AGN-host galaxy connection: morphology and colours of X-ray selected AGN at z ≤ 2
Identifieur interne : 004D15 ( PascalFrancis/Curation ); précédent : 004D14; suivant : 004D16AGN-host galaxy connection: morphology and colours of X-ray selected AGN at z ≤ 2
Auteurs : M. Povic [Espagne, Afrique du Sud] ; M. Sanchez-Portal [Espagne] ; A. M. Perez Garcia [Espagne] ; A. Bongiovanni [Espagne] ; J. Cepa [Espagne] ; M. Huertas-Company [France] ; M. A. Lara-Lopez [Espagne, Australie] ; M. Fernandez Lorenzo [Espagne] ; A. Ederoclite [Espagne] ; E. Alfaro [Espagne] ; H. Castaneda [Mexique] ; J. Gallego [Espagne] ; J. I. Gonzalez-Serrano [Espagne] ; J. J. Gonzalez [Mexique]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.
Descripteurs français
- Pascal (Inist)
- Noyau galactique actif, Galaxies type avancé, Morphologie, Couleur, Déplacement vers le rouge, Classification, Diagramme magnitude couleur, Corrélation, Modèle, Bulbe galaxies, Masse stellaire, Luminosité, Formation stellaire, Boucle réaction, Galaxies elliptiques, Galaxies lenticulaires, Population stellaire, Simulation numérique, Quasar, Galaxies actives, Structure galaxies, Galaxies RX, Noyau galaxies, Source RX cosmique.
- Wicri :
- topic : Classification.
English descriptors
- KwdEn :
- Active galaxies, Active galaxy nuclei, Classification, Color, Color-magnitude diagrams, Correlations, Cosmic x-ray sources, Digital simulation, Elliptical galaxies, Feedback, Galaxy bulge, Galaxy nuclei, Galaxy structure, Late type galaxies, Lenticular galaxies, Luminosity, Models, Morphology, Quasars, Red shift, Star formation, Stellar mass, Stellar population, X-ray galaxies.
Abstract
Context. The connection between active galactic nuclei (AGN) and their host galaxies has been widely studied and found to be of great importance for providing answers to some fundamental questions related to AGN fuelling mechanisms, and both their formation and evolution. Aims. Using X-ray data and one of the deepest broad-band optical data sets available, we study how morphology and colours are related to X-ray properties for sources at redshifts z ≤ 2.0, using a sample of 262 AGN in the Subaru/XMM-Newton Deep Survey (SXDS). Methods. We performed our morphological classification using the galSVM code, which is a new method that is particularly suited to dealing with high-redshift sources. Colour-magnitude diagrams were studied in relationship to redshift, morphology, X-ray obscuration, and X-ray-to-optical flux ratio. We analysed the different regions in the colour-magnitude diagrams, and searched for correlations with the observed properties of AGN populations using models of their formation and evolution. Results. We confirm that a robust and reliable morphological classification of a general galaxy population at high redshift should be based on a multi-parametric approach. At least 50% of X-ray detected AGN at z ≤ 2.0 analysed in this work reside in spheroidal and bulge-dominated galaxies, while at least 18% have disk-dominated hosts. This suggests that different mechanisms may be responsible for triggering the nuclear activity. When analysing populations of X-ray detected AGN in both colour-magnitude and colour-stellar mass diagrams, the highest number of sources is found to reside in the green valley at redshifts ≃0.5-1.5. However, a larger number of low-luminosity AGN have been detected than in previous works owing to the substantial depth of the SXDS optical data. Whether AGN are hosted by early- or late-type galaxies, no clear relationship has been found with the optical colours (independently of redshift), as is typical of normal galaxies. Both early- and late-type AGN cover similar ranges of X-ray obscuration, for both unobscured and obscured sources. Conclusions. Our findings appear to confirm some previous suggestions that X-ray selected AGN residing in the green valley represent a transitional population, quenching star formation by means of different AGN feedback mechanisms and evolving to red-sequence galaxies. They might be hosted by similar sources (the majority of sources being late-type elliptical and lenticular galaxies, and early-type spirals) with similar stellar populations, which are triggered mainly by major and/or minor mergers, and in some cases by means of secular mechanism, as shown in previous numerical simulations. In the aforementioned transition we observe different phases of AGN activity, with some AGN being in the "QSO-mode" detected as compact, blue, and unobscured in X-rays, and with others passing through different phases before and after the "QSO-mode", being obscured and unobscured in X-rays, respectively.
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Povic</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Astrophysics and Cosmology Research Unit (ACRU), School of Mathematical Sciences, University of Kwa-Zulu Natal (UKZN)</s1><s2>Durban</s2><s3>ZAF</s3><sZ>1 aut.</sZ></inist:fA14><country>Afrique du Sud</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Instituto de Astrofísica de Andalucía (IAA-CSIC)</s1><s2>Granada</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>8 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Sanchez Portal, M" sort="Sanchez Portal, M" uniqKey="Sanchez Portal M" first="M." last="Sanchez-Portal">M. 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Fernandez Lorenzo</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Instituto de Astrofísica de Andalucía (IAA-CSIC)</s1><s2>Granada</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>8 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Ederoclite, A" sort="Ederoclite, A" uniqKey="Ederoclite A" first="A." last="Ederoclite">A. Ederoclite</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Centro de Estudios de Física del Cosmos de Aragón (CEFCA)</s1><s2>Teruel</s2><s3>ESP</s3><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Alfaro, E" sort="Alfaro, E" uniqKey="Alfaro E" first="E." last="Alfaro">E. Alfaro</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Instituto de Astrofísica de Andalucía (IAA-CSIC)</s1><s2>Granada</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>8 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Castaneda, H" sort="Castaneda, H" uniqKey="Castaneda H" first="H." last="Castaneda">H. Castaneda</name><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>Escuela Superior de Física y Matemáticas, Intituto Politécnico Nacional (IPN)</s1><s2>Mexico D.F.</s2><s3>MEX</s3><sZ>11 aut.</sZ></inist:fA14><country>Mexique</country></affiliation></author><author><name sortKey="Gallego, J" sort="Gallego, J" uniqKey="Gallego J" first="J." last="Gallego">J. Gallego</name><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Departamento de Astrofísica y CC. de la Atmósfera, Universidad Complutense de Madrid</s1><s2>Madrid</s2><s3>ESP</s3><sZ>12 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Gonzalez Serrano, J I" sort="Gonzalez Serrano, J I" uniqKey="Gonzalez Serrano J" first="J. I." last="Gonzalez-Serrano">J. I. Gonzalez-Serrano</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Instituto de Ffsica de Cantabria, CSIC-Universidad de Cantabria</s1><s2>Santander</s2><s3>ESP</s3><sZ>13 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Gonzalez, J J" sort="Gonzalez, J J" uniqKey="Gonzalez J" first="J. J." last="Gonzalez">J. J. Gonzalez</name><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Instituto de Astronomía UNAM</s1><s2>Mexico D.F.</s2><s3>MEX</s3><sZ>14 aut.</sZ></inist:fA14><country>Mexique</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">12-0321771</idno><date when="2012">2012</date><idno type="stanalyst">PASCAL 12-0321771 INIST</idno><idno type="RBID">Pascal:12-0321771</idno><idno type="wicri:Area/PascalFrancis/Corpus">001202</idno><idno type="wicri:Area/PascalFrancis/Curation">004D15</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">AGN-host galaxy connection: morphology and colours of X-ray selected AGN at z ≤ 2</title><author><name sortKey="Povic, M" sort="Povic, M" uniqKey="Povic M" first="M." last="Povic">M. Povic</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Astrophysics and Cosmology Research Unit (ACRU), School of Mathematical Sciences, University of Kwa-Zulu Natal (UKZN)</s1><s2>Durban</s2><s3>ZAF</s3><sZ>1 aut.</sZ></inist:fA14><country>Afrique du Sud</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Instituto de Astrofísica de Andalucía (IAA-CSIC)</s1><s2>Granada</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>8 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Sanchez Portal, M" sort="Sanchez Portal, M" uniqKey="Sanchez Portal M" first="M." last="Sanchez-Portal">M. Sanchez-Portal</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Herschel Science Centre (HSC), European Space Agency Centre (ESAC)/INSA</s1><s2>Villanueva de la Cañada, Madrid</s2><s3>ESP</s3><sZ>2 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Asociacion ASPID, Apartado de Correos 412</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Perez Garcia, A M" sort="Perez Garcia, A M" uniqKey="Perez Garcia A" first="A. M." last="Perez Garcia">A. M. Perez Garcia</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Asociacion ASPID, Apartado de Correos 412</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Departamento de Astrofísica, Universidad de La Laguna (ULL)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Bongiovanni, A" sort="Bongiovanni, A" uniqKey="Bongiovanni A" first="A." last="Bongiovanni">A. Bongiovanni</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Asociacion ASPID, Apartado de Correos 412</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Departamento de Astrofísica, Universidad de La Laguna (ULL)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Cepa, J" sort="Cepa, J" uniqKey="Cepa J" first="J." last="Cepa">J. Cepa</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Asociacion ASPID, Apartado de Correos 412</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Huertas Company, M" sort="Huertas Company, M" uniqKey="Huertas Company M" first="M." last="Huertas-Company">M. Huertas-Company</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>GEPI, Paris-Meudon Observatory</s1><s2>Meudon</s2><s3>FRA</s3><sZ>6 aut.</sZ></inist:fA14><country>France</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>University of Paris</s1><s2>Paris</s2><s3>FRA</s3><sZ>6 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Lara Lopez, M A" sort="Lara Lopez, M A" uniqKey="Lara Lopez M" first="M. A." last="Lara-Lopez">M. A. Lara-Lopez</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Australian Astronomical Observatory, PO Box 296</s1><s2>Epping NSW 1710</s2><s3>AUS</s3><sZ>7 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Fernandez Lorenzo, M" sort="Fernandez Lorenzo, M" uniqKey="Fernandez Lorenzo M" first="M." last="Fernandez Lorenzo">M. Fernandez Lorenzo</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Instituto de Astrofísica de Andalucía (IAA-CSIC)</s1><s2>Granada</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>8 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Ederoclite, A" sort="Ederoclite, A" uniqKey="Ederoclite A" first="A." last="Ederoclite">A. Ederoclite</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Centro de Estudios de Física del Cosmos de Aragón (CEFCA)</s1><s2>Teruel</s2><s3>ESP</s3><sZ>9 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Alfaro, E" sort="Alfaro, E" uniqKey="Alfaro E" first="E." last="Alfaro">E. Alfaro</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Instituto de Astrofísica de Andalucía (IAA-CSIC)</s1><s2>Granada</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>8 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Castaneda, H" sort="Castaneda, H" uniqKey="Castaneda H" first="H." last="Castaneda">H. Castaneda</name><affiliation wicri:level="1"><inist:fA14 i1="11"><s1>Escuela Superior de Física y Matemáticas, Intituto Politécnico Nacional (IPN)</s1><s2>Mexico D.F.</s2><s3>MEX</s3><sZ>11 aut.</sZ></inist:fA14><country>Mexique</country></affiliation></author><author><name sortKey="Gallego, J" sort="Gallego, J" uniqKey="Gallego J" first="J." last="Gallego">J. Gallego</name><affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Departamento de Astrofísica y CC. de la Atmósfera, Universidad Complutense de Madrid</s1><s2>Madrid</s2><s3>ESP</s3><sZ>12 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Gonzalez Serrano, J I" sort="Gonzalez Serrano, J I" uniqKey="Gonzalez Serrano J" first="J. I." last="Gonzalez-Serrano">J. I. Gonzalez-Serrano</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Instituto de Ffsica de Cantabria, CSIC-Universidad de Cantabria</s1><s2>Santander</s2><s3>ESP</s3><sZ>13 aut.</sZ></inist:fA14><country>Espagne</country></affiliation></author><author><name sortKey="Gonzalez, J J" sort="Gonzalez, J J" uniqKey="Gonzalez J" first="J. J." last="Gonzalez">J. J. Gonzalez</name><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Instituto de Astronomía UNAM</s1><s2>Mexico D.F.</s2><s3>MEX</s3><sZ>14 aut.</sZ></inist:fA14><country>Mexique</country></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2012">2012</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Active galaxies</term><term>Active galaxy nuclei</term><term>Classification</term><term>Color</term><term>Color-magnitude diagrams</term><term>Correlations</term><term>Cosmic x-ray sources</term><term>Digital simulation</term><term>Elliptical galaxies</term><term>Feedback</term><term>Galaxy bulge</term><term>Galaxy nuclei</term><term>Galaxy structure</term><term>Late type galaxies</term><term>Lenticular galaxies</term><term>Luminosity</term><term>Models</term><term>Morphology</term><term>Quasars</term><term>Red shift</term><term>Star formation</term><term>Stellar mass</term><term>Stellar population</term><term>X-ray galaxies</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Noyau galactique actif</term><term>Galaxies type avancé</term><term>Morphologie</term><term>Couleur</term><term>Déplacement vers le rouge</term><term>Classification</term><term>Diagramme magnitude couleur</term><term>Corrélation</term><term>Modèle</term><term>Bulbe galaxies</term><term>Masse stellaire</term><term>Luminosité</term><term>Formation stellaire</term><term>Boucle réaction</term><term>Galaxies elliptiques</term><term>Galaxies lenticulaires</term><term>Population stellaire</term><term>Simulation numérique</term><term>Quasar</term><term>Galaxies actives</term><term>Structure galaxies</term><term>Galaxies RX</term><term>Noyau galaxies</term><term>Source RX cosmique</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Classification</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Context. The connection between active galactic nuclei (AGN) and their host galaxies has been widely studied and found to be of great importance for providing answers to some fundamental questions related to AGN fuelling mechanisms, and both their formation and evolution. Aims. Using X-ray data and one of the deepest broad-band optical data sets available, we study how morphology and colours are related to X-ray properties for sources at redshifts z ≤ 2.0, using a sample of 262 AGN in the Subaru/XMM-Newton Deep Survey (SXDS). Methods. We performed our morphological classification using the galSVM code, which is a new method that is particularly suited to dealing with high-redshift sources. Colour-magnitude diagrams were studied in relationship to redshift, morphology, X-ray obscuration, and X-ray-to-optical flux ratio. We analysed the different regions in the colour-magnitude diagrams, and searched for correlations with the observed properties of AGN populations using models of their formation and evolution. Results. We confirm that a robust and reliable morphological classification of a general galaxy population at high redshift should be based on a multi-parametric approach. At least 50% of X-ray detected AGN at z ≤ 2.0 analysed in this work reside in spheroidal and bulge-dominated galaxies, while at least 18% have disk-dominated hosts. This suggests that different mechanisms may be responsible for triggering the nuclear activity. When analysing populations of X-ray detected AGN in both colour-magnitude and colour-stellar mass diagrams, the highest number of sources is found to reside in the green valley at redshifts ≃0.5-1.5. However, a larger number of low-luminosity AGN have been detected than in previous works owing to the substantial depth of the SXDS optical data. Whether AGN are hosted by early- or late-type galaxies, no clear relationship has been found with the optical colours (independently of redshift), as is typical of normal galaxies. Both early- and late-type AGN cover similar ranges of X-ray obscuration, for both unobscured and obscured sources. Conclusions. Our findings appear to confirm some previous suggestions that X-ray selected AGN residing in the green valley represent a transitional population, quenching star formation by means of different AGN feedback mechanisms and evolving to red-sequence galaxies. They might be hosted by similar sources (the majority of sources being late-type elliptical and lenticular galaxies, and early-type spirals) with similar stellar populations, which are triggered mainly by major and/or minor mergers, and in some cases by means of secular mechanism, as shown in previous numerical simulations. In the aforementioned transition we observe different phases of AGN activity, with some AGN being in the "QSO-mode" detected as compact, blue, and unobscured in X-rays, and with others passing through different phases before and after the "QSO-mode", being obscured and unobscured in X-rays, respectively.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-6361</s0></fA01><fA02 i1="01"><s0>AAEJAF</s0></fA02><fA03 i2="1"><s0>Astron. astrophys. : (Berl., Print)</s0></fA03><fA05><s2>541</s2></fA05><fA06><s3>p. 2</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>AGN-host galaxy connection: morphology and colours of X-ray selected AGN at z ≤ 2</s1></fA08><fA11 i1="01" i2="1"><s1>POVIC (M.)</s1></fA11><fA11 i1="02" i2="1"><s1>SANCHEZ-PORTAL (M.)</s1></fA11><fA11 i1="03" i2="1"><s1>PEREZ GARCIA (A. M.)</s1></fA11><fA11 i1="04" i2="1"><s1>BONGIOVANNI (A.)</s1></fA11><fA11 i1="05" i2="1"><s1>CEPA (J.)</s1></fA11><fA11 i1="06" i2="1"><s1>HUERTAS-COMPANY (M.)</s1></fA11><fA11 i1="07" i2="1"><s1>LARA-LOPEZ (M. A.)</s1></fA11><fA11 i1="08" i2="1"><s1>FERNANDEZ LORENZO (M.)</s1></fA11><fA11 i1="09" i2="1"><s1>EDEROCLITE (A.)</s1></fA11><fA11 i1="10" i2="1"><s1>ALFARO (E.)</s1></fA11><fA11 i1="11" i2="1"><s1>CASTANEDA (H.)</s1></fA11><fA11 i1="12" i2="1"><s1>GALLEGO (J.)</s1></fA11><fA11 i1="13" i2="1"><s1>GONZALEZ-SERRANO (J. I.)</s1></fA11><fA11 i1="14" i2="1"><s1>GONZALEZ (J. J.)</s1></fA11><fA14 i1="01"><s1>Instituto de Astrofísica de Canarias (IAC)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>9 aut.</sZ></fA14><fA14 i1="02"><s1>Astrophysics and Cosmology Research Unit (ACRU), School of Mathematical Sciences, University of Kwa-Zulu Natal (UKZN)</s1><s2>Durban</s2><s3>ZAF</s3><sZ>1 aut.</sZ></fA14><fA14 i1="03"><s1>Instituto de Astrofísica de Andalucía (IAA-CSIC)</s1><s2>Granada</s2><s3>ESP</s3><sZ>1 aut.</sZ><sZ>8 aut.</sZ><sZ>10 aut.</sZ></fA14><fA14 i1="04"><s1>Herschel Science Centre (HSC), European Space Agency Centre (ESAC)/INSA</s1><s2>Villanueva de la Cañada, Madrid</s2><s3>ESP</s3><sZ>2 aut.</sZ></fA14><fA14 i1="05"><s1>Asociacion ASPID, Apartado de Correos 412</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></fA14><fA14 i1="06"><s1>Departamento de Astrofísica, Universidad de La Laguna (ULL)</s1><s2>La Laguna, Tenerife</s2><s3>ESP</s3><sZ>3 aut.</sZ><sZ>4 aut.</sZ></fA14><fA14 i1="07"><s1>GEPI, Paris-Meudon Observatory</s1><s2>Meudon</s2><s3>FRA</s3><sZ>6 aut.</sZ></fA14><fA14 i1="08"><s1>University of Paris</s1><s2>Paris</s2><s3>FRA</s3><sZ>6 aut.</sZ></fA14><fA14 i1="09"><s1>Australian Astronomical Observatory, PO Box 296</s1><s2>Epping NSW 1710</s2><s3>AUS</s3><sZ>7 aut.</sZ></fA14><fA14 i1="10"><s1>Centro de Estudios de Física del Cosmos de Aragón (CEFCA)</s1><s2>Teruel</s2><s3>ESP</s3><sZ>9 aut.</sZ></fA14><fA14 i1="11"><s1>Escuela Superior de Física y Matemáticas, Intituto Politécnico Nacional (IPN)</s1><s2>Mexico D.F.</s2><s3>MEX</s3><sZ>11 aut.</sZ></fA14><fA14 i1="12"><s1>Departamento de Astrofísica y CC. de la Atmósfera, Universidad Complutense de Madrid</s1><s2>Madrid</s2><s3>ESP</s3><sZ>12 aut.</sZ></fA14><fA14 i1="13"><s1>Instituto de Ffsica de Cantabria, CSIC-Universidad de Cantabria</s1><s2>Santander</s2><s3>ESP</s3><sZ>13 aut.</sZ></fA14><fA14 i1="14"><s1>Instituto de Astronomía UNAM</s1><s2>Mexico D.F.</s2><s3>MEX</s3><sZ>14 aut.</sZ></fA14><fA20><s2>A118.1-A118.23</s2></fA20><fA21><s1>2012</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000508321540360</s5></fA43><fA44><s0>0000</s0><s1>© 2012 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1 p.</s0></fA45><fA47 i1="01" i2="1"><s0>12-0321771</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0></fA64><fA66 i1="01"><s0>FRA</s0></fA66><fC01 i1="01" l="ENG"><s0>Context. The connection between active galactic nuclei (AGN) and their host galaxies has been widely studied and found to be of great importance for providing answers to some fundamental questions related to AGN fuelling mechanisms, and both their formation and evolution. Aims. Using X-ray data and one of the deepest broad-band optical data sets available, we study how morphology and colours are related to X-ray properties for sources at redshifts z ≤ 2.0, using a sample of 262 AGN in the Subaru/XMM-Newton Deep Survey (SXDS). Methods. We performed our morphological classification using the galSVM code, which is a new method that is particularly suited to dealing with high-redshift sources. Colour-magnitude diagrams were studied in relationship to redshift, morphology, X-ray obscuration, and X-ray-to-optical flux ratio. We analysed the different regions in the colour-magnitude diagrams, and searched for correlations with the observed properties of AGN populations using models of their formation and evolution. Results. We confirm that a robust and reliable morphological classification of a general galaxy population at high redshift should be based on a multi-parametric approach. At least 50% of X-ray detected AGN at z ≤ 2.0 analysed in this work reside in spheroidal and bulge-dominated galaxies, while at least 18% have disk-dominated hosts. This suggests that different mechanisms may be responsible for triggering the nuclear activity. When analysing populations of X-ray detected AGN in both colour-magnitude and colour-stellar mass diagrams, the highest number of sources is found to reside in the green valley at redshifts ≃0.5-1.5. However, a larger number of low-luminosity AGN have been detected than in previous works owing to the substantial depth of the SXDS optical data. Whether AGN are hosted by early- or late-type galaxies, no clear relationship has been found with the optical colours (independently of redshift), as is typical of normal galaxies. Both early- and late-type AGN cover similar ranges of X-ray obscuration, for both unobscured and obscured sources. Conclusions. Our findings appear to confirm some previous suggestions that X-ray selected AGN residing in the green valley represent a transitional population, quenching star formation by means of different AGN feedback mechanisms and evolving to red-sequence galaxies. They might be hosted by similar sources (the majority of sources being late-type elliptical and lenticular galaxies, and early-type spirals) with similar stellar populations, which are triggered mainly by major and/or minor mergers, and in some cases by means of secular mechanism, as shown in previous numerical simulations. In the aforementioned transition we observe different phases of AGN activity, with some AGN being in the "QSO-mode" detected as compact, blue, and unobscured in X-rays, and with others passing through different phases before and after the "QSO-mode", being obscured and unobscured in X-rays, respectively.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Noyau galactique actif</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Active galaxy nuclei</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Galaxies type avancé</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Late type galaxies</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Galaxias tipo avanzado</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Morphologie</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Morphology</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Couleur</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Color</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Déplacement vers le rouge</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Red shift</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Classification</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Classification</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Diagramme magnitude couleur</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Color-magnitude diagrams</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Corrélation</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Correlations</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Modèle</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Models</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Modelo</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Bulbe galaxies</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Galaxy bulge</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Bulbo galaxias</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Masse stellaire</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Stellar mass</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Luminosité</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Luminosity</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Formation stellaire</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Star formation</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Boucle réaction</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Feedback</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Galaxies elliptiques</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Elliptical galaxies</s0><s5>40</s5></fC03><fC03 i1="16" i2="3" l="FRE"><s0>Galaxies lenticulaires</s0><s5>41</s5></fC03><fC03 i1="16" i2="3" l="ENG"><s0>Lenticular galaxies</s0><s5>41</s5></fC03><fC03 i1="17" i2="X" l="FRE"><s0>Population stellaire</s0><s5>42</s5></fC03><fC03 i1="17" i2="X" l="ENG"><s0>Stellar population</s0><s5>42</s5></fC03><fC03 i1="17" i2="X" l="SPA"><s0>Población estelar</s0><s5>42</s5></fC03><fC03 i1="18" i2="3" l="FRE"><s0>Simulation numérique</s0><s5>43</s5></fC03><fC03 i1="18" i2="3" l="ENG"><s0>Digital simulation</s0><s5>43</s5></fC03><fC03 i1="19" i2="3" l="FRE"><s0>Quasar</s0><s5>44</s5></fC03><fC03 i1="19" i2="3" l="ENG"><s0>Quasars</s0><s5>44</s5></fC03><fC03 i1="20" i2="3" l="FRE"><s0>Galaxies actives</s0><s5>45</s5></fC03><fC03 i1="20" i2="3" l="ENG"><s0>Active galaxies</s0><s5>45</s5></fC03><fC03 i1="21" i2="X" l="FRE"><s0>Structure galaxies</s0><s5>46</s5></fC03><fC03 i1="21" i2="X" l="ENG"><s0>Galaxy structure</s0><s5>46</s5></fC03><fC03 i1="21" i2="X" l="SPA"><s0>Estructura galaxias</s0><s5>46</s5></fC03><fC03 i1="22" i2="3" l="FRE"><s0>Galaxies RX</s0><s5>47</s5></fC03><fC03 i1="22" i2="3" l="ENG"><s0>X-ray galaxies</s0><s5>47</s5></fC03><fC03 i1="23" i2="3" l="FRE"><s0>Noyau galaxies</s0><s5>48</s5></fC03><fC03 i1="23" i2="3" l="ENG"><s0>Galaxy nuclei</s0><s5>48</s5></fC03><fC03 i1="24" i2="3" l="FRE"><s0>Source RX cosmique</s0><s5>49</s5></fC03><fC03 i1="24" i2="3" l="ENG"><s0>Cosmic x-ray sources</s0><s5>49</s5></fC03><fN21><s1>247</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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