We report observation results of the prompt X- and gamma-ray emission from GRB 011211. This event was detected with the Gamma-Ray Burst Monitor and one of the wide-field cameras aboard the BeppoSAX satellite. The optical counterpart of the gamma-ray burst was soon identified and its redshift determined (z=2.140), while the X-ray afterglow emission was detected with the XMM-Newton satellite. Evidence of soft X-ray emission lines was reported by Reeves and colleagues but not confirmed by other authors. In investigating the spectral evolution of the prompt emission, we find the possible evidence of a transient absorption feature at 6.9+0.6-0.5 keV during the rise of the primary event. The significance of the feature is derived with nonparametric tests and numerical simulations, finding a chance probability that ranges from 3×10-3 down to 4×10-4. The feature shows a Gaussian profile and an equivalent width of 1.2+0.5-0.6 keV. We discuss our results and their possible interpretation

The Prompt X-Ray Emission of GRB 011211: Possible Evidence of a Transient Absorption Feature

FRONTERA, Filippo;GUIDORZI, Cristiano;MONTANARI, Enrico;
2004

Abstract

We report observation results of the prompt X- and gamma-ray emission from GRB 011211. This event was detected with the Gamma-Ray Burst Monitor and one of the wide-field cameras aboard the BeppoSAX satellite. The optical counterpart of the gamma-ray burst was soon identified and its redshift determined (z=2.140), while the X-ray afterglow emission was detected with the XMM-Newton satellite. Evidence of soft X-ray emission lines was reported by Reeves and colleagues but not confirmed by other authors. In investigating the spectral evolution of the prompt emission, we find the possible evidence of a transient absorption feature at 6.9+0.6-0.5 keV during the rise of the primary event. The significance of the feature is derived with nonparametric tests and numerical simulations, finding a chance probability that ranges from 3×10-3 down to 4×10-4. The feature shows a Gaussian profile and an equivalent width of 1.2+0.5-0.6 keV. We discuss our results and their possible interpretation
2004
Frontera, Filippo; Amati, L.; ZAND J. J. M., In'T; Lazzati, D.; Knigl, A.; Vietri, M.; Costa, E.; Feroci, M.; Guidorzi, Cristiano; Montanari, Enrico; ...espandi
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11392/1202247
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