SAXGRBMGRB - BeppoSAX/GRBM Gamma-Ray Burst Catalog
The Gamma-Ray Burst catalog obtained with the Gamma-Ray Burst Monitor aboard BeppoSAX. Frontera F., Guidorzi C., Montanari E., Rossi F., Costa E., Feroci M., Calura F., Rapisarda M., Amati L., Carturan D., Cinti M.N., Dal Fiume D., Nicastro L., Orlandini M. <Astrophys. J. Suppl. Ser. 180, 192 (2009)> =2009ApJS..180..192F (SIMBAD/NED BibCode)
The gamma-ray burst designation. The GRB name is formed by prexix 'GRB' followed by the date of the detection, in the form YYDDMM. e.g., 'GRB 960802'. In case of more than one burst in a day, a letter A, B, C is added to distinguish the specific bursts.
The Right Ascension of the GRB in the selected equinox, when known. This was given in J2000.0 decimal degrees to a precision of 0.01 degrees in the original table, although the true positional accuracy (see the error_radius parameter) is typically much larger than this.
The Declination of the GRB in the selected equinox, when known. This was given in J2000.0 decimal degrees to a precision of 0.01 degrees in the original table, although the true positional accuracy (see the error_radius parameter) is typically much larger than this.
The Galactic Longitude of the GRB, when known.
The Galactic Latitude of the GRB, when known.
The mean positional error radius of the GRB, in degrees.
The elevation angle of the GRB (for those with already known positions) with respect to the earth limb, in degrees.
The instrument/catalog reference that provided the best GRB coordinates, as follows:
G = BeppoSAX GRBM W = BeppoSAX Wide Field Cameras A = ASM aboard RXTE 4B = BATSE 4B catalog (Paciesas et al., 1999, CDS Cat. <IX/20>) H = HETE 2 K = Kommers catalog (Kommers et al., 2001, CDS Cat. <J/ApJS/134/385>) I = Inter-Planetary Network P = RXTE PCA S = Stern catalog (Stern et al., 2001, CDS Cat. <J/ApJ/563/80>)
The GRB trigger time in UT, given to a precision of 1 second.
This flag parameter indicates whether ('Y') or not ('N') high time resolution data exists for the particular GRB.
The time elapsed from the earliest GRB onset above a 2-sigma threshold to its final disappearance below the 2-sigma threshold, in seconds.
The mean error in the GRB duration above 2-sigma, t_other, in seconds.
The integrated time over which the GRB emission level was above 2 sigma, in seconds.
The mean error in the integrated time over which the GRB emission level was above 2 sigma, in seconds.
The number of time intervals in which the the GRB emission level was above 2 sigma.
The time interval during which the GRB integrated counts increased from 5% to 95% of the total counts, t_90, in seconds, as defined by the BATSE team (Kouveliotou et al. 1993, ApJ, 413, L101).
The mean error in t_90 for the GRB, in seconds.
The 40 - 700 keV fluence of the GRB, in erg/cm2.
The mean error in the 40 - 700 keV fluence of the GRB, in erg/cm2.
The 40 - 700 keV peak flux of the GRB, in erg/cm2/s.
The mean error in the 40 - 700 keV peak flux of the GRB, in erg/cm2/s.
The best-fit photon index Gamma of the 2-channel (40 - 700 keV and > 100 keV) background-subtracted spectral data of the GRB, derived with the assumption of a power-law spectrum.
The mean error in the best-fit photon index Gamma.
The GRBM detection unit used to derive the time duration parameters (t_90, t_other and t_above_fraction) of the GRB. This unit provided the light curve with the best signal-to-noise ratio.
The GRBM detection unit used for the determination of the GRB fluence, peak flux and spectral hardness. When it was possible to improve the statistical quality of the results, the signal from another unit (detection_unit_3) was added in.
The third GRBM detection unit, used in a number of cases to improve the statistical quality of the results,
The rebinning factor of the default light curve which was adopted to derive the reported parameters of the GRB. The default light curves were: 1 s light curves in the case of long GRB (t_90 > 2s), and 7.8125 ms in the case of short GRBs.