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Fig. 4


X-/gamma-ray, NIR SED at the second prompt emission (T0 + 735   s), which is composed of BAT (green squares), XRT (purple upward-triangles), and GBM’s Na and N9 detectors (red rightward-triangles and cyan leftward-triangles, respectively). To make the plot more clear, the data points have been rebinned in energy, and the BGO detectors’ non-detections are not included but are consistent with the models. The best-fit models for the broken power law and Band models are depicted as the black and brown lines, respectively. The dashed lines correspond to the best-fit model with the effect of Galactic gas absorption. The inset shows a zoom in of the NIR wavelengths. The open green circle and triangles are with the expected afterglow flux subtracted, which was determined from the best-fit temporal power law. The transparent cyan and red dots denote the fluxes measured at T0 + 759 and T0 + 769 s, respectively, which can also be seen in Fig. 5.

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