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 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,
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 between 2002 February 14 and 2008 April 25.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table7.dat 60 427 The RHESSI GRB data set
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See also:
http://grb.web.psi.ch : RHESSI and Gamma Ray Bursts Home Page
http://www.ssl.berkeley.edu/ipn3/masterli.txt : Cosmic burst list
Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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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
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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.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Jun-2009