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Title:
Physics of the GRB 030328 afterglow and its environment
Authors:
Maiorano, E.; Masetti, N.; Palazzi, E.; Savaglio, S.; Rol, E.; Vreeswijk, P. M.; Pian, E.; Price, P. A.; Peterson, B. A.; Jelínek, M.; Amati, L.; Andersen, M. I.; Castro-Tirado, A. J.; Castro Cerón, J. M.; de Ugarte Postigo, A.; Frontera, F.; Fruchter, A. S.; Fynbo, J. P. U.; Gorosabel, J.; Henden, A. A.; Hjorth, J.; Jensen, B. L.; Klose, S.; Kouveliotou, C.; Masi, G.; Møller, 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.
Affiliation:
AA(INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy ; INAF - Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy ; Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40126 Bologna, Italy), AB(INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), AC(INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), AD(The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), AE(Department of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK), AF(European Southern Observatory, Casilla 19001, Santiago 19, Chile), AG(INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy; INAF - Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131 Trieste, Italy), AH(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; Research School of Astronomy and Astrophysics, Australian National University, via Cotter Road, Weston, ACT 2611, Australia), AI(Research School of Astronomy and Astrophysics, Australian National University, via Cotter Road, Weston, ACT 2611, Australia), AJ(Instituto de Astrofísica de Andalucía (IAA-CSIC), PO Box 03004, 18080 Granada, Spain), AK(INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), AL(Astrophysikalisches Institut, 14482 Potsdam, Germany), AM(Instituto de Astrofísica de Andalucía (IAA-CSIC), PO Box 03004, 18080 Granada, Spain), AN(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark), AO(Instituto de Astrofísica de Andalucía (IAA-CSIC), PO Box 03004, 18080 Granada, Spain), AP(INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy; Dipartimento di Fisica, Università di Ferrara, via Saragat 1, 44100 Ferrara, Italy), AQ(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA), AR(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark), AS(Instituto de Astrofísica de Andalucía (IAA-CSIC), PO Box 03004, 18080 Granada, Spain), AT(Universities Space Research Association / US Naval Observatory, PO Box 1149, Flagstaff, AZ 86002, USA), AU(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark), AV(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark), AW(Thüringer Landessternwarte Tautenburg, 07778 Tautenburg, Germany), AX(NASA MSFC, SD-50, Huntsville, AL 35812, USA), AY(Dipartimento di Fisica, Università di Roma "Tor Vergata", via della Ricerca Scientifica 1, 00133 Rome, Italy), AZ(European Southern Observatory, Karl Schwarzschild-Strasse 2, 85748 Garching, Germany), BA(INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, 40129 Bologna, Italy), BB(School of Physics and Astronomy and the Wise Observatory, University of Tel-Aviv, Tel-Aviv 69978, Israel), BC(Instituto de Astrofísica de Andalucía (IAA-CSIC), PO Box 03004, 18080 Granada, Spain ; ARIES Observatory, Manora Peak, Naini Tal, 263129 Uttaranchal, India), BD(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA), BE(Department of Physical Sciences, University of Hertfordshire, College Lane, Hatfield, Herts AL10 9AB, UK), BF(Institute of Astronomy "Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands), BG(Institute of Astronomy "Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands)
Publication:
Astronomy and Astrophysics, Volume 455, Issue 2, August IV 2006, pp.423-431 (A&A Homepage)
Publication Date:
08/2006
Origin:
EDP Sciences
Keywords:
gamma rays: bursts, radiation mechanisms: non-thermal, line: identification, cosmology: observations
DOI:
10.1051/0004-6361:20054728
Bibliographic Code:
2006A&A...455..423M

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.
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