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Fig. 1


Spectral flux per log frequency interval νFν for the downstream synchrotron emission (red), the downstream inverse Compton spectrum (purple), and the precursor synchrotron signal (shaded area). This last shaded area is bracketed by the two extreme models of regular deflection (lower curve, model (1)) or stochastic small-angle deflection (upper curve, model (2)). The parameters of the model are indicated in the figure. For panels a) and b), representative of the external shock of a long gamma-ray burst at different times, the redshift is z = 1; for panel c), representative of a low-luminosity gamma-ray burst or trans-relativistic supernova, z = 0.01.

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