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Fig. 6

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Same as Fig. 5, but including a foreground cloud situated between the GRB and the observed absorber. The solid and dotted lines correspond to the best-fitting model, assuming the default and Littlejohns input flux, respectively. The foreground absorber is mostly ionized by the time of the second epoch UVES spectrum and can therefore escape a clear detection. See the text and Table 3 for more details.

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