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20 April 2024
 
  » arxiv » astro-ph/0303470

 Article overview


HETE-2 Localization and Observation of the Bright, X-Ray-Rich Gamma-Ray Burst GRB021211
G. B. Crew ; D. Q. Lamb ; G. R. Ricker ; J.-L. Atteia ; N. Kawai ; R. Vanderspek ; J. Villasenor ; J. Doty ; G. Prigozhin ; J. G. Jernigan ; C. Graziani ; Y. Shirasaki ; T. Sakamoto ; M. Suzuki ; N. Butler ; K. Hurley ; T. Tamagawa ; A. Yoshida ; M. Matsuoka ; E. E. Fenimore ; M. Galassi ; C. Barraud ; M. Boer ; J.-P. Dezalay ; J.-F. Olive ; A. Levine ; G. Monnelly ; F. Martel ; E. Morgan ; T. Q. Donaghy ; K. Torii ; S. E. Woosley ; T. Cline ; J. Braga ; R. Manchanda ; G. Pizzichini ; K. Takagishi ; M. Yamauchi ;
Date 20 Mar 2003
Journal Astrophys.J. 599 (2003) 387-393
Subject astro-ph
AbstractA bright, x-ray-rich GRB was detected by HETE-2 at 11:18:34.03 UT on 11 Dec 2002. The WXM localization was to 14’ and relayed to the GCN 22 s after the start of the burst. The ground SXC localization was within 2’ of R.A. 08h 09m 00s, Dec 06d 44’ 20" (J2000). GRB021211 consists of a single, FRED-like pulse with t90s of 2.3 s (85-400 keV) and 8.5 s (2-10 keV). The peak photon number and photon energy fluxes in the 2-400 keV band, are 34.0 +/- 1.8 ph cm^-2 s^-1 and 1.68 +/- 0.11 x 10^-6 erg cm^-2 s^-1, respectively. The energy fluences in the 2-30 keV and 30-400 kev energy bands are S_X = 1.36 +/- 0.05 x 10^-6 erg cm^-2 and S_gamma 2.17 +/- 0.15 x 10^-6 erg cm^-2, respectively. Thus GRB021211 is an X-ray-rich GRB (S_X/S_gamma = 0.63 > 0.32). The spectrum is well-fit by a Band function (alpha = -0.805, beta = -2.37, E_peak = 46.8 keV). The prompt localization allowed the detection of an optical afterglow for what would otherwise have been an ``optically dark’’ GRB. GRB 021211 demonstrates that some fraction of burst afterglows are ``optically dark’’ because their optical afterglows at times > 1 hr after the burst are very faint, and thus have often escaped detection. GRB 021211 shows that such ``optically dim’’ bursts can have very bright afterglows at times < 20 min after the burst.
Source arXiv, astro-ph/0303470
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