Table A.1.
Significance of detection and best fit parameters for a power-law model of MeV afterglow.
| Time-bin | Orbits | S/N | Index | Flux | cstat/Dof | ||||
|---|---|---|---|---|---|---|---|---|---|
| [s] | n0 | n3 | n6 | n7 | n9 | [erg cm−2 s−1] | |||
| 10.2–25.0 | ± 14, ±16 | - | - | 5.9 | 6.6 | - | −2.44 ± 0.37 | (6.71 ± 1.59)×10−8 | 260/133 |
| ± 30 | - | - | 6.5 | 8.6 | - | −2.31 ± 0.32 | (8.12 ± 1.66)×10−8 | 248/133 | |
| 25–250 | ± 14, ±16 | - | 9.3 | 5.6 | - | - | −2.94 ± 0.34 | (1.61 ± 0.28)×10−9 | 196/133 |
| ± 30 | - | 12.2 | 7.6 | - | - | −2.40 ± 0.23 | (2.30 ± 0.32)×10−9 | 200/135 | |
| 251.9 - 647.2 | ± 14, ±16 | 1.1 | - | 1.3 | - | 3.0 | −2.0* | < 1.21 × 10−9 | 359/201 |
| ± 30 | 3.2 | - | 3.7 | - | 4.6 | −1.12 ± 0.44 | (7.16 ± 1.84)×10−10 | 323/200 | |
Notes. *3σ flux upper-limits are derived using a photon index of −2. Due to the low photon count rate, the spectral fit fails (no convergence) if index is allowed to vary. We, however, note that the flux upper-limits are consistent with our findings to that of the ±30 orbits where the detection significance is more than 3σ.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.