Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010acasn..51..374l&link_type=abstract
Acta Astronomica Sinica, vol. 51, no. 4, p. 374-383
Astronomy and Astrophysics
Astronomy
Gamma-Ray Burst: General, Methods: Statistical
Scientific paper
Gamma-ray bursts (GRBs) are the most violent events in the universe. The GRB satellite BATSE (Compton Gamma-Ray Observatory/Bursts and Transient Source Experiment) detected more than 2700 GRBs due to its wide energy coverage (~25 keV to ~1 MeV) and all-sky viewing. Swift (Swift Gamma-ray Burst Explorer), a multi-wavelength detector, has refreshed our understanding of the nature of GRBs. Another mission Fermi (Fermi Gamma-ray Space Telescope) can measure the spectra in a very wide energy band (from 8 keV to more than 300 GeV). It opens a new era of observational astronomy in the energetic gamma-ray band. These three satellites together provide us a lot of GRB samples. In order to investigate whether they show any statistical difference, a systematic study on the properties of GRBs detected by these three instruments is presented. Our Swift sample includes the bursts detected by Swift/BAT before March 2010, Fermi sample includes the bursts detected by Fermi/GBM between August 2008 and March 2010. It is shown that, apparently, the amount of bursts with redshifts, the proportion of long bursts in total GRBs and the distribution of photon flux (lgN-lgP) are significantly different. However, there are no significant differences in the time duration T90 and the spectral hardness ratio. All the data of Fermi GRBs are in the energy range 8~1000 keV, much broader than that of Swift/BAT, which is 15~150 keV. In order to make a comparison between the lgN-lgP distribution observed by Swift/BAT and Fermi/GBM, we correct the observed peak fluxes of Fermi GRBs to the same energy band with the spectral information presented in the article. The result shows that the corrected lgN-lgP distribution observed by Fermi/GBM is also consistent with those observed by BATSE and Swift/BAT. The differences in the amount of GRBs with redshifts and the proportion of long events in total GRBs are due to the sensitivity of the instruments, that is, different instruments lead to the different observational properties of GRBs, while the nature of these GRBs may be the same.
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