Ratio of M_dust/SFR plotted against sSFR. As in Fig. 4, the GRBHs observed by Herschel are indicated by filled (for IR detections) and open (IR non-detections) circles, and the other galaxy samples shown are also coded as in Fig. 4. The three curves are the fits of sSFR vs. M_star at z = 0.2 − 0.4 (dotted left), z = 1.0 − 1.2 (dashed middle), and z = 2.0 − 2.5 (dot-dashed right) by Karim et al. (2011) as shown in Fig. 4, but here incorporating the dependence of M_dust on SFR as found at z ≈ 0 by da Cunha et al. (2010b) (see also Fig. 5).