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dc.contributor.authorDiPompeo, M.~A.
dc.contributor.authorRunnoe, J.~C.
dc.contributor.authorHickox, R.~C.
dc.contributor.authorMyers, A.~D.
dc.contributor.authorGeach, J.~E.
dc.date.accessioned2016-10-18T16:12:17Z
dc.date.available2016-10-18T16:12:17Z
dc.date.issued2016-07-01
dc.identifier.citationDiPompeo , M A , Runnoe , J C , Hickox , R C , Myers , A D & Geach , J E 2016 , ' The impact of the dusty torus on obscured quasar halo mass measurements ' , Monthly Notices of the Royal Astronomical Society , vol. 460 , no. 1 , pp. 175-186 . https://doi.org/10.1093/mnras/stw986
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 10175223
dc.identifier.otherPURE UUID: 81609666-c505-4520-bb64-8ef1934352e9
dc.identifier.otherBibtex: urn:093683192719dbf971d2b7904e561f18
dc.identifier.otherScopus: 84978967250
dc.identifier.urihttp://hdl.handle.net/2299/17267
dc.description.abstractRecent studies have found that obscured quasars cluster more strongly and are thus hosted by dark matter haloes of larger mass than their unobscured counterparts. These results pose a challenge for the simplest unification models, in which obscured objects are intrinsically the same as unobscured sources but seen through a dusty line of sight. There is general consensus that a structure like a ‘dusty torus’ exists, meaning that this intrinsic similarity is likely the case for at least some subset of obscured quasars. However, the larger host halo masses of obscured quasars imply that there is a second obscured population that has an even higher clustering amplitude and typical halo mass. Here, we use simple assumptions about the host halo mass distributions of quasars, along with analytical methods and cosmological N-body simulations to isolate the signal from this population. We provide values for the bias and halo mass as a function of the fraction of the ‘non-torus-obscured’ population. Adopting a reasonable value for this fraction of ∼25 per cent implies a non-torus-obscured-quasar bias that is much higher than the observed obscured quasar bias, because a large fraction of the obscured population shares the same clustering strength as the unobscured objects. For this non-torus-obscured population, we derive a bias of ∼3, and typical halo masses of ∼3 × 1013 M⊙ h−1 at z = 1. These massive haloes are likely the descendants of high-mass unobscured quasars at high redshift, and will evolve into members of galaxy groups at z = 0.en
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectgalaxies: active, galaxies: evolution, galaxies: haloes, quasars: general
dc.titleThe impact of the dusty torus on obscured quasar halo mass measurementsen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2016-07-01
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stw986
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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