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dc.contributor.authorBourne, N.en
dc.contributor.authorDunlop, J. S.en
dc.contributor.authorMerlin, E.en
dc.contributor.authorParsa, S.en
dc.contributor.authorSchreiber, C.en
dc.contributor.authorCastellano, M.en
dc.contributor.authorConselice, C. J.en
dc.contributor.authorCoppin, K. E. K.en
dc.contributor.authorFarrah, D.en
dc.contributor.authorFontana, A.en
dc.contributor.authorGeach, J. E.en
dc.contributor.authorHalpern, M.en
dc.contributor.authorKnudsen, K. K.en
dc.contributor.authorMichalowski, M. J.en
dc.contributor.authorMortlock, A.en
dc.contributor.authorSantini, P.en
dc.contributor.authorScott, D.en
dc.contributor.authorShu, X. W.en
dc.contributor.authorSimpson, C.en
dc.contributor.authorSimpson, J. M.en
dc.contributor.authorSmith, D. J. B.en
dc.contributor.authorWerf, P. V. D.en
dc.date.accessioned2017-02-24T17:15:58Zen
dc.date.available2017-02-24T17:15:58Zen
dc.identifier.urihttp://hdl.handle.net/10919/75143en
dc.description.abstractWe present a new exploration of the cosmic star-formation history and dust obscuration in massive galaxies at redshifts $0.5< z<6$. We utilize the deepest 450 and 850$\mu$m imaging from SCUBA-2 CLS, covering 230arcmin$^2$ in the AEGIS, COSMOS and UDS fields, together with 100-250$\mu$m imaging from Herschel. We demonstrate the capability of the T-PHOT deconfusion code to reach below the confusion limit, using multi-wavelength prior catalogues from CANDELS/3D-HST. By combining IR and UV data, we measure the relationship between total star-formation rate (SFR) and stellar mass up to $z\sim5$, indicating that UV-derived dust corrections underestimate the SFR in massive galaxies. We investigate the relationship between obscuration and the UV slope (the IRX-$\beta$ relation) in our sample, which is similar to that of low-redshift starburst galaxies, although it deviates at high stellar masses. Our data provide new measurements of the total SFR density (SFRD) in $M_\ast>10^{10}M_\odot$ galaxies at $0.510$. One third of this is accounted for by 450$\mu$m-detected sources, while one fifth is attributed to UV-luminous sources (brighter than $L^\ast_{UV}$), although even these are largely obscured. By extrapolating our results to include all stellar masses, we estimate a total SFRD that is in good agreement with previous results from IR and UV data at $z\lesssim3$, and from UV-only data at $z\sim5$. The cosmic star-formation history undergoes a transition at $z\sim3-4$, as predominantly unobscured growth in the early Universe is overtaken by obscured star formation, driven by the build-up of the most massive galaxies during the peak of cosmic assembly.en
dc.relation.urihttp://arxiv.org/abs/1607.04283v3en
dc.relation.urihttp://dx.doi.org/10.1093/mnras/stx031en
dc.rightsIn Copyrighten
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en
dc.subjectastro-ph.GAen
dc.subjectastro-ph.GAen
dc.subjectastro-ph.IMen
dc.titleEvolution of cosmic star formation in the SCUBA-2 Cosmology Legacy Surveyen
dc.typeArticleen
dc.contributor.departmentPhysicsen
dc.description.notesMNRAS Accepted 2017 January 5. 29 pages, 18 figuresen
dc.identifier.doihttps://doi.org/10.1093/mnras/stx031en
pubs.organisational-group/Virginia Techen
pubs.organisational-group/Virginia Tech/All T&R Facultyen
pubs.organisational-group/Virginia Tech/Scienceen
pubs.organisational-group/Virginia Tech/Science/COS T&R Facultyen
pubs.organisational-group/Virginia Tech/Science/Physicsen


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