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Table 1.

Best-fit parameters for each different model used in the five SEDs reported in Fig. 4 of GRB 180720B.

Time interval Data Model Flux Ec Em p(β) ΓPL (d.o.f.)
[10−7 erg s−1 cm2] [keV] [keV]
0–35 s GBM Sync > 3.95(<  − 2.98) @ 3σ 1.56 (293)
[10 keV–40 MeV]
LLE PL 0.39 (11)
[30–100 MeV]
GBM+LLE Sync 1.52 (305)
[10 keV–100 MeV]
LAT PL
[100 MeV–100 GeV]

35–70 s GBM+LLE Sync 0.97(286)
[10 keV–100 MeV]
LAT PL
[100 MeV–100 GeV]

70–120 s XRT+BAT+GBM+LLE Sync 0.91 (465)
[0.5 keV–100 MeV]
LAT PL
[100 MeV–100 GeV]

120–200 s XRT+BAT+GBM PL −1.91 ± 0.05 0.86 (490)
[0.5 keV–40 MeV]
LAT PL
[100 MeV–100 GeV]

200–500 s XRT+BAT PL 0.06 ± 0.01 −1.86 ± 0.03 1.03 (276)
[0.5–150 keV]
LAT PL
[100 MeV–100 GeV]

Notes. The first column reports the time interval over which the spectrum has been integrated, the second column the detector whose data have been used to build the SED along with the energy range, and the third column represents the different models used to fit that data. From the fourth column onwards: energy flux computed in the energy range reported in the second column, photon energy corresponding to the electron cooling Lorentz factor Ec, photon energy corresponding to the electron injection Lorentz factor Em, electron energy distribution slope p (corresponding high-energy photon index β = −p/2 − 1 in parentheses), power-law photon index of the LLE/LAT data, and the reduced χ2 of the fit with the degrees of freedom in parentheses.

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