Comparison of observed DFRDs with models. Top: DFRDs color-coded with log₁₀age_main. The individual symbols were computed assuming a PL+OT_MBB emission. We clearly observe an age sequence from right to left. The lines show the trend assuming different dust emissions and different values for κ₀. The top one assumes DL2014 dust emission. The second one from the top was derived when using an optically thin modified blackbody with κ₀ = 0.637 m² kg⁻¹ (PL+OT_MBB). We note that the factor 0.37 needed to match DL2014 to PL+OT_MBB emission was not applied. The third one from the top assumes optically thin modified blackbodies with κ₀ corresponding to SNe dust mass absorption coefficients. It corresponds to the situation before the SNe reverse shock destruction, and the bottom line represents after the reverse shock destruction. Both from Hirashita et al. (2017). Bottom: same models as in as (a). The same objects plotted in (a) are color-coded in M_star. A sample of DSFGs (Table 8), also color-coded in M_star, was added to the plot with the code as follows: the upper triangle shows the maximum value, and the lower triangle shows the minimum value. These high redshift DSFGs are found on the same sequence as the other objects. However, these DSFGs have stellar masses larger than the underlying galaxy population that we study. It is important to note that the physical parameters (especially M_star because the IR emission is dominant) of these high redshift DSFGs have very large uncertainties and their position location in the diagram can almost cover the entire plot. Better estimates of these parameters coming from JWST would help.