AXELSSON, Magnus; BALDINI, Luca; BARBIELLINI, Guido; G. BARING, M.; BELLAZZINI, R.; BREGEON, J.; BRIGIDA, M.; BRUEL, Pascal; BUEHLER, R.; A. CALIANDRO, G.; A. CAMERON, R.; CARAVEO, P. A.; CECCHI, C.; CHAVES, R.C.G.; CHEKHTMAN, A.; CHIANG, J.; CLAUS, R.; CONRAD, J.; CUTINI, S.; D'AMMANDO, F.; DE PALMA, F.; D. DERMER, C.; DO COUTO E SILVA, E.; S. DRELL, P.; FAVUZZI, C.; J. FEGAN, S.; C. FERRARA, E.; B. FOCKE, W.; FUKAZAWA, Y.; FUSCO, P.; GARGANO, F.; GASPARRINI, D.; GEHRELS, N.; GERMANI, S.; GIGLIETTO, N.; GIROLETTI, M.; GODFREY, G.; GUIRIEC, S.; HADASCH, D.; HANABATA, Y.; HAYASHIDA, M.; HOU, X.; IYYANI, S.; S. JACKSON, M.; KOCEVSKI, D.; KUSS, M.; LARSSON, J.; LARSSON, S.; LONGO, F.; LOPARCO, F.; LUNDMAN, C.; N. MAZZIOTTA, M.; E. MCENERY, J.; MIZUNO, T.; E. MONZANI, M.; MORETTI, E.; MORSELLI, A.; MURGIA, S.; NUSS, E.; NYMARK, T.; OHNO, M.; OMODEI, N.; PESCE-ROLLINS, M.; PIRON, F.; PIVATO, G.; L. RACUSIN, J.; RAIN'O, S.; RAZZANO, M.; RAZZAQUE, S.; REIMER, A.; ROTH, M.; RYDE, F.; SANCHEZ, D.A.; SGR'O, C.; J. SISKIND, E.; SPANDRE, G.; SPINELLI, P.; STAMATIKOS, M.; TIBALDO, L.; TINIVELLA, M.; L. USHER, T.; VANDENBROUCKE, J.; VASILEIOU, V.; VIANELLO, G.; VITALE, V.; P. WAITE, A.; L. WINER, B.; S. WOOD, K.; M. BURGESS, J.; N. BHAT, P.; BISSALDI, E.; S. BRIGGS, M.; CONNAUGHTON, V.; FISHMAN, G.; FITZPATRICK, G.; FOLEY, S.; GRUBER, D.; M. KIPPEN, R.; KOUVELIOTOU, C.; JENKE, P.; MCBREEN, S.; MCGLYNN, S.; MEEGAN, C.; S. PACISAS, W.; PELASSA, V.; PREECE, R.; TIERNEY, D.; VON KIENLIN, A.; WILSON-HODGE, C.; XIONG, S.; PE'ER, A.

doi:10.1088/2041-8205/757/2/L31

Metadatos

Mostrar el registro completo del ítem

Licencia de uso del documento

Idioma

Article de revue

Este ítem está publicado en

The Astrophysical journal letters. 2012, vol. 757, p. L31

Bristol : IOP Publishing

Resumen en inglés

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 seconds (in the GBM) and had a peak flux of 5.7\pm0.2 x 10^{-5} erg/s/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\pm2 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\pm0.10. The temperature of the blackbody component also decreased, starting from ~80 keV, and the decay showed a significant break after ~2 seconds. The spectrum provides strong constraints on the standard synchrotron model, indicating that alternative mechanisms may give rise to the emission at these energies.< Leer menos

Metadatos

Licencia de uso del documento

GRB110721A: An extreme peak energy and signatures of the photosphere

Idioma

Este ítem está publicado en

Resumen en inglés

DOI

Orígen

Centros de investigación