HETE Observations of the Gamma-Ray Burst GRB 030329: Evidence for an Underlying Soft X-Ray Component

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

doi:10.1086/423923

論文・著書情報

タイトル

和文:
英文:	HETE Observations of the Gamma-Ray Burst GRB 030329: Evidence for an Underlying Soft X-Ray Component

著者

和文:

Vanderspek, R., Sakamoto, T., Barraud, C., Tamagawa, T., Graziani, C., Suzuki, M., Shirasaki, Y., Prigozhin, G., Villasenor, J., Jernigan, J. G., Crew, G. B., Atteia, J.-L., Hurley, K., 河合誠之, Lamb, D. Q., Ricker, G. R., Woosley, S. E., Butler, N., Doty, J. P., Dullighan, A., Donaghy, T. Q., Fenimore, E. E., Galassi, M., Matsuoka, M., Takagishi, K., Torii, K., Yoshida, A., Boer, M., Dezalay, J.-P., Olive, J.-F., Braga, J., Manchanda, R., Pizzichini, G..

英文:

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

言語

English

掲載誌/書名

和文:
英文:	Astrophysical Journal

巻, 号, ページ

Vol. 617 pp. 1251-1257

出版年月

2004年12月

出版者

和文:
英文:

会議名称

和文:
英文:

開催地

和文:
英文:

DOI

https://doi.org/10.1086/423923

アブストラクト

An exceptionally intense gamma-ray burst, GRB 030329, was detected and localized by the instruments on board the High Energy Transient Explorer satellite (HETE) at 11:37:14 UT on 2003 March 29. The burst consisted of two ~10 s pulses of roughly equal brightness and an X-ray tail lasting more than 100 s. The energy fluence in the 30-400 keV energy band was S_γ=1.2×10^-4 ergs cm^-2, making GRB 030329 one of the brightest GRBs ever detected. Communication of a 2' error box 73 minutes after the burst allowed the rapid detection of a counterpart in the optical, X-ray, and radio and the ensuing discovery of a supernova with most unusual characteristics. Analyses of the burst light curves reveal the presence of a distinct, bright, soft X-ray component underlying the main GRB; the 2-10 keV fluence of this component is ~7×10^-6 ergs cm^-2. The main pulses of GRB 030329 were preceded by two soft, faint, nonthermal bumps. We present details of the HETE observations of GRB 030329.

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