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The complex light curve of the afterglow of GRB071010A

Covino, S, D'Avanzo, P, Klotz, A, Perley, DA, Amati, L, Campana, S, Chincarini, G, Cucchiara, A, D'Elia, V, Guetta, D, Guidorzi, C, Kann, DA, Küpcü Yoldas, A, Misra, K, Olofsson, G, Tagliaferri, G, Antonelli, LA, Berger, E, Bloom, JS, Böer, M , Clemens, C, D'Alessio, F, Della Valle, M, di Serego Alighieri, S, Filippenko, AV, Foley, RJ, Fox, DB, Fugazza, D, Fynbo, J, Gendre, B, Goldoni, P, Greiner, J, Kocevksi, D, Maiorano, E, Masetti, N, Meurs, E, Modjaz, M, Molinari, E, Moretti, A, Palazzi, E, Pandey, SB, Piranomonte, S, Poznanski, D, Primak, N, Romano, P, Rossi, E, Roy, R, Silverman, JM, Stella, L, Stratta, G, Testa, V, Vergani, SD, Vitali, F and Zerbi, F (2008) The complex light curve of the afterglow of GRB071010A. Monthly Notices of the Royal Astronomical Society, 388 (1). pp. 347-356. ISSN 0035-8711

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We present and discuss the results of an extensive observational campaign devoted to GRB071010A, a long-duration gamma-ray burst detected by the Swift satellite. This event was followed for almost a month in the optical/near-infrared (NIR) with various telescopes starting from about 2 min after the high-energy event. Swift XRT observations started only later at about 0.4 d. The light-curve evolution allows us to single out an initial rising phasewith a maximum at about 7min, possibly the afterglow onset in the context of the standard fireball model, which is then followed by a smooth decay interrupted by a sharp rebrightening at about 0.6 d. The rebrightening was visible in both the optical/NIR and X-rays and can be interpreted as an episode of discrete energy injection, although various alternatives are possible. A steepening of the afterglow light curve is recorded at about 1 d. The entire evolution of the optical/NIR afterglow is consistent with being achromatic. This could be one of the few identified GRB afterglows with an achromatic break in the X-ray through the optical/NIR bands. Polarimetry was also obtained at about 1 d, just after the rebrightening and almost coincident with the steepening. This provided a fairly tight upper limit of 0.9 per cent for the polarized-flux fraction. © 2008 The Authors. Journal compilation © 2008 RAS.

Item Type: Article
Additional Information: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2008 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords: 0201 Astronomical And Space Sciences
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: Oxford University Press
Date Deposited: 23 May 2017 10:25
Last Modified: 20 Apr 2022 09:13
DOI or ID number: 10.1111/j.1365-2966.2008.13393.x
URI: https://researchonline.ljmu.ac.uk/id/eprint/6508
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