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dc.contributor.authorSerjeant, S.
dc.contributor.authorBertoldi, F.
dc.contributor.authorBlain, A.W.
dc.contributor.authorClements, D.
dc.contributor.authorCooray, A.
dc.contributor.authorDanese, L.
dc.contributor.authorDunlop, J.S.
dc.contributor.authorDunne, L.
dc.contributor.authorEales, S.
dc.contributor.authorFalder, J.
dc.contributor.authorHatziminaoglou, E.
dc.contributor.authorHughes, D.H.
dc.contributor.authorIbar, E.
dc.contributor.authorJarvis, M.J.
dc.contributor.authorLawrence, A.
dc.contributor.authorLee, M.G.
dc.contributor.authorMichalowski, M.
dc.contributor.authorNegrello, M.
dc.contributor.authorOmont, A.
dc.contributor.authorPage, M.J.
dc.contributor.authorPearson, C.
dc.contributor.authorvan der Werf, P.
dc.contributor.authorWhite, G.J.
dc.contributor.authorAmblard, A.
dc.contributor.authorAuld, R.
dc.contributor.authorBaes, M.
dc.contributor.authorBonfield, D.
dc.contributor.authorBurgarella, D.
dc.contributor.authorButtiglione, S.
dc.contributor.authorCava, A.
dc.contributor.authorDariush, A.
dc.contributor.authorde Zotti, G.
dc.contributor.authorDye, S.
dc.contributor.authorFrayer, D.
dc.contributor.authorFritz, J.
dc.contributor.authorGonzalez-Nuevo, J.
dc.contributor.authorHerranz, D.
dc.contributor.authorIvison, R.J.
dc.contributor.authorLagache, G.
dc.contributor.authorLeeuw, L.
dc.contributor.authorLopez-Caniego, M.
dc.contributor.authorMaddox, S.
dc.contributor.authorPascale, E.
dc.contributor.authorPohlen, M.
dc.contributor.authorRigby, E.
dc.contributor.authorRodighiero, G.
dc.contributor.authorSamui, S.
dc.contributor.authorSibthorpe, B.
dc.contributor.authorSmith, Daniel
dc.contributor.authorTemi, P.
dc.contributor.authorThompson, M.A.
dc.contributor.authorValtchanov, I.
dc.contributor.authorVerma, A.
dc.date.accessioned2010-11-12T09:20:54Z
dc.date.available2010-11-12T09:20:54Z
dc.date.issued2010
dc.identifier.citationSerjeant , S , Bertoldi , F , Blain , A W , Clements , D , Cooray , A , Danese , L , Dunlop , J S , Dunne , L , Eales , S , Falder , J , Hatziminaoglou , E , Hughes , D H , Ibar , E , Jarvis , M J , Lawrence , A , Lee , M G , Michalowski , M , Negrello , M , Omont , A , Page , M J , Pearson , C , van der Werf , P , White , G J , Amblard , A , Auld , R , Baes , M , Bonfield , D , Burgarella , D , Buttiglione , S , Cava , A , Dariush , A , de Zotti , G , Dye , S , Frayer , D , Fritz , J , Gonzalez-Nuevo , J , Herranz , D , Ivison , R J , Lagache , G , Leeuw , L , Lopez-Caniego , M , Maddox , S , Pascale , E , Pohlen , M , Rigby , E , Rodighiero , G , Samui , S , Sibthorpe , B , Smith , D , Temi , P , Thompson , M A , Valtchanov , I & Verma , A 2010 , ' Herschel ATLAS: The cosmic star formation history of quasar host galaxies ' Astronomy and Astrophysics , vol. 518 , L7 . https://doi.org/10.1051/0004-6361/201014565
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 159086
dc.identifier.otherPURE UUID: 6b490957-b243-41e3-b21b-955b3b21719d
dc.identifier.otherdspace: 2299/4979
dc.identifier.otherScopus: 77957819960
dc.identifier.urihttp://hdl.handle.net/2299/4979
dc.descriptionOriginal article can be found at: http://www.aanda.org/ Copyright The European Southern Observatory
dc.description.abstractWe present a derivation of the star formation rate per comoving volume of quasar host galaxies, derived from stacking analyses of far-infrared to mm-wave photometry of quasars with redshifts 0 < z < 6 and absolute I-band magnitudes -22 > IAB > -32 We use the science demonstration observations of the first ~16 deg2 from the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) in which there are 240 quasars from the Sloan Digital Sky Survey (SDSS) and a further 171 from the 2dF-SDSS LRG and QSO (2SLAQ) survey. We supplement this data with a compilation of data from IRAS, ISO, Spitzer, SCUBA and MAMBO. H-ATLAS alone statistically detects the quasars in its survey area at >5σ at 250,350 and 500 μm. From the compilation as a whole we find striking evidence of downsizing in quasar host galaxy formation: low-luminosity quasars with absolute magnitudes in the range -22 > IAB > -24 have a comoving star formation rate (derived from 100 μm rest-frame luminosities) peaking between redshifts of 1 and 2, while high-luminosity quasars with IAB < -26 have a maximum contribution to the star formation density at z ~ 3. The volume-averaged star formation rate of -22 > IAB > -24 quasars evolves as (1 + z)2.3±0.7 at z < 2, but the evolution at higher luminosities is much faster reaching (1 + z)10±1 at -26 > IAB > -28. We tentatively interpret this as a combination of a declining major merger rate with time and gas consumption reducing fuel for both black hole accretion and star formation.en
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.titleHerschel ATLAS: The cosmic star formation history of quasar host galaxiesen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201014565
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstyperestrictedAccess


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