Physics of the GRB 030328 afterglow and its environment

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dc.creatorMaiorano, E.
dc.creatorMasetti, N.
dc.creatorPalazzi, E.
dc.creatorSavaglio, S.
dc.creatorRol, E.
dc.creatorVreeswijk, P. M.
dc.creatorPian, E.
dc.creatorPrice, P. A.
dc.creatorPeterson, B. A.
dc.creatorJelinek, M.
dc.creatorAmati, L.
dc.creatorAndersen, M. I.
dc.creatorCastro-Tirado, A. J.
dc.creatorCerón, J. M. Castro
dc.creatorPostigo, A. de Ugarte
dc.creatorFrontera, F.
dc.creatorFruchter, A. S.
dc.creatorFynbo, J. P. U.
dc.creatorGorosabel, J.
dc.creatorHenden, A. A.
dc.creatorHjorth, J.
dc.creatorJensen, B. L.
dc.creatorKlose, S.
dc.creatorKouveliotou, C.
dc.creatorMasi, G.
dc.creatorMøller, P.
dc.creatorNicastro, L.
dc.creatorOfek, E. O.
dc.creatorPandey, S. B.
dc.creatorRhoads, J.
dc.creatorTanvir, N. R.
dc.creatorWijers, R. A. M. J.
dc.creatorHeuvel, E. P. J. van den
dc.date2006-04-05
dc.date.accessioned2026-07-07T11:57:21Z
dc.date.available2026-07-07T11:57:21Z
dc.descriptionWe report on the photometric, spectroscopic and polarimetric, monitoring of the optical afterglow of Gamma-Ray Burst (GRB) 030328 detected by HETE-2. Photometry, collected at 7 different telescopes, shows that a smoothly broken powerlaw decay, with indices alpha_1 = 0.76 +/- 0.03, alpha_2 = 1.50 +/- 0.07 and a break at t_b = 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} of about 3.2 degrees. 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) degrees, 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 beta_{X} = 1.0 +/- 0.2. The discussion of these 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.
dc.description14 pages, 6 figures, 3 tables, accepted for publication on A&A, main journal. Abstract changed to comply with the new format of A&A abstracts
dc.identifierhttps://arxiv.org/abs/astro-ph/0604093
dc.identifierhttp://arxiv.org/abs/astro-ph/0604093
dc.identifierAstron.Astrophys.455:423-431,2006
dc.identifierdoi:10.1051/0004-6361:20054728
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/205854
dc.subjectAstrophysics
dc.titlePhysics of the GRB 030328 afterglow and its environment
dc.typetext

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