 2013 ) and li & zhang ( 2013 ) , who reported the hot and cool components of flux ropes . however , there exist the flux ropes that could only be observed in hot channels such as 94 and 131 ( zhang et al . 2012 ; cheng et al . 2011 , 2012 ) . the comprehensive characteristics of flux ropes need to be analyzed in further studies . amari , t. , aly , j .- j . , mikic , z. , & linker , j. 2010 , , 717 , l26 amari , t. , & luciani , j. f. 1999 , , 515 , l81 aulanier , g. , trk , t. , dmoulin , p. , & deluca , e. e.2010 , , 708 , 314 boerner , p. , edwards , c. , lemen , j. , et al . 2012 , , 275 , 41 canou , a. , & amari , t. 2010 , , 715 , 1566 chen , j. 1996 , , 101 , 27499 cheng , x. , zhang , j. , liu , y. , & ding , m. d. 2011 , , 732 , l25 cheng , x. , zhang , j. , saar , s. h. , & ding , m. d. 2012 , , 761 , 62 fan , y. 2005 , , 630 , 543 fan , y. , & gibson , s. e. 2004 , , 609 , 1123 gibson , s. e. , foster , d. , burkepile , j. , de toma , g. , & stanger , a. 2006 , , 641 , 590 guo , y. , schmieder , b. , dmoulin , p. , et al . 2010 , , 714 , 343 hudson , h. , & schwenn , r. 2000 , advances in space research , 25 , 1859 illing , r. m. e. , & hundhausen , a. j. 1986 , , 91 , 1095 ji , h. , cao , w. , & goode , p. r. 2012 , , 750 , l25 jing , j. , yuan , y. , wiegelmann , t. , et al . 2010 , , 719 , l56 kaiser , m. l. , kucera , t. a. , davila , j. m. , st . cyr , o. c. , guhathakurta , m. , & christian , e. 2008 , space sci . , 136 , 5 kliem , b. , & trk , t. 2006 , physical review letters , 96 , 255002 li , l. & zhang , j. 2013 , , 552 , l11 lin , y. 2011 , , 158 , 237 liu , y. , zhang , h. , ai , g. , wang , h. , & zirin , h. 1994 , , 283 , 215 lemen , j. r. , title , a. m. , akin , d. j. , et al . 2012 , sol . phys . , 275 , 17 martin , s. f. , lin , y. , & engvold , o. 2008 , , 250 , 31 odwyer , b. , del zanna , g. , mason , h. e. , weber , m. a. , & tripathi , d. 2010 , , 521 , a21 olmedo , o. , & zhang , j. 2010 , , 718 , 433 patsourakos , s. , vourlidas , a. , & stenborg , g. 2013 , , 764 , 125 parenti , s. , schmieder , b. , heinzel , p. , & golub , l. 2012 , , 754 , 66 pesnell , w. d. , thompson , b. j. , & chamberlin , p. c. 2012 , sol . , 275 , 3 raouafi , n .- e . 2009 , , 691 , l128 schou , j. , & larson , t. p. 2011 , bulletin of the american astronomical society , 1605 sung , s .- k . , marubashi , k. , cho , k .- s . , et al . 2009 , , 699 , 298 trk , t. , & kliem , b. 2003 , , 406 , 1043 trk , t. , & kliem , b. 2005 , , 630 , l97 zhang , j. , cheng , x. , & ding , m .- d . 2012 , nature communications , 3 , 747 zhang , j. , wang , j. , wang , h. , & zirin , h. 1998 , , 335 , 341 aia multi - wavelength images and hmi line - of - sight magnetogram showing the evolution of the flux rope on 2012 july 29 ( see animations 1 and 2 , available in the online edition of the journal ) . the red solid rectangle in panel _ c _ denotes the fov of figure 3__a _ _ and the blue one denotes the fov of figure 3__d__. [ fig1 ] ] aia multi - wavelength images and hmi line - of - sight magnetogram showing the evolution of the flux rope on 2012 august 04 ( see animations 3 and 4 , available in the online edition of the journal ) . the red solid rectangle in panel _ c _ denotes the fov of figure 4__a _ _ and the blue one denotes the fov of figure 4__d__. [ fig2 ] ] aia 171 images and hmi magnetograms showing the western ( panels _ a _ and _ b _ ) and eastern ends ( panels _ d _ and _ e _ ) of the flux rope on 2012 july 29 , and the gaussian fitting profiles ( panels _ f _ and _ g _ ) showing the widths of fine - scale structures . the white rectangle in panel _ a _ denotes the fov of panel _ c _ and white rectangles in panels _ d _ and _ e _ denote the fov of figure 5 . the blue and red curves in panels _ f _ and _ g _ are respectively the gaussian fitting profiles of the intensity - location curves ( black ones ) along the blue and red slices ( slices s1 " and s2 " ) in panel _ c_. [ fig3 ] ] aia 171 images and hmi magnetograms showing two main western ends of the flux rope ( one in panels _ _ a__@xmath6_b _ and the other in panels _ _ d__@xmath6_e _ ) on 2012 august 4 , and the gaussian fitting profiles ( panels _ f _ and _ g _ ) showing the widths of fine - scale structures . the white rectangle in panel _ a _ denotes the fov of panel _ c_.[fig4 ] ] hmi magnetograms showing the converging motion of smaller magnetic structures at the fps of the fine - scale structures . blue circles denote one of the eastern fps ( fp 1 " in figure 3__e _ _ ) of the fine - scale structures for the first flux rope on 2012 july 29 . the stack plot along slice a@xmath6b " ( red dashed line in panel _ a _ ) is shown in panel _ e_. [ fig5 ] ]

solar dynamics observatory _ observations of two flux ropes respectively tracked out by material from a surge and a failed filament eruption on 2012 july 29 and august 04 . the two flux ropes are respectively composed of 85@xmath012 and 102@xmath015 fine - scale structures , with an average width of about 1@xmath1.6 . our observations show that two extreme ends of the flux rope are rooted in the opposite polarity fields and each end is composed of multiple footpoints ( fps ) of the fine - scale structures . the fps of the fine - scale structures are located at network magnetic fields , with magnetic fluxes from 5.6@xmath210@xmath3 mx to 8.6@xmath210@xmath4 mx . moreover , almost half of the fps show converging motion of smaller magnetic structures over 10 hr before the appearance of the flux rope . by calculating the magnetic fields of the fps , we deduce that the two flux ropes occupy at least 4.3@xmath210@xmath5 mx and 7.6@xmath210@xmath5 mx magnetic fluxes , respectively .

we present the _ solar dynamics observatory _ observations of two flux ropes respectively tracked out by material from a surge and a failed filament eruption on 2012 july 29 and august 04 . for the first event , the interaction between the erupting surge and a loop - shaped filament in the east seems to peel off " the filament and add bright mass into the flux rope body . the second event is associated with a c - class flare that occurs several minutes before the filament activation . the two flux ropes are respectively composed of 85@xmath012 and 102@xmath015 fine - scale structures , with an average width of about 1@xmath1.6 . our observations show that two extreme ends of the flux rope are rooted in the opposite polarity fields and each end is composed of multiple footpoints ( fps ) of the fine - scale structures . the fps of the fine - scale structures are located at network magnetic fields , with magnetic fluxes from 5.6@xmath210@xmath3 mx to 8.6@xmath210@xmath4 mx . moreover , almost half of the fps show converging motion of smaller magnetic structures over 10 hr before the appearance of the flux rope . by calculating the magnetic fields of the fps , we deduce that the two flux ropes occupy at least 4.3@xmath210@xmath5 mx and 7.6@xmath210@xmath5 mx magnetic fluxes , respectively .

astro-ph9607067

i

the plethora of low column density , intervening ly@xmath0 absorption lines in the spectra of high redshift qso s ( the `` ly@xmath0 forest '' ) was first recognized by lynds ( 1971 ) and has been described in detail by sargent et al . ( 1980 ) and in many recent reviews and articles ( bajtlik 1993 ; weymann 1993 ; bechtold 1993 ; rauch et al . 1992 ; rauch et al . 1993 ; lu , wolfe , & turnshek 1991 ; smette et al . 1992 ) . a considerable amount has been learned about the nature of these systems at redshifts @xmath14 , the redshift above which ly@xmath0 is observable from the ground . these redshifts are generally too large to directly detect the absorbing objects in emission . however , more recently , a modest number of ly@xmath0 absorbers at low redshift have been detected in the uv ( morris et al . 1991 ; bahcall et al . the proximity of these systems make them ideal targets for searches for h i and optical emission from the vicinity of these clouds . one can also seek possible identifications of parent objects with which the clouds might be associated . the first low - redshift ly@xmath0 forest absorption lines were discovered in the iue spectrum of pks 2155 - 304 by maraschi et al . since then , the hst has revealed many low column density absorbers in the nearby universe ( bahcall et al . 1991 ; bahcall et al . 1993 ; morris et al . 1991 ; bruhweiler et al . 1993 ; stocke et al . 1995 ; shull et al . statistical studies have been made to determine the relative correlation between these ly@xmath0 absorbing clouds and optical galaxies ( morris et al . 1991 ; salzer 1992 ; stocke et al . 1995 ; lanzetta et al . 1995 ; mo & morris 1994 ; morris et al . 1993 ; morris & van den bergh 1994 ) . the current consensus is that the systems do correlate weakly with bright galaxies , but less so than these galaxies with other galaxies ( stocke et al . lanzetta et al . ( 1995 ) find good evidence that some of the stronger ly@xmath0 absorbers are physically close to galaxies , but there are also examples of clouds with no optical galaxy to within a few mpc ( stocke et al . 1995 ; shull et al . 1996 ) . morris et al . ( 1991 ) find , in one instance , an anti - correlation between a region of very high galaxy density and ly@xmath0 forest absorbing clouds . stocke et al . ( 1995 ) find more generally that : `` the higher equivalent width absorbers are distributed more like galaxies than the lower equivalent width absorbers , which are distributed in a manner statistically indistinguishable from clouds randomly placed with respect to galaxies . '' in this paper , we present a search for h i emission from the vicinity of seven nearby ly@xmath0 absorbers . h i imaging surveys routinely find gas - rich , optically uncataloged galaxies , and as such our search is complementary to the optical surveys mentioned above . in addition to searching for a possible parent population of the ly@xmath0 absorbers , the h i morphology of galaxies close to the line of sight might betray hints of unusually large gaseous extents . in the first study of this kind ( van gorkom et al . 1993 ) a deep search for h i emission was made around two ly@xmath0 clouds on the 3c 273 line of sight , which are located in the outskirts of the virgo cluster . no obvious associations between these two ly@xmath0 clouds and h i emitting galaxies were found . the seven systems studied here are located in a wide range of cosmic environments . the absorbers seen along the sight line toward mrk 501 are located in a void and a very low density region , respectively , while the other five absorbers are located in regions of moderately high galaxy density , along the sight lines toward pks 2155 - 304 and mrk 335 . the results of the h i search near the sight line toward mrk 501 have already been presented by stocke et al . ( 1995 ) . here , those observations will be presented in somewhat more detail . we describe the systems and observations in 2 and 3 . we present the results in 4 , and in 5 we briefly discuss their implications . throughout this paper we adopt heliocentric velocities , using the optical definition , @xmath15 , where c is the speed of light and the redshift is defined as @xmath16 , where @xmath17 and @xmath18 are the observed and rest wavelengths , respectively .

we present the results of a vla and wsrt search for h i emission from the vicinity of seven nearby clouds , which were observed in ly@xmath0 absorption with hst toward mrk 335 , mrk 501 and pks 2155 - 304 . around the absorbers we detected h i emission in the vicinity of four out of seven absorbers . two other , stronger absorbers toward pks 2155 - 304 at @xmath12 km no h i emission was detected from the vicinity of the two absorbers , which are located in a void and a region of very low galaxy density ; but the limits are somewhat less stringent than for the other sight lines .

we present the results of a vla and wsrt search for h i emission from the vicinity of seven nearby clouds , which were observed in ly@xmath0 absorption with hst toward mrk 335 , mrk 501 and pks 2155 - 304 . around the absorbers , we searched a volume of @xmath1 1000 km s@xmath2 ; for one of the absorbers we probed a velocity range of only 600 km s@xmath2 . the h i mass sensitivity ( 5 @xmath3 ) very close to the lines of sight varies from @xmath4 m@xmath5 at best to @xmath6 m@xmath5 at worst . we detected h i emission in the vicinity of four out of seven absorbers . the closest galaxy we find to the absorbers is a small dwarf galaxy at a projected distance of @xmath7 kpc from the sight line toward mrk 335 . this optically uncataloged galaxy has the same velocity ( @xmath8 km s@xmath2 ) as one of the absorbers , is fainter than the smc , and has an h i mass of only @xmath9 m@xmath5 . we found a somewhat more luminous galaxy at exactly the velocity ( @xmath10 km s@xmath2 ) of one of the absorbers toward pks 2155 - 304 at a projected distance of @xmath11 kpc from the sight line . two other , stronger absorbers toward pks 2155 - 304 at @xmath12 km s@xmath2 appear to be associated with a loose group of three bright spiral galaxies , at projected distances of 300 to @xmath13 kpc . these results support the conclusions emerging from optical searches that most nearby ly@xmath0 forest clouds trace the large - scale structures outlined by the optically luminous galaxies , although this is still based on small - number statistics . we do not find any evidence from the h i distribution or kinematics that there is a physical association between an absorber and its closest galaxy . while the absorbing clouds are at the systemic velocity of the galaxies , the h i extent of the galaxies is fairly typical , and at least an order of magnitude smaller than the projected distance to the sight line at which the absorbers are seen . on the other hand , we also do not find evidence against such a connection . in total , we detected h i emission from five galaxies , of which two were previously uncataloged and one did not have a known redshift . no h i emission was detected from the vicinity of the two absorbers , which are located in a void and a region of very low galaxy density ; but the limits are somewhat less stringent than for the other sight lines . these results are similar to what has been found in optically unbiased h i surveys . thus , the presence of ly@xmath0 absorbers does not significantly alter the h i detection rate in their environment .

astro-ph9607067

c

our search for h i emission from the vicinity of nearby ly@xmath0 absorbers has resulted in the detection of five galaxies , two of which were previously uncataloged . we shall first discuss whether this detection rate is unusual in any sense : does the presence of a ly@xmath0 absorber increase the chance of finding h i in emission ? following that , we shall discuss what we have learned from the detections , and whether there is any indication that the h i in emission is related to the ly@xmath0 absorption . finally we will discuss whether the present observations have illuminated the nature of the nearby ly@xmath0 absorbers . a variety of data is available to assess whether our detection rate of h i - rich systems is unusual in any way . briggs ( 1990 ) summarized the results of all major unbiased h i surveys , while the currently most accurate h i luminosity function has been constructed by rao & briggs ( 1993 ) . more specific and directly comparable to our result is the work by weinberg et al . ( 1991 ) and szomoru et al . ( 1994 , 1996 ) , who used the vla to do unbiased h i surveys in environments of differing galaxian density . szomoru et al . ( 1994 ) probed voids as well as supercluster environments and compared fields centered on optically known galaxies and optically blank fields . for simplicity sake , we take as the volume searched in our survey the region within a radius of 22@xmath23 from the pointing center . this is the 20@xmath38 point of the primary beam ; beyond that , the shape of the beam is highly uncertain . our search within that volume is complete to the 5 @xmath3 limits listed in table 3 , multiplied by five ( correcting for the primary beam response ) . the volume searched down to a mass limit of @xmath53 of h i is @xmath54 mpc@xmath55 . in this volume , we detected three galaxies with h i masses of a few times 10@xmath56 m@xmath57 of h i , giving a density of 0.05 @xmath58 0.02 mpc@xmath59 . the volume searched down to @xmath60 of h i is much smaller , @xmath61 mpc@xmath55 . two galaxies of even smaller masses were detected in that volume , bringing the galaxy density in the mass range of 10@xmath62 m@xmath57 to @xmath63 to @xmath64 mpc@xmath59 . these h i mass densities are quite consistent with the results of briggs ( 1990 ) , who found a density of @xmath65 mpc@xmath59 and @xmath66 mpc@xmath59 for h i masses of a few times 10@xmath56 m@xmath57 and 10@xmath67 m@xmath57 respectively . only a small fraction of the volume searched , @xmath68 mpc@xmath55 , is in a true void ; the remaining volume is more characteristic of supercluster densities . weinberg et al . ( 1991 ) found a cumulative space density of @xmath69 mpc@xmath59 for gas rich dwarfs above 10@xmath67 m@xmath57 of h i in the perseus pisces supercluster , a result similar to ours . in conclusion , although the statistics are small , it appears that the presence of nearby ly@xmath0 forest absorbers has not significantly altered the detection rate of h i emitting objects in either the void or the high - density regions . nevertheless , the detections of two galaxies almost exactly at the velocity of their nearby ly@xmath0 absorbers , and the fact that these are the only detections in a 500 and 1000 km s@xmath2 range for pks 2155 - 304 and mrk 335 respectively , beg the question whether there is a possible association between the galaxies and the absorbers . the most tantalizing system is the uncataloged dwarf galaxy at a projected distance of @xmath47 kpc from the line of sight toward mrk 335 . the absolute magnitude of this dwarf has been estimated to be @xmath70 based upon a linear extrapolation of the calibration supplied by eight , nearby hst guide stars on the digitized version of the poss - e plate material . this approximate magnitude assumes that h@xmath71 = 100 km s@xmath2 mpc@xmath2 despite the location of this object within the bounds of the local supercluster . the proximity , spatially and in velocity , of the ly@xmath0 absorber and dwarf irregular could mean no more than that they originated in a common larger scale structure , e.g. , a filament ( cen et al . 1994 ; hernquist et al . 1996 ; miralda - escud et al . 1996 ; mcket et al . alternatively , it could imply that the ly@xmath0 cloud is gravitationally bound to the dwarf . perhaps , it is still falling in or has been ejected in a galactic wind . the kinematic structure does not help to choose between these various possibilities . the minimum dynamical mass in the ly@xmath0 cloud + dwarf galaxy system needed to make it a bound system can be derived by requiring that the total kinetic energy of the system is less or equal to the potential energy . thus , @xmath72 where g is the gravitational constant , @xmath73 the line - of - sight velocity difference and @xmath74 the projected distance between absorber and galaxy . the minimum dynamical mass is 4.6 @xmath75 10@xmath56 m@xmath57 . a crude estimate of the mass of the dwarf galaxy can be obtained from the h i kinematics . assuming a total h i extent of 3.8 kpc and a rotation velocity of 55 km s@xmath2 , we find @xmath76 . thus , in order for the ly@xmath0 cloud to be bound to the galaxy , the dwarf needs to be embedded in a massive dark halo . an intriguing possibility is that the ly@xmath0 absorption arises from within a mostly ionized gas disk of the dwarf galaxy . maloney ( 1992 ) and stocke et al . ( 1995 ) discussed the possibility that nearby ly@xmath0 lines could be produced by gas at large radii in the disks of spiral and irregular galaxies . maloney concludes that the unexpectedly large number of low - redshift ly@xmath0 absorption lines seen with hst toward 3c 273 can be produced by extended ionized gas disks in the halos of spiral and irregular galaxies . the observed frequency of absorbers requires that either l@xmath77 galaxies have huge ( several hundred kpc ) halos or , more plausibly , that the decrease of absorption cross section with declining luminosity is slow enough for low - luminosity galaxies to dominate the integrated cross section . shull et al . ( 1996 ) make the case that , for absorbers of mean radius @xmath78 , only dwarf galaxies have the comoving space densities , @xmath79 necessary to explain the frequency of low - redshift ly@xmath0 clouds . for reference , this density is over 20 times that of @xmath80 galaxies , recently estimated as @xmath81 mpc@xmath59 ( marzke et al . 1994 ) . a first hint that low - luminosity galaxies may indeed dominate the cross section comes from the discovery ( barcons et al . 1995 ) of possibly corotating ly@xmath0 absorption at large ( 50 kpc ) projected distance from two small , late - type spiral galaxies . contrary to the cases found by barcons et al . ( 1995 ) , we have no evidence for corotation of the ionized gas with the galaxy , the ly@xmath0 absorption occurs too close to the minor axis of the galaxy . the small velocity difference between the absorber and the systemic velocity of the galaxy is of course not inconsistent with corotation , but at that large distance anything that is bound to the galaxy is expected to have a velocity close to the systemic velocity of the galaxy . although stocke et al . ( 1995 ) discussed the problems with huge ionized halos around a single bright spiral galaxy , it might be possible that the ly@xmath0 absorption at @xmath82 kpc from the dwarf arises in an ionized halo . using the model calculations of maloney ( 1992 ) and dove & shull ( 1994 ) , we find that an ionized 80100 kpc halo is not at all unlikely for a dwarf galaxy . for example , consider a spherical dark - matter halo , with central density @xmath83 , core radius @xmath84 , and asymptotic halo velocity @xmath85 . the three - dimensional velocity dispersion is @xmath86 . in equilibrium , the gaseous hydrogen will settle into an atmosphere above the disk plane , with density @xmath87 \;,\eqno(3)\ ] ] where @xmath88 is the vertical scaleheight and @xmath89 is the thermal velocity of hydrogen at temperature @xmath90 . at a radius @xmath91 from the galactic center , we may express the total hydrogen density at the disk midplane as , in the optically - thin limit , the neutral hydrogen density is set by photoionization equilibrium , @xmath94 where we adopt a case - a radiative recombination rate coefficient @xmath95 and a hydrogen photoionization rate @xmath96 . here , we express the metagalactic ionizing radiation field , @xmath97 , with @xmath98 at @xmath99 ev and adopt a spectral index @xmath100 . for a fully ionized gas with @xmath101 and @xmath102 , we find @xmath103 and @xmath104 note that @xmath105 is proportional to @xmath106 , owing to the @xmath107 dependence of the recombinations that form h i. in the inner portions of disks , where the gas layer is optically thick to external ionizing radiation , the h i radial distribution , @xmath108 , closely tracks that of total hydrogen , @xmath109 . however , in the extended disk , beyond the radius at which the integrated column of h i drops below several times @xmath110 @xmath27 , the disk becomes optically thin to ionizing radiation , and the above photoionization analysis applies . in this regime , the radial h i distribution falls off as @xmath106 , which in an exponential gaseous disk results in a very sharp falloff in h i. however , in disks with power - law gaseous distributions , @xmath111 ( @xmath112 ) , the h i decreases with radius as @xmath113 . let us now compare these expectations to the observed ly@xmath0 absorbers , which typically have columns n(h i ) @xmath114 @xmath27 . from eq . ( 8) , if the hst - observed ly@xmath0 cloud has h i column density @xmath115 at @xmath116 , the gaseous disk at that radius must have a total hydrogen column density @xmath117 assuming the optically - thin limit . the vla observations of the dwarf h i galaxy toward mrk 335 yield an h i column of @xmath118 @xmath27 at @xmath119 , corresponding to @xmath120 kpc at the recessional velocity of 1970 km s@xmath2 . if we assume that the radial distribution of total hydrogen column density is @xmath121 ( i.e. , @xmath122 ) and integrate over radii @xmath123 , where @xmath124 kpc , the total gaseous mass of the extended disk is @xmath125 where we adopt a mean molecular mass @xmath126 . the mass of the isothermal dark - matter halo required to confine the gas in equilibrium is given by , @xmath127 the ratio of halo mass to gas mass is therefore @xmath128 , not dissimilar from values in other galaxies . a possible physical association between the ly@xmath0 absorber at 5100 km s@xmath2 seen toward pks 2155 - 304 and eso 466-g032 is even less clear cut . the projected distance between the two is @xmath11 kpc . lanzetta et al . ( 1995 ) find that only 1 out of 9 galaxies at projected distances larger than @xmath129 kpc from the line of sight toward hst spectroscopic target qso s gives rise to associated ly@xmath0 absorption , while 5 out of 5 galaxies at distances less than @xmath130 kpc give rise to associated ly@xmath0 absorption . however more recent data by bowen et al . ( 1996 ) and le brun et al . ( 1996 ) show that the covering factor of galaxies between 50 and @xmath131 kpc is roughly 0.5 for equivalent widths larger than 0.3 . thus , our discovery does not seem that unusual . the galaxy is a small sb spiral with @xmath132 . it would be quite extraordinary if it had a gaseous halo extending out to 250 kpc or so . the long dynamic time scales at those distances make it unlikely that the gas has virialized or settled into a disk ( stocke et al . note , however , that zaritski & white ( 1994 ) find that isolated spirals have dark halos extending out to 200 or 300 kpc , thus even if the ly@xmath0 absorber is not part of a halo of ionized gas , it may still sit in the potential of the galaxy . as in the case of mrk 335 , the kinematics of the galaxy do not help to elucidate the situation , the ly@xmath0 absorber is at the systemic velocity of the galaxy . in the high - velocity range toward pks 2155 - 304 , we see three galaxies at rather large projected distances from the line of sight . the three galaxies have a mean velocity of 17,021 km s@xmath2 and a line of sight velocity dispersion of 138 km s@xmath2 , typical of a loose group of galaxies . the ly@xmath0 absorption at 17,100 km s@xmath2 occurs close to the mean velocity . in this case , it seems more plausible that the absorption arises in some general intergalactic gas within a small group , rather than from one galaxy in particular ( mulchaey et al . 1993 , 1996 ) . the galaxy to the southwest is in projection closest to the line of sight toward the quasar at a distance of @xmath24 kpc . thus , if the absorption arises in the halo of the nearest galaxy , the halo would have to extend well beyond 300 kpc . the existence of such a huge ionized halo is problematic by itself ( stocke et al . 1995 ) , in a group environment it will definitely not survive . of course the intragroup gas may be just that , the remains of the shredded halos . it is interesting that the absorption at 17,100 km s@xmath2 is one of the stronger absorption systems . the situation is reminiscent of the absorbers found toward 3c 273 in the outskirts of the virgo cluster ( bahcall et al . 1991 ; morris et al . several galaxies are found at distances of 200 to 300 kpc from the sight line , but it is not possible to associate the absorbers with individual galaxies ( morris et al . 1993 ; salpeter and hoffman 1995 ; rauch et al . 1996 ) . as in the present case , the absorbers toward 3c 273 have slightly higher column density . although the current data for the pks 2155 - 304 system , plagued as they are by interference , are not sensitive enough to detect small gas rich dwarfs , such as the one found toward mrk 335 , the 3c 273 data definitely rule out the existence of such dwarfs within 100 kpc from the line of sight toward 3c 273 ( van gorkom et al . 1993 ) . the absorption at 16,488 km s@xmath2 seems more difficult to explain . it is quite far off from the mean velocity of the group . the h i emission from f21569 - 330 at a projected distance of @xmath50 kpc comes closest in velocity going down to 16,650 km s@xmath2 , but not only is the distance to the sight line huge , the approaching side of the galaxy is on the far side from the sight line to the quasar . since for this group we have only sampled the upper end of the h i mass function it is not unlikely that other galaxies are present which have h i at the same velocity as the absorber . thus it seems plausible that this absorber is associated with the group as well . in a recent paper lanzetta , webb and barcons ( 1996 ) report the identification of a group of galaxies at a redshift of 0.26 , that produce a complex of corresponding ly @xmath0 absorption lines . as in the present case one of the absorption systems has a slightly higher column density . thus it seems that ly @xmath0 absorption arising in intra group gas may be quite common and that the colomn densities in those environments may be somewhat higher than what is seen near more isolated galaxies . a search for h i emission from the vicinity of nearby ly@xmath0 absorbers has resulted in the discovery of some low luminosity galaxies at the same redshift of some of the absorbers , but at large ( 70 to 250 kpc ) projected distances from the sight line . in addition a group of galaxies was found near two absorbers at a velocity of about 17000 km s@xmath2 . this confirms previous suggestions that nearby ly@xmath0 absorbers are weakly correlated with galaxies . individual , more isolated , galaxies may have absorbers that are physically associated with them , either due to infall , galactic winds or tidal disturbances . in regions of higher galactic density this material may be stripped from individual galaxies and distributed more uniformly through the intergalactic medium . this project was undertaken in the hope of finding a possible parent population associated with nearby ly@xmath0 absorbers : either luminous galaxies with very extended gaseous envelopes or very low luminosity , but gas rich galaxies , which could have escaped optical detection . we did indeed find a few optically uncataloged galaxies , which turned out to be very close in velocity to , but at large projected distances from the ly@xmath0 absorbers . two of the absorbers appear associated with a group of galaxies . these results are very similar to searches for a possible parent population at optical wavelengths . most absorbers at low redshift appear to coincide with the large scale structure outlined by the more luminous galaxies ( rauch et al . 1996 ; stocke et al . 1995 ) as was first suggested by oort ( 1981 ) . one of the outstanding questions is whether the nearby ly@xmath0 absorbers are actually connected to individual galaxies or simply coincide in redshift . our observations do to a certain extent strengthen the idea that at least some nearby ly@xmath0 absorbers may be arising in mostly ionized halos of individual galaxies . the discovery in our most sensitive observation of a very small galaxy at @xmath7 kpc from the line of sight toward mrk 335 , suggests that : ( 1 ) deeper surveys may turn up more such candidates ; and ( 2 ) the suggestion ( maloney 1992 ; shull et al . 1996 ) that the ionized halos of smaller galaxies may contribute significantly to the total ly@xmath0 absorbing cross section in the nearby universe may be valid . the strongest evidence for a physical connection between nearby ly@xmath0 absorbers and galaxies comes from the statistical work by lanzetta et al . ( 1995 ) , who showed that within @xmath130 kpc from a galaxy there is a 100% chance of detecting ly@xmath0 absorption . there are however also some ly@xmath0 clouds with no optical galaxy within a few mpc ( stocke et al . 1995 ; shull et al . 1996 ) . in one case , an anticorrelation between a region of high galaxy density and ly@xmath0 forest absorbing clouds has been found ( morris et al . 1991 ) . the difference between these results may primarily be due to a difference in cloud column densities . the lanzetta et al ( 1995 ) absorbers have significantly higher h i column densities than those studied by morris et al . ( 1991 ) , stocke et al . ( 1995 ) and shull et al . ( 1996 ) . even if a physical connection is apparent , it is not obvious what the nature of the extended gas is . while barcons et al . ( 1995 ) find in two cases ly@xmath0 absorption that could possibly be interpreted as arising in a corotating halo , there are several examples of even higher column density absorbers and metal lines , where the gas , although clearly associated with galaxies , is not corotating , but instead arises in tidally disturbed gas ( e.g. , womble 1992 ; carilli & van gorkom 1992 ; bowen et al . thus the final verdict is not out yet . low column density gas is likely to be found near galaxies , and many possible scenarios can bring it there : retarded infall , outflow , corotating ionized disks , tidal disturbances . quite likely , all of these occur . perhaps most puzzling are the clouds that do nt have any galaxies within many mpcs . these may arise in the filamentary structures as produced in simulations of gravitational structure formation ( cen et al . 1994 ; hernquist et al . 1996 ; miralda - escud et al . 1996 ; mcket et al . 1996 ) , or they may be associated with as yet undetected dwarf galaxies . this brings us to the final question , what is the connection , if any , between the high redshift ly@xmath0 forest clouds and nearby ly@xmath0 absorbers ? as was pointed out by rauch et al . ( 1996 ) , the size estimate for coherent ly@xmath0 absorption at large redshifts ( bechtold et al . 1994 ; dinshaw et al . 1994 ; fang et al . 1996 ) is typically larger than the transverse separation between galaxies near low redshift ly@xmath0 absorbers . this not only argues against single extended galactic disks or halos as the main origin for the coherent absorption on large scales seen at high redshifts . it also argues against the low redshift absorbers being physically the same as the high redshift absorbers . however , it may well be that at low redshifts galaxies and absorption systems trace the general matter distribution on large scales , a hypothesis that can only be tested statistically using a large ensemble of nearby ly@xmath0 clouds . jhvg thanks john hibbard for comments on an earlier version of this manuscript and for stimulating discussions on the nature of ly@xmath0 clouds . we are grateful to tony foley for help with the wsrt observations . we thank the nfra ( netherlands foundation for research in astronomy ) and the nrao ( national radio astronomy observatory ) for allocation of observing time . the nrao is operated by associated universities , inc . under a cooperative agreement with the national science foundation . this research was partly supported by nsf grant ast 90 - 23254 to columbia university , a nova research fellowship to clc at the university of leiden , and through a hst guest observer grant ( go-3584.01 - 91a ) and the nasa astrophysical theory program ( nagw-766 ) at the university of colorado . jhvg thanks the astronomy dept of caltech , where part of this work was done , for hospitality , wal sargent and nick scoville for financial support , and shri kulkarni for entertainment . this research has made use of the nasa / ipac extragalactic database ( ned ) which is operated by the jpl , caltech , under contract with nasa . allen , r. g. , smith , p. s. , anger , j. r. , miller , b. w. , anderson , s. f. & margon , b. 1993 , apj , 403 , 610 bahcall , j. n. , jannuzi , b. t. , schneider , d. p. , hartig , g. f. , bohlin , r. & junkkarinen , v. 1991 , apj , 377 , l5 bahcall , j. n. et al . 1993 , apjs , 87 , 1 bajtlik , s. 1993 , in the evolution and environment of galaxies , ed . j. m. shull & h. a. thronson , ( dordrecht : kluwer ) , 191 barcons , x. , lanzetta , k. m. & webb j. k. 1995 , nature , 376 , 321 bechtold , j. 1993 , in the evolution and environment of galaxies , ed . j. m. shull & h. a. thronson ( dordrecht : kluwer ) , 559 bechtold , j. , crotts , a. p. s. , duncan , r. c. & fang , y. 1994 , apj , 437 , l83 bowen , d. v. , blades , j. c. & pettini , m. 1995 , apj , 448 , 634 bowen , d. v. , blades , j. c. & pettini , m. 1996 , apj , 464 , 141 briggs , f. 1990 , aj , 100 , 999 bruhweiler , f. c. , boggess , a. , norman , d. j. , grady , c. a. , urry , c. m. & kondo , y. 1993 , apj , 409 , 199 carilli , c. l. & van gorkom , j. h. 1992 , apj , 399 , 373 cen , r. , miralda - escud , j. , ostriker , j. p. & rauch , m. 1994 , apj , 437 , l9 cornwell , t. j. , uson , j. m. & haddad , n. 1992 , , 258 , 583 dinshaw , n. , impey , c. d. , foltz , c. b. , weymann , r. j. & chaffee , f. h. 1994 , apj , 437 , l87 dove , j. b. & shull , j. m. 1994 , apj , 423 , 196 fang , y. , duncan , r. c. , crotts , a. p. s. & bechtold , j. 1996 , apj , 462 , 77 hernquist , l. , katz , n. weinberg , d. h. & miralda - escud j. 1996 , apj , 457 , l51 lanzetta , k. , bowen , d. v. , tytler , d. & webb j. k. 1995 , apj , 442 , 538 lanzetta , k. , webb , j. k. & barcons , x. 1996 , apj , 456 , l17 le brun , v. , bergeron , j. & boiss p. 1996 , , 306 , 691 lu , l. , wolfe , a. & turnshek , d. a. 1991 , apj , 367 , 19 lynds , r. 1971 , apj , 164 , l73 maloney , p. 1992 , apj , 398 , l89 maraschi , l. , blades , j. c. , calanchi , c. , tanzi , e. g. & treves , a. 1988 , apj , 333 , 660 marzke , r. o. , huchra , j. p. & geller , m. j. 1994 , apj , 428 , 43 miralda - escud , j. , cen , r. , ostriker , j. p. & rauch , m. 1995 , preprint mo , h. j. & morris , s. l. 1994 , mnras , 269 , 52 morris , s. l. & van den bergh , s. 1994 , apj , 427 , 696 morris , s. l. , weymann , r. j. , dressler , a. , mccarthy , p. j. , smith , b. a. , r. j. , giovanelli , r. & irwin , m. 1993 , apj , 419 , 524 morris , s. l. , weymann , r. j. , savage , b. d. & gilliland , r. l. 1991 , apj , 377 , l21 mcket , j. p. , petitjean , p. & kates , r. e. 1996 , , 308 , 17 mulchaey , j. s. , davis , d. s. , mushotzky , r. f. & burstein , d. 1993 , apj , 404 , l9 mulchaey , j. s. , mushotzky , r. f. , burstein , d. & davis , d. s. 1996 , apj , in press oort , j. h. 1981 , , 94 , 359 rao , s. & briggs , f. 1993 , apj , 419 , 515 rauch , m. , carswell , r. f. , chaffee , f. h. , foltz , c. b. , webb , j. k. , weymann , r. j. , bechtold , j. & green , r. f. 1992 , apj , 390 , 387 rauch , m. , carswell , r. f. , webb , j. k. & weymann , r. j. 1993 , apj , 260 , 589 rauch , m. , weymann , r. j. & morris , s. l. 1996 , apj , 458 , 518 salpeter , e. e. & hoffman , g. l. 1995 , apj , 441 , 51 salzer j. j. , 1992 , aj , 103 , 385 sargent , w. l. w. , young , p. j. , boksenberg , a. & tytler , d. 1980 , apjs , 42 , 41 shull , j.m . , stocke , j. & penton , s. 1996 , aj , 111 , 72 smette , a. , surdej , j. , shaver , p. a. , foltz , c. b. , chaffee , f. h. , weymann , r. j. , williams , r. e. & magian , p. 1992 , apj , 389 , 39 stocke , j. t. , shull , j. m. , penton , s. , donahue , m. & carilli , c. 1995 , apj , 451 , 24 szomoru , a. , guhathakurta , p. , gorkom , j. h. , knapen , j. h. , weinberg , d. h. & fruchter , a. s. 1994 , aj , 108 , 491 szomoru , a. 1994 , ph.d . thesis , university of groningen szomoru , a. van gorkom , j. h. , gregg , m.d . & strauss , m. a. 1996 , aj , 111 , 2150 tytler , d. , 1987 , apj , 321 , 49 van gorkom , j. h. , bahcall , j. n. , jannuzi , b. t. & schneider , d. p. 1993 , aj , 106 , 2213 weinberg , d. h. , szomoru , a. , guhathakurta , p. & van gorkom , j. h. 1991 , apj , 372 , l13 weymann , r. j. 1993 , in the evolution and environment of galaxies , ed . j. m. shull & h. a. thronson , ( dordrecht : kluwer ) , 213 womble , d. s. , 1992 , ph.d . thesis university of california , san diego zaritski , d. & white , s. d. m. 1994 , apj 435 , 599

the closest galaxy we find to the absorbers is a small dwarf galaxy at a projected distance of @xmath7 kpc from the sight line toward mrk 335 . this optically uncataloged galaxy has the same velocity ( @xmath8 km s@xmath2 ) as one of the absorbers , is fainter than the smc , and has an h i mass of only @xmath9 m@xmath5 . we found a somewhat more luminous galaxy at exactly the velocity ( @xmath10 km s@xmath2 ) of one of the absorbers toward pks 2155 - 304 at a projected distance of @xmath11 kpc from the sight line . s@xmath2 appear to be associated with a loose group of three bright spiral galaxies , at projected distances of 300 to @xmath13 kpc . these results support the conclusions emerging from optical searches that most nearby ly@xmath0 forest clouds trace the large - scale structures outlined by the optically luminous galaxies , although this is still based on small - number statistics . , we detected h i emission from five galaxies , of which two were previously uncataloged and one did not have a known redshift . these results are similar to what has been found in optically unbiased h i surveys . thus , the presence of ly@xmath0 absorbers does not significantly alter the h i detection rate in their environment .

we present the results of a vla and wsrt search for h i emission from the vicinity of seven nearby clouds , which were observed in ly@xmath0 absorption with hst toward mrk 335 , mrk 501 and pks 2155 - 304 . around the absorbers , we searched a volume of @xmath1 1000 km s@xmath2 ; for one of the absorbers we probed a velocity range of only 600 km s@xmath2 . the h i mass sensitivity ( 5 @xmath3 ) very close to the lines of sight varies from @xmath4 m@xmath5 at best to @xmath6 m@xmath5 at worst . we detected h i emission in the vicinity of four out of seven absorbers . the closest galaxy we find to the absorbers is a small dwarf galaxy at a projected distance of @xmath7 kpc from the sight line toward mrk 335 . this optically uncataloged galaxy has the same velocity ( @xmath8 km s@xmath2 ) as one of the absorbers , is fainter than the smc , and has an h i mass of only @xmath9 m@xmath5 . we found a somewhat more luminous galaxy at exactly the velocity ( @xmath10 km s@xmath2 ) of one of the absorbers toward pks 2155 - 304 at a projected distance of @xmath11 kpc from the sight line . two other , stronger absorbers toward pks 2155 - 304 at @xmath12 km s@xmath2 appear to be associated with a loose group of three bright spiral galaxies , at projected distances of 300 to @xmath13 kpc . these results support the conclusions emerging from optical searches that most nearby ly@xmath0 forest clouds trace the large - scale structures outlined by the optically luminous galaxies , although this is still based on small - number statistics . we do not find any evidence from the h i distribution or kinematics that there is a physical association between an absorber and its closest galaxy . while the absorbing clouds are at the systemic velocity of the galaxies , the h i extent of the galaxies is fairly typical , and at least an order of magnitude smaller than the projected distance to the sight line at which the absorbers are seen . on the other hand , we also do not find evidence against such a connection . in total , we detected h i emission from five galaxies , of which two were previously uncataloged and one did not have a known redshift . no h i emission was detected from the vicinity of the two absorbers , which are located in a void and a region of very low galaxy density ; but the limits are somewhat less stringent than for the other sight lines . these results are similar to what has been found in optically unbiased h i surveys . thus , the presence of ly@xmath0 absorbers does not significantly alter the h i detection rate in their environment .

1212.5917

r

figure [ fg14nh3moms ] ( top left ) shows the combined ( vla+effelsberg ) zero - order moment map of the nh@xmath0(1,1 ) emission overlaid on the 8 @xmath23 m _ the overall morphology of the nh@xmath0(1,1 ) dense gas consists of extended and clumpy filamentary structures , strikingly mimicking the extinction feature seen in the _ spitzer _ image . while the nh@xmath0(1,1 ) emission is spatially extended , the nh@xmath0(2,2 ) emission is compact ( fig . [ fg14nh3moms]-top right ) , suggesting that the extended emission is at lower temperatures . we identified the most prominent filaments based on the morphology of the nh@xmath0(1,1 ) together with the fact that these structures are coherent in velocity . we used the following criteria : _ i ) _ filaments must have aspect ratio larger than 6 ; _ ii ) _ the signal - to - noise ratio should be larger than 9(1,1 ) , where the rms noise level has been estimated using @xmath24@xmath25/@xmath26 , where @xmath27 is the rms noise of the channel maps and @xmath28@xmath25=0.6 km s@xmath4 . ] ; and _ iii ) _ they must appear in at least two velocity channels and spanning a maximum velocity range of 3 km s@xmath4 . [ fg14nh3moms ] ( top right ) shows , for comparison , the 870 @xmath23 m continuum emission from the laboca bolometer at the apex telescope @xcite , supporting our identification . we identified a network of 8 filaments and two hubs ( named hub - n and hub - s in fig . [ fg14nh3moms ] ) , which were recognized using the nh@xmath0(2,2 ) emission as denser regions in which some filaments intersect . the nh@xmath0 filaments , which cover a total area of 4.7@xmath298.7 pc , appear approximately parallel , in projection , in two preferred directions , at pa of 10@xmath6 and 60@xmath6 , and they contain chains of dense cores(1,1 ) if at least the @xmath30 level is closed , where @xmath27 is the rms noise of the map . ] aligned along the filament axis and distributed at somewhat regular spacings of about @xmath230@xmath14 or 0.33@xmath70.09 pc at the distance of the cloud . the averaged projected separation between adjacent filaments is between 0.5 pc and 1 pc . in table [ g14filaments ] we report on the length and width at full width half maximum ( @xmath31 ) of each filament obtained from nh@xmath0(1,1 ) data . on average , we found that the aspect ratio is @xmath215:1 , with a typical @xmath31 width of @xmath20.12 pc . this value is close to the filament width of 0.1 pc reported for the ic5146 , aquila , and polaris molecular clouds from _ observations @xcite . in fig . [ fg14nh3moms ] ( bottom left ) we present the first - order moment map of the nh@xmath0(1,1 ) main line . within each filament the velocity variations are small , in the range of 12 km s@xmath4 ( see table [ g14filaments ] ) , similar to other filamentary irdcs ( e.g. , * ? ? ? this network of filaments seems to be separated into two main velocity components , one at @xmath32@xmath218.320.8 km s@xmath4 and another one at @xmath32@xmath220.823.2 km s@xmath4 , which overlap in the hubs . the second - order moment map is presented in fig . [ fg14nh3moms ] ( bottom right ) , and shows that the velocity dispersion is locally enhanced ( @xmath27@xmath21 km s@xmath4 ) toward hubs . additionally , a high velocity dispersion ( @xmath27@xmath21.6 km s@xmath4 ) is seen toward an arc - shaped structure connecting filament f10-e with the southern filaments , in a small region intersecting filament f60-c1 and labelled as position ` e ' in fig . [ fg14nh3moms ] . in this region the large values of the velocity dispersion are due to the presence of two velocity components separated by @xmath23 km s@xmath4 ( see fig . [ fg14spec]-e ) . the presence of two velocity components is also found in regions where filaments intersect hubs ( see fig . [ fg14spec]-d , f ) . in contrast , all the other filaments appear more quiescent , with a typical velocity dispersion of @xmath20.40.6 km s@xmath4 . c + [ cols="<,^,^,^,^,^,^,^,^,^,^,^,^,^ " , ] deconvolved size at full width half maximum ( @xmath31 ) not corrected for projection effects . @xmath1 has been derived following the appendix of @xcite . averaged values within the area at @xmath31 . mass per unit length , where the mass , @xmath33(h@xmath12)2.8@xmath34 , has been estimated assuming an nh@xmath0 abundance of @xmath35 ( average value measured in irdcs ; pillai et al . 2006 ) and using the area @xmath36 of the filament at @xmath31 . the uncertainty in the mass is a factor of 3 . virial mass per unit length @xmath37 , and virial paramter @xmath38 @xcite @xmath39 : observed separation between cores within a filament . @xmath40 : predicted core separation @xmath41 , where @xmath42 is the scale height , with @xmath43 the isothermal sound speed ( estimated by converting @xmath1 to kinetic temperature using the expression of @xcite ) , @xmath44 the gravitational constant , and @xmath45 the gas density at the center of the filament , adopted to be @xmath46 @xmath47 . the first value corresponds to the core separation using @xmath43 and the second value was obtained replacing @xmath43 by @xmath48 . number of cores within each filament . [ g14filaments ] to obtain the main physical properties ( rotational temperature @xmath1 , total velocity dispersion @xmath48 , and mass per unit length @xmath49 ) of each filament , we extracted an averaged spectrum of nh@xmath0(1,1 ) and ( 2,2 ) over the filament area at @xmath31 . the results are reported in table [ g14filaments ] . the rotational temperature ranges between 10 k and 16 k. the total velocity dispersion of the gas ranges from @xmath20.5 km s@xmath4 up to 1.1 km s@xmath4 , and the non - thermal velocity dispersion over the isothermal sound speed , @xmath50 , ranges between 2 and 5 , implying that filaments in g14.2 are characterized by supersonic non - thermal motions . in table [ g14filaments ] we also list the mass and virial mass per unit length , the observed separation between cores , and the number of cores in each filament . finally , the total surface density estimated by taking the spectrum averaged over all nh@xmath0 filaments is @xmath51@xmath521.9 g@xmath53 .

the nh@xmath0 emission reveals a network of filaments constituting two hub - filament systems . hubs are associated with gas of rotational temperature @xmath1@xmath215 k , non - thermal velocity dispersion @xmath3@xmath21 km s@xmath4 , and exhibit signs of star formation , while filaments appear to be more quiescent ( @xmath1@xmath211 k , @xmath5@xmath20.6 km s@xmath4 ) . filaments are parallel in projection and distributed mainly along two directions , at pa@xmath210@xmath6 and 60@xmath6 , and appear to be coherent in velocity . the averaged projected separation between adjacent filaments is between 0.5 pc and 1 pc , and the mean width of filaments is 0.12 pc . cores within filaments are separated by @xmath20.33@xmath70.09 pc , which is consistent with the predicted fragmentation of an isothermal gas cylinder due to the ` sausage'-type instability .

we present the results of combined nh@xmath0(1,1 ) and ( 2,2 ) line emission observed with the very large array and the effelsberg 100 m telescope of the infrared dark cloud g14.2250.506 . the nh@xmath0 emission reveals a network of filaments constituting two hub - filament systems . hubs are associated with gas of rotational temperature @xmath1@xmath215 k , non - thermal velocity dispersion @xmath3@xmath21 km s@xmath4 , and exhibit signs of star formation , while filaments appear to be more quiescent ( @xmath1@xmath211 k , @xmath5@xmath20.6 km s@xmath4 ) . filaments are parallel in projection and distributed mainly along two directions , at pa@xmath210@xmath6 and 60@xmath6 , and appear to be coherent in velocity . the averaged projected separation between adjacent filaments is between 0.5 pc and 1 pc , and the mean width of filaments is 0.12 pc . cores within filaments are separated by @xmath20.33@xmath70.09 pc , which is consistent with the predicted fragmentation of an isothermal gas cylinder due to the ` sausage'-type instability . the network of parallel filaments observed in g14.2250.506 is consistent with the gravitational instability of a thin gas layer threaded by magnetic fields . overall , our data suggest that magnetic fields might play an important role in the alignment of filaments , and polarization measurements in the entire cloud would lend further support to this scenario .

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c

in the previous section we presented the main properties of the two hub - filament systems in g14.2250.506 . hubs are more compact ( aspect ratio 5 vs 15 ) , warmer ( @xmath1@xmath5215 k vs 11 k ) , and show larger velocity dispersion and larger masses per unit length than filaments . interestingly , hubs are associated with h@xmath12o maser emission ( wang et al . 2006 ) and mid - infrared sources ( see figs . [ fg14spitzer ] , [ fg14nh3moms ] ) , and they are the main sites of stellar activity within the cloud . the stability of the filaments can be studied by estimating the virial parameter @xmath54=@xmath55 @xcite , which is @xmath562 for all the filaments and hubs except for f10-e , and five out of eight filaments are near virial equilibrium ( @xmath54@xmath521 ) . this indicates that most of the filaments are unstable ( collapsing ) and probably undergoing fragmentation , compatible with the clumpy structure of g14.2 . it is worth noting that filament f10-e has @xmath1 and velocity dispersion values similar to the hub properties . filament f10-e presents some striations converging toward it . however , while hub - n and hub - s seem to be places where two different velocity structures converge , f10-e shows only one velocity component . we speculate that i18153 , an uc hii region with @xmath57@xmath210@xmath58 @xmath10 ( snchez - monge , private communication ) , may compress the gas , heating and injecting turbulence to this filament ( @xmath595 ) . the interaction of this uc hii region with the dense gas is also seen in hub - n , where the nh@xmath0(2,2)/nh@xmath0(1,1 ) map shows a local heating ( fig . [ fg14pvplots ] ) . the position - velocity ( pv ) plot along this hub ( see fig . [ fg14pvplots ] ) reveals an inverted c - like structure , consistent with an expanding shell @xcite . we investigated the fragmentation of filaments in the magnetohydrodynamic ` sausage'-type instability scenario ( chandrasekhar & fermi 1953 , see also jackson et al . 2010 ) , which predicts periodic separation between fragments ( or cores ) for a given density and isothermal sound speed . for an isothermal gas cylinder of finite radius @xmath60 , the core separation can be expressed as @xmath40=22@xmath61 for @xmath60@xmath62@xmath61 , where @xmath61 is the scale height ( see table [ g14filaments ] for the formal expression ) . this is the case of g14.2 , since @xmath60 and @xmath61 are 0.12 pc and 0.04 pc , respectively . adopting a density of @xmath46 @xmath47 , we estimated the predicted core separation using first the isothermal sound speed , yielding @xmath40@xmath20.160.21 pc , and then replacing @xmath43 by the total velocity dispersion @xmath48 , which gives @xmath40@xmath20.40.8 pc ( see table [ g14filaments ] ) . the observed separation , @xmath20.33 pc , is in agreement with these two extreme cases . it is noteworthy that most of the cores appear to be elongated along the direction of the filament , which could imply the possibility of further fragmentation at smaller scales as observed in the irdcg28.34 + 0.06-p1 @xcite . one of the most intriguing features of g14.2 is the network of filaments that are aligned in parallel . the filaments appear to take two preferred directions , one group at a pa of 10@xmath6 , and the others at a pa of 60@xmath6 . this network of filaments may arise from a layer of self - gravitating gas . instability analysis has been performed for a layer of an isothermal infinite sheet under dynamical perturbation @xcite . the gas is unstable to perturbations , which leads to high density columns in the plane as a result of gravitational instability . the spacings between the high density columns of gas correspond to the wavelength of the fastest growth mode . in the absence of magnetic fields , the growth of instability does not have a preferred direction in the plane . as a result , a grid of connected filaments appears in the gas layer . if the gas layer is threaded by magnetic fields , the growth of the instability develops unrestricted in one direction and is suppressed along the orthogonal direction . @xcite analyzed a pressure confined isothermal gas layer threaded by uniform magnetic fields . they found that in the regime of smaller external pressure ( i.e.,the scale height @xmath61@xmath63@xmath64 , where @xmath64 is the thickness of the gas layer ) the instability grows faster along the field lines . as a consequence , high density columns , or filaments develop with their longitudinal axis perpendicular to the field lines . in the high pressure regime ( i.e. , @xmath61@xmath65@xmath64 ) , the fastest growth of instability is perpendicular to the field lines and gives rise to filaments parallel to the magnetic fields . recent numerical simulations ( van loo , private communication ) confirm the linear analysis in @xcite . the simulations show that an array of high density columns develop in the gas layer with magnetic fields . in addition , lower density filamentary structures are also present , inter - connecting the main filaments . the highest density structures are found at the intersections of major and minor filaments , as in this work . furthermore , the simulations show that gravitational instability develops within a filament during the filament formation . this means that fragmentation of a filament into cores occurs simultaneously with the fragmentation of the sheet , but according to @xcite with different free - fall times . the array of filamentary structures in g14.2250.506 may arise from gravitational instability of a thin gas layer with magnetic fields . in fact , preliminary near - infrared polarimetric observations around hub - n ( busquet et al . in prep . ) reveal that the magnetic field is perpendicular to filaments at pa@xmath260@xmath6 ( see fig . [ fg14nh3moms ] ) . therefore , according to @xcite g14.2 would be in the regime of small external pressure ( @xmath66 ) . using the total surface density ( see sect . 3 ) , the scale height @xmath61 of the initial gas layer is @xmath670.09 pc . this value should be regarded with caution , and to definitively assess its validity one would need observations of a low - density gas tracer to be sensitive to the gas layer . the wavelength of the fastest mode can be expressed as @xmath68 ( eq . 60 in @xcite ) . using our estimation of @xmath61 , the predicted separation is @xmath21.1 pc , in agreement with the observed filament separation ( between 0.5 and 1 pc ) . it is not clear how such a large gas layer ( 4.7@xmath298.7 pc ) may form initially . the convergence of dynamic flows could be responsible for the formation of such a large gas layer that subsequently could fragment into parallel filaments as a result of magnetic modulation . our nh@xmath0 data , although showing two velocity components , do not reveal evidence of converging / interacting flows and further observations of low - velocity shock tracers , like sio or ch@xmath0cn @xcite , and a tracer of low density material are required to definitely identify signatures of converging flows . overall , our data suggest that magnetic fields might play an important role in the alignment of filaments , and polarization measurements in the entire cloud would lend further support to this scenario . the authors are grateful to the anonymous referee for valuable comments . is deeply grateful to eugenio schisano for very fruitful discussion on filaments . g.b is funded by an italian space agency ( asi ) fellowship under contract number i/005/07/0 . , r.e . , and i.d.g . are supported by the spanish micinn grant aya2011 - 30228-c03 ( co - funded with feder funds ) . a. p. is supported by a jae - doc csic fellowship co - funded with the european social fund , under the program ` junta para la ampliacin de estudios ' , and by the agaur grant 2009sgr1172 ( catalonia ) . f.p.s . and g.a.p.f . are partially supported by cnpq and fapemig . this work is partially based on observations with the 100 m telescope of the mpifr ( max - planck - institut fr radioastronomie ) at effelsberg .

the network of parallel filaments observed in g14.2250.506 is consistent with the gravitational instability of a thin gas layer threaded by magnetic fields . overall , our data suggest that magnetic fields might play an important role in the alignment of filaments , and polarization measurements in the entire cloud would lend further support to this scenario .

we present the results of combined nh@xmath0(1,1 ) and ( 2,2 ) line emission observed with the very large array and the effelsberg 100 m telescope of the infrared dark cloud g14.2250.506 . the nh@xmath0 emission reveals a network of filaments constituting two hub - filament systems . hubs are associated with gas of rotational temperature @xmath1@xmath215 k , non - thermal velocity dispersion @xmath3@xmath21 km s@xmath4 , and exhibit signs of star formation , while filaments appear to be more quiescent ( @xmath1@xmath211 k , @xmath5@xmath20.6 km s@xmath4 ) . filaments are parallel in projection and distributed mainly along two directions , at pa@xmath210@xmath6 and 60@xmath6 , and appear to be coherent in velocity . the averaged projected separation between adjacent filaments is between 0.5 pc and 1 pc , and the mean width of filaments is 0.12 pc . cores within filaments are separated by @xmath20.33@xmath70.09 pc , which is consistent with the predicted fragmentation of an isothermal gas cylinder due to the ` sausage'-type instability . the network of parallel filaments observed in g14.2250.506 is consistent with the gravitational instability of a thin gas layer threaded by magnetic fields . overall , our data suggest that magnetic fields might play an important role in the alignment of filaments , and polarization measurements in the entire cloud would lend further support to this scenario .

astro-ph0607190

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there is a wide range of photometrically variable systems in the universe . the range of timescales on which these systems vary is as wide as the physical processes that produce their variability . for example we have intrinsically variable stars , where the variability is caused by changes in their internal structure or atmosphere that vary with timescales of minutes to years @xcite . other stars show variability because they rotate and their surface is inhomogeneous , e.g. because of star spots , @xcite , or because they form part of a binary or multiple system and their revolution around the centre of mass of the system results in changes on the detected flux due to the changing aspect of a non - isotropically emitting surface or eclipses . this is also the case for planets orbiting stars . the timescale of the variability in this case is dictated by the orbital parameters of the system and can range from seconds to years . near earth objects ( neos ) , such as asteroids , also show variability as they rotate and are non - spherical . we find photometric variability in extragalactic objects as well , such as quasars , where the variability is probably the result of material being accreted by the central engine , or `` one of '' systems such as gamma ray bursts ( grb ) or supernovae ( sne ) where the variability is produced by intrinsic changes in the structure of an astronomical object that take place only once . the study of variability provides important information about the physical nature of the variable objects , leads to the discovery of new classes of objects , helps to study the physical structure of stars , e.g. pulsating stars , allows us to obtain information on galactic structure through the use of variables such as rr lyrae as standard candles , and is the key to determining extra - galactic distances through the use of standard candles such as cepheids and supernovae type ia . most of our knowledge of variability is based on the study of apparently bright sources , which naturally selects members of _ intrinsically _ bright populations . at present little is known about variability of intrinsically fainter populations because in bright samples they are lacking altogether or are only represented by a few members . the faint sky variability survey ( fsvs ; groot et al . ) was designed to account for this deficit by studying two unexplored regions of the variability space : the short timescale variability region ( down to tens of minutes ) and the intrinsically faint variable sources ( down to v = 24 mag ) at mid and high galactic latitudes . the fsvs also contains colour information for all targets , giving us the option of positioning objects in the colour - colour diagram as well as finding the variability timescales and amplitudes that characterise them . the main aims of the fsvs are thus to obtain a map of a region of the galaxy ( @xmath021deg@xmath1 ) in variability and colour space , to determine the population density of the different variable objects that reside in the galaxy and to find the photometric signature of up - to - now unknown intrinsically faint variable populations . in this paper we explore these three goals . there are other surveys that study the variable optical sky , each emphasising one aspect or one particular region of this parameter space . the timescales sampled , depth and sky coverage of different variability surveys varies depending on the astronomical objects they are designed to study . for example , with a brightness limit similar to the fsvs , street et al . study the variability around an open cluster with timescales longer than a few hours , and ramsay & hakala study the rapid variability ( down to 2 minutes ) of objects as faint as v@xmath022.5 . of great interest is the deep lens survey ( dls ) that , in a similar way to the fsvs , combines colour and variability information and explores similar variability timescales @xcite . becker et al . also provide a comprehensive review of past and on - going variability surveys . the future of optical variability surveys looks quite promising with the advent of large aperture telescopes such as the large - aperture synoptic survey 8.4 m telescope @xcite , the 4 m telescope vista and the 2.5 m vlt survey telescope .

we present the v band variability analysis of the point sources in the faint sky variability survey on time scales from 24 minutes to tens of days . we find that about one percent of the point sources down to v = 24 are variables . we discuss the variability detection probabilities for each field depending on field sampling , amplitude and timescale of the variability . the combination of colour and variability information allows us to explore the fraction of variable sources for different spectral types .

we present the v band variability analysis of the point sources in the faint sky variability survey on time scales from 24 minutes to tens of days . we find that about one percent of the point sources down to v = 24 are variables . we discuss the variability detection probabilities for each field depending on field sampling , amplitude and timescale of the variability . the combination of colour and variability information allows us to explore the fraction of variable sources for different spectral types . we find that about 50 percent of the variables show variability timescales shorter than 6 hours . the total number of variables is dominated by main sequence sources . the distribution of variables with spectral type is fairly constant along the main sequence , with 1 per cent of the sources being variable , except at the blue end of the main sequence , between spectral types f0f5 , where the fraction of variable sources increases to about 2 percent . for bluer sources , above the main sequence , this percentage increases to about 3.5 . we find that the combination of the sampling and the number of observations allows us to determine the variability timescales and amplitudes for a maximum of 40 percent of the variables found . about a third of the total number of short timescale variables found in the survey were not detected in either b or / and i. these show a similar variability timescale distribution to that found for the variables detected in all three bands . [ firstpage ] surveys methods : data analysis stars : general stars : statistics stars : variables : general

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we have analysed the short timescale variability information contained in the fsvs and find that about 1 per cent of all point sources are variable . of those variables , about 50 per cent show variability timescales shorter than 6 hours , 22 per cent show variabilities between 6 hours and 1 day , 20 per cent between 1 and 4 days and 8 per cent show periods longer than 4 days . the distribution of variables with spectral type is fairly constant along the main sequence , with 1 per cent of all the sources being variable , except at the blue end of the main sequence where the fraction of variable sources increases possibly due to contamination by non main sequence sources . above the main sequence , beyond the blue cut - off at ( b@xmath2v)@xmath80.38 , we find that the fraction of variables increases to 3.5 percent . the highest space density of variables found in the fsvs ( i.e. 17 per deg@xmath1 ) show periods below 12 hours . these include cvs , rr lyr stars , and other short period pulsators such as @xmath9scuti stars . we find a density of 4 variables per deg@xmath1 centred at a 1 day period which includes longer period cvs , rr lyr and other pulsators like @xmath10doradus stars and pop ii cepheids . a space density of 2 variables per deg@xmath1 at 3.75 days includes , some longer period cvs , @xmath10doradus stars , pop ii cepheids and longer period pulsators such as subdwarf b stars . at 12.75 days we also find 2 variables per deg@xmath1 . these would be mainly binaries with those orbital periods and pop ii cepheids . it is easier to compare these space densities with those expected for the mentioned populations when we combine the period information with the colours of the populations under study . the case of cvs and many pulsators is complicated as they appear mixed through several period and colour ranges and in many cases it is necessary to obtain spectra to confirm the nature of the variable source . the space densities of cvs and subdwarf b stars will be studied in detail in a future paper . in the case of rr lyr stars , we find 3 certain members and 9 other candidates down to v = 21.6 . assuming we have detected all rr lyr between v = 1622 , we determine a space density of @xmath010@xmath11kpc@xmath11 in agreement with the space density determined by preston , shectman & beers at a distance of 100150kpc from the galactic centre . by using the floating mean periodogram , we have determined the most likely periods and amplitudes of a fraction of the variables found in the fsvs . we find that we are complete down to v = 22 for cvs in the minimum period ( 80 min ) as long as they show variability amplitudes of the order of 0.4 mag . we are complete down to v = 22 for periods between 80 min and 1 day in a 17.82deg@xmath1 area of the survey as long as the amplitude of the variability is at least 0.7 mag . this includes most rr lyr stars . we will be able to detect rr lyr also down to v = 23 when their variability amplitudes are at least 1.5 mag .

the total number of variables is dominated by main sequence sources . the distribution of variables with spectral type is fairly constant along the main sequence , with 1 per cent of the sources being variable , except at the blue end of the main sequence , between spectral types f0f5 , where the fraction of variable sources increases to about 2 percent . for bluer sources , above the main sequence , this percentage increases to about 3.5 .

we present the v band variability analysis of the point sources in the faint sky variability survey on time scales from 24 minutes to tens of days . we find that about one percent of the point sources down to v = 24 are variables . we discuss the variability detection probabilities for each field depending on field sampling , amplitude and timescale of the variability . the combination of colour and variability information allows us to explore the fraction of variable sources for different spectral types . we find that about 50 percent of the variables show variability timescales shorter than 6 hours . the total number of variables is dominated by main sequence sources . the distribution of variables with spectral type is fairly constant along the main sequence , with 1 per cent of the sources being variable , except at the blue end of the main sequence , between spectral types f0f5 , where the fraction of variable sources increases to about 2 percent . for bluer sources , above the main sequence , this percentage increases to about 3.5 . we find that the combination of the sampling and the number of observations allows us to determine the variability timescales and amplitudes for a maximum of 40 percent of the variables found . about a third of the total number of short timescale variables found in the survey were not detected in either b or / and i. these show a similar variability timescale distribution to that found for the variables detected in all three bands . [ firstpage ] surveys methods : data analysis stars : general stars : statistics stars : variables : general

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convection in late - type stars penetrates into the photosphere , producing inhomogeneities . temperature variations of up to a few hundred kelvin are apparent in optical images of the sun , and a velocity field of several kilometers per second is observed in spatially resolved solar spectra . the warmer upflows appear as bright granules surrounded by narrower , cooler downflows . while present technology can not resolve stellar granulation , there is evidence of its presence in all late - type stars . the temperature and velocity inhomogeneities produce absorption line profiles which are shifted and asymmetric , effects that are readily noticed in ultra - high dispersion stellar spectra . an extensive literature exists on solar line asymmetries and shifts ( see , e.g. , neckel & labs 1990 ; asplund et al . 2000 ; pierce & lopresto 2000 ) . modern stellar studies were pioneered by dravins ( 1974 , 1985 ) and gray ( 1980 , 1981 ) . dravins ( 1999 ) provides a short review of recent work . line asymmetries and line shifts are consequences of the same phenomenon and , therefore , give largely equivalent information . when the number of lines measured is limited , but the available features are mostly unblended , line asymmetries carry more information . on the contrary , if the spectrum is heavily crowded , line shifts , which can be measured for many lines , are likely to provide more information . a limited wavelength coverage , largely dictated by the detector size and the scarcity of high - accuracy laboratory wavelengths , steered stellar studies toward the analysis of line asymmetries . line bisectors a measure of the line asymmetry vary smoothly across the hr diagram ( gray & toner 1986 ; dravins 1987 ; gray & nagel 1989 ; dravins & nordlund 1990 ) . other parameters , such as rotation , chemical composition , magnetic fields , or binarity , are likely to play a role , but the limited data available have prevented an in - depth study . a recent comprehensive work on the fe i spectrum ( nave et al . 1994 ) has provided accurate laboratory wavelengths for 9501 lines . these data and improvements in astronomical instrumentation make it feasible and practical to turn to line shifts as a complement to line bisectors . gravitational and convective wavelength shifts systematically affect absolute determinations of radial velocities . other effects can also introduce systematic radial velocity errors , but they are expected to be less important for most stars ( lindegren , dravins , & madsen 1999 ) . gravitational redshifts are proportional to the mass - to - radius ratio . for spectral lines formed in the photospheres of dwarf stars , the gravitational shift is the same for all lines , in the range between 0.4 and 2 km s@xmath0 . when accurate parallaxes and photometry are available , comparison with evolutionary models allows us to determine dwarf masses and radii within 8 % and 6 % , respectively ( allende prieto & lambert 1999 ) . it is therefore possible to estimate the gravitational shift within 10 % , yielding worst - case uncertainties of @xmath1 km s@xmath0 . convective line shifts may vary with spectral type . the velocity difference between weak and strong lines is about @xmath2 km s@xmath0 for the sun ( allende prieto & garca lpez 1998 ) and probably more than 1 km s@xmath0 for the f5 subgiant @xmath3 cmi ( procyon ; allende prieto et al . 2002 ) , but no systematic study across the hr diagram has been published . obviously , accurate spectroscopic studies of absolute radial velocities can not afford to neglect these shifts . in this paper , we analyze optical spectra of several late - type stars obtained with the high resolution spectrograph ( hrs ) coupled to the hobby - eberly telescope ( het ) . the high quality and large spectral coverage of the spectra allow us to measure line shifts for a large number of fe i lines . section [ obs ] describes the observations and the data . in section [ doit ] we describe the analysis , and in [ end ] we discuss the results .

we present ultra - high resolution spectra for a set of nearby f - g - k stars on , or close to , the main sequence . the wavelength shifts of stellar lines relative to their laboratory wavelengths are measured for more than a thousand fe i lines per star , finding a clear correlation with line depth . the velocity span between weak and strong lines for these stars is larger than for the dwarfs and subgiants of similar spectral types .

we present ultra - high resolution spectra for a set of nearby f - g - k stars on , or close to , the main sequence . the wavelength shifts of stellar lines relative to their laboratory wavelengths are measured for more than a thousand fe i lines per star , finding a clear correlation with line depth . the observed patterns are interpreted as convective blue - shifts that become more prominent for weaker lines , which are formed in deeper atmospheric layers . a morphological sequence with spectral type or effective temperature is apparent . two k giant stars have also been studied . the velocity span between weak and strong lines for these stars is larger than for the dwarfs and subgiants of similar spectral types . our results show that convective wavelength shifts may seriously compromise the accuracy of absolute spectroscopic radial velocities , but that an empirical correction may be applied to measured velocities .

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the pattern of the velocity shifts is similar for all the stars , and in qualitative agreement with solar results . the net convective blue shifts of the lines strengthen toward deeper photospheric layers , and therefore affect the weak lines more than the strong ones . despite our limited sample , there is an indication of a smooth dependence of the average velocity shifts with spectral type . this effect is clearer in our analysis of line shifts than in previous studies using bisectors . as argued in the introduction , this is likely the result of line shifts measurements being less affected by blending than line bisectors in late - g and k type stars . our preliminary results indicate that the trend of line shifts as a function of line strength can be determined as a function of spectral type and gravity . at least for late - type dwarfs , assuming the strongest lines in the spectrum are free from convective shifts ( as is the case for the solar photosphere ) , it is possible to correct for convective wavelength shifts to within @xmath33 km s@xmath0 . the measured range of wavelength shifts for neutral iron lines is larger in @xmath3 cmi than in cooler stars of classes iv and v. the range of wavelength shifts is also larger , reaching up to @xmath34 1 km s@xmath0 , for the k giants than for the g - k dwarfs and subgiants in our sample , which is not surprising . although their lower effective temperatures provide less flux to transport , their lower atmospheric pressure implies larger convective velocities . 1 suggests that , once we account for the observational errors , there is little room for intrinsic line - to - line scatter in the f - g - k stars sampled here . convection is supposed to cease in main sequence stars with spectral types earlier than about f2 , but other velocity fields must be present in those atmospheres , judging from the asymmetry of the spectral lines ( e.g. gray & nagel 1989 ) . determining accurate absolute radial velocities demands an understanding of the wavelength shifts in the spectra of these stars too . solar observations have shown differences in the center - to - limb variation of the granulation along the central meridian and the equator ( e.g. beckers & taylor 1980 ; rodrguez hidalgo , collados , & vzquez 1992 ) . observations of a large number of stars may then show peculiarities at a given spectral type depending on the orientation of the rotational axis . stars with enhanced magnetic fields are also expected to be peculiar in terms of observed wavelength shifts , as the enhanced magnetic fields may hinder the convective motions . furthermore , line shifts may vary with time for stars exhibiting an analog of the solar 11 year cycle . observations of line shifts for a significant number of stars with high quality are required for a deeper understanding of granulation in stellar atmospheres , its relationship with other stellar phenomena , and the role of surface convection in the structure and evolution of stars . our first results show that measurements of convective line shifts are a must in order to derive accurate absolute radial velocities . we thank the het staff for their outstanding job making possible science observations with hrs since day one . the hobby - eberly telescope is operated by mcdonald observatory on behalf of the university of texas at austin , the pennsylvania state university , stanford university , ludwig - maximilians - universitt mnchen , and georg - august - universitt gttingen . nso / kitt peak fts data used here were produced by nsf / noao . this research was supported in part by the nsf ( grant ast-0086321 ) .

the observed patterns are interpreted as convective blue - shifts that become more prominent for weaker lines , which are formed in deeper atmospheric layers . a morphological sequence with spectral type or effective temperature is apparent . two k giant stars have also been studied . our results show that convective wavelength shifts may seriously compromise the accuracy of absolute spectroscopic radial velocities , but that an empirical correction may be applied to measured velocities .

we present ultra - high resolution spectra for a set of nearby f - g - k stars on , or close to , the main sequence . the wavelength shifts of stellar lines relative to their laboratory wavelengths are measured for more than a thousand fe i lines per star , finding a clear correlation with line depth . the observed patterns are interpreted as convective blue - shifts that become more prominent for weaker lines , which are formed in deeper atmospheric layers . a morphological sequence with spectral type or effective temperature is apparent . two k giant stars have also been studied . the velocity span between weak and strong lines for these stars is larger than for the dwarfs and subgiants of similar spectral types . our results show that convective wavelength shifts may seriously compromise the accuracy of absolute spectroscopic radial velocities , but that an empirical correction may be applied to measured velocities .

0909.2937

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enormous experimental evidence clearly indicates that neutrinos have tiny but non - zero masses , and understanding the origin of neutrino masses is one of the most pressing problems in particle physics . the minimal higgs boson model with additional right - handed neutrinos provides a simple solution to all the fermion masses including neutrino masses by generating all of them through yukawa interactions . however , the @xmath1 order hierarchy between dimensionless yukawa coupling @xmath2 and neutrino yukawa coupling @xmath3 suggests that neutrino masses may arise from an additional source besides the electroweak symmetry breaking . their electric neutrality allows for the possibility of neutrinos being majorana fermions . within the higgs boson model framework , the seesaw mechanism @xcite is an elegant proposal accounting for the tiny neutrino masses . it is crucial that the small neutrino masses arise as a consequence of the grand unification at ultra high energy scales @xcite . the mechanism is based on the presence of singlet heavy majorana neutrinos of mass @xmath4 , y n_r + m_r n_r , which is impossible to probe directly at the collider experiments . however , there have recently been several proposals to show how to test the origin of neutrino mass directly at the coming cern large hadron collider ( lhc ) @xcite . in the seesaw mechanism , the tiny neutrino masses arise as a consequence of lepton number violation at the ultra high energy scale while if the new physics responsible for neutrino mass is accessible at the lhc , additional tuning may be needed . in the effective theory language , the majorana neutrino mass after integrating out new physics at a scale @xmath5 is due to the term y^2 l_l l_l hh s^n^n+1[llhh ] , where @xmath6 is a dimension one scale and @xmath7 is a dimensionless yukawa coupling . therefore , without tuning @xmath7 in eq . ( [ llhh ] ) , there are only two approaches to generate a tiny majorana neutrino mass . one approach is to impose discrete ( gauge ) symmetries which generate a large value of @xmath8 and tiny neutrino masses arise as high dimensional operators @xcite . another approach is to have a small scale @xmath6 . for instance , in the `` inverse seesaw '' models @xcite or `` tev triplet '' models @xcite , to obtain the correct neutrino mass , a kev order scale needs to be introduced , and this small scale may be identified as a soft breaking of lepton symmetry @xcite . within the framework of minimal type - i seesaw @xcite , where @xmath9 in eq.([llhh ] ) , if the heavy majorana neutrinos are of the electroweak scale , the only way to generate the correct neutrino mass is to require the yukawa coupling @xmath7 to be of @xmath10 . due to the tiny yukawa coupling , the production of @xmath0 can only be enhanced through new gauge interactions such as with a @xmath11 gauge boson @xmath12 or @xmath13 gauge boson @xmath14 @xcite . in this paper , we propose a new model based on extra dimension @xcite . here , neutrino mass is generated by a cooperation with a right - handed singlet field @xmath0 on `` visible brane '' and a lepton number violation at a distant brane , `` hidden brane , '' spatially separated in the extra dimension communicating through a messenger field in the 5d bulk ( see fig . [ fig : extra dimension ] ) . with a messenger field whose zero - mode wave function has an exponential suppression at the hidden brane , even if the lepton number violation on the hidden brane is as large as the electroweak scale , the resultant neutrino mass remains naturally small . differently from existing models in extra dimension @xcite our model predicts two phenomenologically interesting features ( i ) a large yukawa coupling with @xmath0 , which can completely change higgs phenomenology ( ii ) a sizable lepton number violation through mixings with kaluza - klein excitation modes of the messenger field , which can be tested by future collider experiments such as the cern large hadron collider ( lhc ) . are localized on the visible brane located at @xmath15 . the lepton violating sector is on a distant brane located at @xmath16 and has only small overlap with the zero - mode of a messenger field ( @xmath17 ) , which induces a small lepton number violation transmuted to the visible sector and results a small neutrino mass.,scaledwidth=64.5% ]

we propose a model of neutrino mass generation in extra dimension . allowing a large lepton number violation on a distant brane spatially separated from the standard model brane , a small neutrino mass is naturally generated due to an exponential suppression of the messenger field in the 5d bulk . the model accommodates a large yukawa coupling with the singlet neutrino ( @xmath0 ) which may change the standard higgs search and can simultaneously accommodate visible lepton number violation at the electroweak scale , which leads to very interesting phenomenology at the cern large hadron collider .

we propose a model of neutrino mass generation in extra dimension . allowing a large lepton number violation on a distant brane spatially separated from the standard model brane , a small neutrino mass is naturally generated due to an exponential suppression of the messenger field in the 5d bulk . the model accommodates a large yukawa coupling with the singlet neutrino ( @xmath0 ) which may change the standard higgs search and can simultaneously accommodate visible lepton number violation at the electroweak scale , which leads to very interesting phenomenology at the cern large hadron collider .

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our purpose is to build an intensity - based modeling framework that can be used in trading and calibrating across the credit and equity markets . the same company has stocks , stock options , bonds , credit default swaps on these bonds , and several other derivatives . when this company defaults , the payoffs of all of these instruments are affected ; therefore , their prices all contain information about the default risk of the company . we build a model that can be jointly calibrated to corporate bond prices and stock options , and can be used to price more exotic derivatives . in our framework we use the vasicek model for the interest rate , and use doubly stochastic poisson process to model the default of a given company . we assume that the bonds have recovery of market value and that stocks become valueless at the time of default . using the multi - scale modeling approach of @xcite we obtain explicit bond pricing equation with three free parameters which we calibrate to the corporate bond term structure . on the other hand , stock option pricing formula contain seven parameters , three of which are common with the bond option pricing formula . ( the common parameters are multiplied with the loss rate in the bond pricing formula . ) we calibrate the remaining set of parameters to the stock option prices . this hybrid model , therefore , is able to account for the default risk premium in the implied volatility surface . the calibration results reveal that our model is able to produce implied volatility surfaces that match the data closely . we compare the implied volatility surfaces that our model produces to those of @xcite . we see that even for longer maturities our model has a prominent skew : compare figures [ fig : imp7p ] and [ fig : impvfouque ] . even when we ignore the stochastic volatility effects , our model fits the implied volatility of the ford motor company well and performs better than the model of @xcite ; see figure [ fig : impvolford ] . this points to the importance of accounting for the default risk for companies with low ratings . once the model parameters are calibrated , the model can be used to compute the prices of more exotic options . to test whether our model produces correct prices we use the cds spread data and show that the model implied cds spread matches the out of sample " cds data . to compute the cds spread , under our assumption on the recovery , one needs to reconstruct the term structure of the treasury and the corporate bonds . moreover , one needs to separate the loss rate from the other parameters in the bond pricing formula ( see or for the cds spread formula ) . this separation is possible since we calibrate our model to corporate bond data and stock option data jointly as described above . the model - implied cds spread time series matches the observed cds spread time series of ford motor company for over a long period of time ; see figures [ fig : cds3yr ] and [ fig : cds5yr ] . this is an interesting observation since we did not make use of the cds spread data in our calibration . this observation also shows that one can use our model to trade across different markets that contain information about the default risk of a given firm . our model has three building blocks : ( 1 ) we model the default event using the multi - scale stochastic intensity model of @xcite . we also model the interest rate using an ornstein - uhlenbeck process ( vasicek model ) . as it was demonstrated in @xcite , these modeling assumptions are effective in capturing the corporate yield curve ; ( 2 ) we take the stock price process to follow a stochastic volatility model which jumps to zero when the company defaults . this stock price model was considered in @xcite . our model specification for the stock price differs from the jump to default models for the stock price considered by @xcite and @xcite , which take the volatility and the default intensity to be functions of the stock price ; ( 3 ) we also account for the stochastic volatility in the modeling of the stocks since even the index options ( when there is no risk of default ) possess implied volatility skew . we model the volatility using the fast scale stochastic volatility model of @xcite . we demonstrate on index options ( when there is no risk of default ) that ( see section [ sec : demnst ] ) , we match the performance of the two time scale volatility model @xcite . the latter model extends @xcite by including a slow factor in the volatility to get a better fit to longer maturity option . we see from section [ sec : demnst ] that when one assumes the interest rate to be stochastic , the calibration performance of the stochastic volatility model with only the fast factor is as good as the two scale stochastic volatility model , which is why we choose the volatility to be driven by only the fast factor . even though the interest rate is stochastic in our model , we are able to obtain explicit asymptotic pricing formulas for stock options . thanks to these explicit pricing formulas the inverse problem that we face in calibrating to the corporate bond and stock data can be solved with considerable ease . our modeling framework can be thought of as a hybrid of the models of @xcite , which only considers pricing options in a stochastic volatility model with constant interest rate , and @xcite , which only considers a framework for pricing derivatives on bonds . neither of these models has the means to transfer information from the equity markets to bond market or vice versa , which we are set to do in this paper . we should also note that our model also takes input from the treasury yield curve , historical stock prices , and historical spot rate data to estimate some of its parameters ( see section [ sec : calibration ] ) . our model extends @xcite by taking the interest rate process to be stochastic , which leads to a richer theory and more calibration parameters , and therefore , better fit to data : ( i ) when the interest rate is deterministic the corporate bond pricing formula turns out to be very crude and does not fit the bond term structure well ( compare ( 2.57 ) in @xcite and ) ; ( ii ) with deterministic interest rates the bond pricing and the stock option pricing formulas share only one common term , `` the average intensity of default '' ( this parameter is multiplied by the loss rate in the bond pricing equation , under our loss assumptions ) . therefore , the default premium in the implied volatility surface is not accounted for as much as it should be . and our calibration analysis demonstrates that this has a significant impact . when the volatility is taken to be constant , both our new model and the model in @xcite have three free parameters . the model in @xcite produces a below par fit to the implied volatility surface ( see e.g. figure 5 in that paper ) , whereas our model produces an excellent fit ( see section [ sec : fordsimplied ] and figure [ fig : impvolford ] ) ; ( iii ) to calculate the cds spread , in the constant interest rate model , one needs to separate the loss rate and the average intensity of default . this is again established calibrating the model to the bond term structure data and the stock option implied volatility surface . the estimates for the average intensity and the loss rate are not as accurate in @xcite as it is in our model because of ( i ) and ( ii ) . this crude estimation leads to a poor out of sample match to the cds spread time series . the other defaultable stock models are those of @xcite , @xcite and @xcite , which assume that the interest rate is deterministic . @xcite , @xcite take the volatility and the intensity to be functions of the stock price and obtain a one - dimensional diffusion for the pre - default stock price evolution . using the fact that the resolvents of particular markov processes can be computed explicitly , they obtain pricing formulas for stock option prices . on the other hand @xcite uses a cir stochastic volatility model and also models the intensity to be a function of the volatility and another endogenous cir factor . the option prices in this framework are computed numerically using inverse the fourier transform . we , on the other hand , use asymptotic expansions to provide explicit pricing formulas for stock options in a framework that combines a ) the vasicek interest rate model , b ) fast - mean reverting stochastic volatility model , c ) defaultable stock price model , d ) multi - scale stochastic intensity model . our calibration exercise differs from that of @xcite since they perform a time series analysis to obtain the parameters of the underlying factors ( from the the stock option prices and credit default swap spread time series ) , whereas we calibrate our pricing parameters to the daily implied volatility surface and bond term structure data . our purpose is to find a risk neutral model that matches a set of observed market prices . this risk neutral model can then be used to price more exotic , illiquid or over - the - counter derivatives . for further discussion of this calibration methodology we refer to @xcite ( see chapter 13 ) , @xcite , @xcite and @xcite . we also provide daily prediction of the cds spread only using the data from the bond term structure and implied volatility surface of the options . the rest of the paper is organized as follows : in section 2 , we introduce our modeling framework and describe the credit and equity derivatives we will consider and obtain an expression for the cds spread under the assumption that the recovery rate of a bond that defaults is a constant fraction of its predefault value . in section 3 , we introduce the asymptotic expansion method . we obtain explicit ( asymptotic ) prices for bonds and equity options in section 3.3 . in section 4 , we describe the calibration of our parameters and discuss our empirical results . figures , which show our calibration results , are located after the references .

we propose a model which can be jointly calibrated to the corporate bond term structure and equity option volatility surface of the same company . our purpose is to obtain explicit bond and equity option pricing formulas that can be calibrated to find a risk neutral model that matches a set of observed market prices . this risk neutral model can then be used to price more exotic , illiquid or over - the - counter derivatives . we observe that the model implied credit default swap ( cds ) spread matches the market cds spread and that our model produces a very desirable cds spread term structure . this is observation is worth noticing since without calibrating any parameter to the cds spread data , it is matched by the cds spread that our model generates using the available information from the equity options and corporate bond markets . we also observe that our model matches the equity option implied volatility surface well since we properly account for the default risk premium in the implied volatility surface . * keywords : * credit default swap , defaultable bond , defaultable stock , equity options , stochastic interest rate , implied volatility , multiscale perturbation method .

we propose a model which can be jointly calibrated to the corporate bond term structure and equity option volatility surface of the same company . our purpose is to obtain explicit bond and equity option pricing formulas that can be calibrated to find a risk neutral model that matches a set of observed market prices . this risk neutral model can then be used to price more exotic , illiquid or over - the - counter derivatives . we observe that the model implied credit default swap ( cds ) spread matches the market cds spread and that our model produces a very desirable cds spread term structure . this is observation is worth noticing since without calibrating any parameter to the cds spread data , it is matched by the cds spread that our model generates using the available information from the equity options and corporate bond markets . we also observe that our model matches the equity option implied volatility surface well since we properly account for the default risk premium in the implied volatility surface . we demonstrate the importance of accounting for the default risk and stochastic interest rate in equity option pricing by comparing our results to @xcite , which only accounts for stochastic volatility . * keywords : * credit default swap , defaultable bond , defaultable stock , equity options , stochastic interest rate , implied volatility , multiscale perturbation method .

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warped extra dimensions @xcite , which have been proposed as an alternative solution to the gauge hierarchy problem , also provide a simple framework in which fermion masses are explained by the overlap of the fermion and higgs wave functions in the bulk of the warped extra dimension @xcite . having the zero mode fermions peaked at different points in the fifth dimension , the exponentially hierarchical masses of quarks and charged leptons can be obtained with a tiny hierarchy of bulk masses and all 5d yukawa couplings being of order unity @xcite . however , letting the standard model ( sm ) fermion content propagate through the bulk generally results in large contributions to electroweak precision observables , such as the peskin - takeuchi @xmath8 , @xmath9 parameters , unless the lowest kaluza - klein ( kk ) mass scale is unnaturally pushed to values much higher than a tev . to suppress these contributions , more realistic models involving a bulk custodial symmetry , broken differently at the two branes @xcite were constructed . alternatively , large brane kinetic terms were introduced @xcite . in both cases a mass of the first kk excited state as low as @xmath10(3 tev ) , is now allowed by electroweak precision data . another problem arises , this time due to the presence of non degenerate 5d bulk mass parameters , governing the localization of bulk zero modes . the non degeneracy induces new physics ( np ) contributions to flavor changing neutral current ( fcnc ) processes mediated by kk excitations of the gauge bosons and fermions , through gauge interactions in the fermion kinetic terms and 5d yukawa interactions . in the most general case , without imposing any additional flavor symmetry and assuming anarchical 5d yukawa couplings , new physics contributions can already be generated at tree level through a kk gauge boson exchange . even if an rs - gim suppression mechanism @xcite is at work , stringent constraints on the kk scale come from the @xmath11 oscillation parameter @xmath12 and the radiative decays @xmath13 @xcite , the direct cp violation parameter @xmath14 @xcite , and especially the neutron electric dipole moment @xcite , where a mass of the first kk state of @xmath10(3 tev ) gives rise to a np contribution which is roughly twenty times larger than the current experimental bound a cp problem in itself , referred to as little cp problem . stringent constraints on the kk scale are also present in the lepton sector @xcite . even in the absence of neutrino masses , severe bounds arise from contributions to fcnc processes mediated by tree level kk gauge bosons with anarchical 5d yukawa couplings @xcite . it was also recently observed @xcite that the mixing between fermion zero modes and kk modes generally induces a misalignment in the 4d effective theory between the sm fermion masses and the higgs yukawa couplings . this misalignment leads to higgs mediated flavor changing neutral currents , once the fermion mass matrix is diagonalized . in particular , @xmath15 is found @xcite to produce stringent combined lower bounds on the kk gluon and the standard model higgs mass in flavor anarchic models . additional flavor symmetries in the bulk can in principle allow to partially or fully remove these constraints , by forbidding or providing a further suppression of tree level fcncs and one loop contributions induced by the presence of kk modes . one example that removes or suppresses all tree level contributions is the generalization to 5d of minimal flavor violation in the quark sector @xcite and in the lepton sector @xcite . in these settings , the bulk mass matrices are aligned with the 5d yukawa matrices as a result of a bulk @xmath16^{6}$ ] flavor symmetry that is broken in a controlled manner . in @xcite a shining mechanism is proposed , where the suppression of flavor violation in the effective 4d theory on the ir brane is obtained by confining the sources of flavor violation to the uv brane , and communicating its effects through gauge bosons of the gauged bulk flavor symmetry . there , it is also shown that higgs mediated fcncs are eliminated to leading order , and a lowest kk scale of about 2 - 3 tev seems to be allowed , rendering the model testable at collider experiments @xcite . all above considerations suggest that a candidate for a realistic model of lepton and quark masses and mixings in a warped setup should possibly be realized with all standard model fields in the bulk , including the higgs field , a bulk custodial symmetry and an additional flavor symmetry , to avoid large new physics contributions and maintain the kk scale of order a tev . in @xcite , see also @xcite , a bulk @xmath0 family symmetry @xcite was used to explain masses and mixings in the sm lepton sector . in this setting , the three left - handed lepton doublets form a triplet of @xmath0 to generate tribimaximal ( tbm ) neutrino mixing @xcite , in agreement with the recent global fit in @xcite . in addition , tree - level leptonic fcncs are absent in this scheme . while the simplest realization of @xmath0 well describes the lepton sector , it does not give rise to a realistic quark sector . in this paper , we propose a model based on a bulk @xmath6 family symmetry , implemented in a slightly different setup , in an attempt to describe both the quark and lepton sectors . in this setup the scalar fields that transform under non trivial representations of @xmath0 , namely two flavon triplets , reside in the bulk . consequently , they allow for a complete `` cross - talk '' @xcite between the @xmath17 spontaneous symmetry breaking ( ssb ) pattern associated with the heavy neutrino sector - with scalar mediator peaked towards the uv brane - and the @xmath18 ssb pattern associated with the quark and charged lepton sectors - with scalar mediator peaked towards the ir brane . as in previous models based on @xmath0 , the three generations of left - handed quarks transform as triplets of @xmath6 ; this assignment forbids tree level gauge mediated fcncs and will allow to obtain realistic masses and almost realistic mixing angles in the quark sector . it will also be instructive to compare this pattern to the case of larger realizations of the flavor symmetry , like @xmath19 @xcite , which are usually associated with a rather richer flavon sector . an additional feature worth to mention is the constraint on the common left - handed quarks bulk mass parameter implied by the @xmath5 best fits in our model . the numerical significance of such a constraint has been thoroughly investigated in the minimal version of rs models @xcite , and it is largely relaxed in models with ( extended ) @xmath4 custodial symmetry @xcite . the paper is organized as follows . in section [ sec : setup ] we review the basic setup of the model and the various representation assignments . we then present a rs model with custodial symmetry and a bulk @xmath0 family symmetry , and derive the leading order results for masses and mixings . in section [ secho ] we classify all higher order corrections , including cross - talk and cross - brane operators for leptons and quarks and parametrize their effect . section [ findckm ] contains our numerical analysis and results . in section [ alignment ] we discuss the vacuum alignment problem and suggest possible solutions , while in section [ sec : fv ] we briefly discuss constraints from flavor violating processes on the kaluza - klein scale in our model . we conclude in section [ sec : conclusion ] .

we propose a spontaneous @xmath0 flavor symmetry breaking scheme implemented in a warped extra dimensional setup to explain the observed pattern of quark and lepton masses and mixings . finally , we briefly discuss bounds on the kaluza - klein scale implied by flavor changing neutral current processes in our model and show that the residual little cp problem is milder than in flavor anarchic models .

we propose a spontaneous @xmath0 flavor symmetry breaking scheme implemented in a warped extra dimensional setup to explain the observed pattern of quark and lepton masses and mixings . the main advantages of this choice are the explanation of fermion mass hierarchies by wave function overlaps , the emergence of tribimaximal neutrino mixing and zero quark mixing at the leading order and the absence of tree - level gauge mediated flavor violations . quark mixing is induced by the presence of bulk flavons , which allow for `` cross - brane '' interactions and a `` cross - talk '' between the quark and neutrino sectors , realizing the spontaneous symmetry breaking pattern @xmath1 first proposed in [ x.g.he , y.y.keum , r.r.volkas , jhep0604 , 039 ( 2006 ) ] . we show that the observed quark mixing pattern can be explained in a rather economical way , including the cp violating phase , with leading order cross - interactions , while the observed difference between the smallest ckm entries @xmath2 and @xmath3 must arise from higher order corrections . without implementing @xmath4 ( or other versions of ) custodial symmetry , the bulk mass parameter of the left - handed quarks in this model is constrained by the @xmath5 best fits , still allowing for a kaluza - klein scale below 2 tev . finally , we briefly discuss bounds on the kaluza - klein scale implied by flavor changing neutral current processes in our model and show that the residual little cp problem is milder than in flavor anarchic models . a4warpedpics * an @xmath6 flavor model for quarks and leptons in warped geometry * 0.2 cm * avihay kadosh@xmath7 and elisabetta pallante@xmath7 * @xmath7 _ centre for theoretical physics , university of groningen , 9747 ag , netherlands _ a.kadosh@rug.nl , e.pallante@rug.nl 0.3truecm

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we first proceed to set all vevs and mass scales , according to the observed mass spectrum and neutrino oscillation data . once these scales are set , we will be able to quantify the various higher order contributions , starting from the quark sector . we take the fundamental 5d scale to be @xmath271 , where @xmath272 gev is the reduced planck mass . to keep the scale of the ir brane in reach of future collider experiments , but satisfying the constraints from the observed s and t parameters , we will always use values around @xmath273 , such that the mass of the first kk excitation is of a few tev . it is natural to expect all of the scalars in our theory , being bulk fields , to acquire a vev of order @xmath274 . using the known mass of the @xmath275 boson we can set the amplitude of @xmath180 in terms of the 5d weak gauge couplings to be @xmath276 . by exploiting the warped geometry , we can match all the observed 4d fermion masses by taking the bulk fermion parameters @xmath277 to be all of order one , a well known pleasing feature of the warped scenario @xcite ; a large mass hierarchy is seeded by a tiny hierarchy of the @xmath81 parameters . in this setting , fermion masses are determined by the overlap integrals in the corresponding yukawa terms , involving the fermion zero mode profiles and the scalar vev profiles of eqs . ( [ profiles ] ) and ( [ eqn : ffactor ] ) . therefore , if we take the 5d yukawa couplings to be universal and set them to one , all bulk parameters can be matched to the observed mass spectrum . we remind the reader that there is only one bulk parameter @xmath278 for each left - handed quark and lepton doublet , being it a triplet of @xmath6 . also , the @xmath278 are essentially free parameters , since we can always set the mass of each fermion by tuning the bulk mass of the corresponding right handed @xmath6 singlet . for the same reasons , the scalar vev @xmath279 is essentially also a free parameter and we set it to be @xmath280 . however , all fermion zero mode wave functions associated with the various @xmath81 parameters are still constrained by a few important perturbativity bounds @xcite and by precision measurements . the most stringent constraint is on the quark left - handed bulk parameter @xmath281 and comes from the bottom sector , in particular the combined best fits for the ratio of the z - boson decay width into bottom quarks and the total hadronic width @xmath282 , the bottom - quark left - right asymmetry , @xmath283 , and the forward - backward asymmetry , @xmath284 @xcite . a thorough comparison of the combined best fits for @xmath282 , @xmath283 , @xmath284 with the tree - level corrections to the @xmath5 couplings in the minimal ( non custodial ) rs model can be found in @xcite , while the case of @xmath4 custodial symmetry and extended @xmath4 has been recently considered @xcite . these analyses constraints . ] show that the allowed window for new physics corrections to the sm prediction and consequently the window for the corresponding bottom bulk parameter @xmath285 is severely constrained by the @xmath5 best fits , unless an extended custodial symmetry such as @xmath4 custodial , or extended @xmath4 custodial is in place . the model considered here is an intermediate example , which embeds non - extended custodial symmetry , and it is thus expected to be subject to constraints on the left - handed profile @xmath281 more severe than in the @xmath4 custodial case and possibly close to the minimal rs model . on the other hand , the model also differs from the cases analyzed in @xcite in two respects . the additional @xmath6 flavor symmetry might modify the non orthonormality properties of bulk fermions and eventually suppress contributions due to mixing of zero modes with kk states . secondly , a bulk higgs instead of a brane localized higgs generally allows for further suppressions via overlap in the presence of mass insertions . we defer to future work the analysis of these two aspects in the context of @xmath5 . for the purpose of model building we provide here an approximate estimate of the allowed range for @xmath281 in our model , at tree level and in the zma , based on the recent calculations in @xcite . we correct the contributions to the @xmath5 couplings @xmath286 in the minimal rs model of @xcite , with the dominant @xmath287 corrections due to the presence of custodial symmetry @xcite . analogously to @xcite , we conveniently define the functions @xmath288 in terms of the canonically normalized fermion zero mode wave functions @xmath289 of eq . ( [ eqn : ffactor ] ) evaluated at the ir brane @xmath290 we obtain @xmath291 \nonumber\\ & & + \frac{m_b^2}{2m_{kk}^2}\left [ \frac{1}{1 + 2c_b } \left ( \frac{1}{f^2(c_b)}-1+\frac{f^2(c_b)}{3 - 2c_b}\right ) + \sum_{i = d , s } \frac{|(y_d)_{3i}|^2}{|(y_d)_{33}|^2 } \frac{1}{1 + 2c_i}\frac{1}{f^2(c_b ) } \right ] \nonumber\\ g^b_r&= & \frac{s_w^2}{3}\left [ 1-\frac{m_z^2}{2m_{kk}^2}\frac{f^2(c_b)}{3 - 2c_b } \left ( \omega_z^{b_r}\cdot k\pi r - \frac{5 - 2c_b}{2(3 - 2c_b)}\right ) \right ] \nonumber\\ & & -\frac{m_b^2}{2m_{kk}^2}\left [ \frac{1}{1 + 2c^q_l } \left ( \frac{1}{f^2(c^q_l)}-1+\frac{f^2(c^q_l)}{3 - 2c^q_l}\right ) + \sum_{i = d , s } \frac{|(y_d)_{3i}|^2}{|(y_d)_{33}|^2 } \frac{1}{1 + 2c^q_l}\frac{1}{f^2(c^q_l ) } \right ] \ , \label{eq : zbb}\end{aligned}\ ] ] where @xmath292 in the case of equal @xmath293 and @xmath42 gauge couplings . it is instructive to compare the values for @xmath294 in the three different setups . the minimal rs model has @xmath295 , the @xmath4 custodial has @xmath296 and @xmath297 for @xmath298 , while the custodial case as in our model has @xmath299 and @xmath300 . notice that the latter is negative , and would go in the right direction to solve the @xmath284 anomaly . we have however verified that its numerical impact is limited , as it is its positive contribution in the minimal rs setup . in the estimate provided by eq . ( [ eq : zbb ] ) we have disregarded corrections to the @xmath301 dependent terms due to the admixture of the kk partners in the zero modes of the @xmath42 doublets ; the exact form of the corrections depends on the symmetries of the model , also @xmath6 flavor in our case , and weak isospin assignments of bulk fermions . the @xmath301 dependent contribution as in eq . ( [ eq : zbb ] ) is strongly dependent on the right - handed bottom bulk paramater @xmath302 . however , it can be effectively suppressed in the particular case of extended @xmath4 custodial symmetry due to degeneracy of right - handed profiles @xcite . we used the combined best fit values for the couplings @xmath303 and @xmath304 @xcite and the predicted sm values @xmath305 and @xmath306 @xcite at the reference higgs mass of 150 gev , to constrain the new physics contributions defined as @xmath307 . we disregarded the new physics corrections to the sm contributions in the light sector as in @xcite . for a higgs mass of 150 gev , a kk scale @xmath308 tev , and imposing a @xmath309 probability interval for the left - handed coupling given by @xmath310 , we obtain the constraint @xmath311 , as it can be inferred from figure [ fig : zbbconstraint ] . notice that eq . ( [ eq : zbb ] ) has a strong dependence on @xmath302 and only a mild dependence on @xmath312 . thus , lowering the value of @xmath302 towards 0.5 will allow for significantly larger windows for @xmath281 , at the price of higher yukawa couplings . the corrections to the sm prediction for @xmath313 satisfy @xmath314 in the region of interest and have been safely neglected . an illustrative example of the new physics contribution @xmath315 as a function of @xmath281 , with @xmath308 tev , the down - type 5d yukawa couplings in eq . ( [ eq : zbb ] ) set to 1 in magnitude and the right - handed bulk parameters set to the conservative value @xmath316 , and @xmath317 . the shaded horizontal band corresponds to the @xmath309 probability interval allowed by the best fit values for @xmath286 with the sm prediction computed at @xmath318 gev as in @xcite . , width=8 ] the perturbativity constraint on the 5d top yukawa coupling @xmath319 , together with the matching to the @xmath320 top mass at the kk scale @xmath321 @xcite and the constraint @xmath322 , the partner of the @xmath42 top , is sufficiently suppressed in @xmath5 @xcite . ] , implies instead the upper bound @xmath323 . notice that by requiring @xmath324 @xcite , with @xmath325 , the bound on @xmath281 changes significantly to @xmath326 . hence , one obtains @xmath327 in the most conservative case . as expected , the allowed minimal value for @xmath281 is severely constrained by the @xmath5 best fits . for @xmath328 , all the right - handed quark bulk parameters are chosen in order to yield the @xmath320 quark masses at the kk scale of 1.8 tev . their values are @xmath329 , @xmath330 , @xmath331 , @xmath332 , @xmath333 and @xmath334 , corresponding to @xmath335 , @xmath336 , @xmath337 , @xmath338 , @xmath339 and @xmath340 . all 5d yukawa couplings have been set to 1 in magnitude , while the top yukawa coupling slightly breaks universality with @xmath341 . it should be added that lower values for @xmath91 become accessible for a kk scale higher than @xmath308 tev . on the other hand , a kk scale as low as 1 tev would force @xmath342 and the top yukawa coupling to values @xmath343 . another possibility is the one of a heavier higgs . a higgs mass larger than 150 gev would bring the model prediction closer to the best fit values for @xmath344 and @xmath313 , thus allowing for a larger range for @xmath281 . for example , a mass @xmath345 gev would imply a lower bound @xmath346 , within our estimate and using the shifts @xmath347 and @xmath348 @xcite induced by @xmath349 gev . however , a heavier higgs mass in the custodial setup easily induces conflicts with electroweak precision measurements and a careful estimate of the actually allowed range of values for @xmath350 should be produced in each version of the custodial setup . we defer this point to future work on phenomenological applications . for the charged leptons we make the choice @xmath351 , @xmath352 , @xmath353 and @xmath354 , which reproduce the experimental value of the corresponding masses @xmath355 mev , @xmath356 mev and @xmath357 gev . to obtain the neutrino masses we first recall the leading order structure of the light neutrino mass matrix after see - saw , @xmath358 in eq . ( [ eq : mlbare ] ) , for which the eigenvalues are given by:@xmath359\ , . \label{eigen}\ ] ] we now write the neutrino mass - squared splittings , for afterwards we would like to impose the observed values of @xmath360 and @xmath361 , in order to constrain the possible choices of @xmath155 and @xmath362 . given @xmath363\label{ratio1}\,,\ ] ] @xmath364 \label{ratio2},\ ] ] where @xmath365 , @xmath366 and @xmath367 , we obtain the following cubic equation for @xmath368 : @xmath369 where @xmath370 for @xmath371 , and @xmath372 for @xmath373 . given @xmath368 , the ratio @xmath374 can be extracted either in terms of @xmath375 or @xmath376 @xmath377 imposing the measured values @xcite for the mass splittings , @xmath378 and @xmath379 , we find four possible solutions to the above equation , @xmath380 , where the first two correspond to inverted hierarchy , while the second two correspond to normal hierarchy . in addition , once we set @xmath381 , we can constrain @xmath155 and @xmath362 from the same data . this is a nice feature of the light neutrino mass matrix obtained in all @xmath6 models with similar assignments @xcite . since at this stage only the overall light neutrino mass ratios , @xmath382 and @xmath383 are constrained by the observed splittings , we choose not to set @xmath381 and extract @xmath156 from the quark mixing data . it will be possible afterwards to set @xmath381 to a natural value @xmath384 to match the neutrino mass spectrum . we now analyze the ckm matrix resulting from the contributions introduced in eq . ( [ dckm ] ) . using standard perturbative techniques , the left diagonalization matrix @xmath385 is obtained by the unitary diagonalization of @xmath386 , and the right diagonalization matrix @xmath387 is analogously obtained by the unitary diagonalization of @xmath388 . the entries of the ckm matrix are then derived in terms of the @xmath389 , @xmath390 parameters defined in eq . ( [ dckm ] ) , to leading order in perturbation theory . the up and down left - diagonalization matrices turn out to be : @xmath391 with @xmath256 , @xmath392 , and @xmath393 stands for the complex conjugate . in the above matrices , for simplicity , we have redefined the @xmath265 and @xmath266 to absorb the relative factor of @xmath394 compared to the unperturbed mass eigenvalues @xmath395 . furthermore , we have omitted contributions that are suppressed by quadratic quark mass ratios and still linear in @xmath265 , @xmath266 . terms of this kind will be included in the complete expressions derived below , for each of the interesting ckm matrix elements . it is now straightforward to extract the estimations for the upper off - diagonal elements of the ckm matrix out of @xmath396 , in order to eventually match the three mixing angles and the cp violating phase @xmath397 . to leading order in @xmath398 , these elements turn out to be @xmath399 @xmath400 @xmath401 where it is important to observe that the first equality is exact to leading order in @xmath402 and @xmath403 . the diagonal elements of the ckm matrix remain unchanged at this order and equal to one . we recall that @xmath265 and @xmath266 correspond to the @xmath404 and @xmath405 entries of @xmath406 in the interaction basis , respectively . this tells us which fermionic wave function overlaps enter the integral for each of the above parameters . for the 4d couplings we thus obtain @xmath407 to narrow down the parameter space , we choose all the @xmath408 to be universal and equal to one in magnitude , while relative phases between these parameters will be allowed . hence , due to the mass hierarchy of the quarks , which keeps the denominators in eqs . ( [ shoot1])-([shoot3 ] ) proportional to just one quark mass to a good approximation , the resulting corrections to each of the ckm matrix elements are of the generic form , @xmath409}\label{genericckm}\,,\ ] ] with @xmath410 , and where @xmath411 , @xmath412 and @xmath413 or @xmath29 . let us first set @xmath414 according to the experimental value of @xmath415 ; using eq . ( [ shoot1 ] ) and taking into account eq . ( [ genericckm ] ) we obtain : @xmath416 in which we have fixed @xmath417 , @xmath418 , @xmath419 and @xmath420 to be @xmath223 in magnitude , with a relative phase , @xmath421 , between the contributions from the up and down sectors . @xmath422 we want to see if the above value of @xmath414 together with a minimal number of relative phases between the remaining @xmath423 and @xmath424 parameters , are enough to account for the magnitudes of the remaining observed ckm elements . yet , we first want to check the consistency of the scale associated with the above value of @xmath414 with the neutrino mass splittings and the bare majorana mass scale . it turns out that for @xmath425 it is possible to satisfy the constraints in both sectors , namely to have a realistic @xmath415 , while at the same time having a realistic neutrino mass spectrum with a normal or inverted hierarchy . at this level the neutrino mixing matrix is obviously tribimaximal with small deviations , as we saw in section [ secho ] . the numerical results are reported in table [ tab : egmasses ] , once the scales are fixed by @xmath426 . the dominant contributions to @xmath427 ( and @xmath428 ) are given by @xmath429 up till now , we introduced only one phase , @xmath430 , to match @xmath415 ( and @xmath431 ) , but failed to match @xmath427 ( and @xmath432 ) to their central experimental values @xmath433 . the leading order contribution to @xmath2 , without any relative phase assignments , and with the @xmath434 s and @xmath435 s set to 1 , is @xmath436 we see that @xmath2 , and thus @xmath3 , turn out correctly to be of order @xmath437 , but still outside the experimental error . the next to leading order corrections to the various ckm elements enter at @xmath438 . in general , one may still expect them to modify the relatively small values of @xmath2 and @xmath427 , especially in the presence of strong cancellations at leading order , and given that each independent contribution is effectively suppressed by @xmath439 compared to the corrections linear in @xmath265 and @xmath266 . we are going to elaborate on this possibility once we made an attempt to obtain an almost realistic ckm matrix , using the first order results . the only way to obtain a realistic prediction for the independent magnitudes of @xmath2 and @xmath427 , and the related values of @xmath440 and @xmath432 , is to break the universality assumption for the yukawa couplings , @xmath441 , @xmath442 and find their values that match the experimental data . however , we are interested in the smallest possible deviations from the universality assumption which assumes all of the yukawa couplings to be of order one , so that contributions to various flavor violating processes , which are present in any rs - flavor setup @xcite , will not be arbitrarily modified . therefore , while trying to find the minimum number of assignments in the @xmath441 , @xmath442 parameter space , we still require small deviations , in general complex , from the @xmath105 universality assumption . it is obvious that assignments in terms of one parameter will yield results proportional to those of eq . ( [ vcb ] ) and ( [ vub ] ) , and will hence fail again to account for realistic values of @xmath427 and @xmath2 . the minimal viable choice consists of at least 2 parameter assignments . namely , we will have to break the universality assumption for two out of the four @xmath441 , @xmath442 parameters . in addition the only choice of parameter assignments that maintains all coefficients of @xmath105 is to break universality for @xmath443 and @xmath444 , while setting @xmath445 . solving eqs . ( [ vub ] ) and ( [ vcb ] ) for @xmath443 and @xmath444 we obtain : @xmath446 these parameters are almost degenerate , in particular if one considers the overall accuracy of the zero mode approximation , and substituting these values in eqs . ( [ vcb ] ) and ( [ vub ] ) , we obtain @xmath447 which are the central experimental values @xcite . interestingly , we are able to match also the cp violating phase @xmath448 , using the same assignment . we find it to be @xmath449 , which is well within the experimental error . obviously , at this order @xmath450 holds exactly , and this gives a value for @xmath432 close to the central experimental value @xmath451 . we also obtain @xmath452 , and thus fail to match the central experimental value @xmath453 . notice , however , that corrections of the size of the smallest ckm entries , i.e. @xmath454 are below the model theoretical error induced by the zero mode approximation . a realistic value for @xmath3 can easily arise from the subleading corrections in @xmath455 and @xmath268 and from higher dimensional operators beyond the zero mode approximation . we remind that the corrections quadratic in @xmath455 and @xmath268 are generically suppressed by a factor @xmath456 with respect to the linear contributions . we have thus shown that at leading order in the vev expansion the model predicts @xmath457 to be the unit matrix , a rather good first step in the description of quark mixing . at the next to leading order , cross - brane and cross - talk operators induce deviations from unity , parametrized in terms of twelve complex parameters @xmath455 and @xmath268 , with @xmath93 . we have shown that , linearly in these parameters , realistic values of the ckm entries can be obtained within the model theoretical error in a finite portion of the parameter space , with all the @xmath458 and @xmath459 of order one and two non zero relative phases ; however at this order , no corrections to the diagonal unit entries is produced and the two smallest entries @xmath2 and @xmath3 are degenerate . we notice that the possibility of producing hierarchical ckm entries , of order @xmath460 , @xmath461 and @xmath437 , with all parameters of order one stems from the presence of built - in cancellations induced by the hierarchical masses . the presence of the @xmath6 induced phase @xmath206 also produces a pattern in the corrections . in this framework , subleading corrections of order @xmath462 and contributions beyond the zma , must be responsible for the deviation from one of the ckm diagonal entries and the non degeneracy of @xmath2 and @xmath3 . the first is of order @xmath463 , the latter of order @xmath464 , hence a cancellation pattern must again be in place . it is instructive to compare this @xmath6 pattern with other flavor symmetry groups , in particular @xmath465 @xcite . the wolfenstein parametrization would suggest the existence of an expansion parameter to be naturally identified with @xmath460 , offering an elegant and simple description of quark mixing in the standard model . on the other hand , flavor models based on otherwise appealing discrete flavor symmetries such as @xmath6 and @xmath465 must rely on more complicated patterns to produce a realistic ckm matrix . in the case of @xmath465 one needs to postulate a hierarchy of yukawa couplings to distinguish between @xmath466 and @xmath467 entries , and a hierarchy of specific vevs to induce the splitting between @xmath2 and @xmath3 . similar hierarchies can in principle also be postulated in the @xmath6 case , at the price of an increased fine tuning of the input parameters . to complete our analysis we want to ensure that the deviations from tbm induced by cross - talk operators of the characteristic forms @xmath468 and @xmath469 are suppressed and keep the predictions for the neutrino mixing parameters within the @xmath470 range of the experimental error . we first consider the cross - brane operator @xmath471 , already explored in section iii . recall that deviations from @xmath209 and @xmath208 are induced only for complex @xmath224 parameters , and therefore we expect the maximal deviations from tbm when they are purely imaginary . all said , we estimate the magnitude of the @xmath224 coefficients based on the results of the previous section . as we are interested only in the dominant contributions , associated with one insertion of @xmath46 , we are only interested in @xmath228 as defined in eq . ( [ diractextures ] ) . this provides @xmath472 where @xmath473 was introduced in eq . ( [ epschidef ] ) . given @xmath474 we also obtain @xmath475 . taking its phase to be @xmath476 we get the largest possible contribution to the phase @xmath234 defined in eq . ( [ nucp ] ) to be @xmath477 . using eq . ( [ nufix ] ) we can now estimate the deviations from tbm arising from the operator @xmath478 in the worst scenario where its coefficient is purely imaginary . these turn out to be @xmath479 all of these deviations are within @xmath270 from their experimental values . the other class of operators @xmath480 have the same structure as the operators in charge of quark mixing . the perturbative diagonalization procedure can thus be carried out as it is done in the quark sector , in order to determine the deviations from @xmath481 of the rotation matrix for the left handed charged leptons . generically , these operators will induce perturbations to the mass matrix in the form of eq . ( [ dckm ] ) and with characteristic strength @xmath482 , which is of the same order of the model theoretical error . we could have proceeded to explicitly write all of these corrections as we did for the quarks , yet since the structure is practically identical in both cases we can easily deduce the effect of these small terms . for example , in analogy with eqs . ( [ cchi ] ) and ( [ vub ] ) and using no additional phase assignments for @xmath483 and @xmath484 , we get that the contribution to @xmath485 is vanishing , while the contributions to @xmath486 and @xmath487 are of approximate strength @xmath488 , comparable to the model theoretical error . higher order cross - talk operators are not considered , as their contribution lies safely below @xmath489 . we can conclude that the most significant deviations from tbm induced by cross - talk and cross - brane operators on the three mixing angles stay within the experimental errors for these quantities . this can be obtained without making any further assumption on the parameters of the model and maintaining all of them naturally of order one .

we show that the observed quark mixing pattern can be explained in a rather economical way , including the cp violating phase , with leading order cross - interactions , while the observed difference between the smallest ckm entries @xmath2 and @xmath3 must arise from higher order corrections . without implementing @xmath4 ( or other versions of ) custodial symmetry , the bulk mass parameter of the left - handed quarks in this model is constrained by the @xmath5 best fits , still allowing for a kaluza - klein scale below 2 tev .

we propose a spontaneous @xmath0 flavor symmetry breaking scheme implemented in a warped extra dimensional setup to explain the observed pattern of quark and lepton masses and mixings . the main advantages of this choice are the explanation of fermion mass hierarchies by wave function overlaps , the emergence of tribimaximal neutrino mixing and zero quark mixing at the leading order and the absence of tree - level gauge mediated flavor violations . quark mixing is induced by the presence of bulk flavons , which allow for `` cross - brane '' interactions and a `` cross - talk '' between the quark and neutrino sectors , realizing the spontaneous symmetry breaking pattern @xmath1 first proposed in [ x.g.he , y.y.keum , r.r.volkas , jhep0604 , 039 ( 2006 ) ] . we show that the observed quark mixing pattern can be explained in a rather economical way , including the cp violating phase , with leading order cross - interactions , while the observed difference between the smallest ckm entries @xmath2 and @xmath3 must arise from higher order corrections . without implementing @xmath4 ( or other versions of ) custodial symmetry , the bulk mass parameter of the left - handed quarks in this model is constrained by the @xmath5 best fits , still allowing for a kaluza - klein scale below 2 tev . finally , we briefly discuss bounds on the kaluza - klein scale implied by flavor changing neutral current processes in our model and show that the residual little cp problem is milder than in flavor anarchic models . a4warpedpics * an @xmath6 flavor model for quarks and leptons in warped geometry * 0.2 cm * avihay kadosh@xmath7 and elisabetta pallante@xmath7 * @xmath7 _ centre for theoretical physics , university of groningen , 9747 ag , netherlands _ a.kadosh@rug.nl , e.pallante@rug.nl 0.3truecm

1004.0321

c

we have constructed a warped extradimensional realization of an @xmath6 flavor model for quarks and leptons , and implemented the flavor symmetry breaking pattern @xmath1 first suggested in @xcite . in this construction all standard model fields , including the higgs field , propagate in the bulk and a bulk custodial symmetry is broken in two different ways @xcite on the uv and ir brane by orbifold boundary conditions . the spontaneous symmetry breaking of the @xmath6 flavor symmetry is induced by the vevs of two bulk flavon fields @xmath45 and @xmath46 : @xmath45 is responsible of the breaking pattern @xmath163 in the charged fermion sector , while @xmath46 is responsible of the breaking pattern @xmath162 in the neutrino sector . by taking the two flavons to be peaked on different branes , we approximately sequester the two sectors and the associated symmetry breaking patterns : neutrinos with the uv - peaked @xmath46 on one side , charged fermions with the ir - peaked @xmath45 on the other . if the two sectors do not communicate , that is when the interactions of @xmath45 with neutrinos and @xmath46 with charged fermions are switched off , tribimaximal mixing for neutrinos is exactly reproduced , while no quark mixing is generated . in our model the two flavons propagating in the bulk are responsible for cross - brane interactions and a complete cross - talk between the charged fermion and neutrino sectors . as a consequence , quark mixing on the ir brane is generated by contributions which are naturally suppressed by the warped geometry with respect to the leading order pattern in the quark and lepton sectors @xcite . using this realization we have obtained an almost realistic ckm matrix , including its cp violating phase , with almost degenerate order one complex yukawa couplings . the large hierarchy of standard model fermion masses is generated by a tiny hierarchy in the bulk fermion mass parameters , a well known pleasing feature of warped constructions . at the same time the contributions of all cross - talk and cross - brane effects do not spoil the tribimaximal mixing pattern in the neutrino sector , where they produce deviations within @xmath270 from the experimental values , with small non zero contributions also to @xmath216 . the cross - talk / brane induced quark mixing , to leading order in the perturbative diagonalization of the mass matrices , is expressed in terms of six complex parameters in the up and down sectors , @xmath550 , with @xmath93 . it turns out that , with all these parameters of order one and allowing for at least two relative phases , one obtains an almost realistic ckm matrix within the model theoretical error . at this order the diagonal ckm entries remain equal to one , and the two smallest entries @xmath2 and @xmath3 are degenerate . we have also noticed that the possibility of producing hierarchical ckm matrix elements , of order @xmath460 , @xmath461 and @xmath437 , with all parameters of order one stems from the presence of built - in cancellations induced by the hierarchical masses . the presence of the @xmath6 induced phase @xmath206 also produces a pattern in the corrections . analogous cancellations are expected to occur at higher orders . it is instructive to compare this @xmath6 pattern with other flavor symmetry groups , in particular @xmath465 @xcite . the wolfenstein parametrization would suggest the existence of an expansion parameter to be naturally identified with @xmath460 , offering an elegant and simple description of quark mixing in the standard model . on the other hand , flavor models based on otherwise appealing discrete flavor symmetries such as @xmath6 and @xmath465 seem to rely on more complicated patterns in order to produce a realistic ckm matrix . a bulk @xmath6 flavor symmetry is also welcomed in order to suppress the amount of flavor violation induced by the mixing of the standard model particles the zero modes of the 5d theory with their kaluza - klein excitations . the degeneracy of left - handed fermion bulk profiles , due to having assigned the left - handed fermions to triplets of @xmath6 , implies that the tree level contribution from a kk gluon exchange to @xmath15 vanishes . for the same reason , all down - type dipole contributions to the neutron electric dipole moment and @xmath549 also vanish . the situation is different for higgs mediated fcncs @xcite and their contribution to @xmath15 at tree level , since they involve both left- and right - handed fermion profiles . their suppression might require further constraints on the right - handed sector , to be explored in future work . even in the presence of non vanishing amplitudes , an @xmath6 induced cancellation of observable phases and the consequent vanishing of new physics contributions to the edm , @xmath15 and @xmath549 , would obviously be a welcomed feature of the model , removing the most stringent bounds on the kk scale and resolving the little cp problem @xcite . finally , the presence of cross - brane interactions of the flavon fields @xmath45 and @xmath46 inevitably induces deviations from the vevs that realize the two breaking patterns @xmath551 and @xmath162 , leading to the well known vacuum alignment problem . however , in this case such corrections are naturally suppressed , being the two flavons peaked on different branes . in particular , we have shown that the contribution from the most dominant term in the interaction potential @xmath504 can be pushed below the model theoretical error by introducing a bulk mass for the uv - peaked @xmath46 field . obviously , this implies the need to rescale by a global amount all the @xmath455 , @xmath552 parameters entering quark mixing , a rescaling that should anyway maintain all parameters of order one and satisfy all perturbativity bounds . on the other hand , employing a @xmath506 symmetry setup , as suggested in section vi , directly forbids the most dangerous terms and seems to provide a more elegant solution . the @xmath0 flavor symmetry still appears to be the most elegant and economical way to account for the nearly tribimaximal mixing pattern of neutrinos . we have shown here that it is also possible to obtain an almost realistic quark mixing , using a rather simple embedding of @xmath6 in a warped extra dimension and with minimal field content . the main advantage of this construction remains the one of having cross - brane interactions and cross - talk effects sufficiently large to account for the observed quark mixing , without affecting the other results , or spoiling the vacuum alignment . a dynamical completion of this , as of other flavor models involving a discrete flavor symmetry would certainly be desirable . possible scenarios already described in the literature include a spontaneous symmetry breaking of a continuous flavor symmetry @xcite or having @xmath6 as a remnant spacetime symmetry of a toroidal compactification scheme of a six - dimensional spacetime @xcite . it is worth to mention two additional points . it is appealing to explore the effects of a heavier higgs in this context . some of the model predictions would get closer to the best fits for certain observables , such as @xmath5 ratios and asymmetries , allowing for a larger parameter space . however , as discussed in the literature , a heavier higgs mass in a custodial setup easily induces conflicts with electroweak precision measurements and a more careful estimate of the allowed range of values for @xmath350 should be produced in each version of the custodial setup . the final point concerns possible extensions of the warped @xmath6 model . it is interesting and phenomenologically relevant to consider the possibility to embed @xmath4 ( or other versions of ) custodial symmetry @xcite into warped @xmath6 . this would release the most stringent constraint on the model parameter space due to the @xmath5 best fits and could provide new appealing features alternative to flavor anarchic models . we thank yuval grossman and gilad perez for useful discussions . the work of a.k is supported in part by the ubbo emmius scholarship program at the university of groningen .

quark mixing is induced by the presence of bulk flavons , which allow for `` cross - brane '' interactions and a `` cross - talk '' between the quark and neutrino sectors , realizing the spontaneous symmetry breaking pattern @xmath1 first proposed in [ x.g.he , y.y.keum , r.r.volkas , jhep0604 , 039 ( 2006 ) ] . a4warpedpics * an @xmath6 flavor model for quarks and leptons in warped geometry * 0.2 cm * avihay kadosh@xmath7 and elisabetta pallante@xmath7 * @xmath7 _ centre for theoretical physics , university of groningen , 9747 ag , netherlands _

we propose a spontaneous @xmath0 flavor symmetry breaking scheme implemented in a warped extra dimensional setup to explain the observed pattern of quark and lepton masses and mixings . the main advantages of this choice are the explanation of fermion mass hierarchies by wave function overlaps , the emergence of tribimaximal neutrino mixing and zero quark mixing at the leading order and the absence of tree - level gauge mediated flavor violations . quark mixing is induced by the presence of bulk flavons , which allow for `` cross - brane '' interactions and a `` cross - talk '' between the quark and neutrino sectors , realizing the spontaneous symmetry breaking pattern @xmath1 first proposed in [ x.g.he , y.y.keum , r.r.volkas , jhep0604 , 039 ( 2006 ) ] . we show that the observed quark mixing pattern can be explained in a rather economical way , including the cp violating phase , with leading order cross - interactions , while the observed difference between the smallest ckm entries @xmath2 and @xmath3 must arise from higher order corrections . without implementing @xmath4 ( or other versions of ) custodial symmetry , the bulk mass parameter of the left - handed quarks in this model is constrained by the @xmath5 best fits , still allowing for a kaluza - klein scale below 2 tev . finally , we briefly discuss bounds on the kaluza - klein scale implied by flavor changing neutral current processes in our model and show that the residual little cp problem is milder than in flavor anarchic models . a4warpedpics * an @xmath6 flavor model for quarks and leptons in warped geometry * 0.2 cm * avihay kadosh@xmath7 and elisabetta pallante@xmath7 * @xmath7 _ centre for theoretical physics , university of groningen , 9747 ag , netherlands _ a.kadosh@rug.nl , e.pallante@rug.nl 0.3truecm

nucl-ex0610043

c

in summary , we argue that the observation of broadened angular correlations of heavy - flavor hadron pairs in high - energy heavy - ion collisions would be an indication of thermalization at the partonic stage ( among light quarks and gluons ) . we have seen that hadronic interactions at a late stage in the collision evolution can not significantly disturb the azimuthal correlations of @xmath0pairs . thus , a visible decrease or the complete absence of such correlations , would indicate frequent interactions of heavy - flavor quarks and other light partons in the partonic stage , implying early thermalization of light quarks in nucleus - nucleus collisions at rhic and lhc . these measurements require good statistics of events in which _ both _ d mesons are cleanly reconstructed . a complete reconstruction of the d mesons ( i.e. of _ all _ their decay products ) in full azimuth is essential to preserve the kinematic information and to optimize the acceptance for detecting correlated d meson pairs . solid experimental measurements in @xmath40 and light - ion collisions , at the same energy , are crucial for detailed studies of changes in these azimuthal correlations , and should be performed as a function of @xmath2 . proposed upgrades of star @xcite and phenix at rhic and the alice detector @xcite at lhc with micro - vertex capabilities and direct open charm reconstruction should make these measurements possible . * acknowledgements * k.s . acknowledges support by the helmholtz foundation under contract number vh - ng-147 . this work has been supported by gsi and bmbf , in part by the u.s . department of energy under contract no . de - ac03 - 76sf00098 . b. svetitsky and a. uziel , phys . d * 55 * ( 1997 ) 2616 . b. svetitsky and a. uziel , hep - ph/9709228 . b. svetitsky and a. uziel , _ int . europhysics conf . on high - energy physics ( hep 97 ) , jerusalem , israel , 19 - 26 aug 1997 . _

we propose to measure azimuthal correlations of heavy - flavor hadrons to address the status of thermalization at the partonic stage of light quarks and gluons in high - energy nuclear collisions . in particular , we show that hadronic interactions at the late stage can not significantly disturb the initial back - to - back azimuthal correlations of @xmath0pairs . thus , a decrease or the complete absence of these initial correlations does indicate frequent interactions of heavy - flavor quarks and also light partons in the partonic stage , which are essential for the early thermalization of light partons .

we propose to measure azimuthal correlations of heavy - flavor hadrons to address the status of thermalization at the partonic stage of light quarks and gluons in high - energy nuclear collisions . in particular , we show that hadronic interactions at the late stage can not significantly disturb the initial back - to - back azimuthal correlations of @xmath0pairs . thus , a decrease or the complete absence of these initial correlations does indicate frequent interactions of heavy - flavor quarks and also light partons in the partonic stage , which are essential for the early thermalization of light partons .

1306.4128

i

during the last two decades , blind source separation ( bss ) has attracted an important interest . the main idea of bss consists of finding the transmitted signals without using pilot sequences or a priori knowledge on the propagation channel . using bss in communication systems has the main advantage of eliminating training sequences , which can be expensive or impossible in some practical situations , leading to an increased spectral efficiency . several bss criteria have been proposed in the literature e.g. @xcite . the cm criterion is probably the best known and most studied higher order statistics based criterion in blind equalization @xcite and signal separation @xcite areas . it exploits the fact that certain communication signals have the constant modulus property , as for example phase modulated signals . the constant modulus algorithm ( cma ) was developed independently by @xcite and was initially designed for psk signals . the cma principle consists of preventing the deviation of the squared modulus of the outputs at the receiver from a constant . the main advantages of cma , among others , are its simplicity , robustness , and the fact that it can be applied even for non - constant modulus communication signals . many solutions to the minimization of the cm criterion have been proposed ( see @xcite and references therein ) . the cm criterion was first minimized via adaptive stochastic gradient algorithm ( sga ) @xcite and later on many variants have been devised . it is known , in adaptive filtering , that the convergence rate of the sga is slow . to improve the latter , the authors in @xcite proposed an implementation of the cm criterion via the recursive least squares ( rls ) algorithm . the author in @xcite proposed to rewrite the cm criterion as a least squares problem , which is solved using an iterative algorithm named least squares cma ( ls - cma ) . in @xcite , the authors proposed an algebraic solution for the minimization of the cm criterion . the proposed algorithm is named analytical cma ( acma ) and consists of computing all the separators , at one time , through solving a generalized eigenvalue problem . the main advantage of acma is that , in the noise free case , it provides the exact solution , using only few samples ( the number of samples must be greater than or equal to @xmath0 , where @xmath1 is the number of transmitting antennas ) . moreover , the performance study of acma showed that it converges asymptotically to the wiener receiver @xcite . however , the main drawback of acma is its numerical complexity especially for a large number of transmitting antennas . an adaptive version of acma was also developed in @xcite . more generally , an abundant literature on the cm - like criteria and the different algorithms used to minimize them exists including references @xcite . in this paper , we propose two algorithms to minimize the cm criterion . the first one , referred to as givens cma ( g - cma ) , performs prewhitening in order to make the channel matrix unitary then , it applies successive givens rotations to find the resulting matrix through minimization of the cm criterion . for large number of samples , prewhitening is effective and the transformed channel matrix is very close to unitary , however , for small sample sizes , it is not , and hence results in significant performance loss . in order to compensate the effect of the ineffective prewhitening stage , we propose to use shear rotations @xcite . shear rotations are non - unitary hyperbolic transformations which allow to reduce departure from normality . we note that the authors in @xcite used givens and shear rotations in the context of joint diagonalization of matrices . we thus propose a second algorithm , referred to as hyperbolic g - cma ( hg - cma ) , that uses unitary givens rotations in conjunction with non - unitary shear rotations . the optimal parameters of both complex shear and givens rotations are computed via minimization of the cm criterion . the proposed algorithms have a lower computational complexity as compared to the acma . moreover , unlike the acma which requires a number of samples greater than the square of the number of transmitting antennas , g - cma and hg - cma do not impose such a condition . finally , we propose an adaptive implementation of the hg - cma using sliding window which has the advantages of fast convergence and good separation quality for a moderate computational cost comparable to that of the methods in @xcite . the remainder of the paper is organized as follows . section [ sec : formulation ] introduces the problem formulation and assumptions . in sections [ sec : gcma ] and [ sec : hgcma ] , we introduce the g - cma and hg - cma , respectively . section [ sec : ahgcma ] is dedicated to the adaptive implementation of the hg - cma . some numerical results and discussion are provided in section [ sec : results ] , and conclusions are drawn in section [ sec : conclusion ] .

we propose two new algorithms to minimize the constant modulus ( cm ) criterion in the context of blind source separation . the first algorithm , referred to as givens cma ( g - cma ) uses unitary givens rotations and proceeds in two stages : prewhitening step , which reduces the channel matrix to a unitary one followed by a separation step where the resulting unitary matrix is computed using givens rotations by minimizing the cm criterion . however , for small sample sizes , the prewhitening does not make the channel matrix close enough to unitary and hence applying givens rotations alone does not provide satisfactory performance . to remediate to this problem , we propose to use non - unitary shear ( hyperbolic ) rotations in conjunction with givens rotations . this second algorithm referred to as hyperbolic g - cma ( hg - cma ) is shown to outperform the g - cma as well as the analytical cma ( acma ) in terms of separation quality . the last part of this paper is dedicated to an efficient adaptive implementation of the hg - cma and to performance assessment through numerical experiments .

we propose two new algorithms to minimize the constant modulus ( cm ) criterion in the context of blind source separation . the first algorithm , referred to as givens cma ( g - cma ) uses unitary givens rotations and proceeds in two stages : prewhitening step , which reduces the channel matrix to a unitary one followed by a separation step where the resulting unitary matrix is computed using givens rotations by minimizing the cm criterion . however , for small sample sizes , the prewhitening does not make the channel matrix close enough to unitary and hence applying givens rotations alone does not provide satisfactory performance . to remediate to this problem , we propose to use non - unitary shear ( hyperbolic ) rotations in conjunction with givens rotations . this second algorithm referred to as hyperbolic g - cma ( hg - cma ) is shown to outperform the g - cma as well as the analytical cma ( acma ) in terms of separation quality . the last part of this paper is dedicated to an efficient adaptive implementation of the hg - cma and to performance assessment through numerical experiments . blind source separation , constant modulus algorithm , adaptive cma , sliding window , hyperbolic rotations , givens rotations .

1604.06924

i

the goal of this paper is to establish existence and smoothness of the stable foliation for sectional hyperbolic flows . in particular , we treat the case of the classical lorenz equations @xcite @xmath2 showing that the stable foliation for the flow is at least @xmath1 . this regularity ( @xmath3 for some @xmath4 ) is a crucial component of the analysis in @xcite where we prove exponential decay of correlations for the lorenz attractor . an immediate consequence of our result is that the stable foliation for the associated poincar map is also at least @xmath1 . the results are robust in the sense that we obtain smoothness of the stable foliations and exponential decay of correlations for smooth vector fields that are sufficiently @xmath0-close to the classical one . as far as we know , this is the first complete proof that the stable foliation for the classical lorenz equations ( or even for the poincar map ) exists and is better than hlder continuous . by @xcite and @xcite , the classical lorenz attractor is a singular hyperbolic attractor . a consequence is the existence of smooth stable leaves through each point of the attractor . however , _ a priori _ it does not follow that these leaves form a topological foliation in a full neighborhood of the attractor ; nor is there any information about smoothness of such a foliation . these issues are somewhat controversial , with various false claims in the literature . careful analyses ( see for example @xcite ) require additional conditions to establish smoothness and do not apply to the classical lorenz attractor . recently @xcite gave a verifiable criterion for smoothness of the stable foliation that is easily seen to hold for the classical lorenz attractor . however , the argument in @xcite presupposes that the stable leaves topologically foliate a full neighborhood of the attractor a fact that is folklore but for which apparently there is no proof available in the literature . in this paper , we consider general partially hyperbolic attractors and give a complete proof of the existence of a topological foliation @xmath5 in a neighborhood of such attractors . the individual leaves @xmath6 are smoothly embedded stable manifolds . in general , the leaves need not vary smoothly , but under a bunching condition @xcite the foliation is smooth . the argument in @xcite now applies , and we obtain existence and smoothness of the stable foliation for the classical lorenz attractor . our results hold for the flow , and hence also for the poincar map . this resolves an issue in ( * ? ? ? * section 2.4 ) where it is claimed that the stable foliation for the poincar map is smooth but no details are provided . in addition , we extend the verifiable criterion of @xcite to the sectional hyperbolic situation , and we give a lower bound for the smoothness for the classical lorenz attractor . the condition is verifiable in the sense that it depends only on the linearised vector field and the location of the attractor and its equilibria . in section [ sec : lorenzmodel ] , we recall the notion of partially hyperbolic and sectional hyperbolic attractors . section [ sec : cone ] contains general facts about cone fields for partially hyperbolic attractors , as well as the crucial step that the stable bundle extends continuously to a contracting invariant bundle over a neighborhood of the attractor . section [ sec : foliation ] contains general results about the stable foliation of partially hyperbolic attractors . in particular , the stable leaves define a topological foliation of a neighborhood of the attractor and is smooth under a bunching condition . in section [ sec : sd ] , we specialise to sectional hyperbolic attractors . following @xcite , we give a verifiable condition for smoothness of the stable foliation and apply this to the classical lorenz attractor .

we prove the existence of a contracting invariant topological foliation in a full neighborhood for partially hyperbolic attractors . under certain bunching conditions it can then be shown that this stable foliation is smooth . specialising to sectional hyperbolic attractors , we give a verifiable condition for bunching . in particular , we show that the stable foliation for the classical lorenz equation ( and nearby vector fields ) is better than @xmath0 which is crucial for recent results on exponential decay of correlations . in fact the foliation is at least @xmath1 .

we prove the existence of a contracting invariant topological foliation in a full neighborhood for partially hyperbolic attractors . under certain bunching conditions it can then be shown that this stable foliation is smooth . specialising to sectional hyperbolic attractors , we give a verifiable condition for bunching . in particular , we show that the stable foliation for the classical lorenz equation ( and nearby vector fields ) is better than @xmath0 which is crucial for recent results on exponential decay of correlations . in fact the foliation is at least @xmath1 .

1612.03040

i

according to nowadays observations , present acceleration of the universe expansion has been well established @xcite . within the framework of general relativity , the responsible component of energy for this accelerated expansion is known as _ dark energy _ ( de ) with negative pressure . however , the nature of de is still unknown , and some candidates have been proposed to explain it . the earliest and simplest candidate is the cosmological constant with the time independent equation of state @xmath8 which has some problems like fine - tuning and coincidence problems . therefore , other theories have been suggested for the dynamical de scenario to describe the accelerating universe . an interesting attempt for probing the nature of de within the framework of quantum gravity , is the so - called hde proposal . this model which has arisen a lot of enthusiasm recently @xcite , is motivated from the holographic hypothesis @xcite and has been tested and constrained by various astronomical observations @xcite . in holographic principle a short distance cutoff could be related to a long distance cutoff ( infrared cutoff ) due to the limit set by formation of a black hole . based on the holographic principle , it was shown by cohen et al . @xcite that the quantum zero - point energy of a system with size @xmath2 should not exceed the mass of a black hole with the same size , i.e. , @xmath9 where @xmath10 is the reduced planck mass and @xmath2 is the ir cutoff . the largest @xmath2 allowed is the one saturating this inequality so that we get the @xmath11 where @xmath12 is a dimensionless constant . there are many models of hde , depending on the ir cutoff , that have been studied in the literatures @xcite . the simple choice for ir cutoff is the hubble radius , i.e. , @xmath13 which leads to a wrong equation of state ( eos ) and the accelerated expansion of the universe can not be achieved . however , as soon as an interaction between hde and dark matter is taken into account , the identification of ir cutoff with hubble radius @xmath14 , in flat universe , can simultaneously drive accelerated expansion and solve the coincidence problem . @xcite . then , li @xcite showed that taking the particle horizon radius as ir cutoff it is impossible to obtain an accelerated expansion . he also demonstrated that the identification of @xmath2 with the radius of the future event horizon gives the desired result , namely a sufficiently negative equation of state to obtain an accelerated universe . it is worth noting that , for the sake of simplicity , very often the @xmath6 parameter in the hde model is assumed constant . however , there are no strong evidences to demonstrate that @xmath6 should be a constant and one should bear in mind that it is more general to consider it a slowly varying function of time . it has been shown that the parameter @xmath6 can play an essential role in characterizing the model . for example , it was argued that the hde model in the far future can be like a phantom or quintessence de model depending whether the parameter @xmath6 is larger or smaller than @xmath15 , respectively @xcite . by slowly vary function with time , we mean that @xmath16 is upper bounded by the hubble expansion rate , i.e. , @xcite @xmath17 where dot indicates derivative with respect to the cosmic time . in this case the time scale of the evolution of @xmath6 is shorter than @xmath14 and one can be satisfied to consider the time dependency of @xmath6 @xcite . considering the future event horizon as ir cutoff , the hde model with time varying parameter @xmath6 , has been studied in @xcite . it was argued that depending on the parameter @xmath6 , the phantom regime can be achieved earlier or later compared to the usual hde with constant @xmath6 term @xcite . in this paper , we reconsider the hde model with the slowly varying parameter @xmath18 by taking into account the hubble horizon @xmath4 and go cutoff , @xmath19 , as the system s ir cutoffs . we shall study four parameterizations of @xmath20 as follows @xmath21 where ghde stands for the generalized hde model . the above choices for @xmath20 are , respectively , inspired by the parameterizations known as chevallier - polarski - linder parametrization ( cpl ) @xcite , jassal - bagla - padmanabhan ( jbp ) parametrization @xcite , wetterich parametrization @xcite , and ma - zhang parametrization @xcite . setting @xmath22 in all these four parameterizations , the original hde with constant @xmath23 parameter is recovered . this paper is organized as follows . in section ii , we drive the basic equations for the hde with time varying @xmath6 parameter . in this section , we also consider the hubble radius as ir cutoff and derive the evolution of eos and deceleration parameters by choosing @xmath20 . in section iii , we repeat the study for the go cutoff and investigate the evolution of the cosmological parameters . the last section is devoted to conclusions and discussions .

we reconsider the holographic dark energy ( hde ) model with a slowly time varying @xmath0 parameter in the energy density , namely @xmath1 , where @xmath2 is the ir cutoff and @xmath3 is the redshift parameter . as the system s ir cutoff we choose the hubble radius and the granda - oliveros ( go ) cutoffs . the latter inspired by the ricci scalar curvature . we derive the evolution of the cosmological parameters such as the equation of state and the deceleration parameters as the explicit functions of the redshift parameter @xmath3 .

we reconsider the holographic dark energy ( hde ) model with a slowly time varying @xmath0 parameter in the energy density , namely @xmath1 , where @xmath2 is the ir cutoff and @xmath3 is the redshift parameter . as the system s ir cutoff we choose the hubble radius and the granda - oliveros ( go ) cutoffs . the latter inspired by the ricci scalar curvature . we derive the evolution of the cosmological parameters such as the equation of state and the deceleration parameters as the explicit functions of the redshift parameter @xmath3 . then , we plot the evolutions of these cosmological parameters in terms of the redshift parameter during the history of the universe . interestingly enough , we observe that by choosing @xmath4 as the ir cutoff for the hde with time varying @xmath5 term , the present acceleration of the universe expansion can be achieved , even in the absence of interaction between dark energy and dark matter . this is in contrast to the usual hde model with constant @xmath6 term , which leads to a wrong equation of state , namely that for dust @xmath7 , when the ir cutoff is chosen the hubble radius .

1608.05750

c

the study of the galaxy lfs has a long history ( @xcite and references therein ) . the faint end of the galaxy lfs provides strong constraints to the modeling of the formation and evolution of low mass galaxies ( e.g , @xcite ) . however , whether the slope for the faint end of the cluster galaxy lf is steep or flat has been controversial ( @xcite and references therein ) . several studies suggested that the lfs of red dwarf galaxies in galaxy clusters at low to high redshifts are relatively flat , with a power law index @xmath255 to 1.4 ( virgo and fornax @xcite , and clusters at @xmath256 @xcite ) or with @xmath257 to 1.1 ( the hydra i and the centaurus @xcite , and several clusters at @xmath258 @xcite ) . on the other hand , @xcite presented a much steeper lf for sdss galaxy clusters . they derived composite lfs of blue ( @xmath259 ) and red ( @xmath260 ) galaxies ( @xmath261 mag ) in the sdss galaxy clusters at low redshift . the blue galaxy lf is fit well by a single schechter function with a steep faint end ( @xmath262 and @xmath263 mag ) . however , the red galaxy lf becomes flat in the bright part and rises again at @xmath264 mag so that it can be described better by a sum of double schechter components ( see their figure 9 and table 2 ) . the parameters for the fainter component are @xmath265 and @xmath266 mag , and those for the brighter component are @xmath267 and @xmath268 mag . later @xcite presented , from the analysis of the galaxy lfs of nearby abell clusters , the lfs of red galaxies show even steeper faint ends ( @xmath269 ) . they also found that the faint ends ( @xmath270 mag ) of the lfs for red galaxies are steeper in the outer region than in the inner region of the clusters . however their data are more than one magnitude shallower than the @xcite sample so that the uncertainties for the faint ends are larger . in addition , @xcite presented an lf of the galaxies in abell 1689 derived from the f606w and f814w wpfc2 images , which shows an upturn at f814w(ab)@xmath271 mag . the faint end at @xmath272f814w(ab)@xmath273 mag ( @xmath274f814w(vega)@xmath275 mag , @xmath276 mag ) of the red sequence galaxies in this cluster shows a steep lf with @xmath277 ( @xmath278 for all galaxies ) . to make the story more interesting , @xcite and @xcite presented a very steep lf of the faintest compact dwarf galaxies with @xmath279 mag in coma , with a logarithmic slope , @xmath280 ( derived using @xmath281 ) . in contrast , @xcite and @xcite found recently , using spectroscopic members of abell 85 ( at @xmath282 ) , no evidence for a steep upturn of the faint - end slope in the lf of red dwarf galaxies , obtaining @xmath283 for @xmath284 . the lf of the faint end in abell 2744 derived in this study is relatively flat with @xmath285 , showing no evidence for faint upturn . @xcite used shallower @xmath286 images of abell 2744 ( pi : dupke , pid : 11689 ) ) , obtaining @xmath287 ( @xmath288 ) for @xmath289 mag from single schechter function fitting ( see their fig . 11 for the cmd of abell 2744 ) . our data go much deeper than those used in @xcite , and our result for the slope of the faint end , @xmath240 derived from the single schechter function fitting , is slightly steeper than the value given by @xcite . the lf of the faint end for abell 2744 is in strong contrast to the result for abell 1689 given by @xcite . note that the lf of galaxies in abell 1689 presented by @xcite shows , in their fig . 2(f ) , an upturn at the faint end @xmath290f814w(ab)@xmath291 mag ( @xmath292f814w(vega)@xmath275 mag ) , with a slope @xmath277 . our lf of abell 2744 goes much deeper ( @xmath293f814w(vega)@xmath102 mag ) than that given by @xcite . the @xmath294-band lfs of faint galaxies in virgo and fornax given by @xcite ( see also a compilation in fig . 4 of @xcite ) keep increasing until at the current completeness limits , @xmath295 mag and @xmath296 mag , respectively . these correspond to @xmath297 mag and @xmath298 mag , respectively , for @xmath299 . the lfs decrease thereafter until at @xmath300 mag , which is the faintest limit in the cluster galaxy sample . recently @xcite found 11 ultra - faint low surface brightness galaxies with @xmath301 mag in a 576 arcmin@xmath302 field in virgo using the large binocular telescope . these galaxies are much fainter than the previous survey limits , but the covered field is only a small fraction of the virgo cluster . thus the detection limit of the faint galaxies in abell 2744 in this study , f814w@xmath190 mag ( @xmath303 mag ) , is somewhat fainter than those for wide field surveys of virgo and fornax . the faint end slope for abell 2744 , @xmath285 is even slightly flatter than those for virgo and fornax , @xmath304 to 1.4 , given by @xcite , but is similar to the value , @xmath305 , for dwarf galaxies with @xmath306 mag in fornax given by @xcite . the lf of the red sequence galaxies in abell 2744 shows a dip at f814w @xmath223 ( @xmath224 ) mag . the presence of this dip in the galaxy lf has been known in the low density regions of galaxy clusters , while it is rarely seen in the high density regions of galaxy clusters @xcite . the dip magnitude of abell 2744 is similar to the values in the previous studies , @xmath307 mag . it has been suggested that the presence of this gap can be explained by the efficiency of merging of intermediate luminosity galaxies depending on the galaxy density @xcite . low density regions like the galaxy groups , poor galaxy clusters , or outskirt of rich galaxy clusters have a higher efficiency of galaxy merging than that of the high density regions , because they have lower velocity dispersion . merging of intermediate luminosity galaxies ( with a dip magnitude ) produce brighter galaxies , while the lf of the faint galaxies changes little . it results in a dip in the lf of galaxies , showing two components in the galaxy lf . it is noted that the region of abell 2744 used in this study is located at @xmath308 with relatively high density of galaxies , but it shows clearly a dip . this may be related with the dynamical status of abell 2744 , which is still involved with merging of substructures . and @xmath309 mag . ( b ) the mass density map derived with the cats gravitational lensing models @xcite . ] in * figure [ fig_mass ] * we compare the spatial distribution of the gc / ucds with the mass map for the same field derived from the gravitational lensing models by the cats team , which is provided in the hff @xcite . the mass map derived from the lensing model shows a strong concentration around the two bcgs ( see also @xcite ) . thus the spatial distribution of the gcs and ucds is similar to the mass map . however , the degree of central concentration of the gcs and ucds is much stronger than that of the mass density , as shown below . for comparison with the radial number density profiles of the ucds and gcs , we derived the radial number density profiles of the red sequence galaxies in abell 2744 , plotting them in * figure [ fig_raddencomp]*. we subtracted the background contribution using the hxdf data . we divided the red sequence galaxy sample into two groups according to their magnitude : a bright group ( bright galaxies with f814w@xmath310 ( @xmath311 ) mag ) , and a faint group ( dwarf galaxies with @xmath180f814w@xmath211 ( @xmath312 ) mag ) . the number of galaxies detected in the innermost region @xmath313 ( 52 kpc ) is too small for analysis so that only the number density profiles of the galaxies at @xmath314 are useful for analysis . in addition , we derived the radial mass density profile of abell 2744 from the cats model image @xcite provided in the hff . as the center for deriving the radial profiles , we adopted the center of cn-2 as in the case of the gc / ucds . mag , and the red sequence galaxies with f814w@xmath315 mag ) ; and ( c ) for the faint samples ( the ucds with @xmath127f814w@xmath124 mag , and the red sequence galaxies with @xmath180f814w@xmath211 mag ) . two dashed lines in ( a ) indicate the power - low fit results for the profiles of the mass density map ( green line ) and the gc / ucds ( blue line ) for the outer region at @xmath316 . ] * figure [ fig_raddencomp ] * shows a few distinguishable features as follows . first , the radial number density profiles of the red sequence galaxies are almost flat in the outer region at @xmath317 , while the profile of the bright group decreases slowly as the clustercentric distance increases . it is noted that the radial number density profile of the gc / ucds is much steeper than the profile of the red sequence galaxies . second , the mass density radial profile of abell 2744 derived from the cats gravitational lensing models decreases slowly as the clustercentric distance increases . the slope of the mass density profile is much flatter than that of the radial number density profiles of the gc / ucds . the logarithmic slope of the mass density profile for the outer region at @xmath316 is derived from the power fits to be @xmath318 . on the other hand , we derive @xmath319 from the number density profile of the gc / ucds , which is @xmath466 times steeper than that of the mass density profile . however , the mass density profile is consistent with that of the radial number density profiles of the red sequence galaxies in the outer region at @xmath316 . it is noted that , although the spatial distribution of the gc / ucds shows a strong correlation with the mass density map ( see * figure [ fig_mass ] * ) , the gc / ucds show a significant difference in the radial distribution in the sense that the gc / ucds show a much stronger central concentration . these results show that the radial distribution of the gc / ucds in abell 2744 is much steeper than the distribution of dark matter , which is consistent with the case of abell 1689 @xcite . the radial distribution of the dwarf galaxies follows well that of dark matter . since the discovery of ucds , the origin of the ucds has been controversial @xcite . there are three types of scenarios suggested to explain the origin of the ucds . first , the ucds are just the massive end of the normal gcs @xcite . second , they are the nuclei of dwarf galaxies that were stripped due to the tidal interaction with their host galaxies @xcite . direct evidence for this scenario has been found recently by detection of the existence of supermassive black hole in some ucds @xcite , and by finding that some ucds show an extended star formation history ( @xcite , ko et al . ( 2016 , in preparation ) ) . metal - rich ucds with young populations may be the remnants of a dissipative merger of two gas - rich dwarf galaxies @xcite . third , the ucds are the remnants of primordial compact galaxies that have formed early around their host galaxies @xcite . this was suggested to explain the fact that the spatial distribution of the ucds in the fornax cluster show a stronger central concentration than than of the de galaxies . the origin of the ucds may be a combination of these , rather than a single scenario @xcite . recently @xcite and @xcite studied the properties of 97 ucds ( with @xmath320 pc , @xmath321 mag , @xmath322 mag ) in m87 , a cd galaxy in virgo , this is the largest sample of ucds in a single galaxy . they found that there are significant differences in the radial number density profiles and the kinematics between the ucds and the gcs in virgo and that the mean color of the ucds is consistent with that of the blue gcs . from this they concluded that the origin of most ucds in virgo is close to the nuclei of stripped dwarf galaxies , rather than to the massive end of the gcs . this conclusion is in strong contrast to the result for the ucds in coma that @xcite concluded , that most ucds in coma are of the star cluster - origin , noting the similarity in the properties and spatial distribution of ucds and gcs . their sample of ucds covers a similar magnitude range , @xmath323 mag . in the discussion of compact stellar systems ( with @xmath324 pc and @xmath325 ) in various galaxies and galaxy clusters , @xcite and @xcite pointed out that there are two types of ucds : star cluster - type ucds and galaxy - type ucds . the upper magnitude limit of star cluster type ucds is @xmath326 mag ( or @xmath327 ) . they noted that the lf of the ucds and compact galaxies shows a break at @xmath328 mag . it is almost flat at the bright range ( @xmath329 mag ) , but it increases suddenly at the faint end ( @xmath330 mag ) ( see figure 12 in @xcite ) . the bright component represents galaxy - origin ucds , while the faint one does star cluster - type ucds . however , this is based on the sample made of heterogeneous data and the number of the sources brighter than @xmath331 mag is only a handful , as described by @xcite , so that it is only indicative , requiring further confirmation . the lfs of gc / ucds in abell 2744 in this study ( * figure [ fig_lfpoint ] * ) show a break at f814w @xmath195 mag , which corresponds to @xmath196 ( @xmath332 ) mag . thus this value is 0.6 magnitude fainter than @xmath326 mag , noted for the ucds in the local universe @xcite . our result based on the large sample of homogeneous data for abell 2744 confirms the presence of the break , but at a 0.6 magnitude fainter value , @xmath333 mag . in addition , it is noted that the mean color of the faint dwarf galaxies with @xmath334 mag in abell 2744 is similar to that of the ucds / gcs . in summary , there are three clues useful to understand the origin of the ucds in abell 2744 found in this study : ( a ) the presence of a break at @xmath335 mag in the lf of the ucd / gcs , ( b ) the radial number density profiles of the ucds that are much steeper than those of the red sequence galaxies , and ( c ) the mean color of the faint red sequence galaxies that is similar to that of the ucds . these clues support the hypothesis for the dual origin of the ucds : bright ucds are the nuclei of dwarf galaxies that were stripped when they passed the inner region of a galaxy cluster , while faint ucds are the upper end of mass functions of the gcs .

these results support the galaxy - origin scenario for bright ucds : they are the nuclei of dwarf galaxies that were stripped when they pass close to the center of massive galaxies or a galaxy cluster , while some of the faint ucds are the bright end of the gcs .

we report a photometric study of globular clusters ( gcs ) , ultracompact dwarfs ( ucds ) , and dwarf galaxies in the giant merging galaxy cluster abell 2744 at @xmath0 . color - magnitude diagrams of the point sources derived from deep f814w ( restframe @xmath1 ) and f105w ( restframe @xmath2 ) images of abell 2744 in the hubble space telescope frontier field show a rich population of point sources whose colors are similar to those of typical gcs . these sources are as bright as @xmath3 ( @xmath4f814w(vega)@xmath5 ) mag , being mostly ucds and bright gcs in abell 2744 . the luminosity function ( lf ) of these sources shows a break at @xmath6 ( f814w @xmath7 ) mag , indicating a boundary between ucds and bright gcs . the numbers of gcs and ucds are estimated to be @xmath8 , and @xmath9 , respectively . the clustercentric radial number density profiles of the ucds and bright gcs show similar slopes , but these profiles are much steeper than that of the dwarf galaxies and the mass density profile based on gravitational lensing analysis . we derive an lf of the red sequence galaxies for @xmath10 mag . the faint end of this lf is fit well by a flat power law with @xmath11 , showing no faint upturn . these results support the galaxy - origin scenario for bright ucds : they are the nuclei of dwarf galaxies that were stripped when they pass close to the center of massive galaxies or a galaxy cluster , while some of the faint ucds are the bright end of the gcs .

1608.05750

i

we detected a large population of gcs , ucds , and dwarf galaxies in the deep high resolution f814w and f105w images of the sourthern core of abell 2744 in the hff . we could estimate the background field contribution using photometry of the parallel field and the hxdf . then we investigated the photometric properties of these sources in comparison with the results for the parallel field and the hxdf . to date , abell 2744 at the redshift of @xmath0 is the most distant system where gcs and ucds are studied in detail . primary results are summarized as follows . * cmds of the extended sources derived from deep f814w ( restframe @xmath336 ) and f105w ( restframe @xmath2 ) images of abell 2744 show a red sequence reaching down to @xmath303 mag . * cmds of the point sources in abell 2744 show a rich population of point sources whose colors are similar to those of typical gcs . they are as bright as @xmath4f814w@xmath114 ( @xmath337 ) mag , and their color distribution shows a peak at ( f814w - f105w)@xmath122 . they are mostly bright gcs and ucds in abell 2744 . * th spatial distribution of the gcs and ucds shows a strong central concentration to the brightest galaxies . this is consistent with the mass map based on gravitational lensing analysis @xcite . however , the radial number density profile of the gcs and ucds is much steeper than the radial mass density profile based on gravitational lensing models @xcite . the mass density profile is consistent with the radial number density profile of the dwarf galaxies in abell 2744 . * the lf of the gcs and ucds in abell 2744 shows a break at f814w@xmath195 ( @xmath338 ) mag . this is consistent with the one based on the heterogeneous data for the ucds in the local universe @xcite . * the number of ucds with f814w@xmath205 mag in abell 2744 is estimated to be @xmath206 . the number of gcs is derived to be @xmath207 , this value is even larger than that for abell 1689 , @xmath23 , given by @xcite . thus abell 2744 hosts the largest number of gcs among the known systems . * the lf of the red sequence galaxies for a large range of magnitudes @xmath177f814w@xmath102 ( @xmath339 ) mag shows double components , with a dip at f814w @xmath223 ( @xmath224 ) mag . the faint end of the red galaxy lf is fit well by a flat power law with @xmath11 , showing no faint upturn . * these results support the hypothesis for the dual origin of the ucds : bright ucds are nuclei of dwarf galaxies that were stripped when they passed the inner region of a galaxy cluster , while faint ucds are massive gcs at the upper end in the mass function of the gcs . the authors are grateful to john blakeslee for providing their results on abell 2744 presented at the aas meeting , and to brian cho for his help in improving the english in the draft . this work was supported by the national research foundation of korea ( nrf ) grant funded by the korea government ( msip ) ( no . 2013r1a2a2a05005120 ) . this work based on observations obtained with the nasa / esa hubble space telescope , retrieved from the mikulski archive for space telescopes ( mast ) at the space telescope science institute ( stsci ) . stsci is operated by the association of universities for research in astronomy , inc . under nasa contract nas 5 - 26555 . this work also utilizes gravitational lensing models produced by pis bradac , natarajan & kneib ( cats ) , merten & zitrin , sharon , and williams , and the glafic and diego groups . this lens modeling was partially funded by the hst frontier fields program conducted by stsci . stsci is operated by the association of universities for research in astronomy , inc . under nasa contract nas 5 - 26555 . the lens models were obtained from the mikulski archive for space telescopes ( mast ) . agulli , i. , aguerri , j. a. l. , snchez - janssen , r. , et al . 2014 , , 444 , l34 agulli , i. , aguerri , j. a. l. , snchez - janssen , r. , et al . 2016 , , 458 , 1590 alamo - martnez , k. a. , blakeslee , j. 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we report a photometric study of globular clusters ( gcs ) , ultracompact dwarfs ( ucds ) , and dwarf galaxies in the giant merging galaxy cluster abell 2744 at @xmath0 . color - magnitude diagrams of the point sources derived from deep f814w ( restframe @xmath1 ) and f105w ( restframe @xmath2 ) images of abell 2744 in the hubble space telescope frontier field show a rich population of point sources whose colors are similar to those of typical gcs . the clustercentric radial number density profiles of the ucds and bright gcs show similar slopes , but these profiles are much steeper than that of the dwarf galaxies and the mass density profile based on gravitational lensing analysis . we derive an lf of the red sequence galaxies for @xmath10 mag . the faint end of this lf is fit well by a flat power law with @xmath11 , showing no faint upturn .

we report a photometric study of globular clusters ( gcs ) , ultracompact dwarfs ( ucds ) , and dwarf galaxies in the giant merging galaxy cluster abell 2744 at @xmath0 . color - magnitude diagrams of the point sources derived from deep f814w ( restframe @xmath1 ) and f105w ( restframe @xmath2 ) images of abell 2744 in the hubble space telescope frontier field show a rich population of point sources whose colors are similar to those of typical gcs . these sources are as bright as @xmath3 ( @xmath4f814w(vega)@xmath5 ) mag , being mostly ucds and bright gcs in abell 2744 . the luminosity function ( lf ) of these sources shows a break at @xmath6 ( f814w @xmath7 ) mag , indicating a boundary between ucds and bright gcs . the numbers of gcs and ucds are estimated to be @xmath8 , and @xmath9 , respectively . the clustercentric radial number density profiles of the ucds and bright gcs show similar slopes , but these profiles are much steeper than that of the dwarf galaxies and the mass density profile based on gravitational lensing analysis . we derive an lf of the red sequence galaxies for @xmath10 mag . the faint end of this lf is fit well by a flat power law with @xmath11 , showing no faint upturn . these results support the galaxy - origin scenario for bright ucds : they are the nuclei of dwarf galaxies that were stripped when they pass close to the center of massive galaxies or a galaxy cluster , while some of the faint ucds are the bright end of the gcs .

astro-ph0309070

i

broad band color selection , based on ultraviolet ( uv ) spectral breaks caused by neutral hydrogen , is an efficient technique for identifying galaxies at @xmath5 to 4 with imaging from the ground and from the _ hubble space telescope _ @xcite . at higher redshifts and relatively bright magnitudes , @xmath6 colors from the sloan digital sky survey have been used to identify qsos out to @xmath7 @xcite . some galaxies at @xmath8 have also been found in this way , but the required deep imaging and spectroscopy is extremely challenging . a lyman break galaxy ( lbg ) with typical ( @xmath9 ) uv luminosity at @xmath5 ( @xmath10 , adelberger & steidel 2000 ) would have @xmath11 if moved , without evolution , to @xmath4 , and would be undetected in the @xmath12band ( hence , an `` @xmath12dropout '' ) . at @xmath13 , ly@xmath1 shifts through the @xmath14band , and galaxies are lost to optical sight altogether . one goal of the great observatories origins deep survey ( goods ) is to find and study large numbers of galaxies at @xmath15 . here , we report initial results from goods on galaxy candidates at @xmath0 , including spectroscopy for one galaxy , cdfs j033240.0@xmath16274815 ( henceforth sid2 ) , with the acs grism and the keck and vlt observatories . we use ab magnitudes ( ab @xmath17 ) , and assume a cosmology with @xmath18 and @xmath19 km s@xmath20 mpc@xmath20 .

we report early results on galaxies at @xmath0 , selected from _ hubble space telescope _ imaging for the great observatories origins deep survey . spectroscopy of one object with the advanced camera for surveys grism and from the keck and vlt observatories a shows a strong continuum break and asymmetric line emission , identified as ly@xmath1 at @xmath2 .

we report early results on galaxies at @xmath0 , selected from _ hubble space telescope _ imaging for the great observatories origins deep survey . spectroscopy of one object with the advanced camera for surveys grism and from the keck and vlt observatories a shows a strong continuum break and asymmetric line emission , identified as ly@xmath1 at @xmath2 . we detect only five spatially extended , @xmath0 candidates with signal to noise ratios @xmath3 , two of which have spectroscopic confirmation . this is many fewer than would be expected if galaxies at @xmath4 had the same luminosity function as those at @xmath5 . there are many fainter candidates , but we expect substantial contamination from foreground interlopers and spurious detections . our best estimates favor a @xmath4 galaxy population with fainter luminosities , higher space density , and similar co moving ultraviolet emissivity to that at @xmath5 , but this depends critically on counts at fluxes fainter than those reliably probed by the current data .

astro-ph0309070

c

the @xmath35 color limit sets a lower redshift bound for @xmath12dropouts , while igm suppression in makes the upper bound , and hence the sampling volume , a strong function of luminosity . we use simulations @xcite to predict number counts of candidates , including photometric biases . we generated artificial galaxies with a mixture of disk and bulge surface brightness profiles , ellipticities , and orientations . their sizes were drawn from a log normal distribution tuned to reproduce measurements at @xmath315 @xcite . their spectra have a distribution of uv spectral slopes that matches the observed colors of lbgs at @xmath31 @xcite . we distributed the galaxies in redshift , modulated their spectra by igm opacity @xcite , convolved them with acs point spread functions , added them to the goods images at various magnitudes , and recovered them with sextractor . figure [ fig : s2ncount ] compares the number of @xmath12dropout candidates to simulations for various assumptions about the uv luminosity function ( lf ) , which we model as a schechter ( 1976 ) distribution with a faint end slope fixed to @xmath91 , as measured for lbgs at @xmath5 @xcite . the number of _ bright _ galaxies is smaller at @xmath55 than at @xmath5 ( see also sbm ; bremer & lehnert 2003 find a similar result from ground based imaging for lbgs at @xmath92 ) . the @xmath5 lf is excluded with a high degree of confidence ( @xmath93 ) . it predicts 30 galaxies with @xmath54 vs. 5 observed , and 26 with @xmath94 vs. @xmath95 observed . , only one has @xmath54 . the others may be real , but contamination may be substantial . ] a change in the number of bright objects does not require comparable evolution in the total luminosity density of the population ; the number of bright sources is exponentially sensitive to the value of @xmath9 . schechter functions fit to the counts in fig . [ fig : s2ncount]@xmath45 favor fainter @xmath9 and higher @xmath96 compared to their values at @xmath5 . integrating acceptable fits for @xmath97 ( @xmath98 ) , the uv emissivity is similar to that at @xmath5 ( @xmath99 , 95.4% confidence ) . however , these fitted @xmath9 values , and hence most of the inferred luminosity density , are at @xmath100 , where the current data are most uncertain . the lf fit is strongly driven by objects with @xmath101 ( fig . [ fig : s2ncount]@xmath50 ) . a model with @xmath102 and @xmath103 smaller @xmath96 ( and @xmath104 ) is consistent with the data at brighter magnitudes and higher @xmath36 ratios , but drastically underpredicts the counts at low @xmath36 and @xmath105 . fits excluding the lowest @xmath36 bin leave the total @xmath104 essentially unconstrained . a robust determination of the @xmath4 lf and total emissivity requires data significantly deeper than those used here . two other studies have analyzed @xmath12dropouts from somewhat deeper acs images . @xcite found 2.3 candidates / arcmin@xmath21 with @xmath106 in an acs field with exposure time 1.5@xmath107 longer in than the 3epoch goods data , but @xmath108 longer in , thus providing more robust color discrimination against interlopers . their density is @xmath109 larger than ours to the same @xmath36 threshold . they estimate their catalogs are 100% complete for @xmath110 , whereas ours are only 50% complete for point sources at @xmath111 @xcite . yan et al . may have underestimated their source fluxes or spurious detection rate , but it is notable that they also find very few bright candidates ( none with @xmath112 ) . @xcite identified 0.5 candidates / arcmin@xmath21 with @xmath113 from imaging ( 520 orbits in ) covering 46 arcmin@xmath21 . they also find few bright candidates ( only one with @xmath114 ) , and estimate @xmath115 . in summary , we have identified five spatially extended , high@xmath36 candidates for galaxies at @xmath0 in early goods acs imaging . two have confirmed redshifts @xmath116 . there are many fainter candidates , but we estimate that @xmath117 may be spurious detections or foreground interlopers . the number of robust candidates is smaller than is predicted if the lf were the same as that at @xmath118 . our best estimates find fainter @xmath9 , larger @xmath96 , and moderately smaller @xmath104 compared to @xmath119 , but this strongly depends on the number of objects at @xmath120 , which is as yet poorly measured . constant @xmath9 with smaller @xmath96 and @xmath104 are consistent with the bright counts but greatly underpredict the number of faint sources . the measurements do not require ( nor robustly exclude ) a dramatic change in @xmath104 from @xmath0 to 3 , especially if @xmath9 is evolving with redshift . @xcite find only a modest change ( @xmath121 ) in the luminosity density from @xmath5 to @xmath122 where the goods lbg sample is much better characterized . our best estimates are consistent with an extrapolation of those results to @xmath4 , but deeper data are needed for a robust measurement . the final goods images will be deeper , with fewer contaminating artifacts . this , together with much deeper data ( e.g. , the forthcoming acs ultradeep field ) , will provide better constraints on the galaxy population at these highest optically accessible redshifts . we thank the members of the goods team , and the staff at stsci , eso and the keck observatory , who made this project possible . support was provided by nasa through grant go09583.01 - 96a from stsci , which is operated by aura under nasa contract nas5 - 26555 . work by lm and ds was supported by nasa through the _ sirtf _ legacy science program , through contract number 1224666 , issued by jpl , california institute of technology , under nasa contract 1407 . sid001 & 03:32:25.60 & 27:55:48.6 & 20.45 & @xmath123 & @xmath124 & 0.18 & sbm#3 @xmath125 @xcite + sid002 & 03:32:40.02 & 27:48:15.0 & 12.72 & @xmath126 & @xmath127 & 0.19 & sbm#1 @xmath128 ( this paper ) ; isaac + sid003 & 03:32:19.07 & 27:54:21.9 & 11.72 & @xmath129 & @xmath130 & 0.27 & sbm#7 ; faint ir ( sofi ) + nid001 & 12:36:19.90 & 62:09:34.2 & 10.55 & @xmath131 & @xmath132 & 0.19 & + sid004 & 03:32:33.20 & 27:39:49.2 & 10.24 & @xmath133 & @xmath134 & 0.70 & faint ir ( sofi ) + sid005 & 03:32:39.03 & 27:52:23.1 & 9.44 & @xmath135 & @xmath136 & 0.28 & + sid006 & 03:32:45.23 & 27:49:09.9 & 9.05 & @xmath137 & @xmath138 & 0.65 & + nid002 & 12:37:28.62 & 62:20:39.1 & 8.79 & @xmath139 & @xmath140 & 0.77 & + sid007 & 03:32:42.94 & 27:52:00.7 & 8.75 & @xmath141 & @xmath142 & 0.72 & + nid003 & 12:37:35.90 & 62:20:43.4 & 8.67 & @xmath143 & @xmath144 & 0.93 & + sid008 & 03:32:13.06 & 27:49:00.7 & 8.63 & @xmath145 & @xmath146 & 0.34 & + sid009 & 03:32:41.36 & 27:50:04.7 & 8.58 & @xmath147 & @xmath148 & 0.14 & + sid010 & 03:32:26.25 & 27:48:30.3 & 8.50 & @xmath149 & @xmath150 & 0.23 & isaac + nid004 & 12:36:42.15 & 62:09:02.0 & 8.20 & @xmath151 & @xmath152 & 0.75 & + nid005 & 12:35:59.01 & 62:12:45.6 & 8.15 & @xmath153 & @xmath154 & 0.36 & + nid006 & 12:36:18.54 & 62:10:41.9 & 8.13 & @xmath155 & @xmath156 & 0.28 & + nid007 & 12:37:52.57 & 62:17:00.7 & 8.08 & @xmath157 & @xmath158 & 0.21 & + sid011 & 03:32:37.63 & 27:50:22.4 & 8.07 & @xmath159 & @xmath160 & 0.88 & isaac + sid012 & 03:32:23.84 & 27:55:11.5 & 8.02 & @xmath161 & @xmath162 & 0.23 & + nid008 & 12:36:43.53 & 62:10:04.1 & 7.89 & @xmath163 & @xmath164 & 0.19 & + nid009 & 12:37:12.43 & 62:18:28.4 & 7.65 & @xmath165 & @xmath166 & 0.32 & + nid010 & 12:36:48.08 & 62:10:12.6 & 7.60 & @xmath167 & @xmath168 & 0.90 & + sid013 & 03:32:34.69 & 27:50:22.8 & 7.57 & @xmath169 & @xmath170 & 0.87 & isaac ( bright : @xmath171 , @xmath172 ) + nid011 & 12:37:15.75 & 62:22:32.5 & 7.43 & @xmath173 & @xmath174 & 0.13 & + nid012 & 12:36:48.71 & 62:12:17.1 & 7.41 & @xmath175 & @xmath176 & 0.57 & + nid013 & 12:36:13.04 & 62:10:43.6 & 7.34 & @xmath177 & @xmath178 & 0.58 & + nid014 & 12:37:22.51 & 62:18:39.7 & 7.26 & @xmath179 & @xmath180 & 0.68 & + nid016 & 12:35:49.72 & 62:13:29.2 & 7.21 & @xmath181 & @xmath182 & 0.61 & + nid015 & 12:35:50.89 & 62:11:58.8 & 7.21 & @xmath183 & @xmath184 & 0.32 & + sid014 & 03:32:52.22 & 27:48:04.8 & 7.20 & @xmath185 & @xmath186 & 0.25 & + nid017 & 12:35:52.33 & 62:12:08.7 & 7.11 & @xmath187 & @xmath188 & 0.69 & + sid015 & 03:32:54.11 & 27:49:16.0 & 7.06 & @xmath189 & @xmath190 & 0.47 & + sid016 & 03:32:11.93 & 27:41:57.1 & 7.04 & @xmath191 & @xmath192 & 0.27 & + sid017 & 03:32:33.16 & 27:41:17.1 & 6.95 & @xmath193 & @xmath194 & 0.64 & + sid018 & 03:32:54.06 & 27:51:12.0 & 6.91 & @xmath195 & @xmath196 & 0.19 & + sid019 & 03:32:36.34 & 27:43:15.6 & 6.82 & @xmath197 & @xmath198 & 0.49 & + nid018 & 12:36:15.36 & 62:14:56.4 & 6.82 & @xmath199 & @xmath200 & 0.18 & + sid020 & 03:32:22.27 & 27:52:57.2 & 6.80 & @xmath201 & @xmath202 & 0.68 & + sid021 & 03:32:25.15 & 27:48:17.1 & 6.79 & @xmath203 & @xmath204 & 0.58 & isaac + nid019 & 12:37:08.89 & 62:19:19.1 & 6.78 & @xmath205 & @xmath206 & 0.15 & + nid020 & 12:37:35.94 & 62:14:22.4 & 6.78 & @xmath207 & @xmath208 & 0.55 & + sid022 & 03:32:29.84 & 27:52:33.2 & 6.77 & @xmath209 & @xmath210 & 0.24 & + sid023 & 03:32:46.05 & 27:49:29.7 & 6.75 & @xmath211 & @xmath198 & 0.32 & + nid022 & 12:37:12.94 & 62:18:05.6 & 6.75 & @xmath212 & @xmath213 & 0.50 & + nid021 & 12:36:08.21 & 62:09:10.8 & 6.75 & @xmath214 & @xmath215 & 0.13 & + nid023 & 12:37:25.35 & 62:18:45.6 & 6.70 & @xmath216 & @xmath217 & 0.41 & + nid024 & 12:37:42.85 & 62:19:41.8 & 6.64 & @xmath218 & @xmath219 & 0.52 & + nid025 & 12:36:35.63 & 62:09:35.8 & 6.62 & @xmath220 & @xmath221 & 0.30 & + sid024 & 03:32:32.46 & 27:40:02.0 & 6.56 & @xmath222 & @xmath210 & 0.30 & + nid026 & 12:37:34.56 & 62:20:16.6 & 6.54 & @xmath223 & @xmath224 & 0.62 & + nid027 & 12:35:48.66 & 62:12:13.3 & 6.54 & @xmath225 & @xmath210 & 0.71 & + nid028 & 12:36:14.37 & 62:16:17.4 & 6.53 & @xmath226 & @xmath227 & 0.21 & + nid029 & 12:37:32.67 & 62:14:16.6 & 6.47 & @xmath228 & @xmath229 & 0.47 & + nid030 & 12:35:57.59 & 62:12:09.2 & 6.45 & @xmath230 & @xmath231 & 0.50 & + nid031 & 12:36:15.08 & 62:16:34.4 & 6.41 & @xmath232 & @xmath233 & 0.50 & + sid025 & 03:32:36.47 & 27:46:41.5 & 6.40 & @xmath234 & @xmath217 & 0.42 & isaac + nid032 & 12:37:10.96 & 62:19:48.0 & 6.39 & @xmath235 & @xmath236 & 0.60 & + nid033 & 12:37:11.40 & 62:22:17.0 & 6.32 & @xmath237 & @xmath238 & 0.42 & + nid034 & 12:36:45.51 & 62:18:32.7 & 6.30 & @xmath239 & @xmath240 & 0.30 & + nid035 & 12:36:28.03 & 62:13:04.8 & 6.29 & @xmath241 & @xmath242 & 0.50 & + sid026 & 03:32:17.25 & 27:46:46.0 & 6.27 & @xmath243 & @xmath190 & 0.22 & + nid037 & 12:36:50.78 & 62:20:17.3 & 6.27 & @xmath244 & @xmath245 & 0.52 & + nid036 & 12:37:29.93 & 62:12:15.4 & 6.27 & @xmath246 & @xmath247 & 0.26 & + sid027 & 03:32:52.52 & 27:51:44.6 & 6.26 & @xmath248 & @xmath231 & 0.57 & + nid038 & 12:36:27.56 & 62:13:28.3 & 6.25 & @xmath249 & @xmath190 & 0.45 & + nid039 & 12:36:26.93 & 62:17:01.2 & 6.24 & @xmath250 & @xmath251 & 0.41 & + sid028 & 03:32:16.55 & 27:41:03.3 & 6.21 & @xmath252 & @xmath253 & 0.60 & + nid040 & 12:36:33.20 & 62:09:23.4 & 6.20 & @xmath254 & @xmath255 & 0.70 & + nid041 & 12:36:49.93 & 62:08:02.9 & 6.18 & @xmath256 & @xmath182 & 0.16 & + sid029 & 03:32:19.19 & 27:55:37.9 & 6.17 & @xmath257 & @xmath258 & 0.74 & + sid030 & 03:32:29.33 & 27:40:14.4 & 6.16 & @xmath259 & @xmath174 & 0.17 & + sid031 & 03:32:56.37 & 27:53:20.9 & 6.15 & @xmath260 & @xmath162 & 0.53 & + nid042 & 12:36:31.98 & 62:08:26.3 & 6.12 & @xmath261 & @xmath200 & 0.24 & + nid043 & 12:37:43.01 & 62:20:02.2 & 6.09 & @xmath262 & @xmath208 & 0.57 & + nid044 & 12:36:48.50 & 62:10:47.3 & 6.08 & @xmath263 & @xmath264 & 0.49 & + nid045 & 12:36:31.16 & 62:13:34.0 & 6.07 & @xmath265 & @xmath215 & 0.70 & + nid046 & 12:35:48.97 & 62:12:25.1 & 6.07 & @xmath266 & @xmath190 & 0.27 & + nid047 & 12:36:26.22 & 62:11:47.8 & 6.05 & @xmath267 & @xmath198 & 0.52 & + sid032 & 03:32:42.08 & 27:41:37.2 & 6.03 & @xmath268 & @xmath258 & 0.54 & + sid033 & 03:32:39.45 & 27:40:26.4 & 6.02 & @xmath269 & @xmath270 & 0.39 & + nid048 & 12:36:28.26 & 62:08:19.9 & 5.99 & @xmath271 & @xmath272 & 0.33 & + sid035 & 03:32:14.90 & 27:41:02.7 & 5.98 & @xmath273 & @xmath210 & 0.20 & + sid034 & 03:32:27.39 & 27:47:28.3 & 5.98 & @xmath274 & @xmath208 & 0.49 & isaac + nid049 & 12:36:19.17 & 62:12:19.6 & 5.98 & @xmath275 & @xmath206 & 0.42 & + nid050 & 12:37:25.65 & 62:17:43.4 & 5.97 & @xmath276 & @xmath264 & 0.50 & + nid052 & 12:37:37.21 & 62:19:35.8 & 5.95 & @xmath277 & @xmath278 & 0.27 & + nid051 & 12:37:40.42 & 62:13:29.5 & 5.95 & @xmath279 & @xmath280 & 0.55 & + nid053 & 12:37:33.19 & 62:16:42.0 & 5.94 & @xmath281 & @xmath282 & 0.53 & + nid054 & 12:37:10.40 & 62:11:22.1 & 5.94 & @xmath283 & @xmath284 & 0.16 & + sid036 & 03:32:14.75 & 27:45:41.6 & 5.92 & @xmath285 & @xmath270 & 0.24 & isaac + nid055 & 12:36:19.49 & 62:15:43.3 & 5.92 & @xmath286 & @xmath287 & 0.27 & + sid038 & 03:32:44.70 & 27:50:02.2 & 5.90 & @xmath288 & @xmath200 & 0.29 & + sid037 & 03:32:22.52 & 27:56:27.5 & 5.90 & @xmath289 & @xmath231 & 0.45 & + nid056 & 12:37:34.22 & 62:15:23.2 & 5.89 & @xmath290 & @xmath291 & 0.56 & + nid057 & 12:35:47.07 & 62:12:18.7 & 5.88 & @xmath292 & @xmath287 & 0.21 & + sid039 & 03:32:21.62 & 27:50:04.4 & 5.87 & @xmath293 & @xmath264 & 0.69 & isaac + nid058 & 12:35:53.25 & 62:10:45.3 & 5.87 & @xmath294 & @xmath295 & 0.62 & + nid059 & 12:36:28.86 & 62:12:22.6 & 5.86 & @xmath296 & @xmath297 & 0.22 & + nid060 & 12:36:10.31 & 62:10:42.6 & 5.85 & @xmath252 & @xmath190 & 0.58 & + nid061 & 12:36:25.69 & 62:15:09.5 & 5.82 & @xmath298 & @xmath231 & 0.18 & + nid062 & 12:37:43.82 & 62:17:26.5 & 5.80 & @xmath299 & @xmath300 & 0.47 & + nid064 & 12:37:17.86 & 62:18:20.8 & 5.79 & @xmath301 & @xmath302 & 0.51 & + nid063 & 12:36:37.53 & 62:12:36.3 & 5.79 & @xmath303 & @xmath304 & 0.43 & + nid065 & 12:36:58.46 & 62:21:22.4 & 5.78 & @xmath305 & @xmath306 & 0.47 & + nid066 & 12:37:16.14 & 62:13:01.0 & 5.78 & @xmath307 & @xmath190 & 0.45 & + nid067 & 12:36:22.71 & 62:08:37.4 & 5.77 & @xmath234 & @xmath270 & 0.39 & + nid068 & 12:36:48.54 & 62:18:50.7 & 5.76 & @xmath308 & @xmath309 & 0.49 & + nid070 & 12:36:42.10 & 62:09:02.4 & 5.76 & @xmath310 & @xmath311 & 0.51 & + nid069 & 12:35:46.99 & 62:12:28.6 & 5.76 & @xmath312 & @xmath313 & 0.45 & + nid071 & 12:37:01.30 & 62:21:28.2 & 5.75 & @xmath314 & @xmath315 & 0.38 & + nid072 & 12:37:35.60 & 62:14:45.2 & 5.75 & @xmath316 & @xmath217 & 0.42 & + nid074 & 12:35:56.18 & 62:11:45.7 & 5.74 & @xmath317 & @xmath318 & 0.48 & + nid073 & 12:36:10.32 & 62:08:10.9 & 5.74 & @xmath319 & @xmath320 & 0.23 & + nid076 & 12:37:33.97 & 62:19:30.5 & 5.73 & @xmath321 & @xmath270 & 0.30 & + nid075 & 12:37:28.86 & 62:13:21.4 & 5.73 & @xmath322 & @xmath323 & 0.23 & + nid077 & 12:37:38.49 & 62:19:50.9 & 5.71 & @xmath324 & @xmath325 & 0.57 & + nid078 & 12:36:28.30 & 62:13:19.7 & 5.70 & @xmath326 & @xmath327 & 0.35 & + sid040 & 03:32:17.95 & 27:48:16.3 & 5.68 & @xmath328 & @xmath210 & 0.28 & isaac + sid041 & 03:32:44.37 & 27:54:19.1 & 5.68 & @xmath329 & @xmath264 & 0.26 & + nid079 & 12:36:36.34 & 62:16:49.4 & 5.68 & @xmath330 & @xmath224 & 0.14 & + nid082 & 12:37:37.94 & 62:19:33.5 & 5.67 & @xmath331 & @xmath287 & 0.60 & + nid081 & 12:36:09.46 & 62:15:12.6 & 5.67 & @xmath332 & @xmath247 & 0.54 & + nid080 & 12:36:21.37 & 62:09:23.4 & 5.67 & @xmath333 & @xmath208 & 0.42 & + sid042 & 03:32:22.08 & 27:42:35.9 & 5.66 & @xmath334 & @xmath278 & 0.34 & + nid083 & 12:37:33.12 & 62:18:04.6 & 5.66 & @xmath335 & @xmath313 & 0.46 & + nid084 & 12:35:48.44 & 62:13:04.6 & 5.66 & @xmath336 & @xmath337 & 0.49 & + sid043 & 03:32:50.79 & 27:47:46.7 & 5.65 & @xmath338 & @xmath208 & 0.20 & + nid085 & 12:37:19.75 & 62:16:03.1 & 5.63 & @xmath339 & @xmath340 & 0.38 & + sid044 & 03:32:17.78 & 27:48:13.5 & 5.62 & @xmath341 & @xmath342 & 0.40 & isaac + nid087 & 12:37:34.18 & 62:20:55.3 & 5.60 & @xmath343 & @xmath233 & 0.56 & + nid086 & 12:36:46.21 & 62:18:41.7 & 5.60 & @xmath344 & @xmath345 & 0.44 & + sid045 & 03:32:16.66 & 27:47:40.0 & 5.59 & @xmath346 & @xmath221 & 0.52 & isaac + nid089 & 12:36:49.61 & 62:10:39.3 & 5.58 & @xmath347 & @xmath348 & 0.48 & + nid088 & 12:35:54.17 & 62:13:50.4 & 5.58 & @xmath349 & @xmath350 & 0.36 & + sid046 & 03:32:04.52 & 27:45:55.3 & 5.55 & @xmath351 & @xmath284 & 0.53 & isaac + nid090 & 12:37:40.76 & 62:19:46.3 & 5.55 & @xmath352 & @xmath313 & 0.68 & + sid047 & 03:32:44.47 & 27:48:21.2 & 5.54 & @xmath353 & @xmath340 & 0.32 & isaac + nid091 & 12:36:16.97 & 62:12:32.5 & 5.54 & @xmath354 & @xmath345 & 0.19 & + sid048 & 03:32:27.89 & 27:43:15.8 & 5.53 & @xmath355 & @xmath356 & 0.30 & + nid092 & 12:37:09.98 & 62:12:26.9 & 5.53 & @xmath357 & @xmath358 & 0.44 & + sid049 & 03:32:20.50 & 27:54:34.6 & 5.52 & @xmath359 & @xmath360 & 0.47 & + nid093 & 12:36:11.20 & 62:11:07.5 & 5.52 & @xmath361 & @xmath302 & 0.55 & + sid050 & 03:32:53.84 & 27:51:49.2 & 5.51 & @xmath362 & @xmath255 & 0.28 & + nid094 & 12:36:57.72 & 62:12:23.9 & 5.50 & @xmath363 & @xmath309 & 0.19 & + sid051 & 03:32:28.34 & 27:43:15.9 & 5.49 & @xmath364 & @xmath287 & 0.17 & + nid095 & 12:36:57.87 & 62:19:30.7 & 5.49 & @xmath365 & @xmath309 & 0.34 & + sid052 & 03:32:05.46 & 27:46:44.2 & 5.48 & @xmath285 & @xmath366 & 0.44 & + nid096 & 12:36:56.99 & 62:14:05.4 & 5.48 & @xmath367 & @xmath340 & 0.23 & + sid055 & 03:32:34.75 & 27:40:35.2 & 5.47 & @xmath261 & @xmath287 & 0.29 & + sid054 & 03:32:16.64 & 27:47:39.6 & 5.47 & @xmath368 & @xmath272 & 0.46 & isaac + sid053 & 03:32:35.53 & 27:53:37.2 & 5.47 & @xmath369 & @xmath313 & 0.49 & + sid056 & 03:32:43.49 & 27:45:29.2 & 5.46 & @xmath370 & @xmath221 & 0.56 & + nid097 & 12:37:29.90 & 62:14:08.9 & 5.46 & @xmath371 & @xmath231 & 0.49 & + nid099 & 12:36:45.40 & 62:18:02.7 & 5.45 & @xmath372 & @xmath224 & 0.42 & + nid098 & 12:37:07.87 & 62:09:16.9 & 5.45 & @xmath373 & @xmath374 & 0.34 & + nid100 & 12:38:00.87 & 62:16:11.6 & 5.44 & @xmath375 & @xmath190 & 0.43 & + nid102 & 12:36:57.20 & 62:10:24.7 & 5.43 & @xmath376 & @xmath233 & 0.43 & + nid101 & 12:36:00.10 & 62:13:23.6 & 5.43 & @xmath377 & @xmath309 & 0.27 & + sid057 & 03:32:37.96 & 27:42:07.6 & 5.42 & @xmath378 & @xmath287 & 0.24 & + sid058 & 03:32:54.86 & 27:48:39.9 & 5.42 & @xmath379 & @xmath380 & 0.36 & + nid103 & 12:37:31.68 & 62:20:18.7 & 5.42 & @xmath381 & @xmath221 & 0.52 & + sid059 & 03:32:40.70 & 27:53:26.0 & 5.41 & @xmath382 & @xmath264 & 0.40 & + nid104 & 12:36:58.84 & 62:10:34.5 & 5.41 & @xmath383 & @xmath302 & 0.35 & + nid105 & 12:36:22.73 & 62:14:22.0 & 5.40 & @xmath384 & @xmath385 & 0.26 & + nid106 & 12:35:45.44 & 62:12:30.6 & 5.39 & @xmath386 & @xmath356 & 0.37 & + sid061 & 03:32:19.90 & 27:52:06.1 & 5.38 & @xmath387 & @xmath388 & 0.26 & + sid060 & 03:32:36.67 & 27:54:21.0 & 5.38 & @xmath389 & @xmath306 & 0.41 & + nid107 & 12:36:12.10 & 62:14:38.1 & 5.38 & @xmath390 & @xmath345 & 0.39 & + nid108 & 12:35:39.26 & 62:12:29.3 & 5.38 & @xmath391 & @xmath392 & 0.36 & + nid109 & 12:37:09.14 & 62:22:50.6 & 5.37 & @xmath393 & @xmath394 & 0.52 & + sid062 & 03:32:35.98 & 27:46:05.1 & 5.36 & @xmath395 & @xmath396 & 0.29 & isaac + nid111 & 12:36:20.91 & 62:16:50.8 & 5.36 & @xmath397 & @xmath340 & 0.39 & + nid110 & 12:35:47.37 & 62:11:33.2 & 5.36 & @xmath398 & @xmath182 & 0.37 & + sid063 & 03:32:22.39 & 27:48:04.4 & 5.35 & @xmath399 & @xmath221 & 0.44 & isaac + nid113 & 12:36:29.26 & 62:16:31.6 & 5.35 & @xmath400 & @xmath309 & 0.38 & + nid112 & 12:36:22.03 & 62:15:13.8 & 5.35 & @xmath401 & @xmath272 & 0.48 & + nid114 & 12:36:47.23 & 62:09:55.5 & 5.35 & @xmath402 & @xmath403 & 0.42 & + nid116 & 12:36:44.51 & 62:10:28.3 & 5.34 & @xmath404 & @xmath405 & 0.49 & + nid115 & 12:35:57.93 & 62:13:51.6 & 5.34 & @xmath406 & @xmath407 & 0.28 & + nid118 & 12:37:16.16 & 62:18:14.9 & 5.33 & @xmath408 & @xmath356 & 0.56 & + nid117 & 12:37:09.62 & 62:18:14.7 & 5.33 & @xmath409 & @xmath272 & 0.60 & + nid119 & 12:36:12.62 & 62:13:48.0 & 5.32 & @xmath410 & @xmath374 & 0.34 & + sid064 & 03:32:24.80 & 27:47:58.8 & 5.31 & @xmath411 & @xmath309 & 0.35 & isaac + sid065 & 03:32:40.82 & 27:47:43.1 & 5.31 & @xmath412 & @xmath306 & 0.51 & isaac + sid066 & 03:32:44.12 & 27:43:18.4 & 5.30 & @xmath361 & @xmath302 & 0.48 & + nid120 & 12:36:28.07 & 62:13:19.8 & 5.30 & @xmath413 & @xmath414 & 0.37 & + nid121 & 12:37:15.05 & 62:18:17.8 & 5.28 & @xmath415 & @xmath221 & 0.54 & + nid123 & 12:37:14.84 & 62:20:15.0 & 5.27 & @xmath416 & @xmath417 & 0.49 & + nid122 & 12:36:04.56 & 62:09:24.7 & 5.27 & @xmath418 & @xmath403 & 0.49 & + sid067 & 03:32:19.46 & 27:51:59.2 & 5.26 & @xmath419 & @xmath420 & 0.43 & + sid068 & 03:32:53.20 & 27:49:44.3 & 5.26 & @xmath421 & @xmath345 & 0.31 & + nid125 & 12:37:50.65 & 62:17:22.4 & 5.26 & @xmath422 & @xmath340 & 0.40 & + nid124 & 12:36:37.49 & 62:16:57.5 & 5.26 & @xmath423 & @xmath300 & 0.38 & + nid126 & 12:36:17.37 & 62:16:17.7 & 5.26 & @xmath424 & @xmath366 & 0.47 & + sid069 & 03:32:13.06 & 27:51:33.6 & 5.25 & @xmath425 & @xmath426 & 0.26 & + sid070 & 03:32:39.19 & 27:54:13.8 & 5.25 & @xmath427 & @xmath264 & 0.43 & + nid128 & 12:36:57.56 & 62:09:08.5 & 5.25 & @xmath428 & @xmath429 & 0.54 & + nid127 & 12:36:12.41 & 62:14:49.5 & 5.25 & @xmath430 & @xmath356 & 0.45 & + sid071 & 03:32:14.73 & 27:47:58.7 & 5.23 & @xmath431 & @xmath432 & 0.21 & isaac + sid072 & 03:32:47.69 & 27:46:45.1 & 5.23 & @xmath433 & @xmath309 & 0.54 & + nid129 & 12:37:36.60 & 62:14:09.7 & 5.22 & @xmath434 & @xmath270 & 0.45 & + sid073 & 03:32:19.05 & 27:42:44.2 & 5.21 & @xmath435 & @xmath309 & 0.51 & + nid130 & 12:37:31.00 & 62:19:49.0 & 5.21 & @xmath410 & @xmath182 & 0.42 & + nid132 & 12:37:17.48 & 62:17:46.3 & 5.21 & @xmath436 & @xmath302 & 0.56 & + nid131 & 12:36:48.78 & 62:19:39.0 & 5.21 & @xmath437 & @xmath227 & 0.45 & + sid074 & 03:32:34.82 & 27:51:33.1 & 5.20 & @xmath438 & @xmath278 & 0.26 & + nid133 & 12:37:42.08 & 62:15:04.4 & 5.20 & @xmath439 & @xmath345 & 0.28 & + nid134 & 12:36:24.96 & 62:10:56.0 & 5.20 & @xmath440 & @xmath380 & 0.23 & + nid136 & 12:36:51.49 & 62:20:10.8 & 5.18 & @xmath441 & @xmath182 & 0.20 & + nid135 & 12:36:37.86 & 62:14:26.8 & 5.18 & @xmath442 & @xmath255 & 0.47 & + sid075 & 03:32:23.88 & 27:52:04.4 & 5.17 & @xmath443 & @xmath264 & 0.43 & + nid137 & 12:36:27.03 & 62:11:25.9 & 5.16 & @xmath444 & @xmath445 & 0.36 & + sid076 & 03:32:19.90 & 27:47:53.2 & 5.15 & @xmath446 & @xmath366 & 0.44 & isaac + sid077 & 03:32:21.60 & 27:44:23.0 & 5.14 & @xmath447 & @xmath258 & 0.41 & isaac + sid078 & 03:32:18.54 & 27:52:59.9 & 5.14 & @xmath448 & @xmath190 & 0.51 & + nid139 & 12:37:39.99 & 62:20:08.4 & 5.14 & @xmath449 & @xmath313 & 0.34 & + nid138 & 12:37:41.69 & 62:19:29.4 & 5.14 & @xmath450 & @xmath182 & 0.44 & + nid140 & 12:37:15.31 & 62:15:35.7 & 5.14 & @xmath451 & @xmath452 & 0.46 & + sid079 & 03:32:29.41 & 27:43:49.4 & 5.13 & @xmath453 & @xmath302 & 0.28 & + nid141 & 12:36:29.43 & 62:16:44.4 & 5.13 & @xmath454 & @xmath313 & 0.29 & + nid144 & 12:36:41.38 & 62:17:01.9 & 5.11 & @xmath455 & @xmath287 & 0.29 & + nid142 & 12:37:01.34 & 62:11:39.7 & 5.11 & @xmath378 & @xmath403 & 0.57 & + nid143 & 12:36:49.09 & 62:09:12.6 & 5.11 & @xmath456 & @xmath358 & 0.46 & + sid080 & 03:32:18.29 & 27:48:55.6 & 5.10 & @xmath457 & @xmath458 & 0.34 & isaac + sid082 & 03:32:16.26 & 27:44:19.7 & 5.09 & @xmath459 & @xmath460 & 0.34 & isaac + sid083 & 03:32:05.13 & 27:46:40.0 & 5.09 & @xmath461 & @xmath258 & 0.30 & + sid081 & 03:32:52.36 & 27:48:53.0 & 5.09 & @xmath462 & @xmath309 & 0.47 & + sid085 & 03:32:49.63 & 27:49:11.1 & 5.08 & @xmath463 & @xmath356 & 0.23 & + sid084 & 03:32:23.37 & 27:51:55.7 & 5.08 & @xmath464 & @xmath309 & 0.27 & + nid145 & 12:36:50.61 & 62:10:52.7 & 5.08 & @xmath214 & @xmath465 & 0.44 & + nid146 & 12:36:44.70 & 62:10:03.1 & 5.08 & @xmath466 & @xmath272 & 0.40 & + sid086 & 03:32:41.17 & 27:49:47.8 & 5.06 & @xmath467 & @xmath468 & 0.34 & + sid088 & 03:32:39.97 & 27:41:50.0 & 5.05 & @xmath469 & @xmath374 & 0.47 & + sid087 & 03:32:42.16 & 27:54:38.8 & 5.05 & @xmath470 & @xmath345 & 0.52 & + nid147 & 12:37:13.52 & 62:16:20.0 & 5.05 & @xmath427 & @xmath190 & 0.34 & + sid089 & 03:32:29.02 & 27:42:08.0 & 5.04 & @xmath471 & @xmath356 & 0.22 & + nid148 & 12:36:34.17 & 62:16:47.1 & 5.04 & @xmath472 & @xmath313 & 0.42 & + sid092 & 03:32:09.91 & 27:43:36.3 & 5.03 & @xmath473 & @xmath278 & 0.50 & isaac + sid090 & 03:32:33.78 & 27:48:07.6 & 5.03 & @xmath474 & @xmath302 & 0.39 & isaac + sid091 & 03:32:49.83 & 27:48:38.3 & 5.03 & @xmath285 & @xmath302 & 0.40 & + nid149 & 12:37:30.73 & 62:19:44.7 & 5.03 & @xmath418 & @xmath468 & 0.41 & + sid095 & 03:32:07.57 & 27:41:30.3 & 5.02 & @xmath475 & @xmath476 & 0.39 & + sid093 & 03:32:21.35 & 27:50:30.6 & 5.02 & @xmath477 & @xmath478 & 0.33 & isaac + sid094 & 03:32:21.75 & 27:50:52.0 & 5.02 & @xmath479 & @xmath255 & 0.50 & isaac + sid096 & 03:32:20.72 & 27:44:35.3 & 5.01 & @xmath480 & @xmath356 & 0.42 & isaac + nid153 & 12:36:55.43 & 62:20:50.5 & 5.01 & @xmath424 & @xmath429 & 0.36 & + nid151 & 12:37:08.17 & 62:09:42.7 & 5.01 & @xmath481 & @xmath482 & 0.41 & + nid154 & 12:36:29.21 & 62:13:35.6 & 5.01 & @xmath483 & @xmath366 & 0.13 & + nid152 & 12:36:27.41 & 62:12:05.3 & 5.01 & @xmath413 & @xmath219 & 0.25 & + nid150 & 12:36:25.29 & 62:11:41.6 & 5.01 & @xmath484 & @xmath224 & 0.39 & + nid155 & 12:36:24.54 & 62:15:35.8 & 5.00 & @xmath485 & @xmath426 & 0.41 & +

this is many fewer than would be expected if galaxies at @xmath4 had the same luminosity function as those at @xmath5 . there are many fainter candidates , but we expect substantial contamination from foreground interlopers and spurious detections . our best estimates favor a @xmath4 galaxy population with fainter luminosities , higher space density , and similar co moving ultraviolet emissivity to that at @xmath5 , but this depends critically on counts at fluxes fainter than those reliably probed by the current data .

we report early results on galaxies at @xmath0 , selected from _ hubble space telescope _ imaging for the great observatories origins deep survey . spectroscopy of one object with the advanced camera for surveys grism and from the keck and vlt observatories a shows a strong continuum break and asymmetric line emission , identified as ly@xmath1 at @xmath2 . we detect only five spatially extended , @xmath0 candidates with signal to noise ratios @xmath3 , two of which have spectroscopic confirmation . this is many fewer than would be expected if galaxies at @xmath4 had the same luminosity function as those at @xmath5 . there are many fainter candidates , but we expect substantial contamination from foreground interlopers and spurious detections . our best estimates favor a @xmath4 galaxy population with fainter luminosities , higher space density , and similar co moving ultraviolet emissivity to that at @xmath5 , but this depends critically on counts at fluxes fainter than those reliably probed by the current data .

cond-mat9808186

i

the physics of a two - dimensional electron system ( 2des ) in a magnetic field is in many respects unique . since the degeneracy of the discrete landau levels increases in proportion to the magnetic field strength , all electrons can be accommodated in the lowest landau level ( lll ) for sufficiently strong fields . a landau level then behaves , in many respects , like a band of zero width and the system can be regarded as the extreme limit of a strongly correlated narrow - band electronic system . in this paper we focus on the spin magnetism of the electron system at landau level filling factor @xmath1 corresponding , when the spin degree of freedom is accounted for , to the case of a half - filled ` landau band ' . at this filling factor , it is known@xcite that , when disorder can be neglected , the ground state of the 2des is ferromagnetic . we are motivated to study this system because it shares many of the difficulties@xcite , which have confounded attempts to build a complete theory of metallic ferromagnetic systems , yet is free of the troubling but incidental consequences of a complex band structure . the finite temperature properties of metallic ferromagnets are more involved than those of insulating ferromagnets because of the importance of both spin and charge degrees of freedom , so much so that much early theory was based on misguided attempts to assign magnetic and conducting properties to separate classes of electrons . despite an immense effort and many advances@xcite , no completely satisfactory theory of metallic ferromagnets progress in understanding metallic ferromagnets has been hampered in part by the quantitative importance of details of the electronic band - structure , which may not be accurately known or may be difficult to render faithfully in going beyond mean - field theories of many - body effects . the present system has no such difficulties . our work is also motivated by recent experimental progress . _ @xcite were able to measure the temperature - dependence of the spin - polarization and nuclear - spin relaxation rates at fixed filling factors around @xmath1 using nuclear magnetic resonance ( nmr ) techniques . later , manfra _ @xcite extracted the spin magnetization from magneto - optical absorption measurements . it is our hope that critical comparison between experiment and theory will yield insights with wider relevance to the finite temperature properties of itinerant electron ferromagnets . it is , however , important to recognize that the 2des at @xmath0 is different from conventional itinerant electron ferromagnets in several important ways . most importantly , two - dimensionality implies that its spontaneous spin magnetic moment will not survive at finite temperatures ( @xmath2 . ) in addition , the strong magnetic field , which through its coupling to the electron s orbital degrees of freedom produces landau levels , also produces a zeeman coupling to electron s spin degree of freedom . for the most studied 2des s , those formed at gaas / algaas heterojunctions , the zeeman coupling is quite small compared to both landau level separations and the characteristic interaction energy scale . as we discuss below , the main effect of zeeman coupling at low temperatures is to cut - off the decrease of the magnetization due to the thermal excitation of very long wavelength spin - waves and mitigate consequences of the system s reduced dimensionality . the recent experimental work has stimulated two different theoretical approaches , which focus on different aspects of the spin - magnetization physics . read and sachdev@xcite have compared experimental data with large @xmath3 limits of a quantum continuum field theory model , which provides an accurate description of the long - wavelength collective behavior of the electronic spins . in this theory , physical properties are dependent only on the two independent ratios between the thermal energy , @xmath4 , the zeeman coupling strength , @xmath5 , and the spin - stiffness energy , @xmath6 . recently this work has been extended by timm _ et al._.@xcite the field - theory description is expected@xcite to be accurate at low temperature when the zeeman coupling strength is weak . this approach achieves reasonable overall agreement between theory and experiment , at least at low temperatures . our work has somewhat different motivation and follows a different line . we are interested in addressing the temperature dependence of the underlying electronic structure , as it changes in concert with the change in the spin - magnetization . hence we focus on the one - particle green s function . a brief account of some parts of this work has been published previously.@xcite from the green s function we can calculate the electronic spectral function and hence the magnetization , the tunneling density of states , and ( if vertex corrections are neglected ) the nuclear - spin relaxation time . the approximation we use is one , which accounts for the interaction of quasiparticles with thermally excited spin - waves . this approximation has deficiencies . at low - temperatures and at low zeeman energies the magnetizations we calculate do not appear to be in quite as good agreement with experiment as magnetizations from large @xmath3 approximations in the field - theory calculations . at medium and high temperatures , we do not account systematically for temperature - dependent screening effects which are likely to be important . some progress in the latter direction has recently been reported by haussmann@xcite , whose bosonized self - consistent random - phase approximation yields satisfying results at high temperatures , but fails at low temperatures . progress on these fronts , which can be checked by comparison with experiment , may suggest routes toward more generically satisfactory theories of itinerant electron ferromagnets . our paper is organized as follows . in section ii we briefly review established results for the ground state and elementary excitations of the 2des at @xmath0 , which will be important for subsequent discussion . the ground state has all spins aligned by an arbitrarily weak zeeman coupling . if we neglect landau level mixing , and we do throughout this paper , this state has no pure charge excitations . its elementary excitations all have a single reversed spin . it turns out that , in the quantum hall regime , the hartree - fock approximation ( hfa ) is exact for the ground state and the time - dependent hartree - fock approximation is exact for its elementary excitations . the situation is therefore similar to that for many typical metallic ferromagnets , where there is substantial evidence that the ground state is well described by the hartree - fock - like kohn - sham equations@xcite of the spin - density - functional formalism and that its elementary excitations are well - described by the time - dependent generalization of density - functional theory . in section iii we discuss the application of the self - consistent hartree - fock approximation ( shf ) at finite temperature . the failure of this approximation at finite temperatures is analogous to the well known failure of the band theory of magnetism to provide even a rough account of the ordering temperature . the approximation , on which the present work is based , is discussed in section iv . we obtain an expression for the electronic self - energy by analytically evaluating a particle - hole ladder summation involving green s functions of opposite spin . we emphasize that in our microscopic theory , it is essential to account for screening even in the low - temperature limit . section v discusses results for the spin magnetization , the spin - lattice relaxation rate , and the temperature dependent 2d-2d tunneling @xmath7 relation , all based on this self - energy approximation . in this section we also compare our results with available experiments , with other approximate theories , and with data from finite size numerical calculations of the magnetization and the magnetic susceptibility . we conclude that it is necessary to account for the finite thickness of the quantum well in comparing with experiment and that the magnetization will be overestimated at high temperatures by models , which do not account for electronic itinerancy . we predict the occurrence of a sharp peak , with strength approximately proportional to temperature , in the tunneling @xmath7 relation at when @xmath8 is close to the zero - temperature spin - splitting . in section vi we discuss some aspects of our calculation which point to difficulties in developing a completely satisfactory microscopic theory . finally , we conclude in section vii with a brief summary .

our work places emphasis on the role played by the itinerancy of the electrons , which carry the spin magnetization and on analogies between this system and conventional itinerant electron ferromagnets . we discuss the application to this system of the self - consistent hartree - fock approximation , which is analogous to the band theory description of metallic ferromagnetism and fails badly at finite temperatures because it does not account for spin - wave excitations . we report results for the temperature dependence of the spin magnetization , the nuclear spin relaxation rate , and 2d-2d tunneling conductances . we compare with experiment , where available , and with predictions based on numerical exact diagonalization and other theoretical approaches .

we report on a study of the temperature and zeeman - coupling - strength dependence of the one - particle green s function of a two - dimensional ( 2d ) electron gas at landau level filling factor @xmath0 where the ground state is a strong ferromagnet . our work places emphasis on the role played by the itinerancy of the electrons , which carry the spin magnetization and on analogies between this system and conventional itinerant electron ferromagnets . we discuss the application to this system of the self - consistent hartree - fock approximation , which is analogous to the band theory description of metallic ferromagnetism and fails badly at finite temperatures because it does not account for spin - wave excitations . we go beyond this level by evaluating the one - particle green s function using a self - energy , which accounts for quasiparticle spin - wave interactions . we report results for the temperature dependence of the spin magnetization , the nuclear spin relaxation rate , and 2d-2d tunneling conductances . our calculations predict a sharp peak in the tunneling conductance at large bias voltages with strength proportional to temperature . we compare with experiment , where available , and with predictions based on numerical exact diagonalization and other theoretical approaches .

cond-mat9808186

i

in this paper we report on a study of the one - particle green s function of a quantum hall system at filling factor @xmath10 . the ground state of the two - dimensional electron system in this case is a strong ferromagnet . many analogies exist between the properties and the theoretical description of this system and conventional metallic ferromagnets . at @xmath10 the ground state and the elementary excitations of quantum hall ferromagnets are given exactly by time - dependent hartree - fock theory . this success is analogous to the success of band theory in describing the ground state and both collective and particle - hole elementary excitations of band ferromagnets . at finite temperatures , however , we show that hartree - fock theory fails qualitatively for quantum hall ferromagnets , just as band theory fails for metallic ferromagnets . our work is based on an improved approximation for the electron self - energy , which describes the scattering of fermionic quasiparticles off the spin - wave collective excitations composed of coherent combinations of spin - flip particle - hole excitations . this perturbative approximation is equivalent to ones , which have been used@xcite for models of itinerant electron ferromagnets at finite temperatures . here we have the advantage that complicated band - structures do not confuse the comparison of theory and experiment . we find that at intermediate temperatures where the density of spin - wave excitations is high , although our approximation gives a huge improvement over hartree - fock theory , it still overestimates the magnetization by nearly a factor of two . we attribute this failure to the neglect of interactions between spin - waves in our approximation . nevertheless , we expect that the qualitative physics predicted by our approximation is correct . on the basis of our calculations we predict that a sharp peak will occur in 2d-2d tunneling current when the bias energy @xmath8 is approximately equal to the spin - splitting and that the strength of this peak will be approximately proportional to temperature at low @xmath108 . this peak is due to fluctuations in the direction of the exchange field , which separates the energy of majority and minority spin quasiparticles . we have recently argued@xcite that in metallic ferromagnets , this mechanism is responsible for the temperature dependence of magnetoresistance in ferromagnetic tunnel junctions . in that case , however , the mechanism can not be directly verified by tunneling experiments because the width of the quasiparticle bands is comparable to their exchange - spin - splitting . verification of the predicted effect in quantum hall ferromagnets , therefore , has important implications for metallic magnetic tunnel junctions .

we report on a study of the temperature and zeeman - coupling - strength dependence of the one - particle green s function of a two - dimensional ( 2d ) electron gas at landau level filling factor @xmath0 where the ground state is a strong ferromagnet . our calculations predict a sharp peak in the tunneling conductance at large bias voltages with strength proportional to temperature .

we report on a study of the temperature and zeeman - coupling - strength dependence of the one - particle green s function of a two - dimensional ( 2d ) electron gas at landau level filling factor @xmath0 where the ground state is a strong ferromagnet . our work places emphasis on the role played by the itinerancy of the electrons , which carry the spin magnetization and on analogies between this system and conventional itinerant electron ferromagnets . we discuss the application to this system of the self - consistent hartree - fock approximation , which is analogous to the band theory description of metallic ferromagnetism and fails badly at finite temperatures because it does not account for spin - wave excitations . we go beyond this level by evaluating the one - particle green s function using a self - energy , which accounts for quasiparticle spin - wave interactions . we report results for the temperature dependence of the spin magnetization , the nuclear spin relaxation rate , and 2d-2d tunneling conductances . our calculations predict a sharp peak in the tunneling conductance at large bias voltages with strength proportional to temperature . we compare with experiment , where available , and with predictions based on numerical exact diagonalization and other theoretical approaches .

0710.5370

i

our goal is to discuss the statistics of conductance and shot - noise power for chaotic cavities using essentially the properties of selberg s integral . the static conductance @xmath7 relates linearly the time averaged current @xmath8 to the external voltage @xmath9 between two electron reservoirs . fluctuations of the current around its mean value are conventionally described by the spectral noise power @xmath10 , with @xmath11 . as temperature goes to zero , the only source of noise that remains non - vanishing is related to the discreteness of the electric charge carriers , the so - called shot - noise . for mesoscopic conductors , an adequate framework for the problematic is based on random - matrix - theory ( rmt ) approach to quantum transport , we refer to @xcite for reviews . we consider a chaotic cavity with two attached leads supporting @xmath12 and @xmath13 channels , respectively , and coupled perfectly to the interior of the cavity . according to the landauer - bttiker formalism , the conductance @xmath7 and the shot - noise power @xmath14 can be expressed in terms of the transmission eigenvalues @xmath15 as follows : @xmath16 and @xmath17 where @xmath18 is the conductance quantum and @xmath19 . the positive numbers @xmath20 are the @xmath21 non - zero eigenvalues of the matrix @xmath22 , with the transmission matrix @xmath23 being the @xmath24 submatrix of the full scattering matrix and consisting of transition amplitudes from @xmath12 left to @xmath13 right channels . for chaotic cavities , universal fluctuations of @xmath15 can be described by rmt @xcite . considering the moments of @xmath0 and @xmath1 , the exact ( rmt ) results valid at arbitrary channel numbers @xmath2 and repulsion parameter @xmath25 were reported in the literature only for the average and variance of the conductance @xcite : @xmath26 @xmath27 and very recently for the average shot - noise power @xcite : @xmath28 to derive these results in a uniform way , it is convenient to use the known expression for the joint probability density of transmission eigenvalues @xmath15 @xcite @xmath29 to perform the corresponding integrations on eqs . ( [ g])([p ] ) . the normalization constant @xmath30 above is given by @xmath31 and assures that ( [ jpd ] ) is a probability density . it is known for discrete positive @xmath32 and continuous @xmath33 and @xmath25 as selberg s integral @xcite . as to the distribution functions , simple closed expressions can be obtained for the conductance distribution at @xmath34 @xcite and for the shot - noise distribution at @xmath35 only @xcite . to the best of our knowledge , no general results valid at arbitrary @xmath2 and @xmath25 have been presented thus far .

we report on an analytical study of the statistics of conductance , @xmath0 , and shot - noise power , @xmath1 , for a chaotic cavity with arbitrary numbers @xmath2 of channels in two leads and symmetry parameter @xmath3 . with the theory of selberg s we give analytical expressions for the conductance and shot - noise distributions and determine their exact asymptotics near the edges up to linear order in distances from the edges . for @xmath4 + pacs numbers : 73.23.-b , 73.50.td , 05.45.mt , 73.63.kv @xmath5fachbereich physik , universitt duisburg - essen , 47048 duisburg , germany + @xmath6department of mathematical sciences , brunel university , + uxbridge , ub8 3ph , uk

we report on an analytical study of the statistics of conductance , @xmath0 , and shot - noise power , @xmath1 , for a chaotic cavity with arbitrary numbers @xmath2 of channels in two leads and symmetry parameter @xmath3 . with the theory of selberg s integral the first four cumulants of @xmath0 and first two cumulants of @xmath1 are calculated explicitly . we give analytical expressions for the conductance and shot - noise distributions and determine their exact asymptotics near the edges up to linear order in distances from the edges . for @xmath4 a power law for the conductance distribution is exact . all results are also consistent with numerical simulations . + pacs numbers : 73.23.-b , 73.50.td , 05.45.mt , 73.63.kv @xmath5fachbereich physik , universitt duisburg - essen , 47048 duisburg , germany + @xmath6department of mathematical sciences , brunel university , + uxbridge , ub8 3ph , uk

1011.5619

i

the factorization formalism of nonrelativistic qcd ( nrqcd ) @xcite provides a rigorous theoretical framework for the description of heavy - quarkonium production and decay . this implies a separation of process - dependent short - distance coefficients , to be calculated perturbatively as expansions in the strong - coupling constant @xmath5 , from supposedly universal long - distance matrix elements ( ldmes ) , to be extracted from experiment . the relative importance of the latter can be estimated by means of velocity scaling rules ; _ i.e. _ , the ldmes are predicted to scale with a definite power of the heavy - quark ( @xmath6 ) velocity @xmath7 in the limit @xmath8 . in this way , the theoretical predictions are organized as double expansions in @xmath5 and @xmath7 . a crucial feature of this formalism is that it takes into account the complete structure of the @xmath9 fock space , which is spanned by the states @xmath10}$ ] with definite spin @xmath11 , orbital angular momentum @xmath12 , total angular momentum @xmath13 , and color multiplicity @xmath14 . in particular , this formalism predicts the existence of color - octet ( co ) processes in nature . this means that @xmath9 pairs are produced at short distances in co states and subsequently evolve into physical , color - singlet ( cs ) quarkonia by the nonperturbative emission of soft gluons . in the limit @xmath15 , the traditional cs model ( csm ) is recovered in the case of @xmath11-wave quarkonia . in the case of @xmath0 production , the csm prediction is based just on the @xmath16}$ ] cs state , while the leading relativistic corrections , of relative order @xmath17 , are built up by the @xmath18}$ ] , @xmath19}$ ] , and @xmath20}$ ] ( @xmath21 ) co states . the greatest success of nrqcd was that it was able to explain the @xmath0 hadroproduction yield at the fermilab tevatron @xcite , while the csm prediction lies orders of magnitudes below the data , even if the latter is evaluated at nlo @xcite . the situation is similar for the transverse momentum ( @xmath4 ) distribution at bnl rhic @xcite . also in the case of @xmath0 photoproduction at desy hera , the csm cross section at nlo significantly falls short of the data @xcite . complete nlo calculations for the co contributions were performed for inclusive @xmath0 production in two - photon collisions @xcite , @xmath22 annihilation @xcite , and direct photoproduction @xcite . as for hadroproduction at nlo , before this talk was given , the co contributions due to intermediate @xmath18}$ ] and @xmath19}$ ] states @xcite were calculated as well as the complete nlo corrections to @xmath23 production , including both @xmath24}$ ] and @xmath19}$ ] contributions @xcite . in order to convincingly establish the co mechanism and the ldme universality , it had been an urgent task to complete the nlo @xmath0 hadroproduction calculation by including the full co contributions . this was actually achieved in the work @xcite presented at this conference . our strategy for testing nrqcd factorization in @xmath0 production at nlo is as follows . we first perform a common fit of the co ldmes to the @xmath4 distributions measured by cdf in hadroproduction at tevatron run ii @xcite and by h1 in photoproduction at hera1 @xcite and hera2 @xcite ( see table [ tab : fit ] and fig . [ fig : fitgraphs ] ) . we then compare the @xmath4 distributions measured by phenix at rhic @xcite and cms at the lhc @xcite as well as the @xmath25 and @xmath26 distributions measured by h1 at hera1 @xcite and hera2 @xcite with our respective nlo predictions based on these co ldmes ( see fig . [ fig : other ] ) . for details on the calculation and the input parameters used , we refer the reader to ref . @xcite .

we fit the color - octet ( co ) long - distance matrix elements @xmath1 } ) \rangle$ ] , @xmath2 } ) \rangle$ ] and @xmath3 } ) \rangle$ ] to the transverse momentum ( @xmath4 ) distributions measured by cdf at fermilab tevatron and by h1 at desy hera and show that they also successfully describe the @xmath4 distributions from phenix at bnl rhic and cms at the cern lhc as well as the photon - proton c.m . address = ii . institut fr theoretische physik , universitt hamburg , luruper chaussee 149 , 22761 hamburg , germany address = ii .

we report on our recent calculation of the inclusive direct photo- and hadroproduction of the @xmath0 meson at next - to - leading order within the factorization formalism of nonrelativistic qcd . we fit the color - octet ( co ) long - distance matrix elements @xmath1 } ) \rangle$ ] , @xmath2 } ) \rangle$ ] and @xmath3 } ) \rangle$ ] to the transverse momentum ( @xmath4 ) distributions measured by cdf at fermilab tevatron and by h1 at desy hera and show that they also successfully describe the @xmath4 distributions from phenix at bnl rhic and cms at the cern lhc as well as the photon - proton c.m . energy and ( with worse agreement ) the inelasticity distributions from h1 . in all experiments , the co processes are shown to be indispensable . address = ii . institut fr theoretische physik , universitt hamburg , luruper chaussee 149 , 22761 hamburg , germany address = ii . institut fr theoretische physik , universitt hamburg , luruper chaussee 149 , 22761 hamburg , germany

0710.2668

i

the galactic center ( gc ) is the only place where we can observe parsec details of various interaction in and around the galactic nucleus . advances in this research frontier rely primarily on observations at radio , infrared and x - ray wavelengths , because the optical band suffers seriously from a considerable extinction with an @xmath9 ( e.g. , becklin , matthews , neugebauer & willner 1978 ) . one of the most important discoveries in the gc region is perhaps the presence of many structured non - thermal radio filaments ( ntfs ) ( e.g. , yusef - zadeh , morris , & chance 1984 ; morris & serabyn 1996 ; larosa , kassim , lazio , & hyman 2000 ) . while these non - thermal radio filaments have been intensively studied , their origins and implications on the underlying physical processes around the gc region remain largely unclear . in the current analysis of x - ray filaments around the gc region , these x - ray emitting particles are usually expected to be fairly close to their acceleration zone and evolve very rapidly in time . thus , the x - ray study of the same region would be essential to probe the origin of these energetic particles . the _ chandra _ galactic center survey ( cgs ) , with its unprecedented high spatial resolution of @xmath10 and moderate spectroscopy capability , has already revealed remarkable x - ray structures ( including thousands of x - ray bright point sources and some filaments , as well as clumps of diffuse emission ) within the central @xmath11 pc of our galaxy ( e.g. , wang , lu , & lang 2002a ) . in this paper , we mainly concentrate on the nature of those thread - like linear structures or filaments as observed in x - ray bands . up to this point within @xmath12 ( @xmath13 pc at 8 kpc ) from where a @xmath14 black hole resides inside a compact region of less than @xmath15au ( e.g. , shen et al . 2005 ) , 5 x - ray filaments have been studied in details ( see also table 1 ) . for example , g359.95 - 0.04 , a comet - like filament at @xmath16 pc north of , is thought to be a ram - pressure confined pulsar wind nebula ( pwn ) ( wang et al . another prominent filament , g359.89 - 0.08 ( sgra - e ) , at @xmath17 pc southeast of , was first noticed by sakano et al . ( 2003 ) and an interpretation of a possible pwn origin was discussed in details by lu , wang & lang ( 2003 ) . an alternative picture of g359.89 - 0.08 as a source of synchrotron emission from relativistic particles accelerated by a shock wave of w28 snr was suggested recently by yusef - zadeh et al . ( 2005 ) ; in that same paper , they also detected a new x - ray filament g359.90 - 0.06 , which coincides spatially with a radio filament at @xmath18 pc southwest of . they explored the mechanism of an inverse compton scattering ( ics ) for the x - ray emission of g359.90 - 0.06 . another 2 filaments were found in more extensive regions . g0.13 - 0.11 in the radio arc region was first reported by wang , lu & lang ( 2003 ) and was suspected to be also a pwn . of particular interest is the x - ray filament g359.54 + 0.18 ; it associates with only one strand of the obviously bifurcated radio threads ( e.g. , yusef - zadeh et al . 2005 ; lu et al . 2003 ) . a common feature shared in the x - ray energy spectra of these filaments is that they all appear to be non - thermal . it should be noted however that any thermal component to these sources would likely be completely absorbed and unobservable , given the high foreground column density . in these earlier investigations , pulsar wind nebulae ( pwns ) and supernova remnants ( snrs ) seem to offer natural explanations for the appearance of such x - ray filaments . indeed , it is believed that a considerable number of supernovae should have happened in the gc region ( e.g. , figer et al . 1999 , 2004 ; wang et al . 2006 ) . one would naturally expect to find some of their end - products such as pulsars and snrs in the gc region . however , no radio pulsars have yet been found within @xmath19 of the gc ( wang et al . this might be caused by difficulties in radio observations ( cordes & lazio 1997 ; johnston et al . 2006 ) . seeking observational clues in x - ray bands might shed new light to the search for radio pulsars embedded in the gc region . another tempting idea is to use these x - ray filaments as potential tracers for the magnetic field and gas dynamics around the gc region , since the magnetic fields should have played a significant role in producing such non - thermal spectra and the thread - like shapes of these filaments and the gas motion is usually coupled with the magnetic fields . ( e.g. , chevalier 1992 ; boldyrev & yusef - zadeh 2006 ) . magnetic fields exist on all scales of the galaxy as well as in other spiral galaxies and generally trace out spiral patterns on large scales ( e.g. , beck & hoernes 1996 ; fan & lou 1996 ; zweibel & heiles 1997 ; wielebinski 2005 ; ferriere 2001 , 2007 ) , and great progress has been made in measuring them and inferring their influence by various means . for example , the observed high - energy cosmic ray anisotropy at a few times @xmath20 ( e.g. , amenomori et al . 2006 ) might be physically related to large - scale structures of galactic magnetic fields and inhomogeneous cosmic ray source distribution . using diffuse synchrotron radio emissions at 74 and 330 mhz frequencies produced by relativistic cosmic - ray electrons and the magnetic field around the galactic center , larosa et al . ( 2005 ) inferred a weak magnetic field of order of @xmath21 g on size scales @xmath22 based on a minimum - energy analysis . this is about 2 orders of magnitude lower than @xmath15 mg usually estimated for the gc region . very recently , cowin & morris ( 2007 ) argued that the assumption of larosa et al . ( 2005 ) that the magnetic field and cosmic rays are in a minimum - energy state across this region is unlikely to be valid . according to their model estimates , the mean magnetic field is at least 100 microgauss on a scale of several hundred parsecs and peaks at approximately 500 microgauss at the center of the diffuse nonthermal source ( dns ) . this is an important issue to be settled for the gc magnetic environment . most of the gc radio ntfs are found to be perpendicular to the galactic plane , implying a local poloidal magnetic fields of about milli - gauss strengths ( e.g. , yusef - zadeh & morris 1987 ) . however , recent observations revealed that the gc magnetic field may be more complex than a simple globally ordered dipolar field ( e.g. , larosa et al . 2004 ; nord et al . it might be possible for x - ray ntfs to also provide clues of the configuration of the local magnetic field as well as the interaction between it and the ambient gas flow . we report morphological and spectral properties of another 10 newly discovered x - ray filaments within a region of @xmath23 surrounding the ( roughly corresponding to a projected sky area of @xmath1 pc by @xmath1 pc at a presumed distance of 8 kpc to the gc ) . their plausible physical origins are discussed in section 4 . all error bars in the x - ray spectrum parameter measurements are at the 90% confidence level , and we express the fitted parameters in the format of @xmath24 , where @xmath25 is the best fit value while @xmath26 and @xmath27 are the lower and upper limits of the 90% confidence interval , respectively . for all the images in the paper , north is up and east is to the left . we shall adopt a distance of 8 kpc from the solar system to the gc throughout this paper . we note that during the review process of this manuscript , muno et al . ( 2007 ) submitted a paper also on x - ray filaments around the galactic center .

we report the detection of 10 new x - ray filaments using the data from the _ chandra _ x - ray satellite for the inner @xmath0 ( @xmath1 parsec ) around the galactic center ( gc ) . fitted with the simple absorbed power - law model , the measured x - ray flux from an individual filament in the @xmath2 kev band is @xmath3 to @xmath4 ergs @xmath5 s@xmath6 and the absorption - corrected x - ray luminosity is @xmath7 ergs s@xmath6 at a presumed distance of 8 kpc to the gc .

we report the detection of 10 new x - ray filaments using the data from the _ chandra _ x - ray satellite for the inner @xmath0 ( @xmath1 parsec ) around the galactic center ( gc ) . all these x - ray filaments are characterized by non - thermal energy spectra , and most of them have point - like features at their heads that point inward . fitted with the simple absorbed power - law model , the measured x - ray flux from an individual filament in the @xmath2 kev band is @xmath3 to @xmath4 ergs @xmath5 s@xmath6 and the absorption - corrected x - ray luminosity is @xmath7 ergs s@xmath6 at a presumed distance of 8 kpc to the gc . we speculate the origin(s ) of these filaments by morphologies and by comparing their x - ray images with the corresponding radio and infrared images . on the basis of combined information available , we suspect that these x - ray filaments might be pulsar wind nebulae ( pwne ) associated with pulsars of age @xmath8 yr . the fact that most of the filament tails point outward may further suggest a high velocity wind blowing away form the gc .

0710.2668

c

while x - ray photon numbers may not be high enough to constrain the exact shapes of the energy spectra , all spectra appear featureless except for filament f3 showing weak iron line features ( see section 3.3 ) and can be well fitted with power - law models . fitting of some of these energy spectra with thermal emission models is acceptable statistically ; nevertheless , this always gives quite high temperatures , i.e. , @xmath83 kev . we therefore incline to the view that x - ray emissions from these filaments are non - thermal in nature . table 2 sums up the inferred parameters for these 15 non - thermal x - ray filaments in the inner @xmath84 around the gc . in addition to the 10 filaments studied in this paper , we also include the other 5 filaments , namely g359.89 - 0.08 , g359.90 - 0.06 , g359.95 - 0.04 , g359.983 - 0.046 , and g0.13 - 0.11 , reported and studied earlier in the literature . most of their hydrogen column density @xmath53 are of the order of @xmath85 , consistent with other @xmath53 estimates around the gc region . most of their photon indices @xmath86 fall within the range of @xmath87 . the chance of these x - ray filaments being background extragalactic sources is very small according to the spectral and morphological properties . for instance , it would be very difficult to explain the linear filamentary morphology using the hypothesis of extragalactic origins . therefore , these x - ray filaments are most likely unique objects around the gc region . as already discussed in section 1 , there were suggestions that these x - ray filaments may be ram - pressure confined pwne ( wang et al . 2003 , 2006 ) , or synchrotron emissions from mhd shocks associated snrs or emissions resulting from inverse compton scattering ( yusef - zadeh et al . 2005 ; figer et al . 1999 ) . the non - thermal x - ray emission mechanisms may be either synchrotron emission or inverse - compton scattering . magnetohydrodynamic ( mhd ) relativistic pulsar winds ( michel 1969 ; goldreich & julian 1970 ; kennel & coroniti 1984a , b ; lou 1996 , 1998 ) and mhd shock interactions of magnetized outflows ( e.g. , yu & lou 2005 ; yu et al . 2006 ; lou & wang 2006 , 2007 ) with the interstellar medium ( ism ) in snrs and pwne could provide high - energy electrons needed in these two radiation mechanisms ( e.g. , sakano et al . 1993 ; lu et al . 2003 ; wang et al . if these x - ray filaments are snrs , their elongations would probably represent mhd shock fronts and therefore , one would not expect to see a tendency of spectral softening along a filament . the two bright filaments f3 and f10 both show evidence for such a softening tendency . the fact that most of these filaments have point - like sources at the heads also againsts the snr origin . on the other hand , as nonthermal x - ray emission is only detected in several snrs within the entire galaxy , it would be highly unlikely that there are so many nonthermal snrs around the gc region . for this reason , we would argue that most of these x - ray filaments are not snrs . observed properties of these x - ray filaments may be more consistent with those of pwne . typical features of a pwn are : non - thermal x - ray spectrum , with photon index of @xmath88 and a x - ray luminosity @xmath89 range from @xmath90 to @xmath91 in @xmath92 kev band ( e.g. , gaensler & slane 2006 ; kaspi , roberts & harding , 2006 ) . the @xmath86 and @xmath89 of these 10 filaments are consistent with the values of a pwn . the existence of point - like x - ray sources as indicated by the image study also tends to favor a pwn scenario . we may estimate the ages of the putative pulsars with the x - ray luminosities of these x - ray filaments . li et al . ( 2007 ) studied statistically the nonthermal x - ray emission from young rotation powered pulsars and pwne . they noted that there exists a correlation between the pulsar age @xmath93 and the @xmath2 kev pwn luminosity @xmath94 , which can be expressed as @xmath95 . the x - ray luminosities of these 10 filaments are in the range of 0.2 - 2.2@xmath96 erg s@xmath6 . using this empirical formula , ages of these putative pulsars are possibly between @xmath97 to @xmath98 yr . however , given the dispersion about the above empirical relationship ( li et al . 2007 ) , the estimate may be uncertain probably by a factor of 10 . since the ages of pulsars with bright pwne are usually younger than a few tens of thousand years , one may doubt if a pulsar at the age of several @xmath99 years can produce a detectable x - ray nebula . however , the pwn of a relatively old pulsar can be enhanced in surface brightness and thus become detectable if the pulsar wind materials are confined to one direction . psr b0355 + 54 is @xmath100 yr old . it converts @xmath15% of its spin - down luminosity to the cometary - like x - ray nebula ( e.g. , tepedelenliolu & gelman 2007 ) . the old pulsar psr b1929 + 10 ( @xmath101 yr ) also converts @xmath102 of its spin - down luminosity @xmath103 erg s@xmath6 into the emission of the cometary nebula ( e.g. , becker et al . 2006 ) . the x - ray filaments identified in the gc region are similar to these two systems and thus probably powered by pulsars . now we discuss whether the number of x - ray filaments , if identified with pwne , would be consistent with the estimated star formation rate in the gc region . according to figer et al . ( 2004 ) , the star formation rate at the gc is about @xmath104 which is some 250 times higher that the mean star formation rate in the galaxy . in the field of view of our fig . 1 , we take a radius of about @xmath105 pc and estimate the star formation rate to be @xmath106 . if the mean mass of a star is 10@xmath107 , the frequency of supernova explosions would be @xmath108 per year , leading to about 40 pulsars in the field of fig . 1 younger than @xmath109 yr as estimated above . this number is roughly consistent with the 15 candidate pwne identified in the field . filament f10 bears certain unique features to be noted here . first , it has the longest linear structure with the entire image slightly bent towards the northeast , more or less like an arc . second , it is the farthest away from and thus has much less contamination from the strong diffuse x - ray emission of sgr a. third , there is an obvious 20 cm radio ntf coincident spatially with x - ray filament f10 . the spectral indices for different regions along filament f10 show evidence of spectral steepening from the head " to tail " ( see table 1 ) . when @xmath53 is fixed at the best fit value @xmath110 , the @xmath86 values for the head " , middle " , and tail " regions are 1.1(1.0 , 1.3 ) , 1.5(1.4 , 1.6 ) , and 1.8(1.7 , 1.9 ) , respectively . this might suggest an energetic particle flow direction from the southeast ( head ) to the northwest ( tail ) . a pulsar moving through the magnetized interstellar medium seems to give a plausible explanation of this scenario . indeed , the morphology of f10 does imply a point source in the head " region . the corresponding point spread function ( psf ) at g0.029 - 0.06 is an ellipse with a size of @xmath111 . for an updated x - ray versus spin - down luminosity correlation of rotation powered pulsars , a modified empirical relation is given by equation ( 3 ) of possenti et al . ( 2002 ) , namely , @xmath112 where @xmath113 is the x - ray luminosity in @xmath2kev energy band ; using this empirical relation , we would have a @xmath114 . since psrs j1747 - 2958 and b1929 + 10 convert about 2.5% and 2.1@xmath115 of their spin - down powers to their cometary x - ray nebulae ( e.g. , gaensler et al . 2004 ; becker et al . 2006 ) , the ratio @xmath89/@xmath116 of f10 ( @xmath117 ) indicates that the above estimate for @xmath116 is reasonable . the arc - like x - ray morphology of f10 and its coincidence with a radio ntf might be a good indicator of its interaction with the interstellar magnetic field environment of the gc region ( lang et al . 1999 ; wang et al . similar to the discussion about g0.13 - 0.11 by wang et al . ( 2002b ) , we may estimate the magnetic field strength @xmath118 in the current context . first , the lifetime @xmath93 of synchrotron x - ray emitting particles is given by @xmath119 , where @xmath120 is the x - ray photon energy in unit of kev ( a value of 4 kev is adopted here ) and @xmath121 is the magnetic field strength in the filament volume in units of mg . the simulations of bucciantini et al . ( 2005 ) show that the average flow speed in the tail is about 0.8 - 0.9 @xmath122 . for a sustained x - ray linear structure , we estimate by requiring @xmath123 . adopting a characteristic angular length @xmath124 of @xmath125 ( @xmath126 ) , we thus infer a magnetic field strength @xmath127 mg , similar to those in the bright radio ntfs ( e.g , yusef - zadeh & morris 1987 ; lang et al . 1999 ) . we try to outline a few plausible scenarios in the present context and discuss relevant aspects qualitatively . magnetized neutron stars move with peculiar speeds in the range of a few tens of kilometers per second ( a mean space velocities of @xmath128 for young pulsars ; hobbs et al . 2005 ; faucher - gigure & kaspi 2006 ) to well over one thousand kilometers per second ( @xmath129 ) and the surrounding ism is generally magnetized . generally speaking , a typical peculiar velocity of a neutron star is supersonic and super - alfvnic in a magnetized ism . neutron stars or pulsars have different ranges of surface magnetic field strengths : @xmath130 g for millisecond pulsars in binaries , @xmath131 g for a wide range of pulsars , and @xmath132 g inferred for several magnetars . several situations may happen . ( 1 ) if a pulsar does not involve an active pulsar wind , its peculiar motion through the surrounding magnetized ism would sustain an mhd bow shock by its magnetosphere as well as a magnetotail . the faster the pulsar moves , the more linear the system would appear . this is basically like a bullet moving through an air supersonically and generating a mach cone or wake . relativistic electrons can be produced at the mhd bow shock and synchrotron emissions can be generated and sustained at the same time . ( 2 ) in a binary system , the fast wind ( say , with a speed higher than 1000 km s@xmath6 ) from a companion star can blow towards a spinning magnetized pulsar in orbital motion . here , the situations of a companion fast wind blowing across a magnetized pulsar and a pulsar moving through the ism with a high speed are more or less equivalent . again , an mhd bow shock and a magnetotail can form in association with the pulsar system . the stronger the companion wind and the faster the pulsar moves , the more linear the pulsar system would appear . relativistic electron and/or positrons can be generated and sustained to power synchrotron emissions in the bow shock draped around the pulsar magnetosphere . for such a system , one might be able to detect the presence of the companion by various independent means . ( 3 ) for a pulsar emitting an active pulsar wind and with misaligned magnetic and spin axes , spiral forward and reverse shock pairs can be generated in the relativistic pulsar wind as a result of inhomogeneous wind and eventually the pulsar wind is stopped by the ism through a mhd termination shock ( e.g. , lou 1993 , 1996 , 1998 ) . ( 4 ) case ( 3 ) can also happen for a pulsar moving with a high peculiar velocity through a magnetized ism . ( 5 ) case ( 3 ) can also happen for a pulsar in binary orbital motion with the companion blows a powerful wind with a speed higher than 1000 km s@xmath6 . in both cases of ( 2 ) and ( 5 ) , the center of mass of the binary system may also move with a high speed through the ism . one can further speculate several possible combinations along this line of reasoning ( e.g. , chevalier 2000 ; toropina et al . 2001 ; romanova , chulsky & lovelace 2005 ) . there are two clumps ( referred to as the east and west clumps hereafter ) of diffuse x - ray emission surrounding filament f10 . although the west clump is also elongated , it is not called a filament because it contains many substructures . to see if these clumps are physically related to f10 , we extract their energy spectra separately ( see the middle and bottom panels of fig . the fitted parameters are listed in table 3 . the much higher absorbing column densities of the two clumps indicate strongly that they are located farther away from us than f10 is , while these two clumps themselves are almost at the same distance ( see table 3 ) . moreover , their x - ray emissions are very likely powered by the same mechanism , as hinted by the characters of their spectra , which can be fitted well with an absorbed power - law model plus a 6.4 kev emission line . the total emission comes mostly from the photon energy @xmath133 kev band , with a strong 6.4 kev neutral fe k line . in contrast , the fe line feature is not present in the spectrum of f10 . a possible explanation for this non - thermal , apparently broadened iron line emission at 6.4 kev is the collisions of low - energy cosmic - ray electrons with irons in molecular clouds ( e.g. , valinia et al . 2000 ) or by the radiative illumination from the gc massive black hole that was suggested to be very bright in the past ( e.g. , koyama et al . 1989 ) . in conclusion , f10 and the surrounding clumps do not seem to interact directly . the oritentation of the x - ray filaments provides an opportunity to probe the physics conditions of the gc region . as discussed in section 4.1 , the cometary shapes of the x - ray filaments imply that the pulsar wind particles are confined to one direction by the ambient materials . mechanism shaping the filamentary structure could be ordered magnetic fields ( e.g. , yusef - zadeh & morris 1987 ; lang , morris , & echevarria 1999 ) and/or high relative velocity between the pulsars and the surrounding gas ( e.g. , wang et al . 1993 ; shore & larosa 1999 ) . the magnetic field could be the product of the gas motion , and the magnetic field could also control the motion of the gas ( e.g. , heyvaerts et al . 1988 ; chevalier 1992 ) . radio ntfs suggests that the magnetic field is poloidal at large - scale ( e.g. , yusef - zadeh & morris 1987 ; lang , morris , & echevarria 1999 ) with some more complex smaller structures around the gc region ( e.g. , nord et al . 2004 ) . by looking at the x - ray images shown by figures 1 , 2 and 3 , there seems to be a tendency that the pwn tails point away from the gc , indicating that the pulsar wind particles are blown outward . this might imply the presence of a galactic wind of hot plasma blowing away from the center , given the high star formation rate ( and so plenty of hot gas ) in this region . pulsars may have typical peculiar velocities of @xmath134 ( e.g. , hobbs et al . 2005 ; faucher - gigure & kaspi 2006 ) and we would expect them to move in random directions . the tendency for the structures of ten pwns to orient away from the center seems to suggest that the galactic wind has a speed comparable to or greater than @xmath135 . in the above scenario , the particle flow direction of the x - ray filament f3 should be from the southwest ( closer to sgr a * ) to the northeast . this suggests that the pulsar , the origin site of the particles , is actually in the `` tail '' region defined in fig 2 . then the evident spectral steepening from the southwest to the northeast ( see section 3 ) can be naturally expained . therefore , the spectral evolution along f3 also supports the existence of a radial high velocity wind in the gc region . while the x - ray filaments may not completely overlap with their radio ntfs , their overall orientations are similar . this is supported by the four x - ray ntfs ( including filament f10 in our analysis ) that have radio counterparts : g359.54 + 0.18 overlays exactly on the northern part of the two radio filaments ( e.g. , yusef et al . 2005 ; lu et al . 2003 ) ; g359.89 - 0.08 and its radio counterpart sgra - e overlaps partly and extends in the same direction , with a centroid offset of @xmath136 ( e.g. , yusef et al . 2005 ; lu et al . 2003 ) ; g359.90 - 0.06 ( sgra - f ) ( e.g. , yusef et al . 2005 ) and g0.029 - 0.06 ( f10 ) ( see our subsection 3.10 ) also show similar spatial property . generally speaking , the x - ray ntfs tend to be shorter than the radio ntfs . this centroid offset and smaller extent of x - ray filaments could be both explained by the much shorter synchrotron cooling lifetime in x - ray than in radio ( e.g. , ginzburg & syrovatskii 1965 ) .

we speculate the origin(s ) of these filaments by morphologies and by comparing their x - ray images with the corresponding radio and infrared images . on the basis of combined information available , we suspect that these x - ray filaments might be pulsar wind nebulae ( pwne ) associated with pulsars of age @xmath8 yr . the fact that most of the filament tails point outward may further suggest a high velocity wind blowing away form the gc .

we report the detection of 10 new x - ray filaments using the data from the _ chandra _ x - ray satellite for the inner @xmath0 ( @xmath1 parsec ) around the galactic center ( gc ) . all these x - ray filaments are characterized by non - thermal energy spectra , and most of them have point - like features at their heads that point inward . fitted with the simple absorbed power - law model , the measured x - ray flux from an individual filament in the @xmath2 kev band is @xmath3 to @xmath4 ergs @xmath5 s@xmath6 and the absorption - corrected x - ray luminosity is @xmath7 ergs s@xmath6 at a presumed distance of 8 kpc to the gc . we speculate the origin(s ) of these filaments by morphologies and by comparing their x - ray images with the corresponding radio and infrared images . on the basis of combined information available , we suspect that these x - ray filaments might be pulsar wind nebulae ( pwne ) associated with pulsars of age @xmath8 yr . the fact that most of the filament tails point outward may further suggest a high velocity wind blowing away form the gc .

1505.05624

i

electric and spin transport in three - dimensional ( 3d ) topological insulators has received a great deal of attention because of the insulators surface dirac fermions with the unique spin texture . the presence of the spin texture has been confirmed by several experiments employing angle - resolved photoemission spectroscopy ( arpes ) , and a variety of novel transport phenomena have been proposed @xcite . in real materials , however , unavoidable bulk conduction often hinders surface conduction . electric transport in 3d topological insulators has been analyzed with the so - called two - carrier model ; i.e. , the parallel conduction of carriers with different mobility @xcite . within the model , the resistivity @xmath4 in a magnetic field @xmath5 is expressed by the equation @xmath6 where @xmath7 and @xmath8 , @xmath9 and @xmath10 , and @xmath11 and @xmath12 are respectively the charges , densities and mobilities of the carriers . despite its usability , the model contains four active parameters , which lead to large errors in most cases . the errors have not been discussed and their statistical reliability remains unclear . this is a fundamental issue requiring a more elaborate analysis procedure . in this article , we report the electric transport of the 3d topological insulator tlbise@xmath0 . the material is known as one of the simplest and most practical materials for the transport studies @xcite . two - carrier transport properties were precisely determined by applying a newly developed analysis procedure . the procedure enables an analysis with two active parameters and with sufficiently small errors . the magnetotransport properties were well explained accounting for high- and low - mobility electrons in the whole temperature range . the carrier densities were @xmath13 /@xmath14 and @xmath15 /@xmath14 , which were @xmath16 times the values expected from the surface . these results indicate that multicarrier conduction originated from the bulk electrons , and the scattering was insensitive to the magnetic field . the temperature dependence of the hall mobility exhibited a metallic behavior over the whole temperature range , and was explained well by the bloch - grneisen formula . this indicates that the scattering of the bulk electrons was dominated by acoustic phonons . it should be noted that analyses proposed in this article allow a precise identification of the two - carrier transport properties and are therefore useful for all other multicarrier systems .

we report the electric transport study of the three - dimensional topological insulator tlbise@xmath0 . we applied a newly developed analysis procedure and precisely determined two - carrier transport properties . magnetotransport properties revealed a multicarrier conduction of high- and low - mobility electrons in the bulk , which was in qualitative agreement with angle - resolved photoemission results [ k. kuroda @xmath1 , phys . rev . lett . the temperature dependence of the hall mobility was explained well with the conventional bloch - grneisen formula and yielded the debye temperature @xmath3 k. the results indicate that the scattering of bulk electrons is dominated by acoustic phonons . keywords : electric transport , two - carrier model , topological insulator , acoustic phonon scattering

we report the electric transport study of the three - dimensional topological insulator tlbise@xmath0 . we applied a newly developed analysis procedure and precisely determined two - carrier transport properties . magnetotransport properties revealed a multicarrier conduction of high- and low - mobility electrons in the bulk , which was in qualitative agreement with angle - resolved photoemission results [ k. kuroda @xmath1 , phys . rev . lett . @xmath2 , 146801 ( 2010 ) ] . the temperature dependence of the hall mobility was explained well with the conventional bloch - grneisen formula and yielded the debye temperature @xmath3 k. the results indicate that the scattering of bulk electrons is dominated by acoustic phonons . keywords : electric transport , two - carrier model , topological insulator , acoustic phonon scattering

quant-ph0505120

i

although the theory of quantum games , originated in 1999 by meyer @xcite and eisert , wilkens , and lewenstein @xcite is only six years old , numerous results obtained during these years @xcite have shown that extending the classical theory of games to the quantum domain opens new interesting possibilities . although eisert and wilkens @xcite noticed that any quantum system which can be manipulated by two parties or more and where the utility of the moves can be reasonably quantified , may be conceived as a quantum game , the extreme fragility of quantum systems may make playing quantum games difficult . in this respect it is interesting whether quantum games with all their ` genuine quantum ' features could be played with the use of suitably designed macroscopic devices . the aim of this letter is to show that this is possible , at least in the case of a ` restricted ' version of a two - players , two - strategies quantum game proposed by marinatto and weber @xcite in which only identity and spin - flip operators are used . moreover , we show that this can be done at once by anyone equipped with a pack of 10 cards bearing numbers @xmath0 . our idea of playing quantum games with macroscopic devices stems from the invention devices proposed by one of us @xcite that perfectly simulate the behavior and measurements performed on two maximally entangled spin-1/2 particles . for example , they allow to violate the bell inequality with @xmath1 , exactly ` in the same way ' as it is violated in the epr experiments . a more recent and further elaborated model consists of two coupled spin-1/2 for which measurements are defined using ` randomly breaking measurement elastics ' @xcite . in this paper we use the older model for a single spin-1/2 for which measurements are defined using ` randomly selected measurement charges ' @xcite . in order to play marinatto and weber s ` restricted ' version of two - players , two - strategies quantum game we shall not use the ` full power ' of this machine , but we give its complete description such that the principle of what we try to do is clear .

we show that it is perfectly possible to play ` restricted ' two - players , two - strategies quantum games proposed originally by marinatto and weber @xcite having as the only equipment a pack of 10 cards . the ` quantum board ' of such a model of these quantum games is an extreme simplification of ` macroscopic quantum machines ' proposed by aerts et al . in numerous papers @xcite that allow to simulate by macroscopic means various experiments performed on two entangled quantum objects .

we show that it is perfectly possible to play ` restricted ' two - players , two - strategies quantum games proposed originally by marinatto and weber @xcite having as the only equipment a pack of 10 cards . the ` quantum board ' of such a model of these quantum games is an extreme simplification of ` macroscopic quantum machines ' proposed by aerts et al . in numerous papers @xcite that allow to simulate by macroscopic means various experiments performed on two entangled quantum objects .

1303.1311

i

the issue of unifying both classical and quantum cosmology is an open challenge of modern physics partially due to the lack of a self - consistent quantum gravity theory . all the attempts aimed to achieve a quantum gravity theoretical scheme lead to many inconsistencies and it is furthermore not clear how to measure quantum signatures in the context of observational cosmology @xcite . recently , the evidence of cosmic positive acceleration , reported by several observational surveys @xcite , has open further interrogatives , due to the ignorance of the physical nature of the fluid responsible for the cosmic speed up . the standard framework leads to the existence of a vacuum energy cosmological constant @xmath2 , characterized by a negative equation of state @xcite . even though the cosmological constant allows the cosmic acceleration at late times , the observational bounds on @xmath2 are incompatible with theoretical predictions of a gravitational vacuum state . in addition , the @xmath2 and matter order of magnitude are surprisingly close to each other , although @xmath2 is supposed to be constant along the universe evolution . these two thorny shortcomings , namely the _ fine tuning _ and the _ coincidence _ problems , disturb the otherwise appealing picture of a cosmological constant and dramatically plague the so called @xmath2cdm model @xcite . a way out for the above problems is to extend the standard @xmath2 paradigm by postulating the existence of a new ingredient referred to as _ dark energy_. it provides a fluid with an evolving negative equation of state . a solution is that quantum effects at fundamental level could be responsible for the existence of dark energy @xcite . the possibility to relate dark energy with quantum effects has been recently considered by dealing with the existence of a hidden mechanism behind the nature of the cosmological constant as a result of entanglement between cosmological eras @xcite . in doing so , the existence of entangled states was postulated , showing that a running cosmological constant is compatible with early times of the universe evolution , while , at late times , the cosmological constant is recovered as a limiting case . such a result can be achieved also in the framework of alternative theories of gravity @xcite . a key role for this approach is played by quantum information that reached a growing interest during last decades spanning from condensed matter to cosmology @xcite . moreover , relevant entanglement phenomena have been framed into robust theoretical schemes and verified through several experiments @xcite . thus , selection criteria were sought in order to characterize the entanglement amount of quantum states . all of those criteria are essentially based on equivalent forms of non - locality of pure quantum states . in addition , since entanglement can be considered as a fundamental quantity , its physical meaning has been compared with quantities like energy and entropy . the purpose of this work is twofold : we first wonder whether it is possible to consider cosmic dark energy as the result of an entanglement mechanism between two or more than two cosmological eras during the universe evolution . secondly , we show that the corresponding equation of states , derived by the entanglement process , is compatible with the late time universe evolution as a running barotropic fluid equation of state . this approach is justified assuming the entanglement mechanism applicable to the degrees of freedom of macroscopic systems , in this case , the whole observed universe . the latter process is known in the literature as decoherence @xcite . in particular , the challenge of finding decoherence effects in the cosmological scenario is related to the interaction between qubits with their environment @xcite . in particular , quantum coherence and entanglement of the quantum states can lead to _ more decoherence _ if the number of qubits increases @xcite . in this paper , under the hypothesis that the decoherence effects could be related to dark energy , we show that it is possible to associate the von neumann entropy , as a naive selection criterium , to the fluid accelerating the universe . choosing the simplest case in which the dark energy represents the measurement of decoherence in the observable universe , we demonstrate that it is possible to infer a cosmological model which predicts the dark energy effects without introducing a vacuum energy cosmological constant term at late times . the paper is structured as follows : in sec . ii we discuss the thermodynamics of a homogeneous and isotropic universe in the context of entanglement . in sec . iii we describe the cosmological models derived by considering the entanglement decoherence as a source for dark energy . in sec . iv , we draw the conclusions and discuss the perspectives of the present approach .

we show that quantum decoherence , in the context of observational cosmology , can be connected to the cosmic dark energy . the decoherence signature could be characterized by the existence of quantum entanglement between cosmological eras . as a consequence , the von neumann entropy related to the entanglement process , can be compared to the thermodynamical entropy in a homogeneous and isotropic universe .

we show that quantum decoherence , in the context of observational cosmology , can be connected to the cosmic dark energy . the decoherence signature could be characterized by the existence of quantum entanglement between cosmological eras . as a consequence , the von neumann entropy related to the entanglement process , can be compared to the thermodynamical entropy in a homogeneous and isotropic universe . the corresponding cosmological models are compatible with the current observational bounds being able to reproduce viable equations of state without introducing _ a priori _ any cosmological constant . in doing so , we investigate two cases , corresponding to two suitable cosmic volumes , @xmath0 and @xmath1 , and find two models which fairly well approximate the current cosmic speed up . the existence of dark energy can be therefore reinterpreted as a quantum signature of entanglement , showing that the cosmological constant represents a limiting case of a more complicated model derived from the quantum decoherence .

1303.1311

c

quantum decoherence can play an interesting role in the context of observational cosmology . in particular , by assuming a decoherence signature at any epoch , it is possible to trace back the evolution of dark energy by comparing the variation of the von neumann entropy with the thermodynamic entropy . this approach can be pursued for any perfect fluid consistent with a given equation of state . here we have considered a frw universe . in particular , we discussed cosmological models where dark energy behavior can be achieved without postulating _ a priori _ a cosmological constant . the existence of dark energy at our epoch can be seen as a quantum signature resulting from a decoherence process , while along the universe evolution , it is possible to feature different scaling volumes comparable with observational data . in particular , we investigated two cases : a volume @xmath0 and a volume @xmath1 . the corresponding cosmological models fairly well approximate the cosmological behavior at our time , showing that the existence of a cosmological constant appears as the limiting case of a more complicate dynamics . entanglement between different cosmological eras leads to conclude that the existence of dark energy can be seen as the observable effect of such process . in future researches , we are planning to develop in detail such an approach comparing observable cosmographic parameters with thermodynamical quantities related to information theory . f. kaiser , t. coudreau , p. milman , d. b. ostrowsky , s. tanzilli , science , 338 , 637 - 640 , ( 2012 ) ; h. wunderlich , g. vallone , p. mataloni , m. b. plenio , new j. phys . , 13 , 033033 , ( 2011 ) ; b. jungnitsch , s. niekamp , m. kleinmann , o. ghne , h. lu , w. b. gao , y. a. chen , z. b. chen , j. w. pan , phys . rev . , 104 , 210401 , ( 2010 ) . a. cabello , a. rossi , g. vallone , f. de martini , p. mataloni , phys . 102 , 040401 , ( 2009 ) .

the corresponding cosmological models are compatible with the current observational bounds being able to reproduce viable equations of state without introducing _ a priori _ any cosmological constant . in doing so , we investigate two cases , corresponding to two suitable cosmic volumes , @xmath0 and @xmath1 , and find two models which fairly well approximate the current cosmic speed up . the existence of dark energy can be therefore reinterpreted as a quantum signature of entanglement , showing that the cosmological constant represents a limiting case of a more complicated model derived from the quantum decoherence .

we show that quantum decoherence , in the context of observational cosmology , can be connected to the cosmic dark energy . the decoherence signature could be characterized by the existence of quantum entanglement between cosmological eras . as a consequence , the von neumann entropy related to the entanglement process , can be compared to the thermodynamical entropy in a homogeneous and isotropic universe . the corresponding cosmological models are compatible with the current observational bounds being able to reproduce viable equations of state without introducing _ a priori _ any cosmological constant . in doing so , we investigate two cases , corresponding to two suitable cosmic volumes , @xmath0 and @xmath1 , and find two models which fairly well approximate the current cosmic speed up . the existence of dark energy can be therefore reinterpreted as a quantum signature of entanglement , showing that the cosmological constant represents a limiting case of a more complicated model derived from the quantum decoherence .

1107.4095

i

the massive black holes ( mbhs ) that reside at the centers of some nearby galaxies are believed to grow together with their hosts through mergers : mbhs grow partly as a result of gas accretion , and partly by coalescence with other mbhs that are brought into the nucleus during the merger process @xcite . the detailed assembly history of mbhs is poorly understood ; major uncertainties include the `` seed '' mass distribution of mbhs at high redshift , the typical gas accretion efficiency , and the frequency with which mbhs are ejected due to gravitational - wave recoil @xcite . but a robust prediction of the hierarchical models is that galaxies hosting mbhs in the nearby universe were formed from less massive systems , at least some of which already contained mbhs . binary mbhs created during galaxy mergers leave imprints on the stellar distribution : for instance , they create low - density cores , by exchanging energy with passing stars @xcite . such cores are observed to be ubiquitous in stellar spheroids brighter than @xmath1 @xcite and their sizes of order the influence radius of the ( presumably single ) mbh are consistent with the predictions of merger models @xcite . here we define the influence radius as @xmath2 where @xmath3 is the rms velocity of stars in any direction at @xmath4 . cores of radius @xmath5 become difficult to resolve in galaxies beyond the local group if the mbh mass is below @xmath6 . even in the nearest nucleus , that of the milky way , the presence of a parsec - scale core around sgr a@xmath7 was only clearly established in the last few years @xcite . in the absence of mbhs , mergers tend to preserve the form of the stellar distribution near the centers of galaxies @xcite . binary mbhs , however , are efficient at erasing the structure that was present on scales @xmath8 @xcite , and this fact precludes drawing definite conclusions about the nuclear properties of the galaxies that preceded the hosts of observed mbhs . on the other hand , it is well established that low - luminosity galaxies have higher central densities than high - luminosity galaxies @xcite . this is true both in terms of the mean density within the half - mass radius , and also in terms of the density on the smallest resolvable scales : low - luminosity spheroids often contain dense , nuclear stars clusters ( nscs ) , with sizes of order @xmath9 and masses @xmath10 the mass of the galaxy @xcite . nsc masses are therefore comparable to , or somewhat greater than , mbh masses @xcite , although nscs have been shown to coexist with mbhs in only a handful of galaxies @xcite . the nsc in the milky way is believed to be a representative example : its half - light radius is @xmath11 , or @xmath12 , and its mass is a few times @xmath13 , or several times @xmath14 @xcite . in the nsc of the milky way , the two - body relaxation time is comparable with the age of the universe , and this is consistent with the persistence of a core ( as opposed to a @xcite cusp ) in the late - type stars @xcite . but in fainter systems , central relaxation times are shorter . for instance , in the virgo cluster , galaxies with nscs have nuclear half - light relaxation times that scale with host - galaxy luminosity as @xcite t_r,1.210 ^ 10 ( ) . by comparison , the mean time between `` major mergers '' ( mergers with mass ratios @xmath15 or less ) of dark - matter haloes in the hierarchical models varies from @xmath16 gyr at redshift @xmath17 to @xmath18 yr at @xmath19 , with a weak dependence on halo mass @xcite . this comparison suggests that the progenitors of many spheroids in the current universe may have been galaxies containing nuclei that were able to attain a collisionally - relaxed state before the merger that formed them took place . in the absence of a mbh , collisional relaxation implies mass segregation and core collapse . if a mbh is present , mass segregation still occurs , but core collapse is inhibited by the fixed potential due to the mbh . a collisional steady state , which is reached by a time @xmath20 at radii @xmath21 , is characterized by a bahcall - wolf , @xmath22 cusp in the dominant component at @xmath23 . if there is a mass spectrum , less - massive objects follow a shallower profile , @xmath24 , while more - massive objects follow a steeper profile , @xmath25 @xcite . as a first approximation , the mass spectrum of an evolved stellar population can be represented in terms of just two components : objects of roughly one solar mass or less ( main - sequence stars , white dwarfs , neutron stars ) ; and remnant black holes ( bhs ) with masses @xmath26 . standard initial mass functions predict that roughly @xmath27 of the total mass will be in stellar bhs @xcite ; so - called `` top - heavy '' mass functions ( e.g. * ? ? ? * ) predict a larger fraction . in a collisionally relaxed nucleus , the density of stellar bhs will rise more steeply toward the center than the density of the stars . mergers between galaxies with such nuclei would be expected to modify these steady - state distributions substantially , and also to affect ( increase ) the time scale over which a collisionally relaxed cusp could be regenerated following the merger @xcite . these arguments motivated us to carry out merger simulations between galaxies containing multi - component , mass - segregated nuclei around mbhs . as in previous papers from this series @xcite , our merger simulations are purely stellar - dynamical . in some galaxies , torques from gas would assist in the evolution of binary mbhs @xcite . gas also implies star formation , and there is evidence for complex star formation histories in many nscs @xcite . but @xmath0-body simulations that allow for non - spherical geometries @xcite have shown that purely dissipationless energy exchange with ambient stars can bring binary mbhs to milliparsec separations on time scales much shorter than galaxy lifetimes . unless the late evolution of the binary mbh is greatly accelerated by torques from the gas , the influence of the binary on the distribution of the _ stellar _ populations should be accurately reproduced by our dissipationless models . with respect to star formation , population synthesis of nsc spectra suggest that most of the mass typically resides in stars with ages of order 5 - 10 gyr @xcite , i.e. an old population . simulating the merger of galaxy - sized systems , while enforcing the spatial and temporal resolution required to faithfully reproduce the dynamics of stars on scales @xmath28 around the central mbh , is computationally demanding . our simulations used @xmath29 particles per galaxy , and the models were advanced using a parallel , direct - summation @xmath0-body code @xcite . the integrations were accelerated using special - purpose hardware . the galaxy models contained four mass groups , representing an evolved stellar population . initial conditions of the merging galaxies were constructed in a two - stage process : models of mass - segregated nuclei around a mbh were first constructed , then these collisionally - relaxed models were imbedded into larger , spheroid - sized models . mergers were then carried out , assuming a galaxy mass ratio of @xmath30 . a major motivation for our new simulations was the need to understand the distribution of stellar remnants , particularly stellar - mass bhs , near the centers of galaxies . knowledge of the bh density well inside @xmath31 is crucial for predicting the rates of many astrophysically interesting processes ; in particular , the rate of capture of stellar - mass bhs by mbhs , or emris @xcite . published emri rate calculations almost always assume a state of mass segregation , implying a high density of stellar remnants near the mbh @xcite . however , in a nucleus formed via a merger , any pre - existing mass segregation would have been disrupted by the binary mbh when it created a core ; whether or not the massive remnants would have had time to re - segregate following the merger is difficult to assess without full @xmath0-body simulations . our simulations followed the evolution of the binary mbhs for a time almost long enough that gravitational wave emission would dominate the binaries evolution . we then combined the two mbh particles into one , simulating gravitational wave coalescence , and continued the @xmath0-body integrations for a time corresponding to several relaxation times at the ( new ) influence radius . in this post - merger evolutionary phase , we also considered the consequences of varying the relative numbers of the different mass components . in this way , we were able , for the first time , to observe how rapidly the stellar bhs would re - segregate following a merger . we found substantially longer time scales for this evolution than in earlier simulations that started from physically less motivated initial conditions . the paper is organized as follows . in section [ sec : models ] we describe the procedure to generate equilibrium segregated models starting from single - component models . scaling to physical units is discussed in section [ sec : scaling ] . evolution of the binary mbh and its effects on the underlying stellar distribution are described in section [ sec : premerger ] . in section [ sec : postmerger ] we describe the evolution of the light and heavy objects after the massive binary has undergone coalescence . section [ sec : shape ] describes the shapes and kinematics of the merger remnants . section [ sec : disc ] discusses the implications of our results for the formation and observability of bahcall - wolf cusps , and for the distribution of stellar remnants .

we simulate mergers between galaxies containing collisionally - relaxed nuclei around massive black holes ( mbhs ) . our galaxies contain four mass groups , representative of old stellar populations ; a primary goal is to understand the distribution of stellar - mass black holes ( bhs ) after the merger . mergers are followed using direct - summation @xmath0-body simulations , assuming a mass ratio of 1:3 and two different orbits . evolution of the binary mbh is followed until its separation has shrunk by a factor of 20 below the hard - binary separation . during the galaxy merger , large cores are carved out in the stellar distribution , with radii several times the influence radius of the massive binary . much of the pre - existing mass segregation is erased during this phase . we follow the evolution of the merged galaxies for approximately three , central relaxation times after coalescence of the massive binary ; both standard , and top - heavy , mass functions are considered . we discuss the implications of our results for the emri problem and for the existence of bahcall - wolf cusps .

we simulate mergers between galaxies containing collisionally - relaxed nuclei around massive black holes ( mbhs ) . our galaxies contain four mass groups , representative of old stellar populations ; a primary goal is to understand the distribution of stellar - mass black holes ( bhs ) after the merger . mergers are followed using direct - summation @xmath0-body simulations , assuming a mass ratio of 1:3 and two different orbits . evolution of the binary mbh is followed until its separation has shrunk by a factor of 20 below the hard - binary separation . during the galaxy merger , large cores are carved out in the stellar distribution , with radii several times the influence radius of the massive binary . much of the pre - existing mass segregation is erased during this phase . we follow the evolution of the merged galaxies for approximately three , central relaxation times after coalescence of the massive binary ; both standard , and top - heavy , mass functions are considered . the cores that were formed in the stellar distribution persist , and the distribution of the stellar - mass black holes evolves against this essentially fixed background . even after one central relaxation time , these models look very different from the relaxed , multi - mass models that are often assumed to describe the distribution of stars and stellar remnants near a massive bh . while the stellar bhs do form a cusp on roughly a relaxation time - scale , the bh density can be much smaller than in those models . we discuss the implications of our results for the emri problem and for the existence of bahcall - wolf cusps .

1107.4095

i

in galaxies containing a single stellar population , a @xmath212 @xcite cusp is expected to appear at radii @xmath213 around the mbh . while the growth time of the cusp is dependent on the initial conditions , simulations starting from a shallow cusp inside @xmath84 show that the stellar density will have reached an approximate steady state after roughly one relaxation time at @xmath84 . we presented an example of such evolution in figure[fig : c2 ] . in nuclei with two mass groups , e.g. solar - mass stars ( ms ) and @xmath54 black holes ( bhs ) , evolution toward a steady state near the mbh depends on the relative numbers and masses in the two groups , as well as on the initial conditions . the results of our @xmath0-body and fokker - planck integrations of two - component models were presented in section [ sec : fp ] . figure[fig : fp_g0.5_slopes ] showed that addition of the bhs reduces slightly the rate of formation of a bahcall - wolf cusp in the ms ( light ) component , and also affects the final value of the density - profile slope , which varies from @xmath214 when @xmath215 is small , to @xmath216 as @xmath215 is increased @xcite . in addition , if the initial ms distribution is very flat near the mbh , scattering by the heavier bhs can dominate the evolution of the ms component at early times for @xmath157 , converting @xmath217 to @xmath218 at these small radii , even before the bahcall - wolf cusp has fully formed at larger radii . the full galaxy merger simulations presented here allowed us , for the first time , to evaluate the evolution of multi - component nuclei starting from initial conditions that were motivated by a well - defined physical model . our pre - merger galaxies contained mass - segregated nuclei with four mass components , representing an evolved stellar population . these initial distributions were modified both by the galaxy merger , and by the formation of a mbh binary , which created a large core in each of the components ( figures[fig : lagr1 ] , [ fig : density ] ) . the core radius of the heaviest ( bh ) component was somewhat smaller than the cores in the three lighter components , a relic of the earlier mass segregation , and of the incomplete cusp destruction process during the binary mbh phase ( figure[fig : density ] ) . evolution during the merger phase set the `` initial conditions '' of the nucleus at the time when the two mbhs were combined into one . unlike the rather ad hoc initial conditions used in many earlier studies of nuclear evolution ( e.g. * ? ? ? * ; * ? ? ? * ) , our post - merger models have cores that should be reasonable representations of the cores in real galaxies that formed via dissipationless mergers , with mass densities that decline toward the center and anisotropic kinematics that reflect the action of the massive binary on the stellar orbits ( figure[fig : vel ] ) . by continuing the evolution of these multi - component models for a time greater than @xmath219 after coalescence of the two mbhs , we found that the cores characterizing the distribution of the dominant , ms component persisted ; in fact the ms density at radii @xmath220 decreased gradually with time ( figure [ fig : massp ] ) a predictable consequence of the initial extent of the cores , several times @xmath84 , implying @xmath221 , and of continued `` heating '' by the heavier bhs . nevertheless , a bahcall - wolf cusp gradually reformed in the lighter components at radii @xmath222 ; growth times were found to be @xmath223 , somewhat greater than in earlier models with more idealized initial conditions ( e.g. * ? ? ? our pre - merger galaxies ( models a1 , b1 ) contained larger numbers of remnants than would be expected based on a standard imf ; this was done in order to better resolve the distributions of those components near the mbh . we tested the dependence of the _ post_-merger evolution on the assumed mass function by carrying out a second set of integrations in which we decreased the relative numbers of remnants ( ns , wd , bh ) by factors of a few , to values more consistent with standard imfs ( models a2 , b2 ) . evolution of the dominant , ms component in the latter models differed only modestly from its evolution in the models with larger remnant fractions ; the main difference was a lower rate of core expansion reflecting a lower rate of heating by the bhs ( figure[fig : massp ] ) . the rate of growth of the bahcall - wolf cusp in the ms component was essentially unchanged ( figure[fig : profiles ] ) . our results on the regeneration of bahcall - wolf cusps following dissipationless mergers are consistent with those obtained in simulations of single - component galaxies @xcite . we can summarize these results by stating that regrowth of a cusp in the dominant stellar component requires a time comparable with , or somewhat longer than , the relaxation time of that component measured at the mbh influence radius . the new simulations presented here suggest that time scales for cusp regrowth are only weakly dependent on the number of heavy remnants ( bhs ) , at least if the fraction of mass in the heavier population does not exceed a few percent of the total . the milky way nucleus is near enough that a bahcall - wolf cusp could be resolved if present , and the dominant stellar population is believed to be old . since @xmath224 in the milky way , the expected , outer radius of the bahcall - wolf cusp is @xmath225 . as is well known , number counts of the dominant , old stellar population show no evidence of a rise in density at this radius ; instead the number counts are flat , or even falling , from @xmath226 into at least @xmath227 projected radius @xcite . assuming solar - mass stars , the relaxation time at the influence radius of sgr a@xmath7 is 20 - 30 gyr @xcite , while the mean stellar age in the nuclear star cluster is estimated to be @xmath228 gyr @xcite . the time available for formation of a cusp is therefore @xmath229 . our simulations ( e.g. figure[fig : profiles ] ) suggest that a bahcall - wolf cusp in the dominant component is unlikely to have formed in so short a time , and this is consistent with the lack of a bahcall - wolf cusp at the galactic center . the core in the milky way has a radius of @xmath182 , somewhat smaller than @xmath31 or @xmath84 , while the cores formed in our merger models are somewhat larger than @xmath84 ( table 4 ) . it has been argued that the milky way core is small enough that gravitational encounters would cause it to shrink appreciably in 10 gyr , as the stellar distribution evolves toward a bahcall - wolf cusp @xcite . the cores in our @xmath0-body models are so large that they do not evolve appreciably after the binary mbh has been replaced by a single mbh ; the bahcall - wolf cusp forms at radii smaller than @xmath230 , leaving the core structure essentially unchanged . without necessarily advocating a merger model for the origin of the milky way core ( it is unclear whether our galaxy even contains a bulge ; @xcite ) , we note that the sizes of cores formed by binary mbhs scale with the binary mass ratio . presumably , we could have produced cores more similar in size to the milky way s if we had adjusted this ratio . it has been suggested @xcite that heating by bhs could be responsible for the lack of a bahcall - wolf cusp at the galactic center . we do not find support for this hypothesis , either in our four - component @xmath0-body models , nor in our two - component fokker - planck models . the latter showed that even a quite large bh population still allowed a bahcall - wolf cusp to form in the ms stars on a time scale of @xmath231 ; the main effect of the bhs is to decrease the asymptotic slope of the cusp from @xmath232 to @xmath216 . a dense cluster of stellar - mass bhs has been invoked as a potential solution to a number of problems of collisional dynamics at the galactic center . examples include randomization of the orbits of young stars via gravitational scattering ( e.g. * ? ? ? * ) , production of hyper - velocity stars through encounters with bhs ( e.g. * ? ? ? * ) , and warping of young stellar disks @xcite . these treatments typically assume a collisionally - relaxed state for the galactic center . in the relaxed models , the mass in bhs inside @xmath233 is @xmath234 , i.e. @xmath235 and @xmath236 @xcite , assuming `` standard '' imfs . a high density of stellar bhs at the centers of galaxies like the milky way is also commonly assumed in discussions of the emri ( extreme - mass - ratio inspiral ) problem @xcite . models like these are called into question by the lack of a bahcall - wolf cusp in the late - type stars at the center of the milky way @xcite . if the galactic center is not collisionally relaxed , as these observations seem to suggest , then computing the distribution of the heavy remnants becomes a more difficult , time - dependent problem @xcite , and knowledge of the initial conditions is essential . dissipationless mergers imply `` initial conditions '' characterized by a core in the dominant stellar component . the cores formed in our ( major ) merger simulations are large enough that they do not evolve appreciably ( i.e. shrink ) even after @xmath237 relaxation times at the mbh influence radius . as a result , evolution of the bh distribution takes place against a stellar background with a very different density profile than in the steady - state models . in a core around a mbh , dynamical friction is much weaker than one would estimate by plugging the local density into standard formulae for orbital decay , due to the absence of stars moving more slowly than the local circular velocity @xcite . scaling our @xmath0-body models to the milky way , we predicted numbers of bhs inside @xmath31 that were substantially smaller than in the collisionally relaxed models ; in the inner @xmath238 the radii most relevant to the emri problem @xcite the number of bhs was , at most , 10 - 100 times smaller than predicted by these models , even after 10 gyr ( figure[fig : bhs ] ) . it is unclear how relevant merger models are to the center of the milky way . if the core observed at the galactic center had some other origin , the distribution of stellar bhs might have little connection with the distribution of the giant stars . however , if cores of size @xmath239 are common features of galactic nuclei , and if at some early time both the bhs and the stars had a common core radius , our models imply that the distribution of bhs should be considered very uncertain , even in galaxies for which nuclear half - mass relaxation times are as short as the age of the universe . dm acknowledges support from the national science foundation under grants no . ast 08 - 07910 , 08 - 21141 and by the national aeronautics and space administration under grant no . nnx-07ah15 g . we thank tal alexander and eugene vasiliev for useful discussions .

the cores that were formed in the stellar distribution persist , and the distribution of the stellar - mass black holes evolves against this essentially fixed background . even after one central relaxation time , these models look very different from the relaxed , multi - mass models that are often assumed to describe the distribution of stars and stellar remnants near a massive bh . while the stellar bhs do form a cusp on roughly a relaxation time - scale , the bh density can be much smaller than in those models .

we simulate mergers between galaxies containing collisionally - relaxed nuclei around massive black holes ( mbhs ) . our galaxies contain four mass groups , representative of old stellar populations ; a primary goal is to understand the distribution of stellar - mass black holes ( bhs ) after the merger . mergers are followed using direct - summation @xmath0-body simulations , assuming a mass ratio of 1:3 and two different orbits . evolution of the binary mbh is followed until its separation has shrunk by a factor of 20 below the hard - binary separation . during the galaxy merger , large cores are carved out in the stellar distribution , with radii several times the influence radius of the massive binary . much of the pre - existing mass segregation is erased during this phase . we follow the evolution of the merged galaxies for approximately three , central relaxation times after coalescence of the massive binary ; both standard , and top - heavy , mass functions are considered . the cores that were formed in the stellar distribution persist , and the distribution of the stellar - mass black holes evolves against this essentially fixed background . even after one central relaxation time , these models look very different from the relaxed , multi - mass models that are often assumed to describe the distribution of stars and stellar remnants near a massive bh . while the stellar bhs do form a cusp on roughly a relaxation time - scale , the bh density can be much smaller than in those models . we discuss the implications of our results for the emri problem and for the existence of bahcall - wolf cusps .

1701.06029

i

results about hamilton cycles in finite graphs can be extended to locally finite graphs in the following way . for a locally finite graph @xmath3 we consider its freudenthal compactification @xmath4 @xcite , which is a topological space obtained by taking @xmath3 , seen as a @xmath5-complex , and adding the _ ends _ of @xmath3 , which are the equivalence classes of the rays of @xmath3 under the relation of being inseparable by finitely many vertices , as additional points . extending the notion of cycles , we define _ circles _ @xcite in @xmath4 as homeomorphic images of the unit circle @xmath6 in @xmath4 , and we call them _ hamilton circles _ , if they additionally contain all vertices of @xmath3 . as a consequence of being a closed subspace of @xmath4 , hamilton circles also contain all ends of @xmath3 . following this notion we call @xmath3 _ hamiltonian _ ( or say that @xmath3 has a hamilton circle ) if there is a hamilton circle in @xmath4 . one of the first and probably one of the deepest results about hamilton circles was georgakopoulos s extension of fleischner s theorem to locally finite graphs . [ fin_fleisch]@xcite the square of any finite @xmath2-connected graph is hamiltonian . [ inf - fleisch ] ( * ? ? ? 3 ) the square of any locally finite @xmath2-connected graph is hamiltonian . following this breakthrough , more hamiltonicity theorems have been extended to locally finite graphs in this way @xcite . the purpose of this paper is to prove more extensions of hamiltonicity results about finite graphs to locally finite ones and to construct a graph which shows that another result does not extend . the first result we consider is a corollary of the following theorem of harary and schwenk . a _ caterpillar _ is a tree such that after deleting its leaves only a path is left . let @xmath7 denote the graph obtained by taking the star with three leaves , @xmath8 , and subdividing each edge once . [ fin_cater ] ( * ? ? ? 1 ) let @xmath9 be a finite tree with at least three vertices . then the following statements are equivalent : 1 . @xmath10 is hamiltonian . 2 . @xmath9 does not contain @xmath11 as a subgraph . 3 . @xmath9 is a caterpillar . theorem [ fin_cater ] has the following obvious corollary . [ fin_cater_impl ] @xcite the square of every finite graph on at least three vertices that contains a spanning caterpillar is hamiltonian . while the proof of corollary [ fin_cater_impl ] is immediate , the proof of the following extension of it , which is the first result of this paper , needs more work . we call the closure @xmath12 in @xmath4 of a subgraph @xmath13 of @xmath3 a _ standard subspace _ of @xmath4 . extending the notion of trees , we define _ topological trees _ as topologically connected standard subspaces not containing any circles . as an analogue of a path , we define an _ arc _ as a homeomorphic image of the unit interval @xmath14 \subseteq \mathbb{r}$ ] in @xmath4 . for our extension we adapt the notion of a caterpillar to the space @xmath4 and work with _ topological caterpillars _ , which are topological trees @xmath15 such that @xmath16 , where @xmath17 denotes the set of vertices of degree @xmath5 in @xmath9 , is an arc . [ top_catp_hc ] the square of every locally finite connected graph on at least three vertices that contains a spanning topological caterpillar is hamiltonian . the other two results of this paper concern the uniqueness of hamilton circles . the first is about finite _ outerplanar graphs_. these are finite graphs that can be embedded in the plane such that all vertices lie on the boundary of a common face . clearly , finite outerplanar graphs have a hamilton cycle if and only if they are @xmath2-connected . it is also easy to see that finite @xmath2-connected outerplanar graphs have a unique hamilton cycle consisting of precisely its @xmath2-_contractible edges _ , i.e. , those edges each of whose contraction leaves the graph @xmath2-connected ( except for the case where the graph is a @xmath18 ) , as pointed out by syso . we summarise this with the following proposition . [ summary ] 1 . a finite outerplanar graph is hamiltonian if and only if it is @xmath2-connected . 6 ) finite @xmath2-connected outerplanar graphs have a unique hamilton cycle , which consists precisely of the @xmath2-contractible edges if the graph is not isomorphic to a @xmath18 . finite outerplanar graphs can also be characterised by forbidden minors , which was done by chartrand and harary . [ outerplanar_count_char ] ( * ? ? ? 1 ) a finite graph is outerplanar if and only if it contains neither a @xmath0 nor a @xmath19 as a minor.actually these statements can be strengthened a little bit by replacing the part about not containing a @xmath0 as a minor by not containing it as a subgraph . this follows from lemma [ k^4_minor_subgr ] . ] in the light of theorem [ outerplanar_count_char ] we first prove the following extension of statement ( i ) of proposition [ summary ] to locally finite graphs . [ hc_k_4-k_2,3 ] let @xmath3 be a locally finite connected graph . then the following statements are equivalent : 1 . @xmath3 is @xmath2-connected and contains neither @xmath0 nor @xmath1 as a minor.@xmath20 2 . @xmath4 has a hamilton circle @xmath21 and there exists an embedding of @xmath4 into a closed disk such that @xmath21 corresponds to the boundary of the disk . furthermore , if the statements ( i ) and ( ii ) hold , then @xmath4 has a unique hamilton circle . from this we then obtain the following corollary , which extends statement ( ii ) of proposition [ summary ] . given a circle @xmath21 in @xmath4 , we call the edge set @xmath22 whose closure @xmath23 in @xmath4 equals @xmath21 the _ circuit _ of @xmath21 . [ cor_contr ] the circuit of the hamilton circle of a locally finite @xmath2-connected graph not containing @xmath0 or @xmath1 as a minor consists precisely of the @xmath2-contractible edges if the graph is not isomorphic to a @xmath18 .. we should note here that parts of theorem [ hc_k_4-k_2,3 ] and corollary [ cor_contr ] are already known . chan ( * ? ? ? 20 with thm . 27 ) proved that the @xmath2-contractible edges of a locally finite @xmath2-connected graph not containing @xmath0 or @xmath1 as a minor form the circuit of a hamilton circle . he deduces this from other general results about @xmath2-contractible edges in locally finite @xmath2-connected graphs . in our proof , however , we directly construct the hamilton circle and show its uniqueness without working with @xmath2-contractible edges . afterwards , we deduce corollary [ cor_contr ] . our third result is related to the following conjecture sheehan made for finite graphs . [ sheehan]@xcite for every @xmath24 there is no finite @xmath25-regular graph with a unique hamilton cycle . this conjecture is still open , but some partial results have been proved @xcite . for @xmath26 the statement of the conjecture was verified by smith first . this was noted in an article of tutte @xcite where the statement for @xmath26 was published for the first time . for infinite graphs conjecture [ sheehan ] is not true in this formulation . it fails already with @xmath26 . to see this consider the graph depicted in figure [ double_ladder ] , called the _ double ladder_. it is easy to check that the double ladder has a unique hamilton circle , but all vertices have degree @xmath27 . mohar has modified the statement of the conjecture and raised the following question . to state them we need to define two terms . for a graph @xmath3 we call the equivalence classes of rays under the relation of being inseparable by finitely many vertices the _ ends _ of @xmath3 . we define the _ vertex- _ or _ edge - degree _ of an end @xmath28 to be the supremum of the number of vertex- or edge - disjoint rays in @xmath28 , respectively . in particular , ends of a graph @xmath3 can have infinite degree , even if @xmath3 is locally finite . [ q2 ] @xcite does an infinite graph exist that has a unique hamilton circle and degree @xmath24 at every vertex as well as vertex - degree @xmath25 at every end ? our result shows in contrast to conjecture [ sheehan ] and its known cases that there are infinite graphs having the same degree at every vertex and end while being hamiltonian in a unique way . [ q_mohar_yes ] there exists an infinite connected graph @xmath3 with a unique hamilton circle that has degree @xmath27 at every vertex and vertex- as well as edge - degree @xmath27 at every end . so with theorem [ q_mohar_yes ] we answer question [ q2 ] positively and therefore disprove the modified version of conjecture [ sheehan ] for infinite graphs in the way mohar suggested by considering degrees of both vertices and ends . the rest of this paper is structured as follows . in section 2 we establish the notation and terminology we need for the rest of the paper . we also list some lemmas that will serve as auxiliary tools for the proofs of the main theorems . section 3 is dedicated to theorem [ top_catp_hc ] where at the beginning of that section we discuss how one can sensibly extend corollary [ fin_cater_impl ] and which problems arise when we try to extend theorem [ fin_cater ] in a similar way . in section 4 we present a proof of theorem [ hc_k_4-k_2,3 ] and describe afterwards how a different proof of this theorem works that is copying the ideas of a proof of statement ( i ) of proposition [ summary ] . the last section , section 5 , contains the construction of a graph witnessing theorem [ q_mohar_yes ] .

we state a sufficient condition for the square of a locally finite graph to contain a hamilton circle , extending a result of harary and schwenk about finite graphs . we also give an alternative proof of an extension to locally finite graphs of the result of chartrand and harary that a finite graph not containing @xmath0 or @xmath1 as a minor is hamiltonian if and only if it is @xmath2-connected . we show furthermore that , if a hamilton circle exists in such a graph , then it is unique and spanned by the @xmath2-contractible edges .

we state a sufficient condition for the square of a locally finite graph to contain a hamilton circle , extending a result of harary and schwenk about finite graphs . we also give an alternative proof of an extension to locally finite graphs of the result of chartrand and harary that a finite graph not containing @xmath0 or @xmath1 as a minor is hamiltonian if and only if it is @xmath2-connected . we show furthermore that , if a hamilton circle exists in such a graph , then it is unique and spanned by the @xmath2-contractible edges . the third result of this paper is a construction of a graph which answers positively the question of mohar whether regular infinite graphs with a unique hamilton circle exist .

0801.2803

i

the standard model ( sm ) of particle physics successfully describes high - energy experimental data . however , the sm involves the theoretical difficulty referred to as `` hierarchy problem '' : due to large quantum corrections , the energy scale of the higgs potential tends to become similar to the cutoff scale of the sm , in spite of the fact that the energy scale should be similar to the known electroweak one . this suggests that physics beyond the sm appears near the electroweak scale . among several candidates of the physics beyond the sm , unification of gauge and higgs fields , so - called gauge - higgs unification , is known as a promising idea with the help of compactified extra dimensions @xcite . in the gauge - higgs unification scenario , some of the extra - dimensional components of gauge fields are identified to higgs fields at a low - energy regime . phenomenologically viable electroweak higgs sectors are known to appear with orbifold compactification of the extra dimensions . an advantageous point of the idea is finiteness of the higgs potential even at some loop levels ; hence , the potential is not sensitive to unknown ultra - violet ( uv ) physics , and the scenario gives a reasonable resolution to the hierarchy problem . the gauge - higgs unification scenario has been extensively studied @xcite . in addition to the case with flat compactified extra dimensions , the case with a warped extra dimension has been also investigated @xcite . the higgs sector is predictive thanks to the higher dimensional gauge invariance . namely , the scenario predicts light higgs scalars , which can be a key ingredient for the experimental test of the scenario at lhc and ilc . one of the most important subjects is to minutely examine the higgs mass spectrum in the gauge - higgs unification . several models have been proposed and the mass spectrum has been studied . an interesting observation is that multi - higgs scalars appear in some models . the models lead to non - vanishing tree - level higgs potential which has flat directions ; it has revealed that finite radiative corrections to the flat direction lead to the correct electroweak symmetry breaking dynamically @xcite . the higgs scalars associated with the flat directions are massless at the tree - level and become massive through the radiative corrections ; their masses have been studied by the one - loop effective potential @xcite , or even at the two - loop level in a simple model @xcite . the other modes among the multi - higgs scalars , which are associated with the non - flat directions , are massive at the tree - level . loop corrections to their masses , however , have not been focused on even though they are crucial to verify the higgs mass spectrum in the models . it is also important to examine the spectrum in detail for the experimental test of the scenario . in addition , the loop corrections to the non - flat directions are considered to be significant for determining the vacuum structure of the multi - higgs potential . if the corrections are taken into account , then vacua deviated from the flat directions of the tree - level potential may appear . clearly , such a vacuum structure can not be studied when one focus only on the loop corrections to the flat directions . thus , to reveal the correct vacuum structure of multi - higgs models , the loop corrections to the non - flat directions should be incorporated . in this paper , we study the multi - higgs mass spectrum based on one - loop effective potential in a simple 5d model . we take bulk loop corrections into account for all the modes of the higgs scalars : we study not only the loop corrections for the higgs scalars along the flat direction of the tree - level potential , but also the ones for the higgs scalars along the non - flat direction . as mentioned above , in the past studies , the latter has not been focused on though it is important . in our analyses , it is found that the one - loop corrections involve an uv divergence , which is proportional to the tree - level potential and is renormalized . the one - loop corrected multi - higgs mass spectrum is derived through the effective potential after eliminating the divergence . it turns out that both the tree - massless and massive higgs scalars have mass corrections of similar size from finite parts of the one - loop effects . consequently , the loop effects modify multi - higgs mass spectrum and are significant in view of verifications of the scenario in high - energy experiments . the outline of the paper is as follows . in section [ sec : mass ] , an overview of multi - higgs mass spectrum in the gauge - higgs unification scenario is presented . in section [ sec:5dsusy ] , we examine the one - loop corrected multi - higgs mass spectrum in a simple 5d model . a perturbative calculation of the effective potential is developed to estimate the loop corrections . summary and future perspective are given in section [ sec : sum ] . in appendix [ sec : op ] , field dependent operators that are needed to evaluate the effective potential in the model are presented , and appendix [ sec : loop ] provides the evaluation of loop momentum integrals with the summation of kaluza - klein ( k - k ) modes .

multi - higgs spectrum appears in the model at low energy . the corrections modify multi - higgs mass spectrum , and hence , the loop effects are significant in view of future verifications of the gauge - higgs unification scenario in high - energy experiments . kyushu - het-110 + tu-808 + ou - het 595/2008 * multi - higgs mass spectrum in gauge - higgs unification * kentaro kojima@xmath1 , kazunori takenaga@xmath2 , and toshifumi yamashita@xmath3 _ @xmath4 department of physics , kyushu university , fukuoka 812 - 8581 , japan + @xmath5 department of physics , tohoku university , sendai 980 - 8578 , japan + @xmath6 department of physics , osaka university , toyonaka , osaka 560 - 0043 , japan _

we study an @xmath0 supersymmetric gauge model in a framework of gauge - higgs unification . multi - higgs spectrum appears in the model at low energy . we develop a useful perturbative approximation scheme for evaluating effective potential to study the multi - higgs mass spectrum . we find that both tree - massless and massive higgs scalars obtain mass corrections of similar size from finite parts of the loop effects . the corrections modify multi - higgs mass spectrum , and hence , the loop effects are significant in view of future verifications of the gauge - higgs unification scenario in high - energy experiments . kyushu - het-110 + tu-808 + ou - het 595/2008 * multi - higgs mass spectrum in gauge - higgs unification * kentaro kojima@xmath1 , kazunori takenaga@xmath2 , and toshifumi yamashita@xmath3 _ @xmath4 department of physics , kyushu university , fukuoka 812 - 8581 , japan + @xmath5 department of physics , tohoku university , sendai 980 - 8578 , japan + @xmath6 department of physics , osaka university , toyonaka , osaka 560 - 0043 , japan _ ( january , 2008 )

1501.06030

i

a fractional quantum hall ( qh ) system of filling fraction @xmath3 has edge channels that support fractional charges obeying fractional braiding statistics @xcite . at @xmath4 , the edge states are decomposed into a @xmath5 charge mode and a counterpropagating neutral mode @xcite . they originate from renormalization of two counterpropagating charge modes @xcite , @xmath6 and @xmath7 , and stabilize at low temperature under strong disorder . neutral modes have attracted much attention , as they are charge neutral and carry energy . they have been recently detected through shot noise measurements @xcite , and their properties such as energy and decay length have been extensively studied @xcite . electron interaction is a dominant source of dephasing at low temperature @xcite . it leads to electron fractionalization @xcite in quantum wires ; an electron , injected into a wire , splits into constituents ( spin - charge separation , charge fractionalization ) , showing reduction of interference visibility or dephasing @xcite . interestingly , when the wire is finite , the constituents recombine after bouncing at wire ends , resulting in coherence revival @xcite . fractionalization was detected @xcite in a non - chiral wire , and studied in the integer qh edge @xcite . coherent transport , as well as dephasing , can be tackled through the study of low energy dynamics at the edge . this is particularly important in the context of the fractional qh regime . the present study implies that the presence of neutral modes could be a dominant source of dephasing . note that neutral modes have been observed in almost all fractional qh systems @xcite . at the same time there is no uncontested observation of anyonic interference oscillations in the pure aharonov - bohm regime of a fractional qh interferometer . the present study of the @xmath4 qh regime emphasizes two dephasing mechanisms by fractionalization of an electron into charge and neutral components , _ plasmonic dephasing _ and _ topological dephasing_. concerning the plasmonic dephasing mechanism , the overlap between the plasmonic parts of the charge and neutral components decreases with time , as the two components propagate with different velocities in the opposite directions . the resulting dephasing is similar to the plasmonic dephasing that takes place in a quantum wire or in integer qh edges . on the other hand , the topological dephasing is a new mechanism unnoticed so far . it occurs because the zero - mode parts of the components , satisfying fractional statistics , may braid with thermally excited anyons . thermal average of the resulting braiding phase leads to dephasing that occurs only in the interfering processes characterized by particular values of topological winding numbers . , coupled to lead edge states of @xmath4 ( black solid lines ) through quantum point contacts ( qpcs ) at @xmath8 . electron ( rather than fractional quasiparticle ) tunneling occurs through the qpcs ( dotted lines ) . following the tunneling , each electron ( and the hole left behind in the lead edge ) fractionalizes into a charge component propagating at velocity @xmath9 ( solid blue arrow ) and a neutral component counterpropagating at velocity @xmath10 ( dashed red ) . the magnetic flux in the dot area is @xmath11 . ] our analysis addresses the ab oscillation of differential conductance @xmath12 through a quantum dot ( qd ) in the @xmath4 qh regime . we focus on linear response of electron sequential tunneling into the qd . @xmath12 is decomposed into the harmonics of the ab flux @xmath11 in the qd , @xmath13 where @xmath14 is a flux quantum ; see fig . [ setup1 ] . semiclassically , @xmath15 represents the relative winding number of a fractionalized charge component , around the circumference @xmath16 of the qd , between two interfering paths : an electron , after tunneling into the qd , fractionalizes into charge and neutral components ; see fig . [ setup1 ] . the charge ( neutral ) component has propagation velocity @xmath17 , spatial width @xmath18 at temperature @xmath19 , level spacing @xmath20 , and scaling dimension @xmath21 ( @xmath22 ) in the electron tunneling operator at low temperatures . @xmath23 is determined by the overlaps of the components of the same kind between two interfering paths of relative charge winding @xmath15 . we find two mechanisms suppressing @xmath24 , the plasmonic dephasing and the topological dephasing ; the former ( latter ) involves plasmon ( zero - mode ) parts of the components . in the plasmonic dephasing , @xmath23 is contributed from the two interfering paths whose charge components overlap maximally between the paths . but , their neutral components overlap only partially between the interfering paths , reducing @xmath23 ; similar dephasing occurs in other fractionalizations @xcite . the topological dephasing additionally occurs , but depending on @xmath15 , in contrast to the other known mechanisms . when @xmath25 @xcite , the first harmonics @xmath26 is suppressed at @xmath27 ( namely , @xmath28 ) . it is because the charge component gains thermally fluctuating fractional braiding phase of @xmath29 ( leading to @xmath30 ) , while it winds once ( @xmath31 ) around @xmath32 electronic or anyonic thermal excitations on the qd edge or in the bulk . by contrast , the second harmonics @xmath33 is not affected by the topological dephasing ( as braiding phase @xmath34 and @xmath35 are trivial ) and dominates @xmath12 , resulting in @xmath2 ab oscillations . these above findings occur in both the regimes of strong disorder and weak disorder in the edge of the qd . note that the topological dephasing does not occur in the coulomb dominated regime @xcite where coulomb interactions between the bulk and edge of the qd is strong , as discussed later .

tunneling , dephasing occurs due to electron fractionalization into counterpropagating charge and neutral edge modes on the dot . in particular , when the charge mode moves much faster than the neutral mode , and at temperatures higher than the level spacing of the dot , electron fractionalization combined with the fractional statistics of the charge mode leads to the dephasing selectively suppressing @xmath1 aharonov - bohm oscillations but not @xmath2 oscillations , resulting in oscillation - period halving .

we study dephasing in electron transport through a large quantum dot ( a fabry - perot interferometer ) in the fractional quantum hall regime with filling factor @xmath0 . in the regime of sequential tunneling , dephasing occurs due to electron fractionalization into counterpropagating charge and neutral edge modes on the dot . in particular , when the charge mode moves much faster than the neutral mode , and at temperatures higher than the level spacing of the dot , electron fractionalization combined with the fractional statistics of the charge mode leads to the dephasing selectively suppressing @xmath1 aharonov - bohm oscillations but not @xmath2 oscillations , resulting in oscillation - period halving .

1102.5212

i

with the advancement of modern technology , data sets which contain repeated measurements obtained on a dense grid are becoming ubiquitous . such data can be viewed as a sample of curves or functions and are referred to as functional data . we consider here the extension of the linear regression model to the case of functional data . in this extension , both predictors and responses are random functions rather than random vectors . it is well known ( ramsay and dalzell ( @xcite ) ; ramsay and silverman ( @xcite ) ) that the traditional linear regression model for multivariate data , defined as @xmath0 may be extended to the functional setting by postulating the model , for @xmath1 , @xmath2 writing all vectors as row vectors in the classical model ( [ basic ] ) , @xmath3 and @xmath4 are random vectors in @xmath5 , @xmath6 is a random vector in @xmath7 , and @xmath8 and @xmath9 are , respectively , @xmath10 and @xmath11 matrices containing the regression parameters . the vector @xmath4 has the usual interpretation of an error vector , with @xmath12=0 $ ] and @xmath13=\sigma^{2}i$ ] , @xmath14 denoting the identity matrix . in the functional model ( [ linear ] ) , random vectors @xmath15 and @xmath16 in ( [ basic ] ) are replaced by random functions defined on the intervals @xmath17 and @xmath18 . the extension of the classical linear model ( [ basic ] ) to the functional linear model ( [ linear ] ) is obtained by replacing the matrix operation on the right - hand side of ( [ basic ] ) with an integral operator in ( [ linear ] ) . in the original approach of ramsay and dalzell ( @xcite ) , a penalized least - squares approach using l - splines was adopted and applied to a study in temperature - precipitation patterns , based on data from canadian weather stations . the functional regression model ( [ linear ] ) for the case of scalar responses has attracted much recent interest ( cardot and sarda ( @xcite ) ; mller and stadtmller ( @xcite ) ; hall and horowitz ( @xcite ) ) , while the case of functional responses has been much less thoroughly investigated ( ramsay and dalzell ( @xcite ) ; yao , mller and wang ( @xcite ) ) . discussions on various approaches and estimation procedures can be found in the insightful monograph of ramsay and silverman ( @xcite ) . in this paper , we propose an alternative approach to predict @xmath19 from @xmath20 , by adopting a novel canonical representation of the regression parameter function @xmath21 . several distinctive features of functional linear models emerge in the development of this canonical expansion approach . it is well known that in the classical multivariate linear model , the regression slope parameter matrix is uniquely determined by @xmath22 , as long as the covariance matrix @xmath23 is invertible . in contrast , the corresponding parameter function @xmath24 , appearing in ( [ linear ] ) , is typically not identifiable . this identifiability issue is discussed in section [ sec2 ] . it relates to the compactness of the covariance operator of the process @xmath25 which makes it non - invertible . in section [ sec2 ] , we demonstrate how restriction to a subspace allows this problem to be circumvented . under suitable restrictions , the components of model ( [ linear ] ) are then well defined . utilizing the canonical decomposition in theorem [ th3.3 ] below leads to an alternative approach to estimating the parameter function @xmath26 . the canonical decomposition links @xmath27 and @xmath25 through their functional canonical correlation structure . the corresponding canonical components form a bridge between canonical analysis and linear regression modeling . canonical components provide a decomposition of the structure of the dependency between @xmath27 and @xmath25 and lead to a natural expansion of the regression parameter function @xmath24 , thus aiding in its interpretation . the canonical regression decomposition also suggests a new family of estimation procedures for functional regression analysis . we refer to this methodology as _ functional canonical regression analysis_. classical canonical correlation analysis ( cca ) was introduced by hotelling ( @xcite ) and was connected to function spaces by hannan ( @xcite ) . substantial extensions and connections to reproducing kernel hilbert spaces were recently developed in eubank and hsing ( @xcite ) ; for other recent developments see cupidon _ et al . _ ( @xcite ) . canonical correlation is known not to work particularly well for very high - dimensional multivariate data , as it involves an inverse problem . leurgans , moyeed and silverman ( @xcite ) tackled the difficult problem of extending cca to the case of infinite - dimensional functional data and discussed the precarious regularization issues which are faced ; he , mller and wang ( @xcite ) further explored various aspects and proposed practically feasible regularization procedures for functional cca . while cca for functional data is worthwhile , but difficult to implement and interpret , the canonical approach to functional regression is here found to compare favorably with the well established principal - component - based regression approach in an example of an application ( section [ sec5 ] ) . this demonstrates a potentially important new role for canonical decompositions in functional regression analysis . the functional linear model ( [ linear ] ) includes the varying coefficient linear model studied in hoover _ et al . _ ( @xcite ) and fan and zhang ( @xcite ) as a special case , where @xmath28 ; here , @xmath29 is a delta function centered at @xmath30 and @xmath31 is the varying coefficient function . other forms of functional regression models with vector - valued predictors and functional responses were considered by faraway ( @xcite ) , shi , weiss and taylor ( @xcite ) , rice and wu ( @xcite ) , chiou , mller and wang ( @xcite ) and ritz and streibig ( @xcite ) . the paper is organized as follows . functional canonical analysis and functional linear models for @xmath32-processes are introduced in section [ sec2 ] . sufficient conditions for the existence of functional normal equations are given in proposition [ pr2.2 ] . the canonical regression decomposition and its properties are the theme of section [ sec3 ] . in section [ sec4 ] , we propose a novel estimation technique to obtain regression parameter function estimates based on functional canonical components . the regression parameter function is the basic model component of interest in functional linear models , in analogy to the parameter vector in classical linear models . the proposed estimation method , based on a canonical regression decomposition , is contrasted with an established functional regression method based on a principal component decomposition . these methods utilize a dimension reduction step to regularize the solution of the inverse problems posed by both functional regression and functional canonical analysis . as a selection criterion for tuning parameters , such as bandwidths or numbers of canonical components , we use minimization of prediction error via leave - one - curve - out cross - validation ( rice and silverman ( @xcite ) ) . the proposed estimation procedures are applied to mortality data obtained for cohorts of medflies ( section [ sec5 ] ) . our goal in this application is to predict a random trajectory of mortality for a female cohort of flies from the trajectory of mortality for a male cohort which was raised in the same cage . we find that the proposed functional canonical regression method gains an advantage over functional principal component regression in terms of prediction error . additional results on canonical regression decompositions and properties of functional regression operators are compiled in section [ sec6 ] . all proofs are collected in section [ sec7 ] .

we study regression models for the situation where both dependent and independent variables are square - integrable stochastic processes . questions concerning the definition and existence of the corresponding functional linear regression models and some basic properties are explored for this situation . this representation establishes a connection between functional regression and functional canonical analysis and suggests alternative approaches for the implementation of functional linear regression analysis . a specific procedure for the estimation of the regression parameter function using canonical expansions is proposed and compared with an established functional principal component regression approach . as an example of an application , we present an analysis of mortality data for cohorts of medflies , obtained in experimental studies of aging and longevity . , , +

we study regression models for the situation where both dependent and independent variables are square - integrable stochastic processes . questions concerning the definition and existence of the corresponding functional linear regression models and some basic properties are explored for this situation . we derive a representation of the regression parameter function in terms of the canonical components of the processes involved . this representation establishes a connection between functional regression and functional canonical analysis and suggests alternative approaches for the implementation of functional linear regression analysis . a specific procedure for the estimation of the regression parameter function using canonical expansions is proposed and compared with an established functional principal component regression approach . as an example of an application , we present an analysis of mortality data for cohorts of medflies , obtained in experimental studies of aging and longevity . , , +

0907.5134

i

the study of transport phenomena has attracted considerable interest over the years due to its relevance in many physical situations . the latter are often described on the basis of one - dimensional particle motion in a tilted spatially periodic potential @xcite-@xcite . corresponding experimental realisations include josephson junctions @xcite , charge density waves @xcite , superionic conductors @xcite , rotation of dipoles in external fields @xcite , phase - locked loops @xcite and diffusion of dimers on surfaces @xcite to name but a few . in many of these aforementioned situations the particles , in addition to their motion in the periodic potential , interact , which may lead to cooperative effects not found in situations of individual particle motion @xcite-@xcite . the objective of the current work is to investigate the conditions under which it is possible to generate a directed flow along with collective motion in a system of coupled particles . to be precise , we study the transport of a dimer evolving in a washboard potential experiencing a weak tilt force . the nonlinear bond dynamics between the two monomers , constituting the dimer , is modelled by a morse potential allowing for bond breaking , i.e. fragmentation . we focus our interest on the chaos - promoted detrapping mechanism for dimers that initially reside in one well of the washboard potential . provided that such a detrapping transition happens the question then is under which circumstances subsequent directed long - range particle transport is achievable . since the total system energy is too low for both monomers to be able to escape from the potential well simultaneously , we explore whether cooperative energy redistribution is possible allowing at least one of the monomers to escape and subsequently display directed motion . we also elucidate the possible scenario in which the energy exchange between the monomers proceeds in such a well - coordinated manner that the monomers move separately from one well into the next , one following the other , resulting in directed motion of the dimer . the paper is organised as follows : in the next section the model of the dimer system is introduced , followed by the formulation of the escape problem together with a brief discussion of the related phase space structure . in section [ section : current ] the particle current is studied and the occurrence of different transport scenarios is described . afterwards in section [ section : space ] we relate the phase space dynamics to the regime of high particle current . in particular chaotic invariant sets , their connection with singularities of the escape time function , and their relevance for the escape process are considered . in section [ section : potential ] we present an alternative description of the escape problem as the motion of a single particle in a two - dimensional potential landscape . finally we summarise and discuss our results .

moreover , the total energy content is not enough for both particles to be able to escape simultaneously from an initial potential well ; to achieve transport the coupled particles need to interact cooperatively . for low coupling strength one particle followed by the other from consecutive potential wells resulting in directed collective motion .

we study the conservative and deterministic dynamics of two nonlinearly interacting particles evolving in a one - dimensional spatially periodic washboard potential . a weak tilt of the washboard potential is applied biasing one direction for particle transport . however , the tilt vanishes asymptotically in the direction of bias . moreover , the total energy content is not enough for both particles to be able to escape simultaneously from an initial potential well ; to achieve transport the coupled particles need to interact cooperatively . for low coupling strength the two particles remain trapped inside the starting potential well permanently . for increased coupling strength there exists a regime in which one of the particles transfers the majority of its energy to the other one , as a consequence of which the latter escapes from the potential well and the bond between them breaks . finally , for suitably large couplings , coordinated energy exchange between the particles allows them to achieve escapes one particle followed by the other from consecutive potential wells resulting in directed collective motion . the key mechanism of transport rectification is based on the asymptotically vanishing tilt causing a symmetry breaking of the non - chaotic fraction of the dynamics in the mixed phase space . that is , after a chaotic transient , only at one of the boundaries of the chaotic layer do resonance islands appear . the settling of trajectories in the ballistic channels associated with transporting islands provides long - range directed transport dynamics of the escaping dimer .

0907.5134

i

we have analysed the hamiltonian dynamics of two nonlinearly coupled particles evolving in a washboard potential . notably the total energy does not suffice to enable simultaneous escape of the two particles , initially trapped in a well of the washboard potential . due to appropriate energy redistribution , at least one of the particles can achieve escape . ( see also @xcite . ) ideally the two particles share energy almost periodically in such a way that consecutive detrapping - trapping transitions take place during which the particles escape one after another from one well into an adjacent one . it has been demonstrated that a weak tilt force , vanishing asymptotically in the direction of the bias , is sufficient to instigate directed motion of the escaping particles . transport is accomplished for those trajectories which follow a chaotic transient , associated with the dynamics of chaotic saddles , settling afterwards on regular motion . the key mechanism of current rectification is based on the asymptotically vanishing tilt causing a symmetry breaking of the non - chaotic fraction of the dynamics where only at the upper boundary of the chaotic layer resonance islands appear . the latter is supported by transporting island structures in the mixed phase space which serve for long - range directed transport . finally , we mention that it is certainly interesting to extend the study of directed motion to systems involving many more degrees of freedom than in the current dimer case where the dynamics within transporting islands can be investigated utilising two - dimensional poincar surface of sections . in particular , it needs to be examined what structures in higher dimensional phase spaces play the role of possible ballistic channels providing directed collective transport . faucheux , g. stolovitzky , and a. libchaber , phys . e * 51 * , 5239 ( 1995 ) . parris , m. kus , d.h . dunlap , and v.m . kenkre , phys . e * 56 * , 5295 ( 1997 ) . g. constantini and f. marchesoni , eur . . lett . * 48 * , 491 ( 1999 ) . p. reimann _ et al _ , phys . lett . * 87 * , 010602 ( 2001 ) . d. reguera _ et al _ , eur . . lett . * 57 * , 644 ( 2002 ) . tatarkova , w. sibbett , and k. dholakia , phys . * 91 * , 038101 ( 2003 ) . o.m . braun , r. ferrando , and g.e . tommei , phys . e * 68 * , 051101 ( 2003 ) . e. heinsalu , m. patriarca , and f. marchesoni , phys . e * 77 * , 021129 ( 2008 ) . e. pijper and a. fasolino , phys . b * 72 * , 165328 ( 2005 ) . s.h . lee and d.g . grier , phys . 96 * , 190601 ( 2006 ) . j. regtmeier _ et al _ , anal . chem . * 79 * , 3925 ( 2007 ) . f. jlicher , a. ajdari , and j. prost , rev mod . phys . * 69 * , 1269 ( 1997 ) . p. reimann , phys . * 361 * , 57 ( 2002 ) . a. barone and g. patern , _ physics and applications of the josephson effect _ , ( wiley , new york , 1982 ) . g. gruner , a. zawadowski , and p.m. chaikin , phys . lett . * 46 * , 511 ( 1981 ) . p. fulde , l. pietronero , w.r . schneider , and s. strssler , phys . lett . * 35 * , 1776 ( 1975 ) . d. reguera , j.m . rub , and a. prez - madrid , phys . e * 62 * , 5313 ( 2002 ) . lindsey , _ synchronization systems in communication and control _ ( prentice - hall , englewood cliffs , new jersey , 1972 ) . frenken and j.f . van der veen , phys . * 54 * , 34 ( 1985 ) . o.m . braun , surf . sci . * 230 * , 262 ( 1990 ) . m. partriarca and p. szelestey , act . phys . pol . * 36 * , 1745 ( 2005 ) . c. fusco and a. fasolino , thin solid films * 428 * , 34 ( 2003 ) . s. goncalves , v.m . kenkre , and a.r . bishop , phys . b * 70 * , 195415 ( 2004 ) . m. evstigneev , s. von gehlen , and p. reimann , phys . e * 79 * , 011116 ( 2009 ) . p. reimann , r. kawai , c. van den broeck , and p. hnggi , europhys . lett . * 45 * , 545 ( 1999 ) . d. hennig , l. schimansky - geier , and p. hnggi , europhys . lett . * 83 * , 60008 ( 2008 ) . s. martens , d. hennig , s. fugmann , and l. schimansky - geier , phys . e * 78 * 041121 ( 2008 ) . t. tel , in _ directions in chaos _ ( ed . : bai - lin hao , world scientific , singapore , vol . 3 , 1990 ) . t. tel and m. gruiz _ chaotic dynamics _ cambridge university press , cambridge , 2006 ) . m. zaslavsky , _ chaos in dynamical systems _ ( harwood , new york , 1985 ) , _ physics of chaos in hamiltonian systems _ ( imperial college press , london , 1998 ) . o.m . yevtushenko and k. richter , physica e * 4 * , 256 ( 1999 ) ; m. glck , a.r . kolovsky , and h .- j . korsch , physica d * 116 * , 283 ( 1998 ) . e. ott _ chaos in dynamical systems _ ( university of cambridge , cambridge , 1992 ) . s. wiggins , _ chaotic transport in dynamical systems _ ( springer - verlag , new york , 1992 ) . b. rckerl and c. jung , j. phys . a * 27 * , 6741 ( 1994 ) . a. emmanouilidou , c. jung , and l.e . reichl , phys . e * 68 * , 046207 ( 2003 ) . a.m. barr , kyungsun na , and l.e . reichl , phys . e * 79 * , 026215 ( 2009 ) . c. grebogi , e. ott , and j.a . yorke , physica d * 7 * , 181 ( 1983 ) ; s. bleher , c. grebogi , e. ott , and r. brown , phys . a * 38 * , 930 ( 1988 ) ; s. bleher , c. grebogi , and e. ott , physica d * 46 * , 87 ( 1990 ) . alligood , t.d . sauer , and j.a . chaos , an introduction to dynamical systems _ ( springer - verlag , new york , 1997 ) . s. denisov and s. flach , phys . e * 64 * , 056236 ( 2001 ) ; s. denisov , j. klafter , m. urbakh , and s. flach , physica d * 170 * , 131 ( 2002 ) ; s. denisov , j. klafter , and m. urbakh , phys . rev . e * 66 * , 046217 ( 2002 ) ; 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a weak tilt of the washboard potential is applied biasing one direction for particle transport . however , the tilt vanishes asymptotically in the direction of bias . the key mechanism of transport rectification is based on the asymptotically vanishing tilt causing a symmetry breaking of the non - chaotic fraction of the dynamics in the mixed phase space . that is , after a chaotic transient , only at one of the boundaries of the chaotic layer do resonance islands appear .

we study the conservative and deterministic dynamics of two nonlinearly interacting particles evolving in a one - dimensional spatially periodic washboard potential . a weak tilt of the washboard potential is applied biasing one direction for particle transport . however , the tilt vanishes asymptotically in the direction of bias . moreover , the total energy content is not enough for both particles to be able to escape simultaneously from an initial potential well ; to achieve transport the coupled particles need to interact cooperatively . for low coupling strength the two particles remain trapped inside the starting potential well permanently . for increased coupling strength there exists a regime in which one of the particles transfers the majority of its energy to the other one , as a consequence of which the latter escapes from the potential well and the bond between them breaks . finally , for suitably large couplings , coordinated energy exchange between the particles allows them to achieve escapes one particle followed by the other from consecutive potential wells resulting in directed collective motion . the key mechanism of transport rectification is based on the asymptotically vanishing tilt causing a symmetry breaking of the non - chaotic fraction of the dynamics in the mixed phase space . that is , after a chaotic transient , only at one of the boundaries of the chaotic layer do resonance islands appear . the settling of trajectories in the ballistic channels associated with transporting islands provides long - range directed transport dynamics of the escaping dimer .