Skip to content

Opening book details…

Can I read HETE-2 Localization and Observation of the Bright, X-Ray-Rich Gamma-Ray Burst GRB021211 on EtoBox?

HETE-2 Localization and Observation of the Bright, X-Ray-Rich Gamma-Ray Burst GRB021211 by Crew, G. B.; Lamb, D. Q.; Ricker, G. R.; Atteia, J. -L.; Kawai, N.; Vanderspek, R.; Villasenor, J.; Doty, J.; Prigozhin, G.; Jernigan, J. G.; Graziani, C.; Shirasaki, Y.; Sakamoto, T.; Suzuki, M.; Butler, N.; Hurley, K.; Tamagawa, T.; Yoshida, A.; Matsuoka, M.; Fenimore, E. E.; Galassi, M.; Barraud, C.; Boer, M.; Dezalay, J. -P.; Olive, J. -F.; Levine, A.; Monnelly, G.; Martel, F.; Morgan, E.; Donaghy, T. Q.; Torii, K.; Woosley, S. E.; Cline, T.; Braga, J.; Manchanda, R.; Pizzichini, G.; Takagishi, K.; Yamauchi, M. is a scholarly article available to read on EtoBox.

What is HETE-2 Localization and Observation of the Bright, X-Ray-Rich Gamma-Ray Burst GRB021211 about?

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 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

Author
Crew, G. B.; Lamb, D. Q.; Ricker, G. R.; Atteia, J. -L.; Kawai, N.; Vanderspek, R.; Villasenor, J.; Doty, J.; Prigozhin, G.; Jernigan, J. G.; Graziani, C.; Shirasaki, Y.; Sakamoto, T.; Suzuki, M.; Butler, N.; Hurley, K.; Tamagawa, T.; Yoshida, A.; Matsuoka, M.; Fenimore, E. E.; Galassi, M.; Barraud, C.; Boer, M.; Dezalay, J. -P.; Olive, J. -F.; Levine, A.; Monnelly, G.; Martel, F.; Morgan, E.; Donaghy, T. Q.; Torii, K.; Woosley, S. E.; Cline, T.; Braga, J.; Manchanda, R.; Pizzichini, G.; Takagishi, K.; Yamauchi, M.
Published
2003
Language
EN

More by Crew, G. B.; Lamb, D. Q.; Ricker, G. R.; Atteia, J. -L.; Kawai, N.; Vanderspek, R.; Villasenor, J.; Doty, J.; Prigozhin, G.; Jernigan, J. G.; Graziani, C.; Shirasaki, Y.; Sakamoto, T.; Suzuki, M.; Butler, N.; Hurley, K.; Tamagawa, T.; Yoshida, A.; Matsuoka, M.; Fenimore, E. E.; Galassi, M.; Barraud, C.; Boer, M.; Dezalay, J. -P.; Olive, J. -F.; Levine, A.; Monnelly, G.; Martel, F.; Morgan, E.; Donaghy, T. Q.; Torii, K.; Woosley, S. E.; Cline, T.; Braga, J.; Manchanda, R.; Pizzichini, G.; Takagishi, K.; Yamauchi, M.

Browse all works by Crew, G. B.; Lamb, D. Q.; Ricker, G. R.; Atteia, J. -L.; Kawai, N.; Vanderspek, R.; Villasenor, J.; Doty, J.; Prigozhin, G.; Jernigan, J. G.; Graziani, C.; Shirasaki, Y.; Sakamoto, T.; Suzuki, M.; Butler, N.; Hurley, K.; Tamagawa, T.; Yoshida, A.; Matsuoka, M.; Fenimore, E. E.; Galassi, M.; Barraud, C.; Boer, M.; Dezalay, J. -P.; Olive, J. -F.; Levine, A.; Monnelly, G.; Martel, F.; Morgan, E.; Donaghy, T. Q.; Torii, K.; Woosley, S. E.; Cline, T.; Braga, J.; Manchanda, R.; Pizzichini, G.; Takagishi, K.; Yamauchi, M.