GRB110721A: An Extreme Peak Energy and Signatures of the Photosphere
dc.citation.firstpage | L31 | en_US |
dc.citation.journalTitle | The Astrophysical Journal Letters | en_US |
dc.citation.volumeNumber | 757 | en_US |
dc.contributor.author | Baring, M.G. | en_US |
dc.contributor.author | Axelsson, M. | en_US |
dc.contributor.author | Baldini, L. | en_US |
dc.contributor.author | Barbiellini, G. | en_US |
dc.contributor.author | Bellazzini, R. | en_US |
dc.contributor.author | Bregeon, J. | en_US |
dc.contributor.author | Brigida, M. | en_US |
dc.contributor.author | Bruel, P. | en_US |
dc.contributor.author | Buehler, R. | en_US |
dc.contributor.author | Caliandro, G.A. | en_US |
dc.contributor.author | Cameron, R.A. | en_US |
dc.contributor.author | Caraveo, P.A. | en_US |
dc.contributor.author | Cecchi, C. | en_US |
dc.contributor.author | Chaves, R.C.G. | en_US |
dc.contributor.author | Chekhtman, A. | en_US |
dc.contributor.author | Chiang, J. | en_US |
dc.contributor.author | Claus, R. | en_US |
dc.contributor.author | Conrad, J. | en_US |
dc.contributor.author | Cutini, S. | en_US |
dc.contributor.author | D'Ammando, F. | en_US |
dc.contributor.author | de Palma, F. | en_US |
dc.contributor.author | Dermer, C.D. | en_US |
dc.contributor.author | do Couto e Silva, E. | en_US |
dc.contributor.author | Drell, P.S. | en_US |
dc.contributor.author | Favuzzi, C. | en_US |
dc.contributor.author | Fegan, S.J. | en_US |
dc.contributor.author | Ferrara, E.C. | en_US |
dc.contributor.author | Focke, W.B. | en_US |
dc.contributor.author | Fukazawa, Y. | en_US |
dc.contributor.author | Fusco, P. | en_US |
dc.contributor.author | Gargano, F. | en_US |
dc.contributor.author | Gasparrini, D. | en_US |
dc.contributor.author | Gehrels, N. | en_US |
dc.contributor.author | Germani, S. | en_US |
dc.contributor.author | Giglietto, N. | en_US |
dc.contributor.author | Giroletti, M. | en_US |
dc.contributor.author | Godfrey, G. | en_US |
dc.contributor.author | Guiriec, S. | en_US |
dc.contributor.author | Hadasch, D. | en_US |
dc.contributor.author | Hanabata, Y. | en_US |
dc.contributor.author | Hayashida, M. | en_US |
dc.contributor.author | Hou, X. | en_US |
dc.contributor.author | Iyyani, S. | en_US |
dc.contributor.author | Jackson, M.S. | en_US |
dc.contributor.author | Kocevski, D. | en_US |
dc.contributor.author | Kuss, M. | en_US |
dc.contributor.author | Larsson, J. | en_US |
dc.contributor.author | Longo, F. | en_US |
dc.contributor.author | Loparco, F. | en_US |
dc.contributor.author | Lundman, C. | en_US |
dc.contributor.author | Mazziotta, M.N. | en_US |
dc.contributor.author | McEnery, J.E. | en_US |
dc.contributor.author | Mizuno, T. | en_US |
dc.contributor.author | Monzani, M.E. | en_US |
dc.contributor.author | Moretti, E. | en_US |
dc.contributor.author | Morselli, A. | en_US |
dc.contributor.author | Murgia, S. | en_US |
dc.contributor.author | Nuss, E. | en_US |
dc.contributor.author | Nymark, T. | en_US |
dc.contributor.author | Ohno, M. | en_US |
dc.contributor.author | Omodei, N. | en_US |
dc.contributor.author | Pesce-Rollins, M. | en_US |
dc.contributor.author | Piron, F. | en_US |
dc.contributor.author | Pivato, G. | en_US |
dc.contributor.author | Racusin, J.L. | en_US |
dc.contributor.author | Rainò, S. | en_US |
dc.contributor.author | Razzano, M. | en_US |
dc.contributor.author | Razzaque, S. | en_US |
dc.contributor.author | Reimer, A. | en_US |
dc.contributor.author | Roth, M. | en_US |
dc.contributor.author | Ryde, F. | en_US |
dc.contributor.author | Sanchez, D.A. | en_US |
dc.contributor.author | Sgrò, C. | en_US |
dc.contributor.author | Siskind, E.J. | en_US |
dc.contributor.author | Spandre, G. | en_US |
dc.contributor.author | Spinelli, P. | en_US |
dc.contributor.author | Stamatikos, M. | en_US |
dc.contributor.author | Tibaldo, L. | en_US |
dc.contributor.author | Tinivella, M. | en_US |
dc.contributor.author | Usher, T.L. | en_US |
dc.contributor.author | Vandenbroucke, J. | en_US |
dc.contributor.author | Vasileiou, V. | en_US |
dc.contributor.author | Vianello, G. | en_US |
dc.contributor.author | Vitale, V. | en_US |
dc.contributor.author | Waite, A.P. | en_US |
dc.contributor.author | Winer, B.L. | en_US |
dc.contributor.author | Wood, K.S. | en_US |
dc.contributor.author | Burgess, J.M. | en_US |
dc.contributor.author | Bhat, P.N. | en_US |
dc.contributor.author | Bissaldi, E. | en_US |
dc.contributor.author | Briggs, M.S. | en_US |
dc.contributor.author | Connaughton, V. | en_US |
dc.contributor.author | Fishman, G. | en_US |
dc.contributor.author | Fitzpatrick, G. | en_US |
dc.contributor.author | Foley, S. | en_US |
dc.contributor.author | Gruber, D. | en_US |
dc.contributor.author | Kippen, R.M. | en_US |
dc.contributor.author | Kouveliotou, C. | en_US |
dc.contributor.author | Jenke, P. | en_US |
dc.contributor.author | McBreen, S. | en_US |
dc.contributor.author | McGlynn, S. | en_US |
dc.contributor.author | Meegan, C. | en_US |
dc.contributor.author | Paciesas, W.S. | en_US |
dc.contributor.author | Pelassa, V. | en_US |
dc.contributor.author | Preece, R. | en_US |
dc.contributor.author | Tierney, D. | en_US |
dc.contributor.author | von Kienlin, A. | en_US |
dc.contributor.author | Wilson-Hodge, C. | en_US |
dc.contributor.author | Xiong, S. | en_US |
dc.contributor.author | Pe'er, A. | en_US |
dc.contributor.author | Pe'er, A. | en_US |
dc.date.accessioned | 2013-03-14T14:45:23Z | en_US |
dc.date.available | 2014-03-19T05:10:03Z | en_US |
dc.date.issued | 2012 | en_US |
dc.description.abstract | GRB110721A was observed by the Fermi Gamma-ray Space Telescope using its two instruments, the Large Area Telescope (LAT) and the Gamma-ray Burst Monitor (GBM). The burst consisted of one major emission episode which lasted for ~24.5 s (in the GBM) and had a peak flux of (5.7 ± 0.2) × 10–5 erg s–1 cm–2. The time-resolved emission spectrum is best modeled with a combination of a Band function and a blackbody spectrum. The peak energy of the Band component was initially 15 ± 2 MeV, which is the highest value ever detected in a GRB. This measurement was made possible by combining GBM/BGO data with LAT Low Energy events to achieve continuous 10-100 MeV coverage. The peak energy later decreased as a power law in time with an index of –1.89 ± 0.10. The temperature of the blackbody component also decreased, starting from ~80 keV, and the decay showed a significant break after ~2 s. The spectrum provides strong constraints on the standard synchrotron model, indicating that alternative mechanisms may give rise to the emission at these energies. | en_US |
dc.embargo.terms | 1 year | en_US |
dc.identifier.citation | Baring, M.G., Axelsson, M., Baldini, L., et al.. "GRB110721A: An Extreme Peak Energy and Signatures of the Photosphere." <i>The Astrophysical Journal Letters,</i> 757, (2012) The American Astronomical Society: L31. http://dx.doi.org/10.1088/2041-8205/757/2/L31. | en_US |
dc.identifier.doi | http://dx.doi.org/10.1088/2041-8205/757/2/L31 | en_US |
dc.identifier.uri | https://hdl.handle.net/1911/70582 | en_US |
dc.language.iso | eng | en_US |
dc.publisher | The American Astronomical Society | en_US |
dc.rights | Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. | en_US |
dc.subject.keyword | gamma-ray burst: general | en_US |
dc.subject.keyword | gamma-ray burst: individual (GRB110721A) | en_US |
dc.subject.keyword | radiation mechanisms: thermal | en_US |
dc.title | GRB110721A: An Extreme Peak Energy and Signatures of the Photosphere | en_US |
dc.type | Journal article | en_US |
dc.type.dcmi | Text | en_US |
dc.type.publication | publisher version | en_US |