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In this work we investigate the far-UV to NIR shape of the dust attenuationcurve of a sample of IR selected dust obscured (U)LIRGs at z$\sim$2. Thespectral energy distributions (SEDs) are fitted with CIGALE, aphysically-motivated spectral synthesis model based on energy balance. Itsflexibility allows us to test a wide range of different analyticalprescriptions for the dust attenuation curve, including the well-known Calzettiand Charlot & Fall curves, and modified versions of them. The attenuationcurves computed under the assumption of our reference double power-law modelare in very good agreement with those derived, in previous works, withradiative transfer (RT) SED fitting. We investigate the position of ourgalaxies in the IRX-$\beta$ diagram and find this to be consistent with grayerslopes, on average, in the UV. We also find evidence for a flattening of theattenuation curve in the NIR with respect to more classical Calzetti-likerecipes. This larger NIR attenuation yields larger derived stellar masses fromSED fitting, by a median factor of $\sim$ 1.4 and up to a factor $\sim$10 forthe most extreme cases. The star formation rate appears instead to be moredependent on the total amount of attenuation in the galaxy. Our analysishighlights the need for a flexible attenuation curve when reproducing thephysical properties of a large variety of objects.

Characterizing the UV-to-NIR shape of the dust attenuation curve of IR luminous galaxies up to z$\sim$2