J/A+A/685/A97ivo://CDS.VizieR/J/A+A/685/A97doi:10.26093/cds/vizier.36850097CDSPouliasis E.Ruiz A.Georgantopoulos I.Vito F.Gilli R.Vignali C.,Ueda Y.Koulouridis E.Akiyama M.Marchesi S.Laloux B.Nagao T.,Paltani S.Pierre M.Toba Y.Habouzit M.Vijarnwannaluk B.Garrel C.2024-11-07T20:03:35Z2024-05-15T08:56:02ZCDS support team

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

cds-question@unistra.fractive-galactic-nucleiredshiftedx-ray-sourcesThe X-ray luminosity function (XLF) of active galactic nuclei (AGN) of fers a robust tool to study the evolution and the growth of the super-massive black-hole population over cosmic time. Owing to the limited area probed by X-ray surveys, optical surveys are routinely used to probe the accretion in the high redshift Universe z>=3. However, optical surveys may be incomplete because they are strongly affected by dust redenning. In this work, we derive the XLF and its evolution at high redshifts (z>=3) using a large sample of AGNs selected in different fields with various areas and depths covering a wide range of luminosities. Additionally, we put the tightest yet constraints on the absorption function in this redshift regime. In particular, we use more than 600 soft X-ray selected (0.5-2keV) high-z sources in the Chandra Deep fields, the Chandra COSMOS Legacy survey and the XMM-XXL northern field. We derive the X-ray spectral properties for all sources via spectral fitting, using a consistent technique and model. For modeling the parametric form of the XLF and the absorption function, we use a Bayesian methodology allowing us to correctly propagate the uncertainties for the observed X-ray properties of our sources and also the absorption effects. The evolution of XLF is in agreement with a pure density evolution model similar to what is witnessed at optical wavelengths, although a luminosity dependent density evolution model cannot be securely ruled out. A large fraction (~60%) of our sources are absorbed by column densities of N_H_>=10^23^cm^-2^, while ~17% of the sources are Compton-thick. Our results favor a scenario where both the interstellar medium of the host and the AGN torus contribute to the obscuration. The derived black hole accretion rate density is roughly in agreement with the large-scale cosmological hydro-dynamical simulations, if one takes into account the results that the X-ray AGN are hosted by massive galaxies, while it differs from the one derived using JWST data. The latter could be due to the differences in the AGN and host-galaxy properties2024A&A...685A..97Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/685/A97CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJS/184/158 : Chandra COSMOS survey I. (Elvis+, 2009)J/ApJS/224/15 : Improved 2Ms and 250ks Chandra catalogs (Xue+, 2016)J/ApJ/819/62 : The COSMOS-Legacy Survey (CLS) catalog (Civano+, 2016)J/ApJS/228/2 : Chandra Deep Field-South survey: 7Ms sources (Luo+, 2017)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/685/A97https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/685/A97http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/685/A97https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/685/A97https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/685/A97http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/685/A97GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/685/A97/catalog (Main properties of high-z sources)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/685/A97/catalog?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/685/A97/catalog?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/685/A97/catalog?GETtext/xml+votable180.050000true30.04913611-5.148118890.0055555555555555565/4419 4421-4425 4428 6814 6/11252 17503 17525 17674-17675 17681-17683 17705 17708 17716-17717 17730 27245 27247 27344 35935 35957 36798https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/685/A97?format=asciiX-raydefaultJ/A+A/685/A97/catalogMain properties of high-z sourcesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFieldField (1)meta.id;obs.fieldcharIDUnique Identifier in each field (2)meta.id;meta.maincharRAJ2000X-ray right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000X-ray declination (J2000)degpos.eq.dec;meta.mainzRedshiftsrc.redshiftfloatf_z[0/1] Redshift flag: 0 for photo-z, 1 for spec-zmeta.codeintP(z>3)Probability of a sources being at z>3 according to PDF(z)stat.fit.goodnessfloatlogNHHydrogen column density in logarithmic scalelog(cm**-2)phys.columnDensityfloate_logNHHydrogen column density in logarithmic scale lower errorlog(cm**-2)stat.errorfloatE_logNHHydrogen column density in logarithmic scale upper errorlog(cm**-2)stat.error;stat.maxfloatlogFXFlux in 0.5-2 keV band in logarithmic scalelog(mW.m**-2)phot.flux;em.X-rayfloate_logFXFlux in 0.5-2 keV band in logarithmic scale lower errorlog(mW.m**-2)stat.errorfloatE_logFXFlux in 0.5-2 keV band in logarithmic scale upper errorlog(mW.m**-2)stat.error;stat.maxfloatlogLXLuminosity in 2-10 keV band in logarithmic scalelog(1e-07J)phys.luminosity;em.X-rayfloate_logLXLuminosity in 2-10 keV band in logarithmic scale lower errorlog(1e-07J)stat.errorfloatE_logLXLuminosity in 2-10 keV band in logarithmic scale upper errorlog(1e-07J)stat.error;stat.maxfloat