Table 3
Burst parameters (variability timescale, spectral parameters and luminosity) for the three considered time intervals.
| Time interval | c | d 1 | d 2 | |
|
|
||||
| tv (s) | 0.1 ± 0.01 | 0.6 ± 0.1 | 0.5 ± 0.1 | |
| s |
|
|
|
|
| Φ(s) | 0.511 ± 0.009 | 0.463 ± 0.004 | 0.465 ± 0.003 | |
| Ef (GeV) |
|
|
|
|
| Emax (GeV) | 0.85 | 2.04 | 2.66 | |
| E∗ (MeV) | 10 | 2.5 | 1.0 | |
| F(E∗) (10-2 cm-2 MeV-1) | 0.22 ± 0.03 | 4.0 ± 0.8 | 5 ± 1 | |
| Luminosity (1053 erg s-1) | 16.9 ± 3.1 | 1.73 ± 0.14 | 1.85 ± 0.15 | |
Lorentz factor  |
233 ± 18 | 100 ± 8 | 98 ± 9 | |
| Emission radius R = RMeV = RGeV (1014 cm) | 1.1 ± 0.1 | 1.2 ± 0.2 | 1.0 ± 0.1 | |
| Photospheric radius Rph (1014 cm) | 0.5 ± 0.2 | 0.7 ± 0.2 | 0.8 ± 0.2 | |
Lower limit on the Lorentz factor  |
257 ± 17 | 129 ± 8 | 110 ± 8 | |
Notes. The last four lines give the obtained constraints for the two cases considered in Sect. 4.2: either the observed high-energy spectral break Ef is due to gamma-ray opacity to pair creation, which leads to a measurement of the Lorentz factor, or it is a natural break (last line). In this second case only a lower limit on the Lorentz factor can be obtained from the maximum energy Emax of the observed photons. In both cases, the results listed in the table corresponds to the assumption RGeV = RMeV, favored by the observed similar variability at low and high energy. The impact of RGeV>RMeV on these results is illustrated in Fig. 6.
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