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dc.contributor.authorRosario, D.J.
dc.contributor.authorMcIntosh, D.H.
dc.contributor.authorVan Der Wel, A.
dc.contributor.authorKartaltepe, J.
dc.contributor.authorLang, P.
dc.contributor.authorSantini, P.
dc.contributor.authorWuyts, S.
dc.contributor.authorLutz, D.
dc.contributor.authorRafelski, M.
dc.contributor.authorVillforth, C.
dc.contributor.authorAlexander, D.M.
dc.contributor.authorBauer, F.E.
dc.contributor.authorBell, E.F.
dc.contributor.authorBerta, S.
dc.contributor.authorBrandt, W.N.
dc.contributor.authorConselice, C.J.
dc.contributor.authorDekel, A.
dc.contributor.authorFaber, S.M.
dc.contributor.authorFerguson, H.C.
dc.contributor.authorGenzel, R.
dc.contributor.authorGrogin, N.A.
dc.contributor.authorKocevski, D.D.
dc.contributor.authorKoekemoer, A.M.
dc.contributor.authorKoo, D.C.
dc.contributor.authorLotz, J.M.
dc.contributor.authorMagnelli, B.
dc.contributor.authorMaiolino, R.
dc.contributor.authorMozena, M.
dc.contributor.authorMullaney, J.R.
dc.contributor.authorPapovich, C.J.
dc.contributor.authorPopesso, P.
dc.contributor.authorTacconi, L.J.
dc.contributor.authorTrump, J.R.
dc.contributor.authorAvadhuta, S.
dc.contributor.authorBassett, R.
dc.contributor.authorBell, A.
dc.contributor.authorBernyk, M.
dc.contributor.authorBournaud, F.
dc.contributor.authorCassata, P.
dc.contributor.authorCheung, E.
dc.contributor.authorCroton, D.
dc.contributor.authorDonley, J.
dc.contributor.authorDegroot, L.
dc.contributor.authorGuedes, J.
dc.contributor.authorHathi, N.
dc.contributor.authorHerrington, J.
dc.contributor.authorHilton, M.
dc.contributor.authorLai, K.
dc.contributor.authorLani, C.
dc.contributor.authorMartig, M.
dc.contributor.authorMcGrath, E.
dc.contributor.authorMutch, S.
dc.contributor.authorMortlock, A.
dc.contributor.authorMcPartland, C.
dc.contributor.authorO'Leary, E.
dc.contributor.authorPeth, M.
dc.contributor.authorPillepich, A.
dc.contributor.authorPoole, G.
dc.contributor.authorSnyder, D.
dc.contributor.authorStraughn, A.
dc.contributor.authorTelford, O.
dc.contributor.authorTonini, C.
dc.contributor.authorWandro, P.
dc.date.accessioned2015-01-14T15:01:02Z
dc.date.available2015-01-14T15:01:02Z
dc.date.issued2015-01
dc.identifier.citationRosario , D J , McIntosh , D H , Van Der Wel , A , Kartaltepe , J , Lang , P , Santini , P , Wuyts , S , Lutz , D , Rafelski , M , Villforth , C , Alexander , D M , Bauer , F E , Bell , E F , Berta , S , Brandt , W N , Conselice , C J , Dekel , A , Faber , S M , Ferguson , H C , Genzel , R , Grogin , N A , Kocevski , D D , Koekemoer , A M , Koo , D C , Lotz , J M , Magnelli , B , Maiolino , R , Mozena , M , Mullaney , J R , Papovich , C J , Popesso , P , Tacconi , L J , Trump , J R , Avadhuta , S , Bassett , R , Bell , A , Bernyk , M , Bournaud , F , Cassata , P , Cheung , E , Croton , D , Donley , J , Degroot , L , Guedes , J , Hathi , N , Herrington , J , Hilton , M , Lai , K , Lani , C , Martig , M , McGrath , E , Mutch , S , Mortlock , A , McPartland , C , O'Leary , E , Peth , M , Pillepich , A , Poole , G , Snyder , D , Straughn , A , Telford , O , Tonini , C & Wandro , P 2015 , ' The host galaxies of X-ray selected active galactic nuclei to z = 2.5 : structure, star formation, and their relationships from CANDELS and Herschel/PACS ' , Astronomy & Astrophysics , vol. 573 , A85 . https://doi.org/10.1051/0004-6361/201423782en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 161865457
dc.identifier.otherPURE UUID: f72b8c83-ece2-4deb-9170-62f0eefcc662
dc.identifier.otherScopus: 84919781916
dc.identifier.otherWOS: 000346901300013
dc.identifier.urihttps://hdl.handle.net/10023/5994
dc.description.abstractWe study the relationship between the structure and star formation rate (SFR) of X-ray selected low and moderate luminosity active galactic nuclei (AGNs) in the two Chandra Deep Fields, using Hubble Space Telescope imaging from the Cosmic Assembly Near Infrared Extragalactic Legacy Survey (CANDELS) and deep far-infrared maps from the PEP+GOODS-Herschel survey. We derive detailed distributions of structural parameters and FIR luminosities from carefully constructed control samples of galaxies, which we then compare to those of the AGNs. At z ~ 1, AGNs show slightly diskier light profiles than massive inactive (non-AGN) galaxies, as well as modestly higher levels of gross galaxy disturbance (as measured by visual signatures of interactions and clumpy structure). In contrast, at z ~ 2, AGNs show similar levels of galaxy disturbance as inactive galaxies, but display a red central light enhancement, which may arise from a more pronounced bulge in AGN hosts or extinguished nuclear light. We undertake a number of tests of both these alternatives, but our results do not strongly favor one interpretation over the other. The mean SFR and its distribution among AGNs and inactive galaxies are similar at z> 1.5. At z<1, however, clear and significant enhancements are seen in the SFRs of AGNs with bulge-dominated light profiles. These trends suggest an evolution in the relation between nuclear activity and host properties with redshift, towards a minor role for mergers and interactions at z> 1.5.
dc.format.extent24
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsReproduced with permission from Astronomy & Astrophysics, © ESO 2014en
dc.subjectGalaxies: activeen
dc.subjectGalaxies: structureen
dc.subjectGalaxies: star formationen
dc.subjectSurveysen
dc.subjectMethods: statisticalen
dc.subjectX-rays: galaxiesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe host galaxies of X-ray selected active galactic nuclei to z = 2.5 : structure, star formation, and their relationships from CANDELS and Herschel/PACSen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201423782
dc.description.statusPeer revieweden
dc.identifier.urlhttp://www.aanda.org/articles/aa/olm/2015/01/aa23782-14/aa23782-14.htmlen


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