Lo Faro, B.B.Lo FaroBuat, V.V.BuatRoehlly, Y.Y.RoehllyÁlvarez-Márquez, J.J.Álvarez-MárquezBurgarella, D.D.BurgarellaSILVA, LauraLauraSILVAEfstathiou, A.A.Efstathiou2021-04-192021-04-1920170035-8711http://hdl.handle.net/20.500.12386/30795In this work we investigate the far-UV to NIR shape of the dust attenuation curve of a sample of IR selected dust obscured (U)LIRGs at z$\sim$2. The spectral energy distributions (SEDs) are fitted with CIGALE, a physically-motivated spectral synthesis model based on energy balance. Its flexibility allows us to test a wide range of different analytical prescriptions for the dust attenuation curve, including the well-known Calzetti and Charlot & Fall curves, and modified versions of them. The attenuation curves computed under the assumption of our reference double power-law model are in very good agreement with those derived, in previous works, with radiative transfer (RT) SED fitting. We investigate the position of our galaxies in the IRX-$\beta$ diagram and find this to be consistent with grayer slopes, on average, in the UV. We also find evidence for a flattening of the attenuation curve in the NIR with respect to more classical Calzetti-like recipes. This larger NIR attenuation yields larger derived stellar masses from SED fitting, by a median factor of $\sim$ 1.4 and up to a factor $\sim$10 for the most extreme cases. The star formation rate appears instead to be more dependent on the total amount of attenuation in the galaxy. Our analysis highlights the need for a flexible attenuation curve when reproducing the physical properties of a large variety of objects.STAMPAenArticle10.1093/mnras/stx19012-s2.0-85047780332https://academic.oup.com/mnras/article/472/2/1372/4044703FIS/05 - ASTRONOMIA E ASTROFISICA