Table 2.
Data used to determine burst rates and energies for R1 at different epochs, and for reference the same data for the Crab pulsar, XTE J1810−197, and SGR 1900+14.
| Source | Telescope | Bursts | Tobs (h) | Date span | Power-law index (γ) |
|---|---|---|---|---|---|
| R1 | Arecibo(1),(3) | 11 | 4.5 | 2012-11-02–2015-06-02 | −0.8 |
| GBT(2),(3) | 5 | 15.3 | 2015-11-13–2016-01-11 | −0.8 |
|
| VLA(3) | 9 | 28.9 | 2016-08-23–2016-09-22 | −0.6 |
|
| Arecibo(4) | 41 | 3.2 | 2016-09-13–2016-09-14 | −1.8(3) | |
| WSRT(5) | 30 | 128.4 | 2018-11-12–2019-08-30 | −1.7(6) | |
| Crab pulsar giant pulses | WSRT(6) | 13 000 | 6 | 2005-12-10 | −1.79(1) |
| ATCA(7) | 700 | 3 | 2006-01-31 | −1.33(14) | |
| Magnetar XTE J1810−197 | GMRT(8) (650 MHz) | 5597 | 2.05 | 2018-12-18–2019-02-17 | −2.4(2) |
| GMRT(8) (1.36 GHz) | 219 | 0.33 | 2019-02-17 | −0.95(30) | |
| SGR 1900+14 X-ray bursts | BATSE+RXTE(9) | 1000 | ∼50 | 1998–1999 | −0.66(13) |
Notes. The last column shows the derived power-law slope of the cumulative burst rate as function of energy.
References. (1) Spitler et al. (2016); (2) Scholz et al. (2016); (3) Law et al. (2017); (4) Gourdji et al. (2019); (5) this work; (6) Karuppusamy et al. (2010); (7) Bhat et al. (2008); (8) Maan et al. (2019); (9) Göǧüş et al. (1999).
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