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29 March 2024
 
  » arxiv » 0804.4367

 Article overview


The complex light-curve of the afterglow of GRB071010A
S. Covino ; P. D'Avanzo ; A. Klotz ; D.A. Perley ; L. Amati ; S. Campana ; G. Chincarini ; A. Cucchiara ; V. D'Elia ; D. Guetta ; C. Guidorzi ; D.A. Kann ; A. Küpcü Yoldaş ; K. Misra ; G. Olofsson ; G. Tagliaferri ; L.A. Antonelli ; E. Berger ; J.S. Bloom ; M. Böer ; C. Clemens ; F. D'Alessio ; M. Della Valle ; S. di Serego Alighieri ; A.V. Filippenko ; R.J. Foley ; D.B. Fox ; D. Fugazza ; J. Fynbo ; B. Gendre ; P. Goldoni ; J. Greiner ; D. Kocevksi ; E. Maiorano ; N. Masetti ; E. Meurs ; M. Modjaz ; E. Molinari ; A. Moretti ; E. Palazzi ; S.B. Pandey ; S. Piranomonte ; D. Poznanski ; N. Primak ; P. Romano ; E. Rossi ; R. Roy ; J.M. Silverman ; L. Stella ; G. Stratta ; V. Testa ; S.D. Vergani ; F. Vitali ; F. Zerbi ;
Date 28 Apr 2008
AbstractWe 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 2min after the high-energy event. Swift-XRT observations started only later at about 0.4d. The light-curve evolution allows us to single out an initial rising phase with 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 0.6d. 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 1d. 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 1d, just after the rebrightening and almost coincident with the steepening. This provided a fairly tight upper limit of 0.9% for the polarized-flux fraction.
Source arXiv, 0804.4367
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