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dc.contributor.authorBourne, N.
dc.contributor.authorMaddox, S. J.
dc.contributor.authorDunne, L.
dc.contributor.authorAuld, R.
dc.contributor.authorBaes, M.
dc.contributor.authorBaldry, I. K.
dc.contributor.authorBonfield, D. G.
dc.contributor.authorCooray, A.
dc.contributor.authorCroom, S. M.
dc.contributor.authorDariush, A.
dc.contributor.authorde Zotti, G.
dc.contributor.authorDriver, S. P.
dc.contributor.authorDye, S.
dc.contributor.authorEales, S.
dc.contributor.authorGomez, H.L.
dc.contributor.authorGonzalez-Nuevo, J.
dc.contributor.authorHopkins, A. M.
dc.contributor.authorIbar, E.
dc.contributor.authorJarvis, M.J.
dc.contributor.authorLapi, A.
dc.contributor.authorMadore, B.
dc.contributor.authorMichalowski, M. J.
dc.contributor.authorPohlen, M.
dc.contributor.authorPopescu, C. C.
dc.contributor.authorRigby, E. E.
dc.contributor.authorSeibert, M.
dc.contributor.authorSmith, Daniel
dc.contributor.authorTuffs, R. J.
dc.contributor.authorvan der Werf, P.
dc.contributor.authorBrough, S.
dc.contributor.authorButtiglione, S.
dc.contributor.authorCava, A.
dc.contributor.authorClements, D. L.
dc.contributor.authorConselice, C. J.
dc.contributor.authorFritz, J.
dc.contributor.authorHopwood, R.
dc.contributor.authorIvison, R. J.
dc.contributor.authorJones, D. H.
dc.contributor.authorKelvin, L. S.
dc.contributor.authorLiske, J.
dc.contributor.authorLoveday, J.
dc.contributor.authorNorberg, P.
dc.contributor.authorRobotham, A. S. G.
dc.contributor.authorRodighiero, G.
dc.contributor.authorTemi, P.
dc.date.accessioned2012-07-30T14:00:47Z
dc.date.available2012-07-30T14:00:47Z
dc.date.issued2012-04
dc.identifier.citationBourne , N , Maddox , S J , Dunne , L , Auld , R , Baes , M , Baldry , I K , Bonfield , D G , Cooray , A , Croom , S M , Dariush , A , de Zotti , G , Driver , S P , Dye , S , Eales , S , Gomez , H L , Gonzalez-Nuevo , J , Hopkins , A M , Ibar , E , Jarvis , M J , Lapi , A , Madore , B , Michalowski , M J , Pohlen , M , Popescu , C C , Rigby , E E , Seibert , M , Smith , D , Tuffs , R J , van der Werf , P , Brough , S , Buttiglione , S , Cava , A , Clements , D L , Conselice , C J , Fritz , J , Hopwood , R , Ivison , R J , Jones , D H , Kelvin , L S , Liske , J , Loveday , J , Norberg , P , Robotham , A S G , Rodighiero , G & Temi , P 2012 , ' Herschel -ATLAS/GAMA : a census of dust in optically selected galaxies from stacking at submillimetre wavelengths ' , Monthly Notices of the Royal Astronomical Society , vol. 421 , no. 4 , pp. 3027-3059 . https://doi.org/10.1111/j.1365-2966.2012.20528.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 952168
dc.identifier.otherPURE UUID: 20d81c9c-af0f-4ab5-9a2e-cc8243fa3d43
dc.identifier.otherWOS: 000302620700027
dc.identifier.otherScopus: 84862776650
dc.identifier.urihttp://hdl.handle.net/2299/8747
dc.description.abstractWe use the Herschel-ATLAS survey to conduct the first large-scale statistical study of the submillimetre properties of optically selected galaxies. Using similar to 80 000 r-band selected galaxies from 126 deg2 of the GAMA survey, we stack into submillimetre imaging at 250, 350 and 500 mu m to gain unprecedented statistics on the dust emission from galaxies at z < 0.35. We find that low-redshift galaxies account for 5 per cent of the cosmic 250-mu m background (4 per cent at 350 mu m; 3 per cent at 500 mu m), of which approximately 60 per cent comes from blue and 20 per cent from red galaxies (rest-frame g-r). We compare the dust properties of different galaxy populations by dividing the sample into bins of optical luminosity, stellar mass, colour and redshift. In blue galaxies we find that dust temperature and luminosity correlate strongly with stellar mass at a fixed redshift, but red galaxies do not follow these correlations and overall have lower luminosities and temperatures. We make reasonable assumptions to account for the contaminating flux from lensing by red-sequence galaxies and conclude that galaxies with different optical colours have fundamentally different dust emission properties. Results indicate that while blue galaxies are more luminous than red galaxies due to higher temperatures, the dust masses of the two samples are relatively similar. Dust mass is shown to correlate with stellar mass, although the dust-to-stellar mass ratio is much higher for low stellar mass galaxies, consistent with the lowest mass galaxies having the highest specific star formation rates. We stack the 250 mu m-to-NUV luminosity ratio, finding results consistent with greater obscuration of star formation at lower stellar mass and higher redshift. Submillimetre luminosities and dust masses of all galaxies are shown to evolve strongly with redshift, indicating a fall in the amount of obscured star formation in ordinary galaxies over the last four billion years.en
dc.format.extent33
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/embargoed
dc.titleHerschel -ATLAS/GAMA : a census of dust in optically selected galaxies from stacking at submillimetre wavelengthsen
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.embargoedUntil2012-11-01
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2012.20528.x
rioxxterms.licenseref.startdate2012-11-01Z
rioxxterms.typeOther
herts.preservation.rarelyaccessedtrue
herts.date.embargo2012-11-01Z
herts.rights.accesstypeopenAccess


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