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dc.contributor.authorDariush, A.
dc.contributor.authorDib, S.
dc.contributor.authorHony, S.
dc.contributor.authorSmith, D. J. B.
dc.contributor.authorZhukovska, S.
dc.contributor.authorDunne, L.
dc.contributor.authorEales, S.
dc.contributor.authorAndrae, E.
dc.contributor.authorBaes, M.
dc.contributor.authorBaldry, I.
dc.contributor.authorBauer, A.
dc.contributor.authorBland-Hawthorn, J.
dc.contributor.authorBrough, S.
dc.contributor.authorBourne, N.
dc.contributor.authorCava, A.
dc.contributor.authorClements, D.
dc.contributor.authorCluver, M.
dc.contributor.authorCooray, A.
dc.contributor.authorZotti, G. De
dc.contributor.authorDriver, S.
dc.contributor.authorGrootes, M. W.
dc.contributor.authorHopkins, A. M.
dc.contributor.authorHopwood, R.
dc.contributor.authorKaviraj, S.
dc.contributor.authorKelvin, L.
dc.contributor.authorLara-Lopez, M. A.
dc.contributor.authorLiske, J.
dc.contributor.authorLoveday, J.
dc.contributor.authorMaddox, S.
dc.contributor.authorMadore, B.
dc.contributor.authorMichalowski, M. J.
dc.contributor.authorPearson, C.
dc.contributor.authorPopescu, C.
dc.contributor.authorRobotham, A.
dc.contributor.authorRowlands, K.
dc.contributor.authorSeibert, M.
dc.contributor.authorShabani, F.
dc.contributor.authorSmith, M. W. L.
dc.contributor.authorTaylor, E. N.
dc.contributor.authorTuffs, R.
dc.contributor.authorValiante, E.
dc.contributor.authorVirdee, J. S.
dc.date.accessioned2017-07-10T12:08:19Z
dc.date.available2017-07-10T12:08:19Z
dc.date.issued2016-02-21
dc.identifier.citationDariush , A , Dib , S , Hony , S , Smith , D J B , Zhukovska , S , Dunne , L , Eales , S , Andrae , E , Baes , M , Baldry , I , Bauer , A , Bland-Hawthorn , J , Brough , S , Bourne , N , Cava , A , Clements , D , Cluver , M , Cooray , A , Zotti , G D , Driver , S , Grootes , M W , Hopkins , A M , Hopwood , R , Kaviraj , S , Kelvin , L , Lara-Lopez , M A , Liske , J , Loveday , J , Maddox , S , Madore , B , Michalowski , M J , Pearson , C , Popescu , C , Robotham , A , Rowlands , K , Seibert , M , Shabani , F , Smith , M W L , Taylor , E N , Tuffs , R , Valiante , E & Virdee , J S 2016 , ' H-ATLAS/GAMA : The nature and characteristics of optically red galaxies detected at submillimetre wavelengths ' , Monthly Notices of the Royal Astronomical Society , vol. 456 , no. 2 , pp. 2221-2259 . https://doi.org/10.1093/mnras/stv2767
dc.identifier.issn0035-8711
dc.identifier.otherArXiv: http://arxiv.org/abs/1511.08018v1
dc.identifier.otherORCID: /0000-0001-9708-253X/work/69424308
dc.identifier.otherORCID: /0000-0002-5601-575X/work/77850159
dc.identifier.urihttp://hdl.handle.net/2299/18844
dc.descriptionThe Version of Record is available at: https://doi.org/10.1093/mnras/stv2767 © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
dc.description.abstractWe combine Herschel/SPIRE sub-millimeter (submm) observations with existing multi-wavelength data to investigate the characteristics of low redshift, optically red galaxies detected in submm bands. We select a sample of galaxies in the redshift range 0.01$\leq$z$\leq$0.2, having >5$\sigma$ detections in the SPIRE 250 micron submm waveband. Sources are then divided into two sub-samples of $red$ and $blue$ galaxies, based on their UV-optical colours. Galaxies in the $red$ sample account for $\approx$4.2 per cent of the total number of sources with stellar masses M$_{*}\gtrsim$10$^{10}$ Solar-mass. Following visual classification of the $red$ galaxies, we find that $\gtrsim$30 per cent of them are early-type galaxies and $\gtrsim$40 per cent are spirals. The colour of the $red$-spiral galaxies could be the result of their highly inclined orientation and/or a strong contribution of the old stellar population. It is found that irrespective of their morphological types, $red$ and $blue$ sources occupy environments with more or less similar densities (i.e., the $\Sigma_5$ parameter). From the analysis of the spectral energy distributions (SEDs) of galaxies in our samples based on MAGPHYS, we find that galaxies in the $red$ sample (of any morphological type) have dust masses similar to those in the $blue$ sample (i.e. normal spiral/star-forming systems). However, in comparison to the $red$-spirals and in particular $blue$ systems, $red$-ellipticals have lower mean dust-to-stellar mass ratios. Besides galaxies in the $red$-elliptical sample have much lower mean star-formation/specific-star-formation rates in contrast to their counterparts in the $blue$ sample. Our results support a scenario where dust in early-type systems is likely to be of an external origin.en
dc.format.extent9739416
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectastro-ph.GA
dc.titleH-ATLAS/GAMA : The nature and characteristics of optically red galaxies detected at submillimetre wavelengthsen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecord10.1093/mnras/stv2767
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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