Puglisi, A.A.PuglisiRodighiero, G.G.RodighieroFranceschini, A.A.FranceschiniTalia, M.M.TaliaCimatti, A.A.CimattiBaronchelli, I.I.BaronchelliDaddi, E.E.DaddiRenzini, A.A.RenziniSchawinski, K.K.SchawinskiMancini, C.C.ManciniSilverman, J.J.SilvermanGRUPPIONI, CarlottaCarlottaGRUPPIONILutz, D.D.LutzBerta, S.S.BertaOliver, S. J.S. J.Oliver2023-01-162023-01-1620160004-6361http://hdl.handle.net/20.500.12386/32864We combined the spectroscopic information from the 3D-HST survey with Herschel data to characterize the Hα dust attenuation properties of a sample of 79 main sequence star-forming galaxies at z ~ 1 in the GOODS-S field. The sample was selected in the far-IR at λ = 100 and/or 160 μm and only includes galaxies with a secure Hα detection (S/N > 3). From the low resolution 3D-HST spectra we measured the redshifts and the Hα fluxes for the whole sample. (A factor of 1/1.2 was applied to the observed fluxes to remove the [NII] contamination.) The stellar masses (M<SUB>⋆</SUB>), infrared (L<SUB>IR</SUB>), and UV luminosities (L<SUB>UV</SUB>) were derived from the spectral energy distributions by fitting multiband data from GALEX near-UV to SPIRE 500 μm. We estimated the continuum extinction E<SUB>star</SUB>(B-V) from both the IRX = L<SUB>IR</SUB>/L<SUB>UV</SUB> ratio and the UV-slope, β, and found excellent agreement between the two. The nebular extinction was estimated from comparison of the observed SFR<SUB>Hα</SUB> and SFR<SUB>UV</SUB>. We obtained f = E<SUB>star</SUB>(B-V) /E<SUB>neb</SUB>(B-V) = 0.93 ± 0.06, which is higher than the canonical value of f = 0.44 measured in the local Universe. Our derived dust correction produces good agreement between the Hα and IR+UV SFRs for galaxies with SFR ≳ 20M<SUB>☉</SUB>/yr and M<SUB>⋆</SUB> ≳ 5 × 10<SUP>10</SUP>M<SUB>☉</SUB>, while objects with lower SFR and M<SUB>⋆</SUB> seem to require a smaller f-factor (I.e. higher Hα extinction correction). Our results then imply that the nebular extinction for our sample is comparable to extinction in the optical-UV continuum and suggest that the f-factor is a function of both M<SUB>⋆</SUB> and SFR, in agreement with previous studies.STAMPAenArticle10.1051/0004-6361/2015267822-s2.0-84957031643https://www.aanda.org/articles/aa/full_html/2016/02/aa26782-15/aa26782-15.html2016A&A...586A..83PFIS/05 - ASTRONOMIA E ASTROFISICA