dataesr/scientific-paragraphs-categorization huggingface dataset:
2008 , Jonker & Nelemans 2004). Tight constraints to the existence of an outflow were inferred from grating observations for all the sources shown in Fig. 1  except for 4U 1323-62  (Boirin et al. 2005). For NSs showing outflows we plot the plasma location and luminosity inferred from grating observations  (Schulz & Brandt 2002 , Ueda et al. 2004 , Miller et al. 2011 ). The errors in the luminosity are estimated from the error in the distance and for the radius, a default error of 50% is adopted whenever the error is not provided in the discovery papers. The dotted lines have been derived from the lines in Fig. 17  from W96, and set the boundaries for the existence of a wind for NS LMXBs with a T IC ∼ 1. 3 × 10 7 K. The dashed line represents the transition from the corona into a wind when radiation force from electron scattering is included (but note that such limit is applicable only to high luminosities, PK02).
We next look at the sources showing winds, which are represented in Fig. 1  with filled squares. It is evident that such sources show luminosities which are significantly larger than for the sources not showing winds, and which are just above twice the critical luminosity derived to launch a wind (W96). In the case of Cir X-1, the launching radius obtained for the wind observed in the high luminosity observations corresponds to ∼0. 1 R IC. This radius is still plausible for launching winds once the radiation pressure due to electron scattering is considered (see PK02), especially at this high luminosity. In summary, Fig. 1  indicates that a thermal mechanism explains satisfactorily the presence or absence of winds in NS LMXBs. Further support to this conclusion is given by the fact that winds and warm absorbers are preferentially detected in high-inclination sources (all the sources shown in Fig.
The crystal is quartz (10-11) with a 2 d = 0. 668 nm lattice spacing, a 0. 29 mm thickness, and 254 mm bending radius. The crystal is positioned at 600 mm distance from the target, the crystal to slit distance is 105 mm. The nosecone is equipped with a removable pointer and a debris shield  [4]. The TCS was used to record x-ray spectra from laser-induced fluorescence of Mo foils used as the x-ray source for a high-energy Thomson scattering experiment at the OMEGA laser facility. TCS was directly pointed to the source of x rays, collecting data on all four image plate (IP) positions; the first two IP's had a bandwidth coverage that included the Mo K x-ray lines. In the Omega shot #59891 analyzed in this report 16 backlighter beams (~500 J) with a total energy of ~8 kJ were focused to a 12 m thick Mo foil that was serving as the x-ray source in the Thomson scattering experiment.
Acknowledgements. We would like to thank  Massimo Bianchi ,  J. M. Moreno  and  V. Martin-Lozano  for very useful discussions. E. D. , L. H and Y. M thank the  Galileo Galilei Institute for Theoretical Physics  for the hospitality and the  INFN  for partial support during the completion of this work. This work was supported in part by the  European ERC  Advanced Grant 226371 MassTeV, the  French   ANR TAPDMS ANR-09-JCJC-0146  the contract PITN-GA-2009-237920 UNILHC and the  Spanish MICINNs  Consolider- Ingenio 2010 Programme  under grant  Multi-Dark   CSD2009-00064. Y. M. acknowledges partial support from the  European Union   FP7 ITN INVISIBLES (Marie Curie Actions ,  PITN-GA-2011-289442 ), the  ERC  advanced grant Higgs@LHC. B. Z. acknowledges the support of  MICINN, Spain , under the contract  FPA2010-17747 , as well as the hospitality of LPT, Orsay, during the completion of this project.
VII. ACKNOWLEDGMENTS We thank G. A. El, E. V. Ferapontov and R. H. J. Grimshaw for useful discussions, and referees for constructive comments and helpful references. KRK and AOS acknowledge support and hospitality of the Institut de Mathématiques de Bourgogne, where they held visiting positions in the spring-summer of 2012, which has made this collaboration possible. CK and VBM thank for financial support by the ANR via the program ANR-09-BLAN-0117-01. 7 ) -(  13 ) assumes the form Here, we have not shown the explicit form of the higher-order terms in the small parameter ∆ (denoted by O(∆ 2 )) since these terms are not needed in the derivation of our asymptotic equation. -U ζ + P ζ + ∆ [U U ζ + W Uz + PR - R - √ R 2 -A 2 R 2 -A 2 νPν + Rν 2 P ζ + O(∆ 2 ) = 0, -V ζ + 1 √ R 2 -A 2 Pν + R - √ R 2 -A 2 √ R 2 -A 2 νP ζ +∆ U V ζ + W Vz + R - √ R 2 -A 2 √ R 2 -A 2 νPR + (R - √ R 2 -A 2 )(R 2 + A 2 ) 2(R 2 -A 2 ) 3/2 ν 3 P ζ - (R - √ R 2 -A 2 ) 2 + R 2 2(R 2 -A 2 ) 3/2 ν 2 Pν + O(∆ 2 ) = 0, Pz -∆W ζ + O(∆ 2 ) = 0, U ζ + Wz + ∆ UR - R - √ R 2 -A 2 R 2 -A 2 Rν 2 U ζ + νUν + 1 √ R 2 -A 2 (R -.
Once a mathematical description of the galaxy bias has been obtained, cosmological constraints can be derived by marginalizing over the uncertain parameters that describe the bias. Alternatively, observational measurements of the galaxy bias, derived in a given cosmological framework, can be used to constrain the parameters of galaxy formation models. In this paper, we focus on the dependence of galaxy clustering on luminosity and stellar mass, providing new observational constraints at redshift 0. 5 < z < 1. 1, from the first data release of the ongoing VIMOS Public Extragalactic Redshift Survey (VIPERS,  Guzzo et al. 2013). The comparison between VIPERS clustering measurements with similar ones at lower and higher redshifts can constrain the cosmic evolution of the relationship between DM and galaxy properties, hence between gravity and cosmology on one side and processes associated with baryonic physics on the other side.
The large number of objects with accurate spectroscopic redshifts and the large volume covered by the VIPERS survey give us the opportunity to measure the clustering of galaxies over a wide range of luminosities and stellar masses, back to the cosmic epoch when the Universe was still decelerating. In particular, we provide constraints on the projected correlation function, which we model as a single power law. This represents a reasonable, though not optimal, approximation at r p 20 h -1 Mpc , where r p is the direction perpendicular to the line-of-sight, and facilitates the comparison with previous studies. A more detailed interpretation of these data using halo occupation distribution (HOD) modelling is deferred to a future work (see also  de la Torre et al. 2013). The plan of this paper is as follows.
The VIPERS survey We have used the data from the VIPERS Public Data Release 1 (PDR-1), which will be made publicly available in the fall of 2013. VIPERS is an ongoing Large Programme aimed at measuring redshifts for ∼10 5 galaxies at 0. 5 < z 1. 2. One of the main goals of this survey is to characterize the galaxy spatial properties and growth rate of the LSS, measuring galaxy clustering and redshift-space distortions at an epoch when the Universe was about half its current age. Indeed, according to the standard ΛCDM scenario, the redshift range that VIPERS probes is previous to the dark energy (DE) dominated era, crossing the cosmic epoch when the Universe started accelerating (see the bottom labels in Fig. 1 ). The galaxy target sample is selected from the Canada-France-Hawaii Telescope Legacy Survey Wide (CFHTLS-Wide) optical photometric catalogues  (Mellier et al.
The B-band rest-frame magnitude limits in the left panel account for the average luminosity evolution of galaxies, as explained in the text. On the bottom axes, z eq,Λ ∼ 0. 44 is the redshift of DM-DE equality and z acc ∼ 0. 82 is the redshift when the Universe started accelerating, according to ΛCDM predictions with the set of cosmological parameters adopted in this work. The PDR-1 galaxy catalogue includes 53 608 redshifts and corresponds to the reduced data frozen in the VIPERS database at the end of the 2011/2012 observing campaign. The 2PCF of PDR-1 galaxies and the first constraints on the growth rate from redshift-space distortions are presented in a parallel paper (de la  Torre et al. 2013). A measurement of Ω M using a novel clustering statistic is given in  Bel et al. (2013). The galaxy stellar mass function is presented in  Davidzon et al.
(  4 ) can be solved analytically: w p (r p ) = r p r 0 r p γ Γ( 1 2 )Γ( γ-1 2 ) Γ( γ 2 ) , ( 7 ) where Γ is the Euler's gamma function. Hence, a power-law fit to w p (r p ) provides r 0 and γ for the real-space correlation function ξ(r). Finally, the scale-dependent galaxy bias can be estimated as b(r p ) = w p (r p ) w m p (r p ) , (8) where w m p (r p ) is the projected correlation function of matter. This is derived using the software CAMB  (Lewis & Bridle 2002) , which exploits the HALOFIT routine  (Smith et al. 2003)  to reproduce the non-linear evolution of the matter power spectrum.
(2002)  used the 2dF Galaxy Redshift Survey (2dF-GRS) to measure the galaxy clustering up to z = 0. 15. The VIMOS-VLT Deep Survey (VVDS) clustering measurements by  Pollo et al. (2006)  refer to the redshift ranges 0. 1 < z < 0. 5 and 0. 5 < z < 1. 2. Finally, the DEEP2 Galaxy Redshift Survey results have been obtained by  Coil et al. (2006)  at z ∼ 1. The last two clustering measurements are at similar redshifts to VIPERS. The bottom panels of Fig. 5  show the stellar mass dependence of r 0 and γ. We compare our results to data from SDSS  (Li et al. 2006) , VVDS-Deep  (Meneux et al. 2008) , zCOSMOS  (Meneux et al. 2009) , NMBS  (Wake et al. 2011) , DEEP2  (Mostek et al. 2013)  and BzK  (Lin et al. 2012). The best-fit clustering lengths from SDSS-DR2 data in the local Universe  (Li et al. 2006 ) have been fitted by  Mostek et al.
5, 0. 7], z ∈ [0. 7, 0. 9], and z ∈ [0. 9, 1. 1] are shown, respectively, by blue squares, red diamonds, and green circles, as indicated by the labels. The remaining grey symbols refer to measurements based on data from other surveys, reported here for comparison: upper panels -DSS-DR7 data from  Zehavi et al. (2011) , 2dfGRS data from  Norberg et al. (2002) , VVDS-Deep data from  Pollo et al. (2006)  and DEEP2 data from  Coil et al. (2006) ; lower panels -SDSS-DR2 data from  Li et al. (2006) , VVDS-Deep data from  Meneux et al. (2008) , zCOSMOS data from  Meneux et al. (2009) , NMBS data from  Wake et al. (2011) , DEEP2 data from  Mostek et al. (2013)  and BzK data from  Lin et al. (2012). and SDSS. The same behaviour is seen in VIPERS: we find little evolution in the most luminous bin. Additionally, the VIPERS data allow us to track r 0 with precision over a range of luminosities from z = 0.
The last certainly introduce the most relevant effects, as different surveys can be affected by stellar mass incompleteness to varying degrees. In particular, the VIPERS mass-selected samples contain, on average, much brighter galaxies than VVDS and DEEP2, owing to VIPERS higher flux selection cut. Moreover, since the power-law model does not describe the data perfectly, measurements obtained from fitting over different ranges could produce different values of the fit parameters. This effect is especially significant for the most massive bins, where the shape of w p (r p ) is the furthest from a power law and, thus, most sensitive to the range, binning, and choice of points used for fitting. Finally, the impact of sample variance has been estimated with different techniques, and it might be underestimated in some cases.
Both the luminosity and stellar mass dependence of VIPERS clustering appear in overall good agreement with theoretical expectations, though we note that the most luminous and massive VIPERS galaxies are slightly more clustered than the semianalytic ones, especially at high redshift. We notice that the cosmological parameters of the Millennium simulation are based on first-year results from the Wilkinson Microwave Anisotropy Probe (WMAP1). In particular, the value of σ 8 = 0. 9 is significantly higher than the most recent estimates. If the Millennium predictions are properly rescaled to be consistent with the sevenyear WMAP data  (Guo et al. 2013b ), galaxies at z ∼ 1 are predicted to be slightly more clustered for M 10 10. 5 M , while for lower masses the predicted clustering is almost coincident with the WMAP1 case.
Summary and conclusions In this work, we studied how galaxy clustering depends on luminosity and stellar mass in the redshift range 0. 5 < z < 1. 1, using the currently largest complete sample of galaxies with redshift measured in this range. To quantify the effect, we measured the redshift-space 2PCF of VIPERS galaxies in the first data release, PDR-1, and derived the real-space clustering and bias assuming a power-law form for the projected correlation function. Errors were estimated using a set of mock HOD and SHMR catalogues A17, page 11 of 15 that mimick the characteristics and the observational selections of the VIPERS dataset. The main results of this work can be summarized as follows. -We confirm with unprecedented precision at z = 0. 5-1. 1 a monotonic increase in the clustering length r 0 , both as a function of B-band magnitude and stellar mass, in all the three redshift ranges considered.
Acknowledgements. We warmly thank  Simon D. M. White  for helpful suggestions. We acknowledge the crucial contribution of the  ESO  staff for the management of service observations. In particular, we are deeply grateful to  M. Hilker  for his constant help and support of this programme. Italian participation in VIPERS has been funded by  INAF  through  PRIN 2008  and 2010 programmes. L. G. acknowledges support of the  European Research Council  through the  Darklight ERC Advanced Research Grant  (# 291521 ). O. L. F. acknowledges support of the  European Research Council  through the  EARLY ERC Advanced Research Grant  (# 268107 ). Polish participants have been supported by the  Polish Ministry of Science  (grant N  N203 51 29 38 ), the  Polish-Swiss Astro  Project (co-financed by a grant from  Switzerland , through the  Swiss Contribution  to the enlarged European Union), the  European Associated Laboratory Astrophysics Poland-France HECOLS , and a  Japan Society for the Promotion of Science (JSPS)   Postdoctoral Fellowship for Foreign Researchers  ( P11802 ).
GDL acknowledges financial support from the  European Research Council  under the European Community's  Seventh Framework Programme  ( FP7/2007-2013) / ERC  grant agreement No. 202781. W. J. P. and R. T. acknowledge financial support from the  European Research Council  under the European Community's  Seventh Framework Programme  ( FP7/2007-2013) / ERC  grant agreement No. 202686. W. J. P. is also grateful for support from the  UK Science and Technology Facilities Council  through the grant  ST/I001204/1. E. B. , F. M. and L. M. acknowledge the support from grants  ASI-INAF I/023/12/0  and  PRIN MIUR 2010-2011. C. M. is grateful for support from specific project funding of the  Institut Universitaire de France and the  LABEX OCEVU. We would also like to thank the anonymous referee for useful comments and suggestions.
Amplitude spectral distribution of PWA-ELF data The mathematical treatments of the wave field data were designed at least ten years before Huygens landing so as to be performed automatically onboard. The ELF power spectral density (PSD) was computed onboard by applying a DFT after a 16-bit analogdigital conversion of two consecutive waveform samples of 333 ms duration each. The square root of the composite DFT modulus, i. e. the amplitude spectral density (ASD) was logarithmically compressed, and the lower byte (8 bits) was transmitted without the phases to Earth by the telemetry system via the Cassini orbiter  (Lebreton et al. , 2005). Therefore, this study is constrained by the limited performances of usual techniques of wave-data processing of space experiments, but, nevertheless, we take the best advantage of the proper peculiarities of the PWA-ELF instrument, as briefly described here below.
[19, 24]. For each realization, we determine the slope of the measured photodiode voltage versus the piezo displacement in the constant compliance zone when the sphere and the substrate are in contact. This gives the cantilever deflection z c. Extrapolation of the constant compliance zone data to zero intercepts the displacement axis at the contact position (D = 0), allowing us to determine the latter with a precision of roughly 5 nm. This procedure is explained in Fig. 1(a). In order to obtain the actual separation distance, the cantilever deflection was added to the piezo displacement. The actual velocity (during the approach or withdrawal phases) is obtained from the full sphere-substrate distance by calculating its time derivative: V = dD dt. ( 6 ) A typical example of the measurement of the cantilever deflection resulting from the hydrodynamic force acting on the sphere is presented in Fig.
ACKNOWLEDGMENTS This work was partially supported by the  CPER Pôle 4N Nanosciences en Aquitaine  ( GP-206-action 216/1 ) with the contribution of the  Conseil Régional d'Aquitaine , the  FEDER  and the  Ministry of Education and Research , by the  French National Agency  ( MicRheo Project  No. ANR-08-NANO-004 ) and by the  Conseil Régional d'Aquitaine  (Project No. 20091102001 ).
Electrodeposition reaction monitoring Copper electrodeposition has been used for calibrating the gravimetric sensitivity of acoustic sensors thanks to its ability to provide an independent estimate of the deposited metal mass through the measurement of the current generated by the potentiostat  [8]. When using a closed loop strategy in order to keep the phase measurement within measurement range of the analog to digital converter at higher gain, the fast reaction rate and large phase shift provide a challenging measurement condition for validating the phase tracking algorithms. The generation of the voltage driving the potentiostat and electrodeposition parameters (counter electrode voltage and current) are controlled and monitored from the same microcontroller running the SAW monitoring circuits, yielding data synchonization.
2002). We scale the ugriz photometry to the r-band cmodel magnitude, which provides the most reliable estimate of the total (integrated) galaxy flux irrespective of galaxy type  (Abazajian et al. 2004; Bernardi et al. 2010; Blanton et al. 2011). Finally, we supplement our UV and optical photometry with integrated JHK s magnitudes from the 2MASS Extended Source Catalog (XSC;  Jarrett et al. 2000) , and with integrated photometry (or upper limits) at 3. 4 and 4. 6 µm from the WISE All-Sky Data Release. 34 3. SAMPLE SELECTION In Section 3. 1 we define the PRIMUS parent sample, and in Section 3. 2 we describe the criteria we use to select quiescent and actively star-forming galaxies as a function of redshift.
Stellar Masses and Star Formation Rates Modeling the broadband SEDs of galaxies using stellar population synthesis models has become a powerful technique for inferring their physical properties (see the recent review by  Walcher et al. 2011, and references therein). We have developed iSEDfit, a suite of routines written in the idl programming language to determine within a simplified Bayesian framework the stellar masses, SFRs, and other physical properties of galaxies from their observed broadband SEDs (e. g. ,  Kauffmann et al. 2003a; Salim et al. 2007; Auger et al. 2009). We describe iSEDfit in more detail in Appendix A, but in essence the code uses the redshift and observed photometry of each galaxy to compute the statistical likelihood of a large ensemble of model SEDsgenerated using population synthesis models-spanning a wide range of observed colors and physical properties (stellar mass, age, metallicity, star formation history, dust content, etc.
7. SUMMARY We have measured the evolution of the SMFs of quiescent and star-forming galaxies from z = 0 -1 using two large, statistically complete, spectroscopic samples. At low redshift we use a sample of ∼ 170, 000 SDSS galaxies with GALEX, 2MASS, and WISE photometry, and at intermediate redshift we use a sample of ∼ 40, 000 galaxies brighter than i ≈ 23 drawn from PRIMUS with deep GALEX and IRAC imaging. Our PRIMUS sample is notable for its depth, sample size, and area, which totals ≈ 5. 5 deg 2 over five widely-separated fields, while our SDSS-GALEX sample comprises one of the largest statistical samples of local galaxies with SDSS and GALEX photometry ever assembled. The exceptional multi-wavelength coverage of both datasets provides deep UV to mid-infrared imaging over the entire spectroscopic survey area, allowing us to robustly estimate SFRs and stellar masses using a new Bayesian SED-modeling code (iSEDfit; see Appendix A).
Although iSEDfit is capable of reconstructing the full posterior distributions in postprocessing after the computationally intensive fitting has been completed, the code by default provides the median of the posterior PDF as the best estimate of each parameter, and estimates the uncertainty in each parameter as -Effect on the SDSS-GALEX SMF of (left) different prior parameter combinations and (right) different population synthesis models (see the text in Appendix B for acronym definitions and details). We find that assuming that galaxies do not experience stochastic bursts ("no bursts") has a significant effect on the massive end (M 10 11 M ⊙ ) of the SMF, whereas for all other combinations of priors and population synthesis models the effects are relatively small ( 0. 1 dex). 1/4 of the 2.
(2010). The upper-right and lower-left panels compares our masses against the stellar masses publicly released by the MPA/JHU team based on the SDSS DR4 42 and DR7 43 data releases. The MPA/JHU-DR4 masses are based on fitting the Hδ A and D n (4000) optical spectral indices  (Kauffmann et al. 2003a) , and the DR7 stellar masses are derived using a similar technique as iSEDfit, but only fitting to the SDSS ugriz photometry. In both cases the agreement between the various independent determinations is outstanding. Finally, in the lower-right panel we compare our mass estimates against the stellar masses derived by  Salim et al. (2007)  using a similar SED-modeling technique as iSEDfit, but just fitting to the GALEX plus ugriz photometry. Once again, the agreement between the two stellar mass estimates is very good.
Acknowledgements This work is supported by  NNSFC 41031065 ,  41074106  and the  Shandong Natural Science Foundation  (Grant no. JQ201112 ). M. W. D. is partly supported by  Chinese Academy of Sciences  (CAS) visiting professorship for senior international scientists Grant no. 2012T1G0018. We are grateful to  A. M. Du ,  D. Turner ,  Y. S. Ge ,  P. Escoubet  and  H. Hasegawa  for their helpful discussions. Thanks to  Flux Gate Magnetometer ,  Cluster Ion Spectrometry Experiment ,  Plasma Electron  and Current Experiment teams, and  Cluster Active Archive (CAA)  web for providing the CLUSTER data, and  NASA CDAWeb  for providing the OMNI solar wind and magnetic field data.
During 2011 the LHCb experiment at CERN collected 1. 0 fb -1 of √ s = 7 TeV pp collisions. Due to the large heavy quark production cross-sections, these data provide unprecedented samples of heavy flavoured hadrons. The first results from LHCb have made a significant impact on the flavour physics landscape and have definitively proved the concept of a dedicated experiment in the forward region at a hadron collider. This document discusses the implications of these first measurements on classes of extensions to the Standard Model, bearing in mind the interplay with the results of searches for on-shell production of new particles at ATLAS and CMS. The physics potential of an upgrade to the LHCb detector, which would allow an order of magnitude more data to be collected, is emphasised.