J/MNRAS/466/1019ivo://CDS.VizieR/J/MNRAS/466/1019doi:10.26093/cds/vizier.74661019CDSSazonovS.KhabibullinI.2024-08-17T20:17:32Z2017-03-28T15:28:21ZCDS support team

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

cds-question@unistra.frx-ray-binary-starsUsing a spectral analysis of bright Chandra X-ray sources located in 27 nearby galaxies and maps of star-formation rate (SFR) and ISM surface densities for these galaxies, we constructed the intrinsic X-ray luminosity function (XLF) of luminous high-mass X-ray binaries (HMXBs), taking into account absorption effects and the diversity of HMXB spectra. The XLF per unit SFR can be described by a power law dN/dlogL=2.0(L/10^39^erg/s)^(-0.6)^(M_{sun}_/yr)^-1^ from L=10^38^ to 10^40.5^erg/s, where L is the unabsorbed luminosity at 0.25-8 keV. The intrinsic number of luminous HMXBs per unit SFR is a factor of ~2.3 larger than the observed number reported before. The intrinsic XLF is composed of hard, soft and supersoft sources (defined here as those with the 0.25-2keV to 0.25-8keV flux ratio of <0.6, 0.6-0.95 and >0.95, respectively) in ~2:1:1 proportion. We also constructed the intrinsic HMXB XLF in the soft X-ray band (0.25-2keV). Here, the numbers of hard, soft and supersoft sources prove to be nearly equal. The cumulative present-day 0.25-2 keV emissivity of HMXBs with luminosities between 10^38^ and 10^40.5^erg/s is ~5x10^39^erg/s(M_{sun}_/yr)^-1^, which may be relevant for studying the X-ray preheating of the early Universe.2017MNRAS.466.1019Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/466/1019CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toB/chandra : The Chandra Archive Log (CXC, 1999-2014)J/ApJS/224/40 : Catalog of Chandra ACIS point like sources (Wang+, 2016)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/466/1019https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/466/1019http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/466/1019https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/466/1019https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/466/1019http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/466/1019GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/466/1019/table2 (Clean sample of X-ray sources)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/466/1019/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/466/1019/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/466/1019/table2?GETtext/xml+votable180.050000true198.8312542.0505560.0055555555555555566/2320 4511 5715 5751 7241 7602 7606 7624 7743 7799 10841 10856 10911 11027 11434 13522 15592-15593 16441 18398 27030 27514 28015 28167 28631 38390 43881https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/466/1019?format=asciidefaultJ/MNRAS/466/1019/table2Clean sample of X-ray sourcesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintCXOGSGName of the source as in Wang et al. (2016, Cat. J/ApJS/224/40) (JHHMMSS.s+DDMMSS)meta.id;meta.maincharGalNameName of the source's host galaxymeta.id.parentcharr25Source's offset from the center of the galaxy in units of its 25mag/arcsec^2^ radiuspos.angDistance;arith.difffloatObsIDObsId of the Chandra observation used in X-ray data analysismeta.noteintCountsTotal number of counts detected from the source during this observationctphot.count;em.X-rayintModelBest[0/2] Best-fitting spectral model (1)meta.id;stat.fitintNHLosTotal gas column density through the Galaxy and host galaxy in the direction of the source1e+20cm**-2phys.columnDensityfloatNHFitNH from the X-ray spectral fit1e+20cm**-2phys.columnDensityfloatb_NHFitLower limit for NH from the spectral fit1e+20cm**-2stat.fit.param;stat.minfloatB_NHFitUpper limit for NH from the spectral fit1e+20cm**-2stat.fit.param;stat.maxfloatLxFitIntrinsic (i.e. corrected for absorption) luminosity in 0.25-8keV energy range1e+31Wphys.luminosity;em.X-rayfloatb_LxFitLower limit for intrinsic luminosity in 0.25-8keV energy range1e+31Wphys.luminosity;stat.minfloatB_LxFitUpper limit for intrinsic luminosity in 0.25-8keV energy range1e+31Wphys.luminosity;stat.maxfloatLsSFitIntrinsic (i.e. corrected for absorption) luminosity in 0.25-2keV energy range1e+31Wphys.luminosity;em.X-rayfloatb_LsSFitLower limit for intrinsic luminosity in 0.25-2keV energy range1e+31Wphys.luminosity;stat.minfloatB_LsSFitUpper limit for intrinsic luminosity in 0.25-2keV energy range1e+31Wphys.luminosity;stat.maxfloatLxFitObsObserved (i.e. uncorrected for absorption) luminosity in 0.25-8keV energy range1e+31Wphys.luminosity;em.X-rayfloatLsFitObsObserved (i.e. uncorrected for absorption) luminosity in 0.25-2keV energy range1e+31Wphys.luminosity;em.X-rayfloatSpParMain spectral parameter of the best model (ModelBest) (2)stat.param;meta.modelledfloatb_SpParLower limit for main spectral parameter of the best model (ModelBest)stat.param;meta.modelled;stat.minfloatB_SpParUpper limit for main spectral parameter of the best model (ModelBest)stat.param;meta.modelled;stat.maxfloatisHard[0/1] Hard source flagmeta.codeintisSoft[0/1] Soft source flagmeta.codeintisSsoft[0/1] Supersoft source flagmeta.codeintisYSN[0/1] Possible association with a young supernova remnantmeta.codeintisSNR[0/1] Possbile association with a supernova remnantmeta.codeintisNova[0/1] Possible association with a novameta.codeint_RAPosition from CXOGSG name (right ascension part)degpos.eq.ra;meta.main_DEPosition from CXOGSG name (declination part)degpos.eq.dec;meta.main