M_d/M_∗ as a function of SFR. The same galaxy samples are shown as in Fig. 6, in addition to a sample of star forming lensed galaxies from Sklias et al. (2014; small grey squares), and a sample of SMGs from Magnelli et al. (2012b; orange triangles). The solid black line is our best-fit power law to all galaxy samples combined, not including the GRBH sample (M_d/M_∗ = 0.001 × SFR^0.3), and the dashed lines correspond the 3σ dispersion.