Observation of inverse Compton emission from a long γ-ray burst
- Veres, P.
- Bhat, P. N.
- Briggs, M. S.
- Cleveland, W. H.
- Hamburg, R.
- Hui, C. M.
- Mailyan, B.
- Preece, R. D.
- Roberts, O. J.
- von Kienlin, A.
- Wilson-Hodge, C. A.
- Kocevski, D.
- Arimoto, M.
- Tak, D.
- Asano, K.
- Axelsson, M.
- Barbiellini, G.
- Bissaldi, E.
- Dirirsa, F. Fana
- Gill, R.
- Granot, J.
- McEnery, J.
- Omodei, N.
- Razzaque, S.
- Piron, F.
- Racusin, J. L.
- Thompson, D. J.
- Campana, S.
- Bernardini, M. G.
- Kuin, N. P. M.
- Siegel, M. H.
- Cenko, S. B.
- O'Brien, P.
- Capalbi, M.
- Daì, A.
- De Pasquale, M.
- Gropp, J.
- Klingler, N.
- Osborne, J. P.
- Perri, M.
- Starling, R. L. C.
- Tagliaferri, G.
- Tohuvavohu, A.
- Ursi, A.
- Tavani, M.
- Cardillo, M.
- Casentini, C.
- Piano, G.
- Evangelista, Y.
- Verrecchia, F.
- Pittori, C.
- Lucarelli, F.
- Bulgarelli, A.
- Parmiggiani, N.
- Anderson, G. E.
- Anderson, J. P.
- Bernardi, G.
- Bolmer, J.
- Caballero-García, M. D.
- Carrasco, I. M.
- Castellón, A.
- Segura, N. Castro
- Castro-Tirado, A. J.
- Cherukuri, S. V.
- Cockeram, A. M.
- D'Avanzo, P.
- Di Dato, A.
- Diretse, R.
- Fender, R. P.
- Fernández-García, E.
- Fynbo, J. P. U.
- Fruchter, A. S.
- Greiner, J.
- Gromadzki, M.
- Heintz, K. E.
- Heywood, I.
- van der Horst, A. J.
- Hu, Y.-D.
- Inserra, C.
- Izzo, L.
- Jaiswal, V.
- Jakobsson, P.
- Japelj, J.
- Kankare, E.
- Kann, D. A.
- Kouveliotou, C.
- Klose, S.
- Levan, A. J.
- Li, X. Y.
- Lotti, S.
- Maguire, K.
- Malesani, D. B.
- Manulis, I.
- Marongiu, M.
- Martin, S.
- Melandri, A.
- Michalowski, M. J.
- Miller-Jones, J. C. A.
- Misra, K.
- Moin, A.
- Mooley, K. P.
- Nasri, S.
- Nicholl, M.
- Noschese, A.
- Novara, G.
- Pandey, S. B.
- Peretti, E.
- del Pulgar, C. J. Pérez
- Pérez-Torres, M. A.
- Perley, D. A.
- Piro, L.
- Ragosta, F.
- Resmi, L.
- Ricci, R.
- Rossi, A.
- Sánchez-Ramírez, R.
- Selsing, J.
- Schulze, S.
- Smartt, S. J.
- Smith, I. A.
- Sokolov, V. V.
- Stevens, J.
- Tanvir, N. R.
- Thöne, C. C.
- Tiengo, A.
- Tremou, E.
- Troja, E.
- de Ugarte Postigo, A.
- Valeev, A. F.
- Vergani, S. D.
- Wieringa, M.
- Woudt, P. A.
- Xu, D.
- Yaron, O.
- Young, D. R.
- Magic Collaboration
DOIAbstract
Long-duration γ-ray bursts (GRBs) originate from ultra-relativistic jets launched from the collapsing cores of dying massive stars. They are characterized by an initial phase of bright and highly variable radiation in the kiloelectronvolt-to-megaelectronvolt band, which is probably produced within the jet and lasts from milliseconds to minutes, known as the prompt emission1,2. Subsequently, the interaction of the jet with the surrounding medium generates shock waves that are responsible for the afterglow emission, which lasts from days to months and occurs over a broad energy range from the radio to the gigaelectronvolt bands1,2,3,4,5,6. The afterglow emission is generally well explained as synchrotron radiation emitted by electrons acceler...
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