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Observation of inverse Compton emission from a long gamma-ray burst

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posted on 19.03.2020, 14:44 by P Veres, VA Acciari, S Ansoldi, LA Antonelli, A Arbet Engels, D Baack, A Babic, B Banerjee, U Barres de Almeida, JA Barrio, J Becerra Gonzalez, W Bednarek, L Bellizzi, E Bernardini, A Berti, J Besenrieder, W Bhattacharyya, C Bigongiari, A Biland, O Blanch, G Bonnoli, Z Bosnjak, G Busetto, R Carosi, G Ceribella, Y Chai, A Chilingaryan, S Cikota, SM Colak, U Colin, E Colombo, JL Contreras, J Cortina, S Covino, V D'Elia, P Da Vela, F Dazzi, A De Angelis, B De Lotto, M Delfino, J Delgado, D Depaoli, F Di Pierro, L Di Venere, E Do Souto Espineira, D Dominis Prester, A Donini, D Dorner, M Doro, D Elsaesser, V Fallah Ramazani, A Fattorini, G Ferrara, D Fidalgo, L Foffano, MV Fonseca, L Font, C Fruck, S Fukami, RJ Garcia Lopez, M Garczarczyk, S Gasparyan, M Gaug, N Giglietto, F Giordano, N Godinovic, D Green, D Guberman, D Hadasch, A Hahn, J Herrera, J Hoang, D Hrupec, M Hutten, T Inada, S Inoue, K Ishio, Y Iwamura, L Jouvin, D Kerszberg, H Kubo, J Kushida, A Lamastra, D Lelas, F Leone, E Lindfors, S Lombardi, F Longo, M Lopez, R Lopez-Coto, A Lopez-Oramas, S Loporchio, B Machado de Oliveira Fraga, C Maggio, P Majumdar, M Makariev, M Mallamaci, G Maneva, M Manganaro, K Mannheim, L Maraschi, M Mariotti, M Martinez, D Mazin, S Micanovic, D Miceli, M Minev, JM Miranda, R Mirzoyan, E Molina, A Moralejo, D Morcuende, V Moreno, E Moretti, P Munar-Adrover, V Neustroev, C Nigro, K Nilsson, D Ninci, K Nishijima, K Noda, L Nogues, S Nozaki, S Paiano, M Palatiello, D Paneque, R Paoletti, JM Paredes, P Penil, M Peresano, M Persic, PG Prada Moroni, E Prandini, I Puljak, W Rhode, M Ribo, J Rico, C Righi, A Rugliancich, L Saha, N Sahakyan, T Saito, S Sakurai, K Satalecka, K Schmidt, T Schweizer, J Sitarek, I Snidaric, D Sobczynska, A Somero, A Stamerra, D Strom, M Strzys, Y Suda, T Suric, M Takahashi, F Tavecchio, P Temnikov, T Terzic, M Teshima, N Torres-Alba, L Tosti, V Vagelli, J van Scherpenberg, G Vanzo, M Vazquez Acosta, CF Vigorito, V Vitale, I Vovk, M Will, D Zaric, L Nava, PN Bhat, MS Briggs, WH Cleveland, R Hamburg, CM Hui, B Mailyan, RD Preece, OJ Roberts, A von Kienlin, CA Wilson-Hodge, D Kocevski, M Arimoto, D Tak, K Asano, M Axelsson, G Barbiellini, E Bissaldi, F Fana Dirirsa, R Gill, J Granot, J McEnery, N Omodei, S Razzaque, F Piron, JL Racusin, DJ Thompson, S Campana, MG Bernardini, NPM Kuin, MH Siegel, B Cenko, P O'Brien, M Capalbi, A Dai, M De Pasquale, J Gropp, N Klingler, P Osborne, M Perri, RLC Starling, G Tagliaferri, A Tohuvavohu, A Ursi, M Tavani, M Cardillo, C Casentini, G Piano, Y Evangelista, F Verrecchia, C Pittori, F Lucarelli, A Bulgarelli, N Parmiggiani, GE Anderson, JP Anderson, G Bernardi, J Bolmer, MD Caballero-Garcia, IM Carrasco, A Castellon, N Castro Segura, AJ Castro-Tirado, SV Cherukuri, AM Cockeram, P D'Avanzo, A Di Dato, R Diretse, RP Fender, E Fernandez-Garcia, JPU Fynbo, AS Fruchter, J Greiner, M Gromadzki, KE Heintz, I Heywood, AJ van der Horst, Y-D Hu, C Inserra, L Izzo, V Jaiswal, P Jakobsson, J Japelj, E Kankare, DA Kann, C Kouveliotou, S Klose, AJ Levan, XY Li, S Lotti, K Maguire, DB Malesani, I Manulis, M Marongiu, S Martin, A Melandri, MJ Michalowski, JCA Miller-Jones, K Misra, A Moin, KP Mooley, S Nasri, M Nicholl, A Noschese, G Novara, SB Pandey, E Peretti, CJ Perez del Pulgar, MA Perez-Torres, DA Perley, L Piro, F Ragosta, L Resmi, R Ricci, A Rossi, R Sanchez-Ramirez, J Selsing, S Schulze, SJ Smartt, IA Smith, VV Sokolov, J Stevens, NR Tanvir, CC Thone, A Tiengo, E Tremou, E Troja, A de Ugarte Postigo, AF Valeev, SD Vergani, M Wieringa, PA Woudt, D Xu, O Yaron, DR Young
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 bands1–6. The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock7–9. Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C10,11. Here we report multi-frequency observations of GRB 190114C, and study the evolution in time of the GRB emission across 17 orders of magnitude in energy, from 5 × 10−6 to 1012 electronvolts. We find that the broadband spectral energy distribution is double-peaked, with the teraelectronvolt emission constituting a distinct spectral component with power comparable to the synchrotron component. This component is associated with the afterglow and is satisfactorily explained by inverse Compton up-scattering of synchrotron photons by high-energy electrons. We find that the conditions required to account for the observed teraelectronvolt component are typical for GRBs, supporting the possibility that inverse Compton emission is commonly produced in GRBs.

History

Citation

Nature 575, 459–463 (2019).

Published in

NATURE

Volume

575

Issue

7783

Pagination

459 - + (23)

Publisher

NATURE PUBLISHING GROUP

issn

0028-0836

eissn

1476-4687

Acceptance date

18/10/2019

Copyright date

2019

Available date

20/11/2019

Publisher version

https://www.nature.com/articles/s41586-019-1754-6

Spatial coverage

England

Language

English