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dc.contributor.authorSmith, Daniel
dc.contributor.authorDunne, L.
dc.contributor.authorMaddox, S. J.
dc.contributor.authorEales, S.
dc.contributor.authorBonfield, D. G.
dc.contributor.authorJarvis, M.J.
dc.contributor.authorSutherland, W.
dc.contributor.authorFleuren, S.
dc.contributor.authorRigby, E. E.
dc.contributor.authorThompson, Mark
dc.contributor.authorBaldry, I.K.
dc.contributor.authorBamford, S.
dc.contributor.authorButtiglione, S.
dc.contributor.authorCava, A.
dc.contributor.authorClements, D. L.
dc.contributor.authorCooray, A.
dc.contributor.authorCroom, S.
dc.contributor.authorDariush, A.
dc.contributor.authorde Zotti, G.
dc.contributor.authorDriver, S. P.
dc.contributor.authorDunlop, J.S.
dc.contributor.authorFritz, J.
dc.contributor.authorHill, D. T.
dc.contributor.authorHopkins, A.
dc.contributor.authorHopwood, R.
dc.contributor.authorIbar, E.
dc.contributor.authorIvison, R.J.
dc.contributor.authorJones, D. H.
dc.contributor.authorKelvin, L.
dc.contributor.authorLeeuw, L.
dc.contributor.authorLiske, J.
dc.contributor.authorLoveday, J.
dc.contributor.authorMadore, B. F.
dc.contributor.authorNorberg, P.
dc.contributor.authorPanuzzo, P.
dc.contributor.authorPascale, E.
dc.contributor.authorPohlen, M.
dc.contributor.authorPopescu, C. C.
dc.contributor.authorPrescott, M.
dc.contributor.authorRobotham, A.
dc.contributor.authorRodighiero, G.
dc.contributor.authorScott, D.
dc.contributor.authorSeibert, M.
dc.contributor.authorSharp, R.
dc.contributor.authorTemi, P.
dc.contributor.authorTuffs, R. J.
dc.contributor.authorvan der Werf, P.
dc.contributor.authorvan Kampen, E.
dc.date.accessioned2011-10-19T10:01:43Z
dc.date.available2011-10-19T10:01:43Z
dc.date.issued2011-09
dc.identifier.citationSmith , D , Dunne , L , Maddox , S J , Eales , S , Bonfield , D G , Jarvis , M J , Sutherland , W , Fleuren , S , Rigby , E E , Thompson , M , Baldry , I K , Bamford , S , Buttiglione , S , Cava , A , Clements , D L , Cooray , A , Croom , S , Dariush , A , de Zotti , G , Driver , S P , Dunlop , J S , Fritz , J , Hill , D T , Hopkins , A , Hopwood , R , Ibar , E , Ivison , R J , Jones , D H , Kelvin , L , Leeuw , L , Liske , J , Loveday , J , Madore , B F , Norberg , P , Panuzzo , P , Pascale , E , Pohlen , M , Popescu , C C , Prescott , M , Robotham , A , Rodighiero , G , Scott , D , Seibert , M , Sharp , R , Temi , P , Tuffs , R J , van der Werf , P & van Kampen , E 2011 , ' Herschel-ATLAS : Counterparts from the ultraviolet-near-infrared in the science demonstration phase catalogue ' , Monthly Notices of the Royal Astronomical Society , vol. 416 , no. 2 , pp. 857-872 . https://doi.org/10.1111/j.1365-2966.2011.18827.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 423709
dc.identifier.otherPURE UUID: b49ba7d2-5386-43da-bf87-a85015dc35f5
dc.identifier.otherWOS: 000295119900004
dc.identifier.otherScopus: 80052372190
dc.identifier.urihttp://hdl.handle.net/2299/6726
dc.descriptionThe definitive version can be found at: http://onlinelibrary.wiley.com/ Copyright Royal Astronomical Society
dc.description.abstractWe present a technique to identify optical counterparts of 250-mu m-selected sources from the Herschel-ATLAS survey. Of the 6621 250 mu m > 32-mJy sources in our science demonstration catalogue we find that similar to 60 per cent have counterparts brighter than r = 22.4 mag in the Sloan Digital Sky Survey. Applying a likelihood ratio technique we are able to identify 2423 of the counterparts with a reliability R > 0.8. This is approximately 37 per cent of the full 250-mu m catalogue. We have estimated photometric redshifts for each of these 2423 reliable counterparts, while 1099 also have spectroscopic redshifts collated from several different sources, including the GAMA survey. We estimate the completeness of identifying counterparts as a function of redshift, and present evidence that 250-mu m-selected Herschel-ATLAS galaxies have a bimodal redshift distribution. Those with reliable optical identifications have a redshift distribution peaking at z approximate to 0.25 +/- 0.05, while submillimetre colours suggest that a significant fraction with no counterpart above the r-band limit have z > 1. We also suggest a method for selecting populations of strongly lensed high-redshift galaxies. Our identifications are matched to UV-NIR photometry from the GAMA survey, and these data are available as part of the Herschel-ATLAS public data release.en
dc.format.extent16
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/embargoed
dc.subjectmethods: statistical
dc.subjectsubmillimetre: galaxies
dc.titleHerschel-ATLAS : Counterparts from the ultraviolet-near-infrared in the science demonstration phase catalogueen
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.date.embargoedUntil2012-03-01
dc.identifier.urlhttp://www.scopus.com/inward/record.url?partnerID=yv4JPVwI&eid=2-s2.0-80052372190&md5=c42269518c9e5ea744f8dc50c7326e29
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
rioxxterms.versionAM
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2011.18827.x
rioxxterms.licenseref.startdate2012-03-01Z
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.date.embargo2012-03-01Z
herts.rights.accesstypeopenAccess


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