pinecone/core-2020-05-10-deduplication huggingface dataset:
Properties of Submillimeter Galaxies in the CANDELS GOODS-S Field

We derive physical properties of 10 submillimeter galaxies located in the
CANDELS coverage of the GOODS-S field. The galaxies were first identified as
submillimeter sources with the LABOCA bolometer and subsequently targeted for
870um continuum observation with ALMA. The high angular resolution of the ALMA
imaging allows secure counterparts to be identified in the CANDELS multiband
dataset. The CANDELS data provide deep photometric data from UV through
near-infrared wavelengths. Using synthetic spectral energy distributions, we
derive photometric redshifts, stellar masses, extinction, ages, and the star
formation history. The redshift range is z=1.65-4.76, with two of the galaxies
located at z>4. Two SMG counterparts have stellar masses 2-3 orders of
magnitude lower than the rest. The remaining SMG counterparts have stellar
masses around 1x10^11 Msun. The stellar population in the SMGs is typically
older than the expected duration of the submillimeter phase, suggesting that
the star formation history of submillimeter galaxies is more complex than a
single burst. Non-parametric morphology indices suggest that the SMG
counterparts are among the most asymmetric systems compared with galaxies of
the same stellar mass and redshift. The HST images shows that 3 of the SMGs are
associated with on-going mergers. The remaining counterparts are isolated.
Estimating the dust and molecular gas mass from the submm fluxes, and comparing
with our stellar masses shows that the molecular gas mass fraction of SMGs is
~28% and that the final stellar mass is likely to be (1-2)x10^11 Msun.Comment: 51 pages, 9 figures, 5 tables; Submitted to Ap
Flowing from $AdS_5$ to $AdS_3$ with $T^{1,1}$

We construct supersymmetric domain wall solutions of type IIB supergravity
that interpolate between $AdS_5\times T^{1,1}$ in the UV and
$AdS_3\times\mathbb{R}^2\times S^2\times S^3$ solutions in the IR. The
$\mathbb{R}^2$ factor can be replaced with a two-torus and then the solution
describes a supersymmetric flow across dimensions, similar to wrapped brane
solutions. While the domain wall solutions preserve $(0,2)$ supersymmetry, the
$AdS_3$ solutions in the IR have an enhanced $(4,2)$ superconformal
supersymmetry and are related by two T-dualities to the $AdS_3\times S^3\times
S^3\times S^1$ type IIB solutions which preserve a large $(4,4)$ superconformal
supersymmetry. The domain wall solutions exist within the $N=4$ $D=5$ gauged
supergravity theory that is obtained from a consistent Kaluza-Klein truncation
of type IIB supergravity on $T^{1,1}$; a feature driving the flows is that two
$D=5$ axion like fields, residing in the $N=4$ Betti multiplet, depend linearly
on the two legs of the $\mathbb{R}^2$ factor.Comment: 35 pages, 1 figure. References added, minor change
Energy Loss of Solar $p$ Modes due to the excitation of Magnetic Sausage
  Tube Waves: Importance of Coupling the Upper Atmosphere

We consider damping and absorption of solar $p$ modes due to their energy
loss to magnetic tube waves that can freely carry energy out of the acoustic
cavity. The coupling of $p$ modes and sausage tube waves is studied in a model
atmosphere composed of a polytropic interior above which lies an isothermal
upper atmosphere. The sausage tube waves, excited by $p$ modes, propagate along
a magnetic fibril which is assumed to be a vertically aligned, stratified, thin
magnetic flux-tube. The deficit of $p$-mode energy is quantified through the
damping rate, $\Gamma$ and absorption coefficient, $\alpha$. The variation of
$\Gamma$ and $\alpha$ as a function of frequency and the tube's plasma
properties is studied in detail. Previous similar studies have considered only
a subphotospheric layer, modelled as a polytrope that has been truncated at the
photosphere (Bogdan et al. (1996), Hindman & Jain 2008, Gascoyne et al.
(2011)). Such studies have found that the resulting energy loss by the $p$
modes is very sensitive to the upper boundary condition, which because of the
lack of a upper atmosphere have been imposed in a somewhat ad hoc manner. The
model presented here avoids such problems by using an isothermal layer to model
the overlying atmosphere (chromosphere), and consequently, allows us to analyse
the propagation of $p$-mode driven sausage waves above the photosphere. In this
paper we restrict our attention to frequencies below the acoustic cut-off
frequency. We demonstrate the importance of coupling all waves (acoustic,
magnetic) in the subsurface solar atmosphere with the overlying atmosphere in
order to accurately model the interaction of solar $f$ and $p$ modes with
sausage tube waves
Measurement of the pp to ZZ production cross section and constraints on
  anomalous triple gauge couplings in four-lepton final states at sqrt(s) = 8
  TeV

A measurement of inclusive ZZ production cross section and constraints on
anomalous triple gauge couplings in proton-proton collisions at sqrt(s) = 8 TeV
are presented. A data sample, corresponding to an integrated luminosity of 19.6
inverse femtobarns was collected with the CMS experiment at the LHC. The
measurements are performed in the leptonic decay modes ZZ to lll'l', where l =
e, mu and l' = e, mu, tau. The measured total cross section, sigma(pp to ZZ) =
7.7 +/- 0.5 (stat.) +0.5-0.4 (syst.) +/- 0.4 (theo.) +/- 0.2 (lum.) pb for both
Z bosons produced in the mass range 60 < m[Z] < 120 GeV, is consistent with
standard model predictions. Differential cross sections are measured and well
described by the theoretical predictions. The invariant mass distribution of
the four-lepton system is used to set limits on anomalous ZZZ and ZZ gamma
couplings at the 95% confidence level: -0.004 < f[4,Z] < 0.004, -0.004 < f[5,Z]
< 0.004, -0.005 < f[4,gamma] < 0.005, and -0.005 < f[5,gamma] < 0.005.Comment: Replaced with published version. Added journal reference and DO
The Appell Function $F_1$ and Regge String Scattering Amplitudes

We show that each 26D open bosonic Regge string scattering amplitude (RSSA)
can be expressed in terms of one single Appell function $F_1$ in the Regge
limit. This result enables us to derive infinite number of recurrence relations
among RSSA at arbitrary mass levels, which are conjectured to be related to the
known SL(5,C) dynamical symmetry of $F_1$. In addition, we show that these
recurrence relations in the Regge limit can be systematically solved so that
all RSSA can be expressed in terms of one amplitude. All these results are dual
to high energy symmetries of fixed angle string scattering amplitudes
discovered previously [4-8].Comment: 12 pages,no figur
The evolution of galaxy star formation activity in massive halos

There is now a large consensus that the current epoch of the Cosmic Star
Formation History (CSFH) is dominated by low mass galaxies while the most
active phase at 1<z<2 is dominated by more massive galaxies, which undergo a
faster evolution. Massive galaxies tend to inhabit very massive halos such as
galaxy groups and clusters. We aim to understand whether the observed "galaxy
downsizing" could be interpreted as a "halo downsizing", whereas the most
massive halos, and their galaxy populations, evolve more rapidly than the halos
of lower mass. Thus, we study the contribution to the CSFH of galaxies
inhabiting group-sized halos. This is done through the study of the evolution
of the Infra-Red (IR) luminosity function of group galaxies from redshift 0 to
~1.6. We use a sample of 39 X-ray selected groups in the Extended Chandra Deep
Field South (ECDFS), the Chandra Deep Field North (CDFN), and the COSMOS field,
where the deepest available mid- and far-IR surveys have been conducted with
Spitzer MIPS and Hersche PACS. Groups at low redshift lack the brightest,
rarest, and most star forming IR-emitting galaxies observed in the field. Their
IR-emitting galaxies contribute <10% of the comoving volume density of the
whole IR galaxy population in the local Universe. At redshift >~1, the most
IR-luminous galaxies (LIRGs and ULIRGs) are preferentially located in groups,
and this is consistent with a reversal of the star-formation rate vs .density
anti-correlation observed in the nearby Universe. At these redshifts, group
galaxies contribute 60-80% of the CSFH, i.e. much more than at lower redshifts.
Below z~1, the comoving number and SFR densities of IR-emitting galaxies in
groups decline significantly faster than those of all IR-emitting galaxies. Our
results are consistent with a "halo downsizing" scenario and highlight the
significant role of "environment" quenching in shaping the CSFH.Comment: 14 pages, 10 figures, accepted for publication by A&
Measurement of the average polarization of b baryons in hadronic $Z^0$ decays

In the Standard Model, b quarks produced in e^+e^- annihilation at the Z^0 peak have a large average longitudinal polarization of -0.94. Some fraction of this polarization is expected to be transferred to b-flavored baryons during hadronization. The average longitudinal polarization of weakly decaying b baryons, <P_L^{\Lambda_b}>, is measured in approximately 4.3 million hadronic Z^0 decays collected with the OPAL detector between 1990 and 1995 at LEP. Those b baryons that decay semileptonically and produce a \Lambda baryon are identified through the correlation of the baryon number of the \Lambda and the electric charge of the lepton. In this semileptonic decay, the ratio of the neutrino energy to the lepton energy is a sensitive polarization observable. The neutrino energy is estimated using missing energy measurements. From a fit to the distribution of this ratio, the value <P_L^{\Lambda_b}> = -0.56^{+0.20}_{-0.13} +/- 0.09 is obtained, where the first error is statistical and the second systematic.In the Standard Model, b quarks produced in e^+e^- annihilation at the Z^0 peak have a large average longitudinal polarization of -0.94. Some fraction of this polarization is expected to be transferred to b-flavored baryons during hadronization. The average longitudinal polarization of weakly decaying b baryons, <P_L^{\Lambda_b}>, is measured in approximately 4.3 million hadronic Z^0 decays collected with the OPAL detector between 1990 and 1995 at LEP. Those b baryons that decay semileptonically and produce a \Lambda baryon are identified through the correlation of the baryon number of the \Lambda and the electric charge of the lepton. In this semileptonic decay, the ratio of the neutrino energy to the lepton energy is a sensitive polarization observable. The neutrino energy is estimated using missing energy measurements. From a fit to the distribution of this ratio, the value <P_L^{\Lambda_b}> = -0.56^{+0.20}_{-0.13} +/- 0.09 is obtained, where the first error is statistical and the second systematic.In the Standard Model, b quarks produced in e + e − annihilation at the Z 0 peak have a large average longitudinal polarization of −0.94. Some fraction of this polarization is expected to be transferred to b-flavored baryons during hadronization. The average longitudinal polarization of weakly decaying b baryons, 〈 P L Λ b 〉, is measured in approximately 4.3 million hadronic Z 0 decays collected with the OPAL detector between 1990 and 1995 at LEP. Those b baryons that decay semileptonically and produce a Λ baryon are identified through the correlation of the baryon number of the Λ and the electric charge of the lepton. In this semileptonic decay, the ratio of the neutrino energy to the lepton energy is a sensitive polarization observable. The neutrino energy is estimated using missing energy measurements. From a fit to the distribution of this ratio, the value 〈 P L Λ b 〉=−0.56 +0.20 −0.13 ±0.09 is obtained, where the first error is statistical and the second systematic
Affleck-Dine leptogenesis with triplet Higgs

We study an extension of the supersymmetric standard model introducing a pair of electroweak triplet Higgs fields $ \Delta $ and $ {\bar \Delta} $. The neutrinos acquire Majorana masses mediated by the triplet Higgs fields rather than the heavy right-handed neutrinos. The successful leptogenesis for baryogenesis can be realized after inflation through the Affleck-Dine mechanism with a novel flat direction consisting of the triplet Higgs $ \Delta $, $ {\bar \Delta} $ and anti-slepton $ {\tilde e}^c $, even if the triplet Higgs mass is much larger than the gravitino mass $ m_{3/2} \sim 10^3 {\rm GeV} $. In this model, the leptogenesis and neutrino masses stem from different sources, though the triplet Higgs fields are involved in both of them. Hence, the leptogenesis does not provide a direct constraint on the neutrino masses. This is in contrast to the case with the $ {\tilde L} H_u $ flat direction, where one of the neutrinos should be ultra light ($ \lesssim 10^{-8} {\rm eV} $) for sufficient leptogenesis
Search for Odderon-Induced Contributions to Exclusive pi^0 Photoproduction at HERA

A search for contributions to the reaction ep-> e pi^0 N^* from photon-Odderon fusion in the photoproduction regime at HERA is reported, at an average photon-proton centre-of-mass energy <W> = 215 GeV. The measurement proceeds via detection of the pi^0 decay photons, a leading neutron from the N^* decay, and the scattered electron. No pi^0 signal is observed and an upper limit on the cross section for the photon-Odderon fusion process of sigma(gamma p -> pi^0 N^*) < 49 nb at the 95% confidence level is derived, integrated over the experimentally accessible range of the squared four-momentum transfer at the nucleon vertex 0.02 < |t| < 0.3 Gev^2. This excludes a recent prediction from a calculation based on a non-perturbative QCD model of a photon-Odderon fusion cross section above 200 nb.A search for contributions to the reaction ep-> e pi^0 N^* from photon-Odderon fusion in the photoproduction regime at HERA is reported, at an average photon-proton centre-of-mass energy <W> = 215 GeV. The measurement proceeds via detection of the pi^0 decay photons, a leading neutron from the N^* decay, and the scattered electron. No pi^0 signal is observed and an upper limit on the cross section for the photon-Odderon fusion process of sigma(gamma p -> pi^0 N^*) < 49 nb at the 95% confidence level is derived, integrated over the experimentally accessible range of the squared four-momentum transfer at the nucleon vertex 0.02 < |t| < 0.3 Gev^2. This excludes a recent prediction from a calculation based on a non-perturbative QCD model of a photon-Odderon fusion cross section above 200 nb.A search for contributions to the reaction ep→eπ 0 N ∗ from photon–odderon fusion in the photoproduction regime at HERA is reported, at an average photon–proton centre-of-mass energy 〈 W 〉=215 GeV. The measurement proceeds via detection of the π 0 decay photons, a leading neutron from the N ∗ decay, and the scattered electron. No π 0 signal is observed and an upper limit on the cross section for the photon–odderon fusion process of σ(γp→π 0 N ∗ )<49  nb at the 95% confidence level is derived, integrated over the experimentally accessible range of the squared four-momentum transfer at the nucleon vertex 0.02<| t |<0.3 GeV 2 . This excludes a recent prediction from a calculation based on a non-perturbative QCD model of a photon–odderon fusion cross section above 200 nb
Nuclear Modification Factor for Charged Pions and Protons at Forward
  Rapidity in Central Au+Au Collisions at 200 GeV

We present spectra of charged pions and protons in 0-10% central Au+Au
collisions at $\sqrt{s_{NN}}=200$ GeV at mid-rapidity ($y=0$) and forward
pseudorapidity ($\eta=2.2$) measured with the BRAHMS experiment at RHIC. The
spectra are compared to spectra from p+p collisions at the same energy scaled
by the number of binary collisions. The resulting nuclear modification factors
for central Au+Au collisions at both $y=0$ and $\eta=2.2$ exhibit suppression
for charged pions but not for (anti-)protons at intermediate $p_T$. The
$\bar{p}/\pi^-$ ratios have been measured up to $p_T\sim 3$ GeV/$c$ at the two
rapidities and the results indicate that a significant fraction of the charged
hadrons produced at intermediate $p_T$ range are (anti-)protons at both
mid-rapidity and $\eta = 2.2$
Spin and Electron Structure

The recent literature shows a renewed interest, with various independent
approaches, in the classical models for spin. Considering the possible interest
of those results, at least for the electron case, we purpose in this paper to
explore their physical and mathematical meaning, by the natural and powerful
language of Clifford algebras (which, incidentally, will allow us to unify
those different approaches). In such models, the ordinary electron is in
general associated to the mean motion of a point--like "constituent" Q, whose
trajectory is a cylindrical helix. We find, in particular, that the object Q
obeys a new, non-linear Dirac--like equation, such that --when averaging over
an internal cycle (which corresponds to a linearization)-- it transforms into
the ordinary Dirac equation (valid, of course, for the electron as a whole).Comment: LaTeX; 14 page
The Sloan Digital Sky Survey Reverberation Mapping Project: No Evidence
  for Evolution in the M-sigma Relation to z~1

We present host stellar velocity dispersion measurements for a sample of 88
broad-line quasars at 0.1<z<1 (46 at z>0.6) from the Sloan Digital Sky Survey
Reverberation Mapping (SDSS-RM) project. High signal-to-noise ratio coadded
spectra (average S/N~30 per 69 km/s pixel) from SDSS-RM allowed decomposition
of the host and quasar spectra, and measurement of the host stellar velocity
dispersions and black hole (BH) masses using the single-epoch (SE) virial
method. The large sample size and dynamic range in luminosity
(L5100=10^(43.2-44.7) erg/s) lead to the first clear detection of a correlation
between SE virial BH mass and host stellar velocity dispersion far beyond the
local universe. However, the observed correlation is significantly flatter than
the local relation, suggesting that there are selection biases in high-z
luminosity-threshold quasar samples for such studies. Our uniform sample and
analysis enable an investigation of the redshift evolution of the M-sigma
relation free of caveats by comparing different samples/analyses at disjoint
redshifts. We do not observe evolution of the M-sigma relation in our sample,
up to z~1, but there is an indication that the relation flattens towards higher
redshifts. Coupled with the increasing threshold luminosity with redshift in
our sample, this again suggests certain selection biases are at work, and
simple simulations demonstrate that a constant M-sigma relation is favored to
z~1. Our results highlight the scientific potential of deep coadded
spectroscopy from quasar monitoring programs, and offer a new path to probe the
co-evolution of BHs and galaxies at earlier times.Comment: replaced with the accepted version (minor changes and updated
  references); ApJ in press; changed title to highlight the main resul
Moving contact line dynamics: from diffuse to sharp interfaces

We reconcile two scaling laws that have been proposed in the literature for
the slip length associated with a moving contact line in diffuse interface
models, by demonstrating each to apply in a different regime of the ratio of
the microscopic interfacial width $l$ and the macroscopic diffusive length
$l_D= (M\eta)^{1/2}$, where $\eta$ is the fluid viscosity and $M$ the mobility
governing intermolecular diffusion. For small $l_D/l$ we find a diffuse
interface regime in which the slip length scales as $\xi \sim(l_Dl)^{1/2}$. For
larger $l_D/l>1$ we find a sharp interface regime in which the slip length
depends only on the diffusive length, $\xi \sim l_D \sim (M\eta)^{1/2}$, and
therefore only on the macroscopic variables $\eta$ and $M$, independent of the
microscopic interfacial width $l$. We also give evidence that modifying the
microscopic interfacial terms in the model's free energy functional appears to
affect the value of the slip length only the diffuse interface regime,
consistent with the slip length depending only on macroscopic variables in the
sharp interface regime. Finally, we demonstrate the dependence of the dynamic
contact angle on the capillary number to be in excellent agreement with the
theoretical prediction of \cite{Cox1986}, provided we allow the slip length to
be rescaled by a dimensionless prefactor. This prefactor appears to converge to
unity in the sharp interface limit, but is smaller in the diffuse interface
limit. The excellent agreement of results obtained using three independent
numerical methods, across several decades of the relevant dimensionless
variables, demonstrates our findings to be free of numerical artifacts.Comment: 24 pages, 5 figure
Summary of the ATLAS experiment's sensitivity to supersymmetry after LHC
  Run 1 - interpreted in the phenomenological MSSM

A summary of the constraints from the ATLAS experiment on $R$-parity
conserving supersymmetry is presented. Results from 22 separate ATLAS searches
are considered, each based on analysis of up to 20.3 fb$^{-1}$ of proton-proton
collision data at the centre-of-mass energy of $\sqrt{s}$ = 7 and 8 TeV at the
Large Hadron Collider. The results are interpreted in the context of the
19-parameter phenomenological minimal supersymmetric standard model, in which
the lightest supersymmetric particle is a neutralino, taking into account
constraints from previous precision electroweak and flavour measurements as
well as from dark matter related measurements. The results are presented in
terms of constraints on supersymmetric particle masses and are compared to
limits from simplified models. The impact of ATLAS searches on parameters such
as the dark matter relic density, the couplings of the observed Higgs boson,
and the degree of electroweak fine-tuning is also shown. Spectra for surviving
supersymmetry model points with low fine-tunings are presented.Comment: 58 pages plus author list + cover page (75 pages total), 21 figures,
  7 tables, submitted to JHEP; all figures including additional auxiliary
  figures are available at
  https://atlas.web.cern.ch/Atlas/GROUPS/PHYSICS/PAPERS/SUSY-2014-08
Evolution of field line helicity during magnetic reconnection

This work was supported by the Science and Technology Facilities Council (UK) through consortium Grant Nos. ST/K000993/1 and ST/K001043 to the University of Dundee and Durham University.We investigate the evolution of field line helicity for magnetic fields that connect two boundaries without null points, with emphasis on localized finite-B magnetic reconnection. Total ( relative) magnetic helicity is already recognized as an important topological constraint on magnetohydrodynamic processes. Field line helicity offers further advantages because it preserves all topological information and can distinguish between different magnetic fields with the same total helicity. Magnetic reconnection changes field connectivity and field line helicity reflects these changes; the goal of this paper is to characterize that evolution. We start by deriving the evolution equation for field line helicity and examining its terms, also obtaining a simplified form for cases where dynamics are localized within the domain. The main result, which we support using kinematic examples, is that during localized reconnection in a complex magnetic field, the evolution of field line helicity is dominated by a work-like term that is evaluated at the field line endpoints, namely, the scalar product of the generalized field line velocity and the vector potential. Furthermore, the flux integral of this term over certain areas is very small compared to the integral of the unsigned quantity, which indicates that changes of field line helicity happen in a well-organized pairwise manner. It follows that reconnection is very efficient at redistributing helicity in complex magnetic fields despite having little effect on the total helicity.Publisher PDFPeer reviewe