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
Abstract
A 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 SX = 1.36 +/- 0.05 x 10-6 erg cm-2 and Sgamma 2.17 +/- 0.15 x 10-6 erg cm-2, respectively. Thus GRB021211 is an X-ray-rich GRB (SX/Sgamma = 0.63 > 0.32). The spectrum is well-fit by a Band function (alpha = -0.805, beta = -2.37, Epeak = 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.
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