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dc.contributor.authorRowlands, K.
dc.contributor.authorDunne, L.
dc.contributor.authorMaddox, S.
dc.contributor.authorBourne, N.
dc.contributor.authorBamford, S. P.
dc.contributor.authorSmith, Daniel
dc.contributor.authorDye, S.
dc.contributor.authorRigby, E.E.
dc.contributor.authorGomez, H.L.
dc.contributor.authorEales, S.A.
dc.contributor.authorKaviraj, S.
dc.contributor.authorDariush, A.
dc.contributor.authorHopwood, R.
dc.contributor.authorBrough, S.
dc.contributor.authorHopkins, A. M.
dc.contributor.authorCharlot, S.
dc.contributor.authorda Cunha, E.
dc.contributor.authorDriver, S. P.
dc.contributor.authorKelvin, L.
dc.contributor.authorRobotham, A.
dc.contributor.authorNichol, R.C.
dc.contributor.authorSansom, A. E.
dc.contributor.authorPopescu, C.C.
dc.contributor.authorSharp, R.
dc.contributor.authorTemi, P.
dc.contributor.authorvan der Werf, P.
dc.contributor.authorBaes, M.
dc.contributor.authorFritz, J.
dc.contributor.authorCava, A.
dc.contributor.authorCooray, A.
dc.contributor.authorCroom, S. M.
dc.contributor.authorde Zotti, G.
dc.contributor.authorRodighiero, G.
dc.contributor.authorIbar, E.
dc.contributor.authorIvison, R.J.
dc.contributor.authorNorberg, P.
dc.contributor.authorLiske, J.
dc.contributor.authorLoveday, J.
dc.contributor.authorMadore, B.
dc.contributor.authorSeibert, M.
dc.contributor.authorTuffs, R. J.
dc.date.accessioned2013-08-14T12:15:07Z
dc.date.available2013-08-14T12:15:07Z
dc.date.issued2012
dc.identifier.citationRowlands , K , Dunne , L , Maddox , S , Bourne , N , Bamford , S P , Smith , D , Dye , S , Rigby , E E , Gomez , H L , Eales , S A , Kaviraj , S , Dariush , A , Hopwood , R , Brough , S , Hopkins , A M , Charlot , S , da Cunha , E , Driver , S P , Kelvin , L , Robotham , A , Nichol , R C , Sansom , A E , Popescu , C C , Sharp , R , Temi , P , van der Werf , P , Baes , M , Fritz , J , Cava , A , Cooray , A , Croom , S M , de Zotti , G , Rodighiero , G , Ibar , E , Ivison , R J , Norberg , P , Liske , J , Loveday , J , Madore , B , Seibert , M & Tuffs , R J 2012 , ' Herschel -ATLAS/GAMA : Dusty early-type galaxies and passive spirals ' , Monthly Notices of the Royal Astronomical Society , vol. 419 , no. 3 , pp. 2545-2578 . https://doi.org/10.1111/j.1365-2966.2011.19905.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 2067755
dc.identifier.otherPURE UUID: a8cae11c-e172-4dcc-9ce5-a3525aaad6f5
dc.identifier.otherScopus: 84855344802
dc.identifier.urihttp://hdl.handle.net/2299/11347
dc.description.abstractWe present the dust properties and star-formation histories of local submillimetre-selected galaxies, classified by optical morphology. Most of the galaxies are late types and very few are early types. The early-type galaxies that are detected contain as much dust as typical spirals, and form a unique sample that has been blindly selected at submillimetre wavelengths. Additionally, we investigate the properties of the most passive, dusty spirals. We morphologically classify 1087 galaxies detected in the Herschel -ATLAS Sci- ence Demonstration Phase data. Comparing to a control sample of optically selected galaxies, we find 5.5% of luminous early-type galaxies are detected in H-ATLAS. The H-ATLAS early-type galaxies contain a significant mass of cold dust: the mean dust mass is 5.5×107M⊙, with individual galaxies ranging from 9×105−4×108M⊙. This is comparable to that of spiral galaxies in our sample, and is an order of magnitude more dust than that found for the control early-types, which have a median dust mass inferred from stacking of (0.8− 4.0)×106M⊙ for a cold dust temperature of 25-15 K. The early-types detected in H-ATLAS tend to have bluer NUV −r colours, higher specific star-formation rates and younger stellar populations than early-types which are optically selected, and may be transitioning from the blue cloud to the red sequence. We also find that H-ATLAS and control early-types inhabit similar low-density environments. We investigate whether the observed dust in H-ATLAS early-types is from evolved stars, or has been acquired from external sources through interactions and mergers. We conclude that the dust in H-ATLAS and control ETGs cannot be solely from stellar sources, and a large contribution from dust formed in the ISM or external sources is required. Alternatively, dust destruction may not be as efficient as predicted. We also explore the properties of the most passive spiral galaxies in our sample with SSFR< 10−11yr−1. We find these passive spirals have lower dust-to-stellar mass ratios, higher stellar masses and older stellar population ages than normal spirals. The passive spirals inhabit low density environments similar to those of the normal spiral galaxies in our sample. This shows that the processes which turn spirals passive do not occur solely in the intermediate density environments of group and cluster outskirts.en
dc.format.extent34
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.titleHerschel -ATLAS/GAMA : Dusty early-type galaxies and passive spiralsen
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=84855344802&partnerID=8YFLogxK
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeSubmitted Version
dcterms.dateAccepted2012
rioxxterms.versionSMUR
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2011.19905.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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