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J/A+A/498/399       GRB observed with RHESSI satellite       (Ripa+, 2009)

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
ADC_Keywords: Gamma rays Keywords: gamma rays: bursts Abstract: We study a sample of 427 gamma-ray bursts (GRBs), measured by the RHESSI satellite, statistically with respect to duration and hardness ratio. Standard statistical tests were used, such as chi2, F-test, and the maximum likelihood ratio test, to compare the number of GRB groups in the RHESSI database with that of the BATSE database. Description: The Ramaty High Energy Solar Spectroscopic Imager (RHESSI) is a NASA Small Explorer satellite designed to study hard X-rays and gamma-rays from solar flares (Lin et al., 2002, Sol. Phys., 210, 3). We used the RHESSI GRB Catalog (Wigger et al., 2008, and the Cosmic Burst List (Hurley, 2008, ) to detect 487 GRBs in the RHESSI data between 2002 February 14 and 2008 April 25. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table7.dat 60 427 The RHESSI GRB data set
See also: : RHESSI and Gamma Ray Bursts Home Page : Cosmic burst list Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 6 I6 --- GRB GRB name which correspond to date 7 A1 --- m_GRB [ABC] Internal multiplicity code (1) 9- 10 I2 h Time.h GRB peak time, hours (UTC) 12- 13 I2 min Time.m GRB peak time, minutes (UTC) 15- 20 F6.3 s Time.s GRB peak time, seconds (UTC) 22- 28 E7.3 s T90 T90 duration (2) 30- 36 E7.3 s e_T90 rms uncertainty on T90 38- 43 E6.2 s dtres Time resolution of derived light curve 45- 52 E8.4 --- HR Hardness ratio (3) 54- 60 E7.3 --- e_HR rms uncertainty on logHR
Note (1): The letters after GRB names are internal and do not have to be in accordance with e.g. GCN GRB names. Note (2): Time interval during which the cumulative counts increase from 5% to 95% above background. Note (3): The hardness ratio is defined to be the ratio of two fluences F in two different energy bands integrated over the time interval T90. For the RHESSI data set, we used the energy bands (25-120)keV and (120-1500)keV, i.e., HR=F(120-1500)/F(25-120). The published table caption indicates "log H" but the hardnesses cannot be expressed in a log scale.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Jun-2009
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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