The complex light curve of the afterglow of GRB 071010A

被引：47

作者：

Covino, S. ^{[1
]}

D'Avanzo, P. ^{[1
,2
]}

Klotz, A. ^{[3
,4
]}

Perley, D. A. ^{[5
]}

Amati, L. ^{[6
]}

Campana, S. ^{[1
]}

Chincarini, G. ^{[1
,7
]}

Cucchiara, A. ^{[8
]}

D'Elia, V. ^{[9
]}

Guetta, D. ^{[9
]}

Guidorzi, C. ^{[1
,7
]}

Kann, D. A. ^{[10
]}

Yoldas, A. Kuepcue ^{[11
]}

Misra, K. ^{[12
,13
]}

Olofsson, G. ^{[14
]}

Tagliaferri, G. ^{[1
]}

Antonelli, L. A. ^{[9
]}

Berger, E. ^{[15
]}

Bloom, J. S. ^{[5
]}

Boeer, M. ^{[3
]}

Clemens, C.

D'Alessio, F. ^{[9
]}

Della Valle, M. ^{[16
,17
,18
]}

Alighieri, S. di Serego ^{[19
]}

Filippenko, A. V. ^{[5
]}

Foley, R. J. ^{[5
]}

Fox, D. B.

Fugazza, D. ^{[1
]}

Fynbo, J. ^{[20
]}

Gendre, B. ^{[21
]}

Goldoni, P. ^{[22
,23
]}

Greiner, J. ^{[11
]}

Kocevksi, D. ^{[5
]}

Maiorano, E. ^{[6
]}

Masetti, N. ^{[6
]}

Meurs, E. ^{[24
,25
,26
]}

Modjaz, M. ^{[5
]}

Molinari, E. ^{[1
]}

Moretti, A. ^{[1
]}

Palazzi, E. ^{[6
]}

Pandey, S. B. ^{[12
]}

Piranomonte, S. ^{[9
]}

Poznanski, D. ^{[5
]}

Primak, N. ^{[11
]}

Romano, P. ^{[1
]}

Rossi, E. ^{[27
]}

Roy, R. ^{[12
]}

Silverman, J. M. ^{[5
]}

Stella, L. ^{[9
]}

Stratta, G. ^{[28
]}

机构：

[1] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy

[2] Univ Insubria, Dipartimento Matemat & Fis, I-22100 Como, Italy

[3] Observ Haute Provence, F-04870 St Michel Lobservatoire, France

[4] Univ Toulouse, CESR, F-31400 Toulouse, France

[5] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[6] Ist Astrofis Spaziale & Fis Cosm Bologna, INAF, I-40129 Bologna, Italy

[7] Univ Milan, I-20126 Milan, Italy

[8] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[9] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Roma, Italy

[10] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany

[11] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[12] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263129, India

[13] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[14] Stockholm Observ, S-10691 Stockholm, Sweden

[15] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA

[16] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy

[17] Int Ctr Relativist Astrophys Network, Icranet, Pescara, Italy

[18] European So Observ, D-8046 Garching, Germany

[19] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy

[20] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, Copenhagen 2100, Denmark

[21] Univ Aix Marseille 1, CNRS, Astrophys Lab, F-13376 Marseille 12, France

[22] Lab Astroparticule & Cosmol, F-75205 Paris 13, France

[23] CEA Saclay, DSM DAPNIA SAp, Serv Astrophys, F-91191 Gif Sur Yvette, France

[24] Dunsink Observ DIAS, Dublin 2, Ireland

[25] Dublin City Univ, Sch Phys Sci, Dublin 9, Ireland

[26] Dublin City Univ, NCPST, Dublin 9, Ireland

[27] Univ Colorado, JILA, Boulder, CO 80309 USA

[28] ASI Sci Data Ctr ASDC, I-00044 Frascati, Italy

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2008年 / 388卷 / 01期

基金：

美国国家科学基金会;

关键词：

methods : observational; gamma-rays : bursts; X-rays : individual : GRB071010A;

D O I：

10.1111/j.1365-2966.2008.13393.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present and discuss the results of an extensive observational campaign devoted to GRB 071010A, 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 phase with a maximum at about 7 min, 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.

引用

页码：347 / 356

页数：10

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