of time, it is possible to create time slices that can track the evolution of [$E_{\rm peak}$]{} (and $\alpha$) with good precision, while for the same temporal accumulations, $\beta$ can not be determined with any precision. The reason for this is that both the effective area and the flux fall rapidly with increasing energy, resulting in too few counts above [$E_{\rm peak}$]{} to determine the spectrum. Indeed, one of the results from the Compton Observatory’s Burst And Transient Source Experiment (BATSE) Catalog of time-resolved spectroscopy of bright bursts [@KanekoCat] was that the COMP function was preferred over the Band function in a majority of the spectra fit (34.9% vs. 33.7% for the BEST model; see Table 8 in the Catalog). It is possible that some GRB spectra arise from synchrotron emission from thermal electrons, especially just after the photosphere has become optically thin. In that case, the emission should resemble the COMP function with $\alpha \sim -2/3$. Even when a Band function fit is preferred, for example, as in the spectral analysis of the first pulse of the bright GRB 130427A [@preece2014], the Band $\beta$ parameter was required to be held fixed for each 0.1 s accumulation; otherwise, the extra 