Bourne, N.N.BourneDunlop, J. S.J. S.DunlopMERLIN, EmilianoEmilianoMERLINParsa, S.S.ParsaSchreiber, C.C.SchreiberCASTELLANO, MARCOMARCOCASTELLANOConselice, C. J.C. J.ConseliceCoppin, K. E. K.K. E. K.CoppinFarrah, D.D.FarrahFONTANA, AdrianoAdrianoFONTANAGeach, J. E.J. E.GeachHalpern, M.M.HalpernKnudsen, K. K.K. K.KnudsenMichałowski, M. J.M. J.MichałowskiMortlock, A.A.MortlockSANTINI, PaolaPaolaSANTINIScott, D.D.ScottShu, X. W.X. W.ShuSimpson, C.C.SimpsonSimpson, J. M.J. M.SimpsonSmith, D. J. B.D. J. B.Smithvan der Werf, P. P.P. P.van der Werf2021-02-082021-02-0820170035-8711http://hdl.handle.net/20.500.12386/30241We 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-μm imaging from SCUBA-2 CLS, covering 230 arcmin<SUP>2</SUP> in the AEGIS, COSMOS and UDS fields, together with 100-250 μm imaging from Herschel. We demonstrate the capability of the t-phot deconfusion code to reach below the confusion limit, using multiwavelength 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 ∼ 5, indicating that UV-derived dust corrections underestimate the SFR in massive galaxies. We investigate the relationship between obscuration and the UV slope (the IRX-β 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_{☉} galaxies at 0.5 < z < 6. This is dominated by obscured star formation by a factor of >10. One third of this is accounted for by 450-μm-detected sources, while one-fifth is attributed to UV-luminous sources (brighter than L_UV^\ast), 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 ≲ 3, and from UV-only data at z ∼ 5. The cosmic star formation history undergoes a transition at z ∼ 3-4, 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.STAMPAenArticle10.1093/mnras/stx0312-s2.0-85018275840000398416700009https://academic.oup.com/mnras/article/467/2/1360/28772302017MNRAS.467.1360BFIS/05 - ASTRONOMIA E ASTROFISICA