Science-advisor
REGISTER info/FAQ
Login
username
password
     
forgot password?
register here
 
Research articles
  search articles
  reviews guidelines
  reviews
  articles index
My Pages
my alerts
  my messages
  my reviews
  my favorites
 
 
Stat
Members: 3643
Articles: 2'487'895
Articles rated: 2609

29 March 2024
 
  » arxiv » astro-ph/0408453

 Article overview


High Energy Observations of XRF 030723: Evidence for an Off-axis Gamma-Ray Burst?
N. R. Butler ; T. Sakamoto ; M. Suzuki ; N. Kawai ; D. Q. Lamb ; C. Graziani ; T. Q. Donaghy ; A. Dullighan ; R. Vanderspek ; G. B. Crew ; P. Ford ; G. Ricker ; J-L. Atteia ; A. Yoshida ; Y. Shirasaki ; T. Tamagawa ; K. Torii ; M. Matsuoka ; E. E. Fenimore ; M. Galassi ; J. Doty ; J. Villasenor ; G. Prigozhin ; J. G. Jernigan ; C. Barraud ; M. Boer ; J-P. Dezalay ; J-F. Olive ; K. Hurley ; A. Levine ; F. Martel ; E. Morgan ; S. E. Woosley ; T. Cline ; J. Braga ; R. Manchanda ; G. Pizzichini ;
Date 24 Aug 2004
Journal Astrophys.J. 621 (2005) 884-893
Subject astro-ph
AbstractWe report High Energy Transient Explorer 2 (HETE-2) Wide Field X-ray Monitor/French Gamma Telescope observations of XRF030723 along with observations of the XRF afterglow made using the 6.5m Magellan Clay telescope and the Chandra X-ray Observatory. The observed peak energy E_pk_obs 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 E_pk_obs=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 E_iso and E_pk_rest 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 due to a progenitor wind.
Source arXiv, astro-ph/0408453
Services Forum | Review | PDF | Favorites   
 
Visitor rating: did you like this article? no 1   2   3   4   5   yes

No review found.
 Did you like this article?

This article or document is ...
important:
of broad interest:
readable:
new:
correct:
Global appreciation:

  Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.

browser claudebot






ScienXe.org
» my Online CV
» Free


News, job offers and information for researchers and scientists:
home  |  contact  |  terms of use  |  sitemap
Copyright © 2005-2024 - Scimetrica