J.M. Castro Cerón
A. de Ugarte Postigo
E.P.J. van den Heuvel
- Physics of the GRB 030328 afterglow and its environment
- Astronomy & Astrophysics
- Volume | Issue number
- 455 | 2
- Pages (from-to)
- Document type
- Faculty of Science (FNWI)
- Anton Pannekoek Institute for Astronomy (API)
Aims.To investigate the physical nature of the afterglow emission. We report on the photometric, spectroscopic and polarimetric observations of the optical afterglow of Gamma-Ray Burst (GRB) 030328 detected by HETE-2.
Methods.Photometric, spectroscopic and polarimetric monitoring of the optical afterglow.
Results.Photometry, collected at 7 different telescopes, shows that a smoothly broken powerlaw decay, with indices alpha1 = 0.76 ± 0.03, alpha2 = 1.50 ± 0.07 and a break at tb = 0.48 ± 0.03 days after the GRB, provides the best fit of the optical afterglow decline. This shape is interpreted as due to collimated emission, for which we determine a jet opening angle theta_jet ~ 3.2 °. An achromatic bump starting around ~0.2 d after the GRB is possibly marginally detected in the optical light curves. Optical spectroscopy shows the presence of two rest-frame ultraviolet metal absorption systems at z = 1.5216 ± 0.0006 and at z = 1.295 ± 0.001, the former likely associated with the GRB host galaxy. Analysis of the absorption lines at z = 1.5216 suggests that the host of this GRB may be a Damped Lyman-alpha Absorber. The optical V-band afterglow appears polarized, with P = (2.4 ± 0.6)% and theta = 170° ± 7°, suggesting an asymmetric blastwave expansion. An X-ray-to-optical spectral flux distribution of the GRB 030328 afterglow was obtained at 0.78 days after the GRB and fitted using a broken powerlaw, with an optical spectral slope beta_opt = 0.47 ± 0.15, and an X-ray slope betaX = 1.0 ± 0.2.
Conclusions.The discussion of the results in the context of the "fireball model" shows that the preferred scenario for this afterglow is collimated structured jet with fixed opening angle in a homogeneous medium.
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- © EDP Sciences 2006
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