All Tables

Table 1: Properties of the X-ray afterglows detected by BeppoSAX. We indicate the absorbed flux extrapolated or interpolated to 11 h after the burst, the temporal decay and the energy spectral index, the Galactic column density from Dickey & Lockman (1990), the excess of absorption at z=0, and the excess of absorption at the proper redshift of the burst (assuming a distance of z=1 when the host galaxy redshift was unknown).
Table 2: Results reported from previous analysis of X-ray afterglows detected by BeppoSAX. In this table, we indicate the temporal decay, the energy index, the fitted value of $n_{\rm H}$ compared to the galactic column density and the associated reference. A label "W'' close to the decay index indicates that this value was obtained by means of WFC and NFI data.
Table 3: X-ray luminosity (assuming isotropy, $L_{\rm X} ^{\rm iso}$ , and after beaming correction, $L_{\rm X} ^{\rm corr}$ ), energy emitted during the prompt $\gamma$ -ray event (assuming isotropy, $E_{\gamma } ^{\rm iso}$ ) in units of 10⁵¹ erg, and beaming angle for BeppoSAX GRBs with a measured beaming angle (extracted from literature).
Table 4: Mean closure relationships from our sample. We indicate the wind and ISM closure relationships, depending on the cooling frequency position.
Table 5: Optical decay indexes and comparison with the X-ray band decay indexes.
Table 6: GRBs localized and/or observed by BeppoSAX. We indicate the position of the first TOO start and end times, the sum of the Good Time Interval (GTI), and the date of the subsequent TOOs. "WFC'' following the position means that this GRB was localized only the the WFC, "NFI'' a localization obtained by NFI. An external trigger of a BeppoSAX TOO is indicated by giving the satellite that localized the burst in parenthesis, but the localization displayed has been provided by NFI. We also indicate in the table if an optical afterglow was detected together with the distance and other information obtained from the optical study.
Table 7: Properties of the prompt emission of BeppoSAX Gamma Ray Bursts reported in Table 6. We indicate the duration and fluence both in the X-ray (2.0-10.0 keV band) and the $\gamma$ -ray (40.0-700 keV band). An X following the source name denotes an X-ray-rich GRB or an X-ray flash.