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Caption: Figure 9.
Zoom in of our spectra around the expected locations of strong absorption lines, in particular the Mg II doublet in our blue FORS2 spectrum and Ca H and K in our MUSE observations. In addition to our observations, we also overplot the composite GRB afterglow spectrum from L. Christensen et al. (2011) as a comparison. We note that Mg II at z = 0.401 does not match; an offset to z = 0.398 (500 km s−1) would line up with some strong features in the FORS2 spectrum. The low S/N in the spectrum means that the lack of strong absorption does not imply an unusually low-density line of site. For Ca H and K, the observations are also not sufficiently sensitive to strongly constrain the absorption properties, although they do imply that any absorption is likely somewhat less pronounced than in the average GRB spectrum.
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