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dc.contributor.authorDunlop, J.S.
dc.contributor.authorAde, P.A.R.
dc.contributor.authorBock, J.J.
dc.contributor.authorChapin, E.L.
dc.contributor.authorCirasuolo, M.
dc.contributor.authorCoppin, Kristen
dc.contributor.authorDevlin, M.J.
dc.contributor.authorGriffin, M.
dc.contributor.authorGreve, T.R.
dc.contributor.authorGundersen, J.O.
dc.contributor.authorHalpern, M.
dc.contributor.authorHargrave, P.C.
dc.contributor.authorHughes, D.H.
dc.contributor.authorIvison, R.J.
dc.contributor.authorKlein, J.
dc.contributor.authorKovacs, A.
dc.contributor.authorMarsden, G.
dc.contributor.authorMauskopf, P.
dc.contributor.authorNetterfield, Calvin B.
dc.contributor.authorOlmi, L.
dc.contributor.authorPascale, E.
dc.contributor.authorPatanchon, G.
dc.contributor.authorRex, M.
dc.contributor.authorScott, D.
dc.contributor.authorSemisch, C.
dc.contributor.authorSmail, I.
dc.contributor.authorTargett, T.A.
dc.contributor.authorThomas, N.
dc.contributor.authorTruch, M.D.P.
dc.contributor.authorTucker, C.
dc.contributor.authorTucker, G.S.
dc.contributor.authorViero, M.P.
dc.contributor.authorWalter, F.
dc.contributor.authorWardlow, J. L.
dc.contributor.authorWeiss, A.
dc.contributor.authorWiebe, D.V.
dc.date.accessioned2014-01-27T14:00:35Z
dc.date.available2014-01-27T14:00:35Z
dc.date.issued2010-11-01
dc.identifier.citationDunlop , J S , Ade , P A R , Bock , J J , Chapin , E L , Cirasuolo , M , Coppin , K , Devlin , M J , Griffin , M , Greve , T R , Gundersen , J O , Halpern , M , Hargrave , P C , Hughes , D H , Ivison , R J , Klein , J , Kovacs , A , Marsden , G , Mauskopf , P , Netterfield , C B , Olmi , L , Pascale , E , Patanchon , G , Rex , M , Scott , D , Semisch , C , Smail , I , Targett , T A , Thomas , N , Truch , M D P , Tucker , C , Tucker , G S , Viero , M P , Walter , F , Wardlow , J L , Weiss , A & Wiebe , D V 2010 , ' The BLAST 250 μm-selected galaxy population in GOODS-South ' Monthly Notices of the Royal Astronomical Society , vol. 408 , no. 4 , pp. 2022-2050 . https://doi.org/10.1111/j.1365-2966.2010.17278.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 2712657
dc.identifier.otherPURE UUID: 7c922fba-cd99-4e1e-84a1-a1884dd7015a
dc.identifier.otherScopus: 78049470288
dc.identifier.otherORCID: /0000-0002-0729-2988/work/30423088
dc.identifier.urihttp://hdl.handle.net/2299/12686
dc.descriptioncopyright Royal Astronomical Society
dc.description.abstractWe identify and investigate the nature of the 20 brightest 250 μm sources detected by the Balloon-borne Large Aperture Submillimetre Telescope (BLAST) within the central 150 arcmin of the Great Observatories Origins Deep Survey (GOODS) South field. Aided by the available deep VLA 1.4 GHz radio imaging, reaching S 40-μJy (4α), we have identified radio counterparts for 17/20 of the 250 μm sources. The resulting enhanced positional accuracy of ≃1 arcsec has then allowed us to exploit the deep optical (Hubble Space Telescope), near-infrared (VLT) and mid-infrared (Spitzer) imaging of GOODS-South to establish secure galaxy counterparts for the 17 radio-identified sources, and plausible galaxy candidates for the three radio-unidentified sources. Confusion is a serious issue for this deep BLAST 250 μm survey, due to the large size of the beam. Nevertheless, we argue that our chosen counterparts are significant, and often dominant contributors to the measured BLAST flux densities. For all of these 20 galaxies we have been able to determine spectroscopic (eight) or photometric (12) redshifts. The result is the first near-complete redshift distribution for a deep 250 μm-selected galaxy sample. This reveals that 250 μm surveys reaching detection limits of ≃40 mJy have a median redshift z≃ 1, and contain not only low-redshift spirals/LIRGs, but also the extreme z≃ 2 dust-enshrouded starburst galaxies previously discovered at sub-millimetre wavelengths. Inspection of the LABOCA 870 μm imaging of GOODS-South yields detections of ≃1/3 of the proposed BLAST sources (all at z > 1.5), and reveals 250/870 μm flux-density ratios consistent with a standard 40 K modified blackbody fit with a dust emissivity index β= 1.5. Based on their Infrared Array Camera (IRAC) colours, we find that virtually all of the BLAST galaxy identifications appear better described as analogues of the M82 starburst galaxy, or Sc star-forming discs rather than highly obscured ULIRGs. This is perhaps as expected at low redshift, where the 250 μm BLAST selection function is biased towards spectral energy distributions which peak longward of λ= 100 μm. However, it also appears largely true at z≃ 2.en
dc.format.extent29
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.titleThe BLAST 250 μm-selected galaxy population in GOODS-Southen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=78049470288&partnerID=8YFLogxK
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeSubmitted Version
rioxxterms.versionSMUR
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2010.17278.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstyperestrictedAccess


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