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Table A.1.

Best fit parameters inferred from the time-integrated analysis of the ten long GRBs analysed in this work.

Name Time interval Norm α1 (α) Ebreak α2 Epeak β χ2/d.o.f. Ftest
(s) (ph s−1 cm2 keV) (keV) (keV)
171010 [0.003 − 100.35 s] 829.22/335 > 8σ
160625 [187.43 − 212.00 s] 638.55/342 > 8σ
160821 [117.76 − 154.63 s] 411.91/226 > 8σ
170409 [17.66 − 116.99 s] 527.62/347 > 8σ
180720 [ − 1.02 − 56.32 s] 589.06/343 > 8σ
171227 [0.003 − 58.24 s] 466.24/344 > 8σ
090618 [0.003 − 161.28 s] 339.3/231 4.1σ
100724 [ − 5.12 − 137.22 s] 444.62/339 1.0σ
130606 [ − 3.07 − 70.66 s] 483.38/333 2.0σ
101014 [0.003 − 466.44 s] 488.14/342 7.4σ

Notes. In bold are flagged those GRBs with a statistically significant spectral break Ebreak in the low-energy part of their spectrum. The table lists the GRB name, the time interval over which the spectrum has been accumulated, and the results from the spectral analysis: best fit normalisation (see Ravasio et al. 2018), photon index α1 (or α when the best fit model is a SBPL), break energy Ebreak (only if the best fit model is a 2SBPL), photon index α2 (only if the best fit model is a 2SBPL), peak energy Epeak, photon index β, total χ2 and degrees of freedom (d.o.f.), and the significance of the improvement of the fit from a SBPL to a 2SBPL (estimated according to the F-test).

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