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HerMES: SPIRE galaxy number counts at 250, 350, and 500 µm

dc.contributor.authorOliver, S. J.
dc.contributor.authorWang, L.
dc.contributor.authorSmith, A. J.
dc.contributor.authorAltieri, B.
dc.contributor.authorAmblard, A.
dc.contributor.authorArumugam, V.
dc.contributor.authorAuld, R.
dc.contributor.authorAussel, H.
dc.contributor.authorBabbedge, T.
dc.contributor.authorBlain, A.
dc.contributor.authorBock, J.
dc.contributor.authorBoselli, A.
dc.contributor.authorBuat, V.
dc.contributor.authorBurgarella, D.
dc.contributor.authorCastro-Rodríguez, N.
dc.contributor.authorCava, A.
dc.contributor.authorChanial, P.
dc.contributor.authorClements, D. L.
dc.contributor.authorConley, A.
dc.contributor.authorConversi, L.
dc.contributor.authorCooray, A.
dc.contributor.authorDowell, C.D.
dc.contributor.authorDwek, E.
dc.contributor.authorEales, S.
dc.contributor.authorElbaz, D.
dc.contributor.authorFox, M.
dc.contributor.authorFranceschini, A.
dc.contributor.authorGear, W.
dc.contributor.authorGlenn, J.
dc.contributor.authorGriffin, M.
dc.contributor.authorHalpern, M.
dc.contributor.authorHatziminaoglou, E.
dc.contributor.authorIbar, E.
dc.contributor.authorIsaak, K.
dc.contributor.authorIvison, R.J.
dc.contributor.authorLagache, G.
dc.contributor.authorLevenson, L.
dc.contributor.authorLu, N.
dc.contributor.authorMadden, S.
dc.contributor.authorMaffei, B.
dc.contributor.authorMainetti, G.
dc.contributor.authorMarchetti, L.
dc.contributor.authorMitchell-Wynne, K.
dc.contributor.authorMortier, A. M. J.
dc.contributor.authorNguyen, H.T.
dc.contributor.authorO'Halloran, B.
dc.contributor.authorOmont, A.
dc.contributor.authorPage, M.J.
dc.contributor.authorPanuzzo, P.
dc.contributor.authorPapageorgiou, A.
dc.contributor.authorPearson, C.P.
dc.contributor.authorPérez-Fournon, I.
dc.contributor.authorPohlen, M.
dc.contributor.authorRawlings, J.I.
dc.contributor.authorRaymond, G.
dc.contributor.authorRigopoulou, D.
dc.contributor.authorRizzo, D.
dc.contributor.authorRoseboom, I.G.
dc.contributor.authorRowan-Robinson, M.
dc.contributor.authorSánchez Portal, M.
dc.contributor.authorSavage, R.
dc.contributor.authorSchulz, B.
dc.contributor.authorScott, D.
dc.contributor.authorSeymour, N.
dc.contributor.authorShupe, D. L.
dc.contributor.authorStevens, Jason
dc.contributor.authorSymeonidis, M.
dc.contributor.authorTrichas, M.
dc.contributor.authorTugwell, K.E.
dc.contributor.authorVaccari, M.
dc.contributor.authorValiante, E.
dc.contributor.authorValtchanov, I.
dc.contributor.authorVieira, J. D.
dc.contributor.authorVigroux, L.
dc.contributor.authorWard, R.
dc.contributor.authorWright, G.
dc.contributor.authorXu, C.K.
dc.contributor.authorZemcov, M.
dc.date.accessioned2012-03-21T09:00:41Z
dc.date.available2012-03-21T09:00:41Z
dc.date.issued2010-07-01
dc.identifier.citationOliver , S J , Wang , L , Smith , A J , Altieri , B , Amblard , A , Arumugam , V , Auld , R , Aussel , H , Babbedge , T , Blain , A , Bock , J , Boselli , A , Buat , V , Burgarella , D , Castro-Rodríguez , N , Cava , A , Chanial , P , Clements , D L , Conley , A , Conversi , L , Cooray , A , Dowell , C D , Dwek , E , Eales , S , Elbaz , D , Fox , M , Franceschini , A , Gear , W , Glenn , J , Griffin , M , Halpern , M , Hatziminaoglou , E , Ibar , E , Isaak , K , Ivison , R J , Lagache , G , Levenson , L , Lu , N , Madden , S , Maffei , B , Mainetti , G , Marchetti , L , Mitchell-Wynne , K , Mortier , A M J , Nguyen , H T , O'Halloran , B , Omont , A , Page , M J , Panuzzo , P , Papageorgiou , A , Pearson , C P , Pérez-Fournon , I , Pohlen , M , Rawlings , J I , Raymond , G , Rigopoulou , D , Rizzo , D , Roseboom , I G , Rowan-Robinson , M , Sánchez Portal , M , Savage , R , Schulz , B , Scott , D , Seymour , N , Shupe , D L , Stevens , J , Symeonidis , M , Trichas , M , Tugwell , K E , Vaccari , M , Valiante , E , Valtchanov , I , Vieira , J D , Vigroux , L , Ward , R , Wright , G , Xu , C K & Zemcov , M 2010 , ' HerMES: SPIRE galaxy number counts at 250, 350, and 500 µm ' , Astronomy & Astrophysics , vol. 518 , L21 . https://doi.org/10.1051/0004-6361/201014697
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 519879
dc.identifier.otherPURE UUID: 4460bdf6-ed24-45f3-a774-4c41671c02d5
dc.identifier.otherBibtex: urn:6ae22cd80850196ef9dcc07f8b523424
dc.identifier.otherScopus: 77957855162
dc.identifier.otherORCID: /0000-0002-4010-8310/work/62747647
dc.identifier.urihttp://hdl.handle.net/2299/8013
dc.description.abstractEmission at far-infrared wavelengths makes up a significant fraction of the total light detected from galaxies over the age of Universe. Herschel provides an opportunity for studying galaxies at the peak wavelength of their emission. Our aim is to provide a benchmark for models of galaxy population evolution and to test pre-existing models of galaxies. With the Herschel Multi-tiered Extra-galactic survey, HerMES, we have observed a number of fields of different areas and sensitivity using the SPIRE instrument on Herschel. We have determined the number counts of galaxies down to ~20 mJy. Our constraints from directly counting galaxies are consistent with, though more precise than, estimates from the BLAST fluctuation analysis. We have found a steep rise in the Euclidean normalised counts <100 mJy. We have directly resolved ~15% of the infrared extra-galactic background at the wavelength near where it peaks.en
dc.format.extent5
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysics
dc.subjectgalaxies: evolution, submillimeter: galaxies, surveys
dc.titleHerMES: SPIRE galaxy number counts at 250, 350, and 500 µmen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/201014697
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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