Fig. 1
Lightcurve of the Fermi burst 091030.613 measured by the 3rd GBM-detector without any background filtering with 1-s bins. The grey line is a fitted polynomial function of time of order 3 for the ranges of [− 200:− 20] and [38:200] s, which does not seem to be a correct model for this whole background. Reduced chi-square statistics are given in the top right corner (Szécsi et al. 2012a).
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