Star formation rate density found by integrating the best-fit curves of Figure A.1 between 8.0 < L_IR/L_⊙ < 14.0. Similarly to Figure 7, the black solid line represents the IR ρ_SFR evolution found in Madau & Dickinson (2014), while the blue dotted line shown the evolution of the UV ρ_SFR of Dunlop (2016). The shaded region shows the results of Casey et al. (2018), bounded at the bottom by the dust-poor models and at the top by the dust-rich models of the early Universe. The black circles with the solid curve represent this work’s results found in Section 3.2. Values of ρ_SFR corresponding to the modified Schechter fits (Eqaution A.1) with the best-fit α and σ parameters of −0.26 and 0.31, respectively, are shown with blue squares. Data found from modified Schechter fits with α and σ fixed at recent literature z ≪ 1 values of −0.2 and 0.5, respectively, are depicted with red crosses. It can be seen that, while using the modified Schechter function with all the parameters allowed to vary freely produces results almost identical to the classical Schechter results of this work, setting α and σ at the z ≪ 1 best-fit values if Gruppioni et al. (2013), produces significantly larger numbers at highest redshift bins.