I've found 24 bursts in the 30 simulation days of ST checkout 2 data. These bursts were identified by eye with the aid of these scripts, which provide an interactive environment for finding the bursts by scanning the light curves and plotting the event distributions on the sky for selected time intervals of the data. A method exists for generating .pha files using gtbin and .rsp files using gtrspgen automatically and for optionally performing a likelihood analysis of the selected events using Likelihood's python interface.
Both Xspec12 and Likelihood have been used to analyze these data. Here are the filtered FT1 files, .pha, and .rsp files used in those analyses, and this table summarizes the results:
burst id |
RA |
Dec |
tstart |
tstop |
Likelihood |
|
Xspec12 |
|
|---|---|---|---|---|---|---|---|---|
|
|
|
|
|
flux |
index |
flux |
index |
grb0_0 |
258.96 |
29.80 |
9999.31003 |
10002.48448 |
4.09e-03 |
-2.41+/-0.19 |
3.20e-03 |
-2.29+0.38-0.47 |
grb1_0 |
168.71 |
-62.10 |
197523.10377 |
197524.16672 |
2.25e-02 |
-2.38+/-0.14 |
1.36e-02 |
-2.33+0.29-0.32 |
grb1_1 |
133.44 |
-59.34 |
231529.08539 |
231532.21719 |
3.15e-03 |
-2.39+/-0.22 |
1.69e-03 |
-2.20+0.59-0.80 |
grb2_0 |
164.92 |
-61.08 |
266223.64072 |
266226.93157 |
2.45e-03 |
-2.25+/-0.22 |
1.20e-03 |
-2.09+0.68-0.95 |
grb3_0 |
104.91 |
-54.20 |
425980.67104 |
425984.26350 |
8.58e-03 |
-2.35+/-0.13 |
6.06e-03 |
-2.49+0.29-0.31 |
grb4_0 |
131.58 |
-57.13 |
598219.15218 |
598223.30969 |
1.49e-02 |
-2.25+/-0.08 |
1.26e-02 |
-2.21+0.12-0.14 |
grb6_0 |
318.40 |
54.60 |
773003.44612 |
773004.95784 |
3.66e-03 |
-2.12+/-0.20 |
3.03e-03 |
-2.16+0.69-1.11 |
grb6_1 |
231.95 |
-26.47 |
840044.49845 |
840046.72695 |
4.59e-03 |
-2.55+/-0.21 |
4.28e-03 |
-2.48+0.47-0.60 |
grb6_2 |
178.77 |
8.88 |
878984.84348 |
878985.85143 |
2.91e-02 |
-2.31+/-0.12 |
2.63e-02 |
-2.31+0.23-0.26 |
grb7_0 |
149.17 |
3.89 |
993153.51892 |
993157.81280 |
1.43e-02 |
-2.41+/-0.09 |
1.17e-02 |
-2.43+0.15-0.17 |
grb7_1 |
206.03 |
-28.57 |
1011648.49924 |
1011650.64103 |
1.98e-03 |
-2.36+/-0.31 |
1.69e-03 |
-2.19+0.68-0.99 |
grb8_0 |
304.23 |
51.32 |
1030614.92544 |
1030618.47925 |
5.10e-03 |
-2.37+/-0.16 |
3.90e-03 |
-2.29+0.27-0.34 |
grb8_1 |
333.99 |
-8.75 |
1150763.14475 |
1150763.58054 |
9.57e-02 |
-2.34+/-0.10 |
7.21e-02 |
-2.20+0.15-0.17 |
grb9_0 |
225.33 |
48.52 |
1269479.99643 |
1269483.06536 |
2.97e-03 |
-2.75+/-0.30 |
2.00e-03 |
-2.70+0.64-0.98 |
grb10_0 |
39.33 |
-44.20 |
1306582.30555 |
1306584.60743 |
8.46e-03 |
-2.40+/-0.16 |
6.00e-03 |
-2.32+0.30-0.36 |
grb11_0 |
182.66 |
-13.72 |
1527086.53909 |
1527089.61078 |
3.02e-03 |
-2.37+/-0.22 |
1.91e-03 |
-2.14+0.38-0.46 |
grb12_0 |
82.08 |
-62.25 |
1593795.11799 |
1593799.12337 |
1.92e-03 |
-2.12+/-0.19 |
1.72e-03 |
-2.59+0.77-0.84 |
grb12_1 |
177.68 |
33.35 |
1646760.87621 |
1646764.05591 |
6.11e-03 |
-2.37+/-0.15 |
4.70e-03 |
-2.71+0.65-0.78 |
grb13_0 |
329.19 |
21.62 |
1707036.30918 |
1707039.43815 |
1.50e-02 |
-2.50+/-0.11 |
1.14e-02 |
-2.46+0.18-0.22 |
grb16_0 |
357.64 |
-51.42 |
2182472.32856 |
2182473.43197 |
1.47e-02 |
-2.31+/-0.16 |
1.17e-02 |
-2.26+0.29-0.36 |
grb17_0 |
32.95 |
-54.57 |
2217299.83125 |
2217303.15968 |
1.44e-03 |
-2.01+/-0.22 |
1.05e-03 |
-2.03+0.65-0.92 |
grb18_0 |
128.22 |
-18.07 |
2351082.69869 |
2351084.12367 |
1.59e-02 |
-2.51+/-0.16 |
1.27e-02 |
-2.51+0.25-0.29 |
grb19_0 |
290.30 |
25.22 |
2565444.02851 |
2565445.39056 |
4.56e-02 |
-2.31+/-0.08 |
3.82e-02 |
-2.29+0.14-0.16 |
grb19_1 |
63.13 |
-42.00 |
2567335.49848 |
2567337.57950 |
3.72e-03 |
-2.80+/-0.37 |
1.72e-03 |
-2.50+100.00-100.00 |
The units of flux are photons cm 2 s -1 , integrated above 30 MeV. The Likelihood photon index errors are 1 sigma while the Xspec12 photon index errors correspond to a change in chi-square of 2.706. The +/ 100 errors for the Xspec12 estimate of the photon index for grb19_1 indicate an (unrecoverable) error encountered by Xspec12 in trying to estimate the index errors.
Here is a plot comparing these results:
The red curves are 45 degree lines corresponding to perfect agreement between the two sets of analyses. The fluxes found by Xspec12 are systematically lower than the fluxes found by Likelihood by about 20%.
Maps of the counts and plots of the light curves for all 24 bursts are available here.