5 & 24017 & 29718 & 23631\
Hard blackbody & temperature & keV & 1.830.03 & 2.50.2 & 2.520.14 & 1.990.11\
Hard blackbody & normalization & km & 14.70.3 & 6.20.5 & 6.80.4 & 10.50.7\
Gaussian line & line energy & keV & 1.050.02 & & & 1.050.02\
Gaussian line & standard deviation& keV & 0.05\_[-0.02]{}\^[+0.07]{}& & & 0.070.02\
Gaussian line & normalization & [[ph[cm$^{-2}$]{}[s$^{-1}$]{}]{}]{}& 0.270.07 & & & 0.260.07\
diskline & line energy & keV & 6.7\_[-0.3]{}\^[+0.1]{} & 6.70.1 & 6.70.1 & 6.80.1\
diskline & inclination & degrees & 65 & 65 & 65 & 65\
diskline & inner radius & GM/c$^2$& 11 & 11 & 11 & 11\
diskline & normalization & [[ph[cm$^{-2}$]{}[s$^{-1}$]{}]{}]{}& 0.620.16 & 0.470.14 & 0.50.2 & 0.450.16\
[$\chi^2_r$]{}/ dof & & & 1.07/624 & 1.13/182 & 1.05/264 & 1.17/487\

Time-resolved spectroscopy {#sec:time resolved}
--------------------------

To investigate the full spectral evolution of the X-ray burst, we applied high-resolution time-resolved spectroscopy. We extracted [133]{} spectra from dynamically allocated intervals. Each interval was constructed to have at least [0.125[[s]{}]{}]{} of exposure, and was increased as needed to include a minimum of [2000]{} counts. Each spectrum was then fit using the double blackbody model. For simplicity we did not 