of all, the light curve clearly mimics the observations, as expected, given that the Norris pulse model was designed for this purpose (e.g. Figure \[htslc\]). We should mention that a pulse stacking analysis by @hakkilapreece14 has shown that significant residuals exist on top of the Norris pulse shape that do not represent separate pulses; for example, there is a shoulder after the peak in Figure \[htslc\] at T+3 s as well as in the published GBM NaI light curve for GRB 130427A at roughly T+1.2 s. To keep the analysis simple, we do not include this effect here. Upon performing spectral fitting of each time bin, the simulated power-law [$E_{\rm peak}$]{} evolution from hard to soft ($E_{\rm hi} = 1500$ keV and $E_{\rm lo} = 100$ keV) is recovered from the simulation, as can be seen in Figure \[Sim\_EP\_Fit\]. In this simulation, the peak count rate was chosen to be extremely high, 40,000 count/s, even so, during the rise and decay portion of the pulse some low-count time bins had to be combined to achieve a minimum signal to noise threshold of 45. This threshold ensures that there are enough total counts in the binned spectra to do useful spectroscopy, 