(Left) Distribution of “distance” with respect to the main sequence observed in our SMG sample having accurate stellar masses estimates (empty histogram). The hatched histogram shows the distribution observed in a subsample of luminous SMGs with SFR > SFR, i.e., at 0 < z < 2 and L_IR ≳ 10^12.7   L_⊙ at z > 2. (Right) Dust temperature of SMGs as function of their distance with respect to the main sequence of star-formation. Blue squares show luminous SMGs with at 0 < z < 2 and L_IR ≳ 10^12.7   L_⊙ at z > 2. Green squares show SMGs with infrared luminosities below these thresholds. Red points represent the OFRGs, i.e., galaxies with relatively low infrared luminosities below our treshold. In both plots the location of the main sequence as function of the redshift is taken from Rodighiero et al. (2010). The 1σ scatter around this main sequence is illustrated by the shaded area.