the burst and emission features in the burst spectrum. We now discuss each of these findings.

Reflection
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We find that the burst spectrum shows a strong excess at the lowest energies that requires the inclusion of a second blackbody in the spectral model. A similar strong soft excess was previously observed in [SAX J1808]{}by @Zand2013. In contrast to that work, however, we also observe emission features at 1 keV and 6.7keV. A similar complex of emission features has been seen in the intermediate-duration X-ray bursts from IGR J17062–6143 [@Degenaar2013; @Keek2017], which were associated with ionized FeL and FeK emission lines. Thus, the detection of these lines provides strong evidence that we are seeing the burst emission reflected from the accretion disk. Applying a physically motivated disk reflection model to our data (Section \[sec:spectra\]) indicates that such a reflection component provides a satisfactory description of the soft excess, but cannot fully account for the emission feature observed at 1keV. We suggest that this may be due to the presence of additional elements not currently incorporated in these models (e.g. Ne). Additionally, this model fit indicated a strong reflection signal, which may indicate that the accretion disk structure is significantly impacted 