Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/26691
 Title: When GRB afterglows get softer, hard components come into play Authors: Moretti, A.Margutti, R.Pasotti, F.Campana, S.Chincarini, G.Covino, S.Guidorzi, C.Romano, P.Tagliaferri, G.Margutti, R.Pasotti, F.Chincarini, G.Guidorzi, C.Romano, P.Beardmore, A. P.Godet, O.Osborne, J. P. First Published: Feb-2008 Publisher: EDP Sciences for European Southern Observatory (ESO) Citation: Astronomy & Astrophysics, 2008, 478 (2), pp. 409-417 Abstract: Aims.We aim to investigate the ability of simple spectral models to describe the early afterglow emission of GRBs. Methods.We performed a time-resolved spectral analysis of a bright GRB sample detected by the Swift Burst Alert Telescope and promptly observed by the Swift X-ray Telescope,with spectroscopically measured redshift in the period April 2005-January 2007. The sample consists of 22 GRBs and a total of 214 spectra. We restricted our analysis to the softest spectra sub-sample which consists of 13 spectra with photon index >3. Results.In this sample we found that four spectra, belonging to the GRB 060502A, GRB 060729, GRB 060904B, GRB 061110A prompt-afterglow transition phase, can be modeled neither by a single power-law nor by the Band model. Instead we find that the data present high-energy (>3 keV, in the observer frame) excesses with respect to these models. We estimated the joint statistical significance of these excesses at the level of 4.3$\sigma$. In all four cases, the deviations can be modeled well by adding either a second power law or a blackbody component to the usual synchrotron power law spectrum. The additional power law would be explained by the emergence of the afterglow, while the blackbody could be interpreted as the photospheric emission from X-ray flares or as the shock breakout emission. In one case these models leave a 2.2$\sigma$ excess that can be fit by a Gaussian line at the energy of the highly ionized nickel recombination. Conclusions.Although the data do not allow an unequivocal interpretation, the importance of this analysis consists in showing that a simple power-law model or a Band model is insufficient to describe the X-ray spectra of a small homogeneous sample of GRBs at the end of their prompt phase. DOI Link: 10.1051/0004-6361:20078805 ISSN: 0004-6361 eISSN: 1432-0746 Links: http://hdl.handle.net/2381/26691http://www.aanda.org/articles/aa/abs/2008/05/aa8805-07/aa8805-07.html Version: Publisher Version Status: Peer-reviewed Type: Journal Article Rights: Copyright © 2008 ESO. Reproduced with permission from Astronomy & Astrophysics, © ESO. Appears in Collections: Published Articles, Dept. of Physics and Astronomy

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