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dc.contributor.authorClements, D.
dc.contributor.authorRigby, E.
dc.contributor.authorMaddox, S.
dc.contributor.authorDunne, L.
dc.contributor.authorMortier, A.M.J.
dc.contributor.authorPearson, C.
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.authorCooray, A.
dc.contributor.authorDariush, A.
dc.contributor.authorde Zotti, G.
dc.contributor.authorDye, S.
dc.contributor.authorEales, S.
dc.contributor.authorFrayer, D.
dc.contributor.authorFritz, J.
dc.contributor.authorGardner, J.P.
dc.contributor.authorGonzalez-Nuevo, J.
dc.contributor.authorHerranz, D.
dc.contributor.authorIbar, E.
dc.contributor.authorIvison, R.J.
dc.contributor.authorJarvis, M.J.
dc.contributor.authorLagache, G.
dc.contributor.authorLeeuw, L.
dc.contributor.authorLopez-Caniego, M.
dc.contributor.authorNegrello, M.
dc.contributor.authorPascale, E.
dc.contributor.authorPohlen, M.
dc.contributor.authorRodighiero, G.
dc.contributor.authorSamui, S.
dc.contributor.authorSerjeant, S.
dc.contributor.authorSibthorpe, B.
dc.contributor.authorScott, D.
dc.contributor.authorSmith, Daniel
dc.contributor.authorTemi, P.
dc.contributor.authorThompson, M.A.
dc.contributor.authorValtchanov, I.
dc.contributor.authorvan der Werf, P.
dc.contributor.authorVerma, A.
dc.date.accessioned2010-11-12T08:59:44Z
dc.date.available2010-11-12T08:59:44Z
dc.date.issued2010
dc.identifier.citationClements , D , Rigby , E , Maddox , S , Dunne , L , Mortier , A M J , Pearson , C , Amblard , A , Auld , R , Baes , M , Bonfield , D , Burgarella , D , Buttiglione , S , Cava , A , Cooray , A , Dariush , A , de Zotti , G , Dye , S , Eales , S , Frayer , D , Fritz , J , Gardner , J P , Gonzalez-Nuevo , J , Herranz , D , Ibar , E , Ivison , R J , Jarvis , M J , Lagache , G , Leeuw , L , Lopez-Caniego , M , Negrello , M , Pascale , E , Pohlen , M , Rodighiero , G , Samui , S , Serjeant , S , Sibthorpe , B , Scott , D , Smith , D , Temi , P , Thompson , M A , Valtchanov , I , van der Werf , P & Verma , A 2010 , ' Herschel-ATLAS: Extragalactic number counts from 250 to 500 microns ' , Astronomy and Astrophysics , vol. 518 , L8 . https://doi.org/10.1051/0004-6361/201014581
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 158908
dc.identifier.otherPURE UUID: d1266690-d6c6-4b97-a98b-7422993b74ba
dc.identifier.otherdspace: 2299/4978
dc.identifier.otherScopus: 77954786256
dc.identifier.otherORCID: /0000-0001-5392-909X/work/30970846
dc.identifier.otherORCID: /0000-0001-9708-253X/work/69424396
dc.identifier.urihttp://hdl.handle.net/2299/4978
dc.descriptionOriginal article can be found at: http://www.aanda.org/ Copyright The European Southern Observatory
dc.description.abstractAims. The Herschel-ATLAS survey (H-ATLAS) will be the largest area survey to be undertaken by the Herschel Space Observatory. It will cover 550 sq. deg. of extragalactic sky at wavelengths of 100, 160, 250, 350 and 500 μm when completed, reaching flux limits (5σ) from 32 to 145 mJy. We here present galaxy number counts obtained for SPIRE observations of the first ~14 sq. deg. observed at 250, 350 and 500 μm. Methods. Number counts are a fundamental tool in constraining models of galaxy evolution. We use source catalogs extracted from the H-ATLAS maps as the basis for such an analysis. Correction factors for completeness and flux boosting are derived by applying our extraction method to model catalogs and then applied to the raw observational counts. Results. We find a steep rise in the number counts at flux levels of 100–200 mJy in all three SPIRE bands, consistent with results from BLAST. The counts are compared to a range of galaxy evolution models. None of the current models is an ideal fit to the data but all ascribe the steep rise to a population of luminous, rapidly evolving dusty galaxies at moderate to high redshift.en
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.titleHerschel-ATLAS: Extragalactic number counts from 250 to 500 micronsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201014581
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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