Comparison between star-formation rates derived from SED fitting (SFR_SED) and from the extinction-corrected Hα luminosity (SFR_Hα), for different calculations of the extinction coefficient c(Hβ) for the galaxies without an available Balmer decrement. From left to right: E(B−V)_gas = E(B−V)_stellar (Reddy et al. 2010); E(B−V)_gas = E(B−V)_stellar + E(B−V)_extra (Wuyts et al. 2013); E(B−V)_gas = E(B−V)_stellar/ 0.44 (Calzetti et al. 2000). In the last panel, the orange crosses represent the galaxies with Balmer decrement available, for which the SFR_Hα are consistent with the SFR_SED and no systematic trend is observed.