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Issue A&A
Volume 478, Number 2, February I 2008
Page(s) 409 - 417
Section Extragalactic astronomy
DOI http://dx.doi.org/10.1051/0004-6361:20078805



A&A 478, 409-417 (2008)
DOI: 10.1051/0004-6361:20078805

When GRB afterglows get softer, hard components come into play

A. Moretti1, R. Margutti1, 2, F. Pasotti1, 2, A. P. Beardmore3, S. Campana1, G. Chincarini2, 1, S. Covino1, O. Godet3, C. Guidorzi2, 1, J. P. Osborne3, P. Romano2, 1, and G. Tagliaferri1

1  INAF - Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy
    e-mail: alberto.moretti@brera.inaf.it
2  Università degli Studi di Milano-Bicocca, Dipartimento di Fisica, Piazza delle Scienze 3, 20126 Milano, Italy
3  University of Leicester, LE1 7RH, UK

(Received 6 October 2007 / Accepted 21 November 2007)

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.


Key words: gamma rays: bursts



© ESO 2008


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