Table 5.
Ultra-long GRBs with widely-spaced emission episodes.
| GRB | Duration (a) | z | Fluence (b) | Energy range (c) | Eγ, iso(d) | Episodes(e) | GeV (f) | Afterglow (g) | Refs. |
|---|---|---|---|---|---|---|---|---|---|
| (s) | (10−5 erg cm−2) | (keV) | (1052 erg) | ||||||
| 020410A | 1550 | ∼0.5 | 2.8 | 15–1000 | ∼1.8 | 4 | – | X,O | 1,2 |
| 080407A | 2100 | – | 44 | 20–1000 | ∼120 | 2 | – | – | 3 |
| 091024A | 1300 | 1.092 | 1.5 | 10–10000 | 44 | 3 | ND | X,O | 4,5 |
| 110709B | 900 | – | 0.22 | 15–150 | ∼10 | 2 | – | X,R | 6 |
| 130925A | 4500 | 0.347 | 62 | 20–10000 | 19 | 3 | ND | X,O,R | 7,8,9,10,11 |
| 150201A (h) | 1400 | – | 6.8 | 10–1000 | ∼36 | 2 | – | X | 12 |
| 160625B | 800 | 1.406 | 66 | 10–1000 | 334 | 3 | D | X,O,R | 13,14 |
| 220627A | 1200 | 3.08 | 4.5 | 10–1000 | 480 | 2 | D | X,O,R | 15, this work |
Notes.
GeV γ-ray emission detected with Fermi/LAT. ND indicates a non detection, D indicates a detection.
GRB 150201A triggered Fermi/GBM twice separated by 23 min. The burst position was earth-occulted during the second trigger, so the association between the two triggers is not beyond doubt.
References. (1) Nicastro (2004); (2) Levan et al. (2005); (3) Pal’shin et al. (2012); (4) Gruber et al. (2011); (5) Virgili et al. (2013); (6) Zhang et al. (2012); (7) Golenetskii et al. (2013); (8) Evans et al. (2014); (9) Piro et al. (2014); (10) Greiner et al. (2014); (11) Horesh et al. (2015); (12) Yu & Pelassa (2015); (13) Zhang et al. (2018); (14) Alexander et al. (2017); (15) Huang et al. (2022).
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