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dc.contributor.authorHickox, Ryan C.
dc.contributor.authorJones, Christine
dc.contributor.authorForman, William R.
dc.contributor.authorMurray, Stephen
dc.contributor.authorKochanek, Christopher S.
dc.contributor.authorEisenstein, Daniel
dc.contributor.authorJannuzi, Buell T.
dc.contributor.authorDey, Arjun
dc.contributor.authorBrown, Michael J. I.
dc.contributor.authorStern, Daniel
dc.contributor.authorEisenhardt, Peter R.
dc.contributor.authorGorjian, Varoujan
dc.contributor.authorBrodwin, Mark
dc.contributor.authorNarayan, Ramesh
dc.contributor.authorCool, Richard J.
dc.contributor.authorKenter, Almus
dc.contributor.authorCaldwell, Nelson
dc.contributor.authorAnderson, Michael E.
dc.date.accessioned2016-04-12T17:30:01Z
dc.date.issued2009
dc.identifier.citationHickox, Ryan C., Christine Jones, William R. Forman, Stephen S. Murray, Christopher S. Kochanek, Daniel Eisenstein, Buell T. Jannuzi, et al. 2009. “Host Galaxies, Clustering, Eddington Ratios, and Evolution of Radio, X-Ray, and Infrared-selected AGNs." The Astrophysical Journal 696 (1) (April 21): 891–919. doi:10.1088/0004-637x/696/1/891.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:26526400
dc.description.abstractWe explore the connection between different classes of active galactic nuclei (AGNs) and the evolution of their host galaxies, by deriving host galaxy properties, clustering, and Eddington ratios of AGNs selected in the radio, Xray, and infrared (IR) wavebands. We study a sample of 585 AGNs at 0.25 <z< 0.8 using redshifts from the AGN and Galaxy Evolution Survey (AGES). We select AGNs with observations in the radio at 1.4 GHz from the Westerbork Synthesis Radio Telescope, X-rays from the Chandra XBootes Survey, and mid-IR from ¨ the Spitzer IRAC Shallow Survey. The radio, X-ray, and IR AGN samples show only modest overlap, indicating that to the flux limits of the survey, they represent largely distinct classes of AGNs. We derive host galaxy colors and luminosities, as well as Eddington ratios, for obscured or optically faint AGNs. We also measure the two-point cross-correlation between AGNs and galaxies on scales of 0.3–10 h−1 Mpc, and derive typical dark matter halo masses. We find that: (1) radio AGNs are mainly found in luminous red sequence galaxies, are strongly clustered (with Mhalo ∼ 3 × 1013 h−1 M), and have very low Eddington ratios λ 10−3; (2) X-ray-selected AGNs are preferentially found in galaxies that lie in the “green valley” of color–magnitude space and are clustered similar to the typical AGES galaxies (Mhalo ∼ 1013 h−1 M), with 10−3 λ 1; (3) IR AGNs reside in slightly bluer, slightly less luminous galaxies than X-ray AGNs, are weakly clustered (Mhalo 1012h−1 M), and have λ > 10−2. We interpret these results in terms of a simple model of AGN and galaxy evolution, whereby a “quasar” phase and the growth of the stellar bulge occurs when a galaxy’s dark matter halo reaches a critical mass between ∼ 1012 and 1013 M. After this event, star formation ceases and AGN accretion shifts from radiatively efficient (optical- and IR-bright) to radiatively inefficient (optically faint, radio-bright) modes. Keen_US
dc.description.sponsorshipAstronomyen_US
dc.language.isoen_USen_US
dc.publisherIOP Publishingen_US
dc.relation.isversionofdoi::10.1088/0004-637X/696/1/891en_US
dc.relation.hasversionhttp://arxiv.org/pdf/0901.4121v2.pdfen_US
dash.licenseLAA
dc.subjectgalaxies: activeen_US
dc.subjectlarge-scale structure of universeen_US
dc.subjectquasars: generalen_US
dc.subjectradio continuum: galaxiesen_US
dc.subjectsurveysen_US
dc.subjectX-rays: galaxiesen_US
dc.titleHost Galaxies, Clustering, Eddington Ratios, and Evolution of Radio, X-Ray, and Infrared-selected AGNs.en_US
dc.typeJournal Articleen_US
dc.description.versionVersion of Recorden_US
dc.relation.journalApJen_US
dash.depositing.authorNarayan, Ramesh
dc.date.available2016-04-12T17:30:01Z
dc.identifier.doi10.1088/0004-637X/696/1/891*
dash.authorsorderedfalse
dash.contributor.affiliatedKenter, Almus
dash.contributor.affiliatedCaldwell, Nelson
dash.contributor.affiliatedNarayan, Ramesh
dash.contributor.affiliatedForman, William
dash.contributor.affiliatedMurray, Stephen


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