The spectral energy distribution of the combined early emission during the time when the first six optical data points were obtained by Swift/UVOT white and v filters. The corresponding time intervals are listed in Table 2. The fluxes of the curves #2, 3, 4, 5, and 7 have been multiplied for clarity by 10^-1, 10^-2, 10^-3, 10^-4, and 10^-5, respectively. The fits for #2, 3 were obtained by fixing the high-energy slope to the corresponding slope obtained for SED #1, the low-energy slope to 1/3, and by matching the expected break energy following the nonstandard LAE model (Sect. 3.1.3).