J/ApJ/764/41ivo://CDS.VizieR/J/ApJ/764/41doi:10.26093/cds/vizier.17640041CDSFragos T.Lehmer B.Tremmel M.Tzanavaris P.Basu-Zych A.,Belczynski K.Hornschemeier A.Jenkins L.Kalogera V.Ptak A.Zezas A.2014-11-26T11:40:48Z2014-11-12T16:51:23ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frstellar-evolutionary-modelsx-ray-binary-starsHigh-redshift galaxies permit the study of the formation and evolution of X-ray binary (XRB) populations on cosmological timescales, probing a wide range of metallicities and star formation rates (SFRs). In this paper, we present results from a large-scale population synthesis study that models the XRB populations from the first galaxies of the universe until today. We use as input to our modeling the Millennium II cosmological simulation (Boylan-Kolchin et al. 2009MNRAS.398.1150B) and the updated semi-analytic galaxy catalog by Guo et al. (2011MNRAS.413..101G) to self-consistently account for the star formation history and metallicity evolution of the universe. Our modeling, which is constrained by the observed X-ray properties of local galaxies, gives predictions about the global scaling of emission from XRB populations with properties such as SFR and stellar mass, and the evolution of these relations with redshift. Our simulations show that the X-ray luminosity density (X-ray luminosity per unit volume) from XRBs in our universe today is dominated by low-mass XRBs, and it is only at z>~2.5 that high-mass XRBs become dominant. We also find that there is a delay of ~1.1Gyr between the peak of X-ray emissivity from low-mass XRBs (at z~2.1) and the peak of SFR density (at z~3.1). The peak of the X-ray luminosity from high-mass XRBs (at z~3.9) happens ~0.8Gyr before the peak of the SFR density, which is due to the metallicity evolution of the universe.2013ApJ...764...41Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/764/41CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/chandra : The Chandra Archive Log (CXC, 1999-2014)V/106 : Catalogue of X-ray binaries (Liu+ 2001)J/MNRAS/420/2190 : ECDFS sources with radio counterparts (Vattakunnel+, 2012)J/MNRAS/419/2095 : HMXBs in nearby galaxies (Mineo+, 2012)J/ApJ/749/130 : X-ray binaries in NGC 1291 with Chandra (Luo+, 2012)J/A+A/533/A33 : LMXBs detected in nearby galaxies (Zhang+, 2011)J/ApJS/195/10 : The CDF-S survey: 4Ms source catalogs (Xue+, 2011)J/MNRAS/417/2239 : SPIRE (f250um>17.4mJy) GOODS-N galaxies (Symeonidis+, 2011)J/ApJ/721/1843 : Swift-BAT survey of Galactic sources (Voss+, 2010)J/ApJ/719/L79 : BH spin-orbit misalignment in Galactic XRBs (Fragos+, 2010)J/ApJ/689/983 : LMXBs in early-type galaxies. I. Chandra (Humphrey+, 2008)J/ApJ/681/1163 : Late-type galaxies in Chandra deep fields (Lehmer+, 2008)J/A+A/469/807 : Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)J/A+A/455/1165 : Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)J/MNRAS/360/974 : Proper motions of pulsars (Hobbs+, 2005)J/A+A/442/1135 : High-mass XRBs in the Magellanic Clouds (Liu+, 2005)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/764/41https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/764/41http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/764/41https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/764/41https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/764/41http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/764/41GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/764/41/table3A complete list of all Population Synthesis (PS) models used in this workSeq[1/288] Model identifiermeta.idintprimaryalpha[0.1/0.5] Common envelope efficiency parameter {alpha}_CE_stat.paramfloatIMFExponent of high-mass IMF power law component (1)stat.paramfloateta[0.2/2] Stellary wind strength parameter {eta} (2)stat.paramfloatCE-HG[Yes No] Common Envelope in Hertzspring Gap (3)meta.codecharqBinary mass ratio distribution (4)meta.notecharkappa[0/0.1] {kappa}_DC_ kick distribution mutiplier, Hobbs et al. 2005 (J/MNRAS/360/974) (5)stat.fit.paramfloatRank[1/288] Model ranking in our statistical comparisonstat.fit.paramintlogL[-255/0] Log of likelihood ratio (6)stat.likelihooddouble