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 α1 = 0.76 ± 0.03, α2 = 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 θ_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-α Absorber. The optical V-band afterglow appears polarized, with P = (2.4 ± 0.6)% and θ = 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 β_opt = 0.47 ± 0.15, and an X-ray slope βX = 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.

Physics of the GRB 030328 afterglow and its environment

FRONTERA, Filippo;
2006

Abstract

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 α1 = 0.76 ± 0.03, α2 = 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 θ_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-α Absorber. The optical V-band afterglow appears polarized, with P = (2.4 ± 0.6)% and θ = 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 β_opt = 0.47 ± 0.15, and an X-ray slope βX = 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.
2006
Maiorano, E; Masetti, N; Palazzi, E; Savaglio, S; Rol, E; Vreeswijk, P. M.; Pian, E; Price, P. A.; Peterson, B. A.; Jelnek, M; Amati, L; Andersen, M. I.; CASTRO TIRADO, A. J.; CASTRO CERN, J. M.; DE UGARTE POSTIGO, A; Frontera, Filippo; Fruchter, A. S.; Fynbo, J. P. U.; Gorosabel, J; Henden, A. A; Hjorth, J; Jensen, B. L.; Klose, S; Kouveliotou, C; Masi, G; Mller, P; Nicastro, L; Ofek, E. O.; Pandey, S. B.; Rhoads, J; Tanvir, N. R.; Wijers, R. A. M. J.; VAN DEN HEUVEL, E. P. J.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11392/494465
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