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dc.contributor.authorGeach, J. E.
dc.contributor.authorPeacock, J. A.
dc.contributor.authorMyers, A. D.
dc.contributor.authorHickox, R. C.
dc.contributor.authorBurchard, M. C.
dc.contributor.authorJones, M. L.
dc.date.accessioned2019-05-16T14:04:37Z
dc.date.available2019-05-16T14:04:37Z
dc.date.issued2019-03-27
dc.identifier.citationGeach , J E , Peacock , J A , Myers , A D , Hickox , R C , Burchard , M C & Jones , M L 2019 , ' The Halo Mass of Optically Luminous Quasars at z ,F≈ ,F1-2 Measured via Gravitational Deflection of the Cosmic Microwave Background ' , The Astrophysical Journal , vol. 874 , no. 1 , 85 , pp. 1-6 . https://doi.org/10.3847/1538-4357/ab0894
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 16400760
dc.identifier.otherPURE UUID: f7aa8b2f-cf0a-4a1a-ba4a-ff1fc6611617
dc.identifier.otherArXiv: http://arxiv.org/abs/1902.06955v1
dc.identifier.otherScopus: 85064446859
dc.identifier.urihttp://hdl.handle.net/2299/21334
dc.description© 2019. The American Astronomical Society. All rights reserved.
dc.description.abstractWe measure the average deflection of cosmic microwave background photons by quasars at 〈Z〉= 1.7. Our sample is selected from the Sloan Digital Sky Survey to cover the redshift range 0.9 ≤z≤2.2 with absolute i-band magnitudes of M i ≤-24 (K-corrected to z = 2). A stack of nearly 200,000 targets reveals an 8δ detection of Planck's estimate of the lensing convergence toward the quasars. We fit the signal with a model comprising a Navarro-Frenk-White density profile and a two-halo term accounting for correlated large-scale structure, which dominates the observed signal. The best-fitting model is described by an average halo mass log 10 (M h h -1 M)12.6 ±0.2 = and linear bias b=2.7±0.3 at 〈Z 〉= 1.7, in excellent agreement with clustering studies. We also report a hint, at a 90% confidence level, of a correlation between the convergence amplitude and luminosity, indicating that quasars brighter than Mi≲ -26 reside in halos of typical mass M h ≈ 10 13 h -1 M, scaling roughly as M h ∞ L opt 3/4 at M i ≲-24 mag, in good agreement with physically motivated quasar demography models. Although we acknowledge that this luminosity dependence is a marginal result, the observed Mh-L opt relationship could be interpreted as a reflection of the cutoff in the distribution of black hole accretion rates toward high Eddington ratios: the weak trend of Mh with Lopt observed at low luminosity becomes stronger for the most powerful quasars, which tend to be accreting close to the Eddington limit.en
dc.format.extent6
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.rightsOpen
dc.subjectgalaxies: evolution
dc.subjectgalaxies: halos
dc.subjectgalaxies: high-redshift
dc.subjectlarge-scale structure of universe
dc.subjectquasars: general
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleThe Halo Mass of Optically Luminous Quasars at z ,F≈ ,F1-2 Measured via Gravitational Deflection of the Cosmic Microwave Backgrounden
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionCentre of Data Innovation Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85064446859&partnerID=8YFLogxK
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2019-03-27
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.3847/1538-4357/ab0894
rioxxterms.licenseref.uriOther
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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