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The complex light curve of the afterglow of GRB071010A

Covino, S and D'Avanzo, P and Klotz, A and Perley, DA and Amati, L and Campana, S and Chincarini, G and Cucchiara, A and D'Elia, V and Guetta, D and Guidorzi, C and Kann, DA and Küpcü Yoldas, A and Misra, K and Olofsson, G and Tagliaferri, G and Antonelli, LA and Berger, E and Bloom, JS and Böer, M and Clemens, C and D'Alessio, F and Della Valle, M and di Serego Alighieri, S and Filippenko, AV and Foley, RJ and Fox, DB and Fugazza, D and Fynbo, J and Gendre, B and Goldoni, P and Greiner, J and Kocevksi, D and Maiorano, E and Masetti, N and Meurs, E and Modjaz, M and Molinari, E and Moretti, A and Palazzi, E and Pandey, SB and Piranomonte, S and Poznanski, D and Primak, N and Romano, P and Rossi, E and Roy, R and Silverman, JM and Stella, L and Stratta, G and Testa, V and Vergani, SD and 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: 23 May 2017 10:25
DOI or Identification number: 10.1111/j.1365-2966.2008.13393.x
URI: http://researchonline.ljmu.ac.uk/id/eprint/6508

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