Статья

High‐Energy Observations of XRF 030723: Evidence for an Off‐Axis Gamma‐Ray Burst?

N. ButlerCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139T. SakamotoDepartment of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, JapanM. SuzukiDepartment of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, JapanN. KawaiDepartment of Physics, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, JapanD. Q. LambDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637C. GrazianiDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637T. DonaghyDepartment of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637A. DullighanCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139R. VanderspekCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139G. CrewCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139P. G. FordCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139G. RickerCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139J. L. AtteiaLaboratoire d’Astrophysique, Observatoire Midi-Pyreńeés, 14 Avenue Edouard Belin, 31400 Toulouse, FranceA. YoshidaDepartment of Physics, Aoyama Gakuin University, Chitosedai 6-16-1, Setagaya-ku, Tokyo 157-8572, JapanY. ShirasakiNational Astronomical Observatory, Osawa 2-21-1, Mitaka, Tokyo 181-8588, JapanToru TamagawaRIKEN (Institute of Physical and Chemical Research), 2-1 Hirosawa, Wako, Saitama 351-0198, JapanK. ToriiDepartment of Earth and Space Science, Graduate School of Science, Osaka University 1-1 Machikaneyama-cho, Toyonaka, Osaka 560-0043, JapanM. MatsuokaE. E. FenimoreLos Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545M. GalassiLos Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545J. DotyCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139J. VillaseñorCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139G. PrigozhinCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139J. G. JerniganSpace Sciences Laboratory, University of California, Berkeley, CA 94720-7450C. BarraudLaboratoire d’Astrophysique, Observatoire Midi-Pyreńeés, 14 Avenue Edouard Belin, 31400 Toulouse, FranceM. BoërCentre d’Etude Spatiale des Rayonnements, CNRS/UPS, Boite Postale 4346, 31028 Toulouse Cedex 4, FranceJ. P. DezalayCentre d’Etude Spatiale des Rayonnements, CNRS/UPS, Boite Postale 4346, 31028 Toulouse Cedex 4, FranceJ.‐F. OliveCentre d’Etude Spatiale des Rayonnements, CNRS/UPS, Boite Postale 4346, 31028 Toulouse Cedex 4, FranceK. HurleySpace Sciences Laboratory, University of California, Berkeley, CA 94720-7450A. M. LevineCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139F. MartelCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139E. MorganCenter for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139S. E. WoosleyDepartment of Astronomy and Astrophysics, University of California at Santa Cruz, 477 Clark Kerr Hall, Santa Cruz, CA 95064T. L. ClineNASA Goddard Space Flight Center, Greenbelt, MD 20771J. BragaInstituto Nacional de Pesquisas Espaciais, Avenida Dos Astronautas 1758, Saõ Josédos Campos 12227-010, BrazilR. ManchandaDepartment of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai, 400 005, IndiaG. Pizzichini

2005en

ABI

Аннотация

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 &nu;F&nu; 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 &gamma;-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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Идентификаторы

DOI: 10.1086/427746

Цитирования и источники

Цитирований: 3Использованных источников: 0

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