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dc.contributor.authorLapi, A.
dc.contributor.authorGonzález-Nuevo, J.
dc.contributor.authorFan, L.
dc.contributor.authorBressan, A.
dc.contributor.authorde Zotti, G.
dc.contributor.authorDanese, L.
dc.contributor.authorButtiglione, S.
dc.contributor.authorNegrello, M.
dc.contributor.authorHopwood, R.
dc.contributor.authorSerjeant, S.
dc.contributor.authorDunne, L.
dc.contributor.authorMaddox, S.
dc.contributor.authorRigby, E.
dc.contributor.authorEales, S.
dc.contributor.authorAuld, R.
dc.contributor.authorDariush, A.
dc.contributor.authorDye, S.
dc.contributor.authorKaviraj, S.
dc.contributor.authorPascale, E.
dc.contributor.authorPohlen, M.
dc.contributor.authorBaes, M.
dc.contributor.authorFritz, J.
dc.contributor.authorBonfield, D.G.
dc.contributor.authorJarvis, M.J.
dc.contributor.authorSmith, Daniel
dc.contributor.authorCava, A.
dc.contributor.authorClements, D. L.
dc.contributor.authorDariush, A.
dc.contributor.authorHopwood, R.
dc.contributor.authorCooray, A.
dc.contributor.authorWardlow, J.
dc.contributor.authorHerranz, D.
dc.contributor.authorLópez-Caniego, M.
dc.contributor.authorIbar, E.
dc.contributor.authorIvison, R.
dc.contributor.authorMichałowski, M. J.
dc.contributor.authorJarvis, M.J.
dc.contributor.authorMassardi, M.
dc.contributor.authorRodighiero, G.
dc.contributor.authorTemi, P.
dc.contributor.authorVan Der Werf, P.
dc.date.accessioned2011-11-29T14:01:04Z
dc.date.available2011-11-29T14:01:04Z
dc.date.issued2011
dc.identifier.citationLapi , A , González-Nuevo , J , Fan , L , Bressan , A , de Zotti , G , Danese , L , Buttiglione , S , Negrello , M , Hopwood , R , Serjeant , S , Dunne , L , Maddox , S , Rigby , E , Eales , S , Auld , R , Dariush , A , Dye , S , Kaviraj , S , Pascale , E , Pohlen , M , Baes , M , Fritz , J , Bonfield , D G , Jarvis , M J , Smith , D , Cava , A , Clements , D L , Dariush , A , Hopwood , R , Cooray , A , Wardlow , J , Herranz , D , López-Caniego , M , Ibar , E , Ivison , R , Michałowski , M J , Jarvis , M J , Massardi , M , Rodighiero , G , Temi , P & Van Der Werf , P 2011 , ' Herschel-atlas galaxy counts and high-redshift luminosity functions : The formation of massive early-type galaxies ' , The Astrophysical journal , vol. 742 , no. 1 , 24 . https://doi.org/10.1088/0004-637X/742/1/24
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 463352
dc.identifier.otherPURE UUID: 200dbda9-f6a7-4361-b41a-05680ca553bc
dc.identifier.otherScopus: 80755171478
dc.identifier.otherORCID: /0000-0001-9708-253X/work/69424285
dc.identifier.urihttp://hdl.handle.net/2299/7183
dc.description‘In these times, during the rise in the popularity of institutional repositories, the Society does not forbid authors from depositing their work in such repositories. However, the AAS regards the deposit of scholarly work in such repositories to be a decision of the individual scholar, as long as the individual's actions respect the diligence of the journals and their reviewers.’ Original article can be found at : http://iopscience.iop.org/ Copyright American Astronomical Society
dc.description.abstractExploiting the Herschel Astrophysical Terahertz Large Area Survey Science Demonstration Phase survey data, we have determined the luminosity functions (LFs) at rest-frame wavelengths of 100 and 250 μm and at several redshifts z ≳ 1, for bright submillimeter galaxies with star formation rates (SFRs) ≳ 100 M yr. We find that the evolution of the comoving LF is strong up to ≈ z 2.5, and slows down at higher redshifts. From the LFs and the information on halo masses inferred from clustering analysis, we derived an average relation between SFR and halo mass (and its scatter). We also infer that the timescale of the main episode of dust-enshrouded star formation in massive halos (M ≳ 3 × 10 M ) amounts to ∼7 × 10 yr. Given the SFRs, which are in the range of 10-10 M yr, this timescale implies final stellar masses of the order of 10-10 M . The corresponding stellar mass function matches the observed mass function of passively evolving galaxies at z ≳ 1. The comparison of the statistics for submillimeter and UV-selected galaxies suggests that the dust-free, UV bright phase is ≳ 10 times shorter than the submillimeter bright phase, implying that the dust must form soon after the onset of star formation. Using a single reference spectral energy distribution (SED; the one of the z ≈ 2.3 galaxy SMM J2135-0102), our simple physical model is able to reproduce not only the LFs at different redshifts >1 but also the counts at wavelengths ranging from 250 μm to 1mm. Owing to the steepness of the counts and their relatively broad frequency range, this result suggests that the dispersion of submillimeter SEDs of z > 1 galaxies around the reference one is rather small.en
dc.format.extent21
dc.language.isoeng
dc.relation.ispartofThe Astrophysical journal
dc.subjectgalaxies: evolution
dc.subjectgalaxies: formation
dc.subjectgalaxies: high-redshift
dc.subjectsubmillimeter: galaxies
dc.titleHerschel-atlas galaxy counts and high-redshift luminosity functions : The formation of massive early-type galaxiesen
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=80755171478&partnerID=8YFLogxK
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-637X/742/1/24
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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