Fig. A.2
The afterglow of GRB 090426 after it has been shifted to the z = 1 system, again in comparison with the samples (shifted using the same method) of Kann et al. (2011, 2010). The labelling is identical to that in Fig. A.1. It can now clearly be seen that the afterglow of GRB 090426 is readily comparable to the afterglow of type II GRBs (collapsar events), while it is much brighter than any type I GRB afterglow (merging compact objects), with the exception of GRB 060121, which is a controversial case.
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