This page contains an index of burst data from KS 1731-260. Click on the burst number/time to go to the page for each burst

ID flag1 ObsID UT MJD PRE?
1 10416-01-01-00 1996 Jul 14 04:16:13 50278.177940 Y
2 20085-01-01-02 1997 Oct 29 08:15:51 50750.344340 Y
3 30061-01-02-00 1998 Oct 2 07:36:57 51088.317340 N
4 30061-01-02-01 1998 Oct 2 14:02:32 51088.585100 Y?
5 30061-01-02-03 1998 Oct 3 09:14:06 51089.384800 N
6 30061-01-02-06 1998 Oct 6 03:29:32 51092.145520 Y?
7 40409-01-01-00 1999 Feb 23 03:09:01 51232.131270 N
8 30061-01-04-00 1999 Feb 26 17:13:09 51235.717470 Y
9 30061-01-04-02 1999 Feb 27 17:25:08 51236.725800 Y
10 40025-02-01-02 1999 Jun 26 08:33:37 51355.356680 N
11 40025-02-03-00 1999 Aug 7 06:15:09 51397.260530 N
12 40025-02-04-00 1999 Aug 14 06:18:53 51404.263120 N
13 40025-02-05-01 1999 Aug 26 07:36:46 51416.317200 N
14 50031-02-01-00 2000 Aug 6 16:23:58 51762.683320 N
15 50031-02-01-00 2000 Aug 6 18:54:53 51762.788120 N
16 50031-02-01-10 2000 Aug 6 23:49:58 51762.993030 N
17 50031-02-01-01 2000 Aug 7 07:36:19 51763.316900 N
18 50031-02-01-02 2000 Aug 7 12:44:27 51763.530870 N
19 50031-02-01-02 2000 Aug 7 17:47:39 51763.741440 N
20 50031-02-01-03 2000 Aug 7 20:23:26 51763.849610 N
21 50031-02-01-05 2000 Aug 8 17:25:09 51764.725800 N
22 50031-02-02-05 2000 Sep 28 22:18:43 51815.929670 N
23 50031-02-02-01 2000 Sep 29 06:16:15 51816.261290 N
24 50031-02-02-03 2000 Sep 29 14:08:35 51816.589300 N
25 50031-02-02-03 2000 Sep 29 19:23:29 51816.807990 N
26 50031-02-02-03 2000 Sep 29 22:01:31 51816.917730 N
27 50031-02-02-08 2000 Sep 30 06:00:00 51817.250000 N

Flag values indicates a range of potential analysis issues, as follows:

  1. The burst was observed during a slew, and thus offsetfrom the source position.
  2. The observation was offset from the source position. In cases (a) and (b) we scaled the flux and fluence by the mean collimator response appropriate for the position of the source in the field of view, as described in Appendix B.
  3. The origin of the burst is uncertain; the burst may have been from another source in the field of view (we rescaled the flux and fluence, if necessary, based on the assumed origin).
  4. Buffer overruns (or some other instrumental effect) caused gaps in the high time resolution data.
  5. The burst was so faint that only the peak flux could be measured, and not the fluence or other parameters.
  6. An extremely faint burst or possibly problems with the background subtraction, resulting in no fit results.
  7. The full burst profile was not observed, so that the event can be considered an unconfirmed burst candidate. Typically in these cases the initial burst rise is missed, so that the measured peak flux and fluence are lower limits only.
  8. High time resolution data modes did not cover the burst.