Notes. Column description: Burst: name of the event (YYMMDD); ScW: pointing ID in which the event occurred; UT: trigger time; T₉₀: duration of the event; Fluence: fluence in units of counts, referring to the T₉₀ interval and to the energy interval given in column 7; Peak Flux: in units of count/s in the same time and energy intervals as for fluence; Instrument: telescopes/instruments that observed the event (A = AGILE, B= Swift/BAT, F = Fermi/GBM, II = INTEGRAL/ISGRI, IA = INTEGRAL/SPI-ACS, K= Wind/Konus, R = RHESSI, S = Suzaku/WAM). (a) = T₉₀ refers to the 260–312 keV range, that gives a better signal to noise ratio. (b) = The bright GRB 060901, detected by INTEGRAL over  ~20 s, saturated ISGRI telemetry but did not affect PICsIT data. In PICsIT light curve the burst shows a multipeak structure extending over 8 s, in accordance with Konus main event (followed, in Konus data, by a faint tail up to 15 s). (c) = GRB 060928 is structured in two main episodes at 01:17:05 and 01:17:20, with duration  ~14 s and  ~25 s, respectively. PICsIT observed both events (Fig. 13) but our analysis has been restricted to the main second event (Fig. 14). (d) = A linear fit of the background was required for T₉₀ computation. (e) = PICsIT light curves are severely affected by data gaps at all energies (Fig. 16). A T₉₀ of 11 s was obtained by McGlynn et al. (2009) with SPI. (f) = For T₉₀ computation the background was fitted to a polynomial function of the third degree. (g) = For T₉₀ computation the background was fitted to a polynomial function of the second degree.

References. GRBs have been documented by: (1) Hurley et al. (2006b); (2) Mereghetti et al. (2006b); (3) Hurley et al. (2006a); (4) Mereghetti et al. (2006a); (5) Grupe et al. (2006); (6) Golenetskii et al. (2007c); (7) Schady et al. (2007); (8) Cummings (2007).

Notes. (h) = We analyzed the main pulse of the event, which is composed of three peaks over  ~70 s. (i) = The burst was observed by PICsIT in two main episodes separated by 50 s and extending over 120 s. The first smaller peak seems to be affected by count drops and therefore the analysis was conducted on the second event only. (j) = The bright GRB 080723B fell in the ISGRI FoV, with an off-axis angle Θ ~ 8°, and saturated the available telemetry. PICsIT data show gaps at all energies that are limited to few time bins, however, and did not affect the T₉₀ computation. We report the lower limits of the peak flux and fluence. (k) = in PICsIT data the burst occurs  ~60 s after the Swift/BAT trigger and coincides with the brightest portion of this long event (~130 s).

References. GRBs have been documented by: (9) Hurley et al. (2008); (10) Golenetskii et al. (2008f); (11) Racusin et al. (2008); (12) Perri et al. (2008); (13) Rapisarda et al. (2008); (14) Mangano et al. (2008); (15) Markwardt et al. (2008); (16) Marshall et al. (2008); (17) Götz et al. (2008); (18) Bissaldi et al. (2008); (19) von Kienlin (2009a); (20) Schady et al. (2009); (21) Rau (2009); (22) von Kienlin (2009b); (23) van der Horst (2009).