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Fig. 7


Band functions for the six prompt emission peaks. Each coloured column shows the wavelength coverage of the instruments (We neglect GBM for clarity as it covers parts of the XRT and BAT.). They show that as the peak energy moves to lower energies the flux in the gamma-ray wavelengths decreases substantially in comparison to the higher peak energy. It can be seen that a higher flux in gamma-rays corresponds to a lower flux in the optical/NIR regime. No constraint on the peak energy was possible for 3a, 3d, and 3e, because they could lie anywhere below 0.1 keV, so were refit with a power law. The open circle depicts the (unsubtracted) J-band flux measured with GROND during Peak 2. The filled triangles are the X-ray and BAT gamma-ray data, and for reasons of clarity, we only show them for peaks 3b and 3d. The data has been corrected for the Galactic and host hydrogen absorption from the best-fit models. The best-fit parameters and goodness-of-fit for each of the peaks can be found in Table 3.

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