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Title:
GRB081028 and its late-time afterglow re-brightening
Authors:
Margutti, R.; Genet, F.; Granot, J.; Duran, R. Barniol; Guidorzi, C.; Chincarini, G.; Mao, J.; Schady, P.; Sakamoto, T.; Miller, A. A.; Olofsson, G.; Bloom, J. S.; Evans, P. A.; Fynbo, J. P. U.; Malesani, D.; Moretti, A.; Pasotti, F.; Starr, D.; Burrows, D. N.; Barthelmy, S. D.; Roming, P. W. A.; Gehrels, N.
Affiliation:
AA(Università degli studi Milano Bicocca, P.za della Scienza 3, Milano 20126, Italy; INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy), AB(Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB), AC(Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB), AD(Department of Physics, University of Texas at Austin, Austin, TX 78712, USA), AE(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy; Dipartimento di Fisica, Università di Ferrara, via Saragat 1, 44100 Ferrara, Italy), AF(Università degli studi Milano Bicocca, P.za della Scienza 3, Milano 20126, Italy; INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy), AG(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy; Yunnan Observatory, Chinese Academy of Sciences, PO Box 110, Kunming, Yunnan Province 650011, China), AH(The UCL Mullard Space Science Laboratory, Holmbury St Mary, Dorking, Surrey RH5 6NT), AI(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA), AJ(Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA), AK(Stockholm Observatory, Stockholm University, Astronomy Department AlbaNova Research Center, 106 91 Stockholm, Sweden), AL(Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA), AM(X-ray and Observational Astronomy Group, Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH), AN(Dark Cosmology Centre, Niels Bohr Institute, University of Cøpenhagen, Juliane MariesVej 30, 2100 Copenhagen O, Denmark), AO(Dark Cosmology Centre, Niels Bohr Institute, University of Cøpenhagen, Juliane MariesVej 30, 2100 Copenhagen O, Denmark), AP(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy), AQ(INAF Osservatorio Astronomico di Brera, via Bianchi 46, Merate 23807, Italy), AR(Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA), AS(Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA), AT(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA), AU(Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA), AV(NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 402, Issue 1, pp. 46-64. (MNRAS Homepage)
Publication Date:
02/2010
Origin:
MNRAS
MNRAS Keywords:
radiation mechanisms: non-thermal, gamma-rays: bursts, X-rays: individual: GRB081028
Abstract Copyright:
(c) Journal compilation © 2010 RAS
DOI:
10.1111/j.1365-2966.2009.15882.x
Bibliographic Code:
2010MNRAS.402...46M

Abstract

ABSTRACT Swift captured for the first time a smoothly rising X-ray re-brightening of clear non-flaring origin after the steep decay in a long gamma-ray burst (GRB): GRB081028. A rising phase is likely present in all GRBs but is usually hidden by the prompt tail emission and constitutes the first manifestation of what is later to give rise to the shallow decay phase. Contemporaneous optical observations reveal a rapid evolution of the injection frequency of a fast cooling synchrotron spectrum through the optical band, which disfavours the afterglow onset (start of the forward shock emission along our line of sight when the outflow is decelerated) as the origin of the observed re-brightening. We investigate alternative scenarios and find that the observations are consistent with the predictions for a narrow jet viewed off-axis. The high on-axis energy budget implied by this interpretation suggests different physical origins of the prompt and (late) afterglow emission. Strong spectral softening takes place from the prompt to the steep decay phase: we track the evolution of the spectral peak energy from the γ-rays to the X-rays and highlight the problems of the high latitude and adiabatic cooling interpretations. Notably, a softening of both the high and low spectral slopes with time is also observed. We discuss the low on-axis radiative efficiency of GRB081028 comparing its properties against a sample of Swift long GRBs with secure Eγ,iso measurements.
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