Fudamoto, Y.Y.FudamotoOesch, P. A.P. A.OeschFaisst, A.A.FaisstBéthermin, M.M.BétherminGinolfi, M.M.GinolfiKhusanova, Y.Y.KhusanovaLoiacono, F.F.LoiaconoLe Fèvre, O.O.Le FèvreCapak, P.P.CapakSchaerer, D.D.SchaererSilverman, J. D.J. D.SilvermanCassata, P.P.CassataYan, L.L.YanAmorin, R.R.AmorinBARDELLI, SandroSandroBARDELLIBoquien, M.M.BoquienCimatti, A.A.CimattiDessauges-Zavadsky, M.M.Dessauges-ZavadskyFujimoto, S.S.FujimotoGRUPPIONI, CarlottaCarlottaGRUPPIONIHathi, N. P.N. P.HathiIbar, E.E.IbarJones, G. C.G. C.JonesKoekemoer, A. M.A. M.KoekemoerLagache, G.G.LagacheLemaux, B. C.B. C.LemauxMaiolino, R.R.MaiolinoNarayanan, D.D.NarayananPozzi, F.F.PozziRiechers, D. A.D. A.RiechersRodighiero, G.G.RodighieroTalia, M.M.TaliaToft, S.S.ToftVALLINI, LiviaLiviaVALLINIVERGANI, DANIELADANIELAVERGANIZamorani, G.G.ZamoraniZUCCA, ElenaElenaZUCCA2025-03-142025-03-1420200004-6361http://hdl.handle.net/20.500.12386/36776We present dust attenuation properties of spectroscopically confirmed star forming galaxies on the main sequence at a redshift of ∼4.4 - 5.8. Our analyses are based on the far infrared continuum observations of 118 galaxies at rest-frame 158 μm obtained with the Atacama Large Millimeter Array (ALMA) Large Program to INvestigate [CII] at Early times (ALPINE). We study the connection between the ultraviolet (UV) spectral slope (β), stellar mass (M<SUB>⋆</SUB>), and infrared excess (IRX = L<SUB>IR</SUB>/L<SUB>UV</SUB>). Twenty-three galaxies are individually detected in the continuum at > 3.5σ significance. We perform a stacking analysis using both detections and nondetections to study the average dust attenuation properties at z ∼ 4.4 - 5.8. The individual detections and stacks show that the IRX-β relation at z ∼ 5 is consistent with a steeper dust attenuation curve than typically found at lower redshifts (z < 4). The attenuation curve is similar to or even steeper than that of the extinction curve of the Small Magellanic Cloud. This systematic change of the IRX-β relation as a function of redshift suggests an evolution of dust attenuation properties at z > 4. Similarly, we find that our galaxies have lower IRX values, up to 1 dex on average, at a fixed mass compared to previously studied IRX-M<SUB>⋆</SUB> relations at z ≲ 4, albeit with significant scatter. This implies a lower obscured fraction of star formation than at lower redshifts. Our results suggest that dust properties of UV-selected star forming galaxies at z ≳ 4 are characterised by (i) a steeper attenuation curve than at z ≲ 4, and (ii) a rapidly decreasing dust obscured fraction of star formation as a function of redshift. Nevertheless, even among this UV-selected sample, massive galaxies (log M<SUB>⋆</SUB>/M<SUB>⊙</SUB> > 10) at z ∼ 5 - 6 already exhibit an obscured fraction of star formation of ∼45%, indicating a rapid build-up of dust during the epoch of reionization.STAMPAenArticle10.1051/0004-6361/2020381632-s2.0-85095114868https://www.aanda.org/articles/aa/full_html/2020/11/aa38163-20/aa38163-20.htmlhttp://arxiv.org/abs/2004.10760v22020A&A...643A...4FFIS/05 - ASTRONOMIA E ASTROFISICA