RHESSIGRB - RHESSI Gamma-Ray Burst Catalog
The authors used the RHESSI GRB Catalog (Wigger et al., 2008, http://grb.web.psi.ch/) and the Cosmic Burst List (Hurley, 2008, http://www.ssl.berkeley.edu/ipn3/masterli.html) to detect 487 GRBs in the RHESSI data over the time period between 2002 February 14 and 2008 April 25. For a deeper analysis, they chose a subset of 427 GRBs with data with a signal-to-noise ratio higher than 6. This table contains this subset.
Search for gamma-ray burst classes with the RHESSI satellite. Ripa J., Meszaros A., Wigger C., Huja D., Hudec R., Hajdas W. <Astron. Astrophys., 498, 399-406 (2009)> =2009A&A...498..399R
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. These letters after the GRB names are internal and do not have to be in accordance with e.g. GCN GRB names.
The GRB peak time (UTC). This was given to a precision of 0.001 seconds in the original table.
The T_90 duration of the GRB, in seconds. T_90 is defined as the time interval during which the cumulative counts in the GRB increase from 5% to 95% above the background.
The RMS uncertainty in T90, in seconds.
The time resolution of the derived GRB light curve, in seconds.
The hardness ratio HR of the GRB, defined as the ratio of the two fluences F in two different energy bands and integrated over the time interval T90. For the RHESSI data set, the authors used the energy bands 25 - 120 keV and 120 - 1500 keV, i.e., HR = F(120-1500 keV)/F(25-120 keV). The published table caption indicates this parameter as being "log H" but, as the CDS notes, the hardness ratios being in the range from -1 to +1, they cannot be expressed in a log scale.
The RMS uncertainty in the hardness ratio HR.