Please use this identifier to cite or link to this item: http://hdl.handle.net/2307/236
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dc.contributor.authorBonoli, Silvia-
dc.contributor.authorMarulli, Federico-
dc.contributor.authorSpringel, Volker-
dc.contributor.authorWhite, Simon D. M.-
dc.contributor.authorBranchini, Enzo-
dc.contributor.authorMoscardini, Lauro-
dc.date.accessioned2010-07-06T09:46:49Z-
dc.date.available2010-07-06T09:46:49Z-
dc.date.issued2009-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/2307/236-
dc.description.abstractWe use semi-analytic modelling on top of the Millennium simulation to study the joint formation of galaxies and their embedded supermassive black holes. Our goal is to test scenarios in which black hole accretion and quasar activity are triggered by galaxy mergers, and to constrain different models for the light curves associated with individual quasar events. In the present work, we focus on studying the spatial distribution of simulated quasars. At all luminosities, we find that the simulated quasar two-point correlation function is fit well by a single power law in the range 0.5 less than or similar to r less than or similar to 20 h(-1) Mpc, but its normalization is a strong function of redshift. When we select only quasars with luminosities within the range typically accessible by today's quasar surveys, their clustering strength depends only weakly on luminosity, in agreement with observations. This holds independently of the assumed light-curve model, since bright quasars are black holes accreting close to the Eddington limit, and are hosted by dark matter haloes with a narrow mass range of a few 10(12) h(-1) M-circle dot. Therefore, the clustering of bright quasars cannot be used to disentangle light-curve models, but such a discrimination would become possible if the observational samples can be pushed to significantly fainter limits.Overall, our clustering results for the simulated quasar population agree rather well with observations, lending support to the conjecture that galaxy mergers could be the main physical process responsible for triggering black hole accretion and quasar activity.en
dc.language.isoenen
dc.publisherWiley-Blackwell Publishing, Incen
dc.relation.ispartofMonthly notices of the Royal Astronomical Societyen
dc.rightsc2009 Royal Astronomical Society ; c2009 The Authors. Journal compilationen
dc.subjectACTIVE GALACTIC NUCLEIen
dc.subjectDIGITAL SKY SURVEYen
dc.subjectQSO REDSHIFT SURVEYen
dc.subjectBULGEen
dc.subjectMASS RELATIONen
dc.subjectHOST HALO MASSen
dc.subjectLUMINOSITY FUNCTIONen
dc.subjectFUNDAMENTALen
dc.subjectRELATIONen
dc.subjectCOSMIC EVOLUTIONen
dc.subjectPOPULATION-IIIen
dc.subjectMATTER HALOESen
dc.titleModelling the cosmological co-evolution of supermassive black holes and galaxies - II. The clustering of quasars and their dark environmenten
dc.typeArticleen
dc.subject.miurSettori Disciplinari MIUR::Scienze fisiche::ASTRONOMIA E ASTROFISICAen
dc.subject.isicruiCategorie ISI-CRUI::Scienze fisicheen
dc.subject.anagraferoma3Scienze fisicheen
dc.relation.volumenumber396en
dc.relation.pagenumber423-438en
dc.identifier.doi10.1111/j.1365-2966.2009.14701.x-
dc.relation.issuenumber1en
item.languageiso639-1other-
item.fulltextWith Fulltext-
item.grantfulltextrestricted-
Appears in Collections:A - Articolo su rivista
X_Dipartimento di Fisica 'Edoardo Amaldi'
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