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American Astronomical Society, Astrophysical Journal, 2(729), p. 114, 2011

DOI: 10.1088/0004-637x/729/2/114

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Detection of a spectral break in the extra hard component of GRB 090926A

Journal article published in 2011 by M. G. Baring, Baring Mg, P. N. Bhat, M.; Ajello M.; /Stanford U. HEPL /KIPAC Menlo Park /SLAC /Stanford U. Phys Dept.;Asano K.; /RLNR Tokyo;Axelsson M.; /Stockholm U. /Lund Observ. /Stockholm U. OKC;Baldini L.; /INFN Pisa;Ballet J.; /AIM Saclay;Barbiellini G.; /INFN Trieste /Trieste U.;Baring Ackermann ORCID, R. D. Blandford, Bhat Pn, Marco Ajello ORCID, Blandford Rd, K. Asano, A. W. Borgland, M. S. Briggs, Magnus Axelsson, L. Baldini ORCID, J. M. Casandjian, Caliandro Ga and other authors.
This paper is made freely available by the publisher.
This paper is made freely available by the publisher.

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Data provided by SHERPA/RoMEO

Abstract

31 pages, 6 figures, accepted by ApJ for publication Contact Authors: Johan Bregeon (johan.bregeon@pi.infn.it), Adam Goldstein (adam.m.goldstein@nasa.gov), Rob Preece (Rob.Preece@nasa.gov), Hiromitsu Takahashi (hirotaka@hep01.hepl.hiroshima-u.ac.jp), Kenji Toma (toma@astro.psu.edu), Takeshi Uehara (uehara@hep01.hepl.hiroshima-u.ac.jp) ; We report on the observation of the bright, long gamma-ray burst, GRB 090926A, by the Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) instruments on board the \Fermi\ Gamma-ray Space Telescope. GRB 090926A shares several features with other bright LAT bursts. In particular, it clearly shows a short spike in the light curve that is present in all detectors that see the burst, and this in turn suggests that there is a common region of emission across the entire \Fermi\ energy range. In addition, while a separate high-energy power-law component has already been observed in other GRBs, here we report for the first time the detection with good significance of a high-energy spectral break (or cutoff) in this power-law component around 1.4 GeV in the time-integrated spectrum. If the spectral break is caused by opacity to electron-positron pair production within the source, then this observation allows us to compute the bulk Lorentz factor for the outflow, rather than a lower limit.