Chandra HEG spectra of 1A 0535+262 taken at the times indicated in Figure  1. Emission lines from Fe Kα & Kβ are clearly detected in both observations and are consistent with no change within the errors. In contrast, absorption consistent with Fe xxv is only detected in the first observation. The exposure time was ~10 ks in each observation. Note: the data have been rebinned for visual clarity.