we also fit the spectrum using the reflection models of @Ballantyne2004b. This overall model is summarized as

> `tbabs( bbodyrad + diskbb + nthcomp + rdblur*atable{reflection} )`

where `rdblur` is a convolution component that applies the relativistic effects associated with an accretion disk around a compact object, and the `reflection` component tabulates reflection spectra calculated for a hydrogen density of $n_H=10^{18}\,{\rm cm}^{-3}$, using a grid in temperature ($kT$), ionization ($\log \xi$), and Fe abundance ($\log
  {\rm Fe}$). As before, we kept the parameters for the absorption column and preburst components fixed. The temperature parameter of the reflection table was linked to the blackbody temperature, and the `rdblur` parameters were identical to those of the `diskline` component discussed above. This model yielded a reasonable description of the continuum ([$\chi^2_r$]{}of 1.2 for 628 dof), but left a large residual at 1 keV. Adding in a Gaussian component gave a good fit to the data at a [$\chi^2_r$]{}of 0.95 for 633 dof, with a normalization of $0.86\pm0.15$[[ph[cm$^{-2}$]{}[s$^{-1}$]{}]{}]{}and standard deviation $0.09\pm0.02$[[keV]{}]{}. The best-fit parameters for the reflection component were $\log \xi=3.79_{-0.08}^{+0.11}$, $\log {\rm Fe}=0.51_{-0.24}^{+0.10}$, and an unabsorbed bolometric reflection flux of $(1.87\pm0.13){\ensuremath{\times 10^{-7}} }$[[erg[s$^{-1}$]{}[cm$^{-2}$]{}]{}]{}, indicating the reflection fraction is $F_{\rm refl} / F_{\rm bb} 