Global characteristics of X-ray flashes and X-ray rich GRBs observed by HETE-2

By T. Sakamoto, D. Lamb, C. Graziani, T. Donaghy, Masaya Suzuki, G. Ricker, J. Atteia, N. Kawai, A. Yoshida, Y. Shirasaki and 28 more. 2004

161 citations recorded by the source corpus.

We describe and discuss the global properties of 45 gamma-ray bursts (GRBs) observed by HETE-2 during the first three years of its mission, focusing on the properties of X-Ray Flashes (XRFs) and X-ray-rich GRBs (XRRs). We find that the numbers of XRFs, XRRs, and GRBs are comparable. We find that the durations and the sky distributions of XRFs and XRRs are similar to those of GRBs. We also find that the spectral properties of XRFs and XRRs are similar to those of GRBs, except that the values of the peak energy $E^{\rm obs}_{\rm peak}$ of the burst spectrum in $\nu F_\nu$, the peak energy flux $\Fp$, and the energy fluence $S_E$ of XRFs are much smaller -- and those of XRRs are smaller -- than those of GRBs. Finally, we find that the distributions of all three kinds of bursts form a continuum in the [$S_E$(2-30 keV),$S_E$(30-400) keV]-plane, the [$S_E$(2-400 keV), $E_{\rm peak}$]-plane, and the [$F_{\rm peak}$(50-300 keV), $E_{\rm peak}$]-plane. These results provide strong evidence that all three kinds of bursts arise from the same phenomenon.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/78266a3a6b462e3d828292db3eaec11b6377fa76

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In Astronomy and Astrophysics

1. Bing Zhang
2. L. Amati
3. E. Liang
4. M. Briggs
5. R. Preece
6. W. Paciesas
7. C. Meegan
8. Pawan Kumar

In Instrumentation

1. Bing Zhang
2. E. Liang
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4. F. Ryde
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In Nuclear and High Energy Physics

1. Bing Zhang
2. E. Liang
3. L. Amati
4. Pawan Kumar
5. E. Berger

Citations in the corpus

• The Ep,i–Eiso correlation in gamma-ray bursts: updated observational status, re-analysis and main implications (2006, methodology): “In the simplest assumption of isotropic emission, the radiated energy, Eiso , ranges from ∼10 50 erg to ∼1054 erg for most GRBs and extends down to ∼1049 erg when including XRFs (Lamb, Donaghy & Graziani 2004; Sakamoto et al. 2004).”
• The Complete Spectral Catalog of Bright BATSE Gamma-Ray Bursts (2006, background): “Having a variety of models in fitting each spectrum eliminates the need for manipulating one model, such as the “constrained” Band function introduced by Sakamoto et al. (2004), which requires some presumptions of the form for the original photon spectrum.”