\approx2.3$. Finally, we note that in this model, the photosphere blackbody had a temperature of $2.05\pm0.06$keV and a radius of $6.6\pm0.7$km. While the temperature is consistent with the double blackbody model, the radius is significantly smaller.

The double blackbody and reflection models both provide a statistically acceptable description of the spectrum, and give a roughly equivalent interpretation. Since the double blackbody model is phenomenologically simpler, it can be fit robustly to much shorter integration times, yielding a higher time resolution view of the spectral evolution in the burst. In the following we will therefore focus our analysis on this model.

We extracted spectra from three other distinct time intervals during the burst: the pause (0.6[[s]{}]{}), the dip (0.7[[s]{}]{}), and the second peak (2[[s]{}]{}). Each spectrum could be described with the double blackbody spectrum plus $6.7$[[keV]{}]{}`diskline` component. The second peak additionally required an emission line at 1 keV. These spectra are shown in Figure \[fig:spectra\] and their best-fit parameters are listed in Table \[tab:spectra\].

[ l l l C C C C ]{} & & & & & &\
Soft blackbody & temperature & keV & 0.2330.003 & 0.2280.007 & 0.2100.005 & 0.220.01\
Soft blackbody & normalization & km & 318 