Extended Data Figure 1: Multiwavelength light curves for GRB 160625B and its afterglow.
From: Significant and variable linear polarization during the prompt optical flash of GRB 160625B
Different emission components shape the temporal evolution of GRB 160625B. On timescales of seconds to minutes after the explosion, we observe bright prompt (solid lines) and reverse-shock (dotted lines) components. On timescales of hours to weeks after the burst, emission from the forward shock (dashed lines) becomes the dominant component from X-rays down to radio energies. After about 14 days, the afterglow emission falls off at all wavelengths. This phenomenon, known as jet-break, is caused by the beamed geometry of the outflow. Error bars denote 1σ limits; upper limits are 3σ. Times are given with reference to the LAT trigger time T0. FS, forward shock; RS, reverse shock; a subscript ‘v’ refers to frequency; u, V, r, i, z, y, J and H denote specific optical filters.
