Please use this identifier to cite or link to this item: http://hdl.handle.net/2307/238
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dc.contributor.authorMarulli, Federico-
dc.contributor.authorBonoli, Silvia-
dc.contributor.authorBranchini, Enzo-
dc.contributor.authorGilli, Roberto-
dc.contributor.authorMoscardini, Lauro-
dc.contributor.authorSpringel, Volker-
dc.date.accessioned2010-07-06T11:37:19Z-
dc.date.available2010-07-06T11:37:19Z-
dc.date.issued2009-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/2307/238-
dc.description.abstractWe study the spatial distribution of X-ray selected active galacticnuclei (AGN) in the framework of hierarchical coevolution ofsupermassive black holes and their host galaxies and dark matterhaloes. To this end, we have applied the theoretical model developed byCroton et al., De Lucia & Blaizot and Marulli et al. to the output ofthe Millennium Run and obtained hundreds of realizations of past lightcones from which we have extracted realistic mock AGN catalogues thatmimic the Chandra deep fields. We find that the model AGN number countsare in fair agreement with observations both in the soft and in thehard X-ray bands, except at fluxes <= 10(-15) erg cm(-2) s(-1), wherethe model systematically overestimates the observations. However, alarge fraction of these faint objects are typically excluded from thespectroscopic AGN samples of the Chandra fields. We find that thespatial two-point correlation function predicted by the model is welldescribed by a power-law relation out to 20 h(-1) Mpc, in closeagreement with observations. Our model matches the correlation lengthr(0) of AGN in the Chandra Deep Field-North but underestimates it inthe Chandra Deep Field-South. When fixing the slope to gamma = 1.4, asin Gilli et al., the statistical significance of the mismatch is 2sigma-2.5 sigma, suggesting that the predicted cosmic variance, whichdominates the error budget, may not account for the differentcorrelation length of the AGN in the two fields. However, the overallmismatch between the model and the observed correlation functiondecreases when both r(0) and gamma are allowed to vary, suggesting thatmore realistic AGN models and a full account of all observationalerrors may significantly reduce the tension between AGN clustering inthe two fields. While our results are robust to changes in the modelprescriptions for the AGN light curves, the luminosity dependence ofthe clustering is sensitive to the different light-curve modelsadopted. However, irrespective of the model considered, the luminositydependence of the AGN clustering in our mock fields seems to be weakerthan in the real Chandra fields. The significance of this mismatchneeds to be confirmed using larger data sets.en
dc.language.isoenen
dc.publisherWILEY-BLACKWELL PUBLISHING, INCen
dc.relation.ispartofMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETYen
dc.subjectSUPERMASSIVE BLACK-HOLESen
dc.subjectACTIVE GALACTIC NUCLEIen
dc.subjectHIERARCHICAL GALAXYen
dc.subjectFORMATIONen
dc.subjectQUASAR LUMINOSITY FUNCTIONen
dc.subjectSTAR-FORMING GALAXIESen
dc.subjectREDSHIFTen
dc.subjectSURVEYen
dc.subjectCOSMOLOGICAL SIMULATIONSen
dc.subjectELLIPTIC GALAXIESen
dc.subjectSOURCE CATALOGSen
dc.subjectUNIFIED MODELen
dc.titleThe spatial distribution of X-ray selected AGN in the Chandra deepfields: a theoretical perspectiveen
dc.typeArticleen
dc.subject.miurSettori Disciplinari MIUR::Scienze fisicheen
dc.subject.isicruiCategorie ISI-CRUI::Scienze fisicheen
dc.subject.anagraferoma3Scienze fisicheen
dc.relation.volumenumber396en
dc.relation.pagenumber1404-1414en
dc.identifier.doi10.1111/j.1365-2966.2009.14851.x-
dc.relation.issuenumber3en
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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