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論文・著書情報
| タイトル |
| 和文: | |
| 英文: | High-Energy Observations of XRF 030723: Evidence for an Off-Axis Gamma-Ray Burst? |
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| 著者 |
| 和文: |
Butler, N. R.,
Sakamoto, T.,
Suzuki, M.,
河合 誠之,
Lamb, D. Q.,
Graziani, C.,
Donaghy, T. Q.,
Dullighan, A.,
Vanderspek, R.,
Crew, G. B.,
Ford, P.,
Ricker, G.,
Atteia, J.-L.,
Yoshida, A.,
Shirasaki, Y.,
Tamagawa, T.,
Torii, K.,
Matsuoka, M.,
Fenimore, E. E.,
Galassi, M.,
Doty, J.,
Villasenor, J.,
Prigozhin, G.,
Jernigan, J. G.,
Barraud, C.,
Boer, M.,
Dezalay, J.-P.,
Olive, J.-F.,
Hurley, K.,
Levine, A.,
Martel, F.,
Morgan, E.,
Woosley, S. E.,
Cline, T.,
Braga, J.,
Manchanda, R.,
Pizzichini, G..
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| 英文: |
Butler, N. R.,
Sakamoto, T.,
Suzuki, M.,
Kawai, N.,
Lamb, D. Q.,
Graziani, C.,
Donaghy, T. Q.,
Dullighan, A.,
Vanderspek, R.,
Crew, G. B.,
Ford, P.,
Ricker, G.,
Atteia, J.-L.,
Yoshida, A.,
Shirasaki, Y.,
Tamagawa, T.,
Torii, K.,
Matsuoka, M.,
Fenimore, E. E.,
Galassi, M.,
Doty, J.,
Villasenor, J.,
Prigozhin, G.,
Jernigan, J. G.,
Barraud, C.,
Boer, M.,
Dezalay, J.-P.,
Olive, J.-F.,
Hurley, K.,
Levine, A.,
Martel, F.,
Morgan, E.,
Woosley, S. E.,
Cline, T.,
Braga, J.,
Manchanda, R.,
Pizzichini, G..
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| 言語 |
English |
| 掲載誌/書名 |
| 和文: | |
| 英文: | Astrophysical Journal |
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巻, 号, ページ
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Vol. 621
pp. 884-893
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| 出版年月 |
2005年3月 |
| 出版者 |
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| 会議名称 |
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| 開催地 |
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| DOI |
https://doi.org/10.1086/427746 |
| アブストラクト |
We report High Energy Transient Explorer 2 (HETE-2) Wide Field X-ray Monitor (WXM) and French Gamma Telescope observations of XRF 030723 along with observations of the XRF afterglow made using the 6.5 m Magellan Clay telescope and Chandra. The observed peak energy Eobspk of the νFν burst spectrum is found to lie within (or below) the WXM 2-25 keV passband at 98.5% confidence, and no counts are detected above 30 keV. Our best-fit value is Eobspk=8.4+3.5-3.4 keV. The ratio of X-ray to γ-ray flux for the burst follows a correlation found for GRBs observed with HETE-2, and the duration of the burst is similar to that typical of long-duration GRBs. If we require that the burst isotropic equivalent energy Eiso and Epk satisfy the relation discovered by Amati et al. (2002), a redshift of z=0.38+0.36-0.18 can be determined, in agreement with constraints determined from optical observations. We are able to fit the X-ray afterglow spectrum and to measure its temporal fade. Although the best-fit fade is shallower than the concurrent fade in the optical, the spectral similarity between the two bands indicates that the X-ray fade may actually trace the optical fade. If this is the case, the late-time rebrightening observed in the optical cannot be due to a supernova bump. We interpret the prompt and afterglow X-ray emission as arising from a jetted GRB observed off-axis and possibly viewed through a complex circumburst medium that is due to a progenitor wind. |
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