The GRBM + WFC events database

In table 5.1 we report the sample of GRB simultaneously detected by the GRBM and the WFC. For each event we report the interested detector, the offset angle (computed in the way described in chapter 4), and the 1s gamma and X peak fluxes and durations. The gamma peak fluxes have been obtained by means the GRBM ratemeters data analysis.

   

$$\gamma _{\gamma}$$ GRB Detector Offset wrt X-ray^(a) T_x

inst. axis peak flux (s) peak flux (s)

$$^{\circ}$$ GRB960720 LS1 0.25 17 10 8

$$^{\circ}$$ GRB970111 LS3 1.4 60 56 43

$$^{\circ}$$ GRB970228 LS1 1.4 77 37 77

$$^{\circ}$$ GRB970402 LS1 0.16 150 3.2 150

$$^{\circ}$$ GRB970508 LS3 0.35 25 5.6 15

$$^{\circ}$$ GRB971214 LS1 0.2 35 6.8 35

$$^{\circ}$$ GRB971227 LS1 0.36 7 3.8 7

$$^{\circ}$$ GRB980109 LS1 0.16 20 3.9 20

$$^{\circ}$$ GRB980326 LS3 0.84 9 2.7 9

$$^{\circ}$$ GRB980329 LS3 1.3 53 51 35

$$^{\circ}$$ GRB980425 LS3 0.61 45 2.4 25

$$^{\circ}$$ GRB980515 LS1 0.3 20 3 15

$$^{\circ}$$ GRB980519 LS3 0.51 190 13 28

$$^{\circ}$$ GRB980613 LS3 0.13 50 12 50

$$^{\circ}$$ GRB981226 LS1 0.085 260 0.56 20

• [^(a)] Peak fluxes in units of 10^-7 erg cm^-2 s^-1

For all these events GRBM spectral evolution and average spectra analysis have been performed. The estimated fluences in the 40-700 keV, obtained by integrating the best-fitting photon spectrum to the average spectrum, and peak fluxes, obtained by integrating the power-law inferred from the GRBM and AC counts ratio in the time bin corresponding to the peak count rate, were compared to the BATSE results for those events detected by both experiments. The results are consistent, accounting for errors and the different instrument band.
WFC spectral analysis and GRBM+WFC spectral analysis has been performed on a sub-sample of 8 events, that were chosen on the basis of statistical quality of the data. For the WFC spectra and light curves, the background level is estimated using an equivalent section of the detector area not illuminated by the burst or other known X-ray sources.
Many of the results of these analysis have been published in specific papers, were the GRB event spectral properties are also compared to the afterglow properties. Some of them have been attached in section A2; the complete list is reported in section A1.

In the next subsections we discuss the results for some of the most interesting events.