X-ray constraints on the fraction of obscured active galactic nuclei at high accretion luminosities

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dc.contributor.authorGeorgakakis, A.
dc.contributor.authorSalvato, M.
dc.contributor.authorLiu, Z.
dc.contributor.authorBuchner, J.
dc.contributor.authorBrandt, W. N.
dc.contributor.authorAnanna, T. Tasnim
dc.contributor.authorSchulze, A.
dc.contributor.authorShen, Yue
dc.contributor.authorLaMassa, S.
dc.contributor.authorNandra, K.
dc.contributor.authorMerloni, A.
dc.contributor.authorMcGreer, I. D.
dc.date.accessioned2024-01-10T13:44:15Z
dc.date.available2024-01-10T13:44:15Z
dc.date.issued2017
dc.description.abstractThe wide-area XMM-XXL X-ray survey is used to explore the fraction of obscured active galactic nuclei (AGNs) at high accretion luminosities, L-X(2-10 keV) greater than or similar to 10(44) erg s(-1), and out to redshift z approximate to 1.5. The sample covers an area of about 14 deg(2) and provides constraints on the space density of powerful AGNs over a wide range of neutral hydrogen column densities extending beyond the Compton-thick limit, N-H approximate to 10(24) cm(-2). The fraction of obscured Compton-thin (N-H = 10(22) - 10(24) cm(-2)) AGNs is estimated to be approximate to 0.35 for luminosities L-X(2-10 keV) > 10(44) erg s(-1), independent of redshift. For less luminous sources, the fraction of obscured Compton-thin AGNs increases from 0.45 +/- 0.10 at z = 0.25 to 0.75 +/- 0.05 at z = 1.25. Studies that select AGNs in the infrared via template fits to the observed spectral energy distribution of extragalactic sources estimate space densities at high accretion luminosities consistent with the XMM-XXL constraints. There is no evidence for a large population of AGNs (e.g. heavily obscured) identified in the infrared and missed at X-ray wavelengths. We further explore the mid-infrared colours of XMM-XXL AGNs as a function of accretion luminosity, column density and redshift. The fraction of XMM-XXL sources that lie within the mid-infrared colour wedges defined in the literature to select AGNs is primarily a function of redshift. This fraction increases from about 20-30 per cent at z = 0.25 to about 50-70 per cent at z = 1.5.
dc.description.funderTHALES - European Union
dc.description.funderGreek Government of the programme 'Education and lifelong learning'
dc.description.funderFONDECYT Postdoctorados
dc.description.funderMinistry of Economy, Development, and Tourism's Millennium Science Initiative
dc.description.funderMillennium Institute of Astro-physics MAS
dc.description.funderAlfred P. Sloan Foundation
dc.description.funderNational Science Foundation
dc.description.funderU.S. Department of Energy Office of Science
dc.description.funderUniversity of Arizona
dc.description.funderBrazilian Participation Group
dc.description.funderBrookhaven National Laboratory
dc.description.funderCarnegie Mellon University
dc.description.funderUniversity of Florida
dc.description.funderFrench Participation Group
dc.description.funderGerman Participation Group
dc.description.funderHarvard University
dc.description.funderInstituto de Astrofisica de Canarias
dc.description.funderMichigan State/Notre Dame/JINA Participation Group
dc.description.funderJohns Hopkins University
dc.description.funderLawrence Berkeley National Laboratory
dc.description.funderMax Planck Institute for Astrophysics
dc.description.funderMax Planck Institute for Extraterrestrial Physics
dc.description.funderNew Mexico State University
dc.description.funderNew York University
dc.description.funderOhio State University
dc.description.funderPennsylvania State University
dc.description.funderUniversity of Portsmouth
dc.description.funderPrinceton University
dc.description.funderSpanish Participation Group
dc.description.funderUniversity of Tokyo
dc.description.funderUniversity of Utah
dc.description.funderVanderbilt University
dc.description.funderUniversity of Virginia
dc.description.funderUniversity of Washington
dc.description.funderYale University
dc.description.funderDirect For Mathematical & Physical Scien
dc.fechaingreso.objetodigital2024-04-29
dc.format.extent20 páginas
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stx953
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stx953
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/78875
dc.identifier.wosidWOS:000406836200050
dc.information.autorucFísica;Buchner J ;S/I;1018064
dc.issue.numero3
dc.language.isoen
dc.nota.accesocontenido parcial
dc.pagina.final3251
dc.pagina.inicio3232
dc.publisherOXFORD UNIV PRESS
dc.revistaMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
dc.rightsacceso restringido
dc.subjectgalaxies: active
dc.subjectquasars: general
dc.subjectquasars: supermassive black holes
dc.subjectgalaxies: Seyfert
dc.subjectX-rays: diffuse background
dc.subjectABSORPTION-LINE QUASARS
dc.subjectSUPERMASSIVE BLACK-HOLES
dc.subjectNUSTAR EXTRAGALACTIC SURVEY
dc.subjectSTAR-FORMING GALAXIES
dc.subjectPHOTON IMAGING CAMERA
dc.subjectCOMPTON-THICK AGN
dc.subjectXMM-NEWTON
dc.subjectPHOTOMETRIC REDSHIFTS
dc.subjectSPECTROSCOPIC SURVEY
dc.subjectLEGACY SURVEY
dc.titleX-ray constraints on the fraction of obscured active galactic nuclei at high accretion luminosities
dc.typeartículo
dc.volumen469
sipa.codpersvinculados1018064
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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