Novak, M.M.NovakSmolčić, V.V.SmolčićDelhaize, J.J.DelhaizeDELVECCHIO, IVANIVANDELVECCHIOZamorani, G.G.ZamoraniBaran, N.N.BaranBONDI, MARCOMARCOBONDICapak, P.P.CapakCarilli, C. L.C. L.CarilliCILIEGI, PaoloPaoloCILIEGICivano, F.F.CivanoIlbert, O.O.IlbertKarim, A.A.KarimLaigle, C.C.LaigleLe Fèvre, O.O.Le FèvreMARCHESI, STEFANOSTEFANOMARCHESIMcCracken, H.H.McCrackenMiettinen, O.O.MiettinenSalvato, M.M.SalvatoSargent, M.M.SargentSchinnerer, E.E.SchinnererTasca, L.L.Tasca2021-01-132021-01-1320170004-6361http://hdl.handle.net/20.500.12386/29738We make use of the deep Karl G. Jansky Very Large Array (VLA) COSMOS radio observations at 3 GHz to infer radio luminosity functions of star-forming galaxies up to redshifts of z 5 based on approximately 6000 detections with reliable optical counterparts. This is currently the largest radio-selected sample available out to z 5 across an area of 2 square degrees with a sensitivity of rms ≈ 2.3 μJy beam<SUP>-1</SUP>. By fixing the faint and bright end shape of the radio luminosity function to the local values, we find a strong redshift trend that can be fitted with a pure luminosity evolution L<SUB>1.4 GHz</SUB> ∝ (1 + z)<SUP>(3.16 ± 0.2)-(0.32 ± 0.07)z</SUP>. We estimate star formation rates (SFRs) from our radio luminosities using an infrared (IR)-radio correlation that is redshift dependent. By integrating the parametric fits of the evolved luminosity function we calculate the cosmic SFR density (SFRD) history since z 5. Our data suggest that the SFRD history peaks between 2 < z < 3 and that the ultraluminous infrared galaxies (100 M<SUB>☉</SUB> yr<SUP>-1</SUP> < SFR < 1000 M<SUB>☉</SUB> yr<SUP>-1</SUP>) contribute up to 25% to the total SFRD in the same redshift range. Hyperluminous infrared galaxies (SFR > 1000 M<SUB>☉</SUB> yr<SUP>-1</SUP>) contribute an additional ≲2% in the entire observed redshift range. We find evidence of a potential underestimation of SFRD based on ultraviolet (UV) rest-frame observations of Lyman break galaxies at high redshifts (z ≳ 4) on the order of 15-20%, owing to appreciable star formation in highly dust-obscured galaxies, which might remain undetected in such UV observations.STAMPAenArticle10.1051/0004-6361/2016294362-s2.0-85020720103000404648300024https://www.aanda.org/articles/aa/full_html/2017/06/aa29436-16/aa29436-16.html2017A&A...602A...5NFIS/05 - ASTRONOMIA E ASTROFISICA