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1. Observation of inverse Compton emission from a long γ-ray burst

Author

P. Veres, P. N. Bhat, M. S. Briggs, W. H. Cleveland, R. Hamburg, C. M. Hui, B. Mailyan, R. D. Preece, O. J. Roberts, A. von Kienlin, C. A. 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, J. L. Racusin, D. J. Thompson, S. Campana, M. G. Bernardini, N. P. M. Kuin, M. H. Siegel, S. B. Cenko, P. O’Brien, M. Capalbi, A. Daì, M. De Pasquale, J. Gropp, N. Klingler, J. P. Osborne, M. Perri, R. L. C. 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, G. E. Anderson, J. P. Anderson, G. Bernardi, J. Bolmer, M. D. Caballero-García, I. M. Carrasco, A. Castellón, N. Castro Segura, A. J. Castro-Tirado, S. V. Cherukuri, A. M. Cockeram, P. D’Avanzo, A. Di Dato, R. Diretse, R. P. Fender, E. Fernández-García, J. P. U. Fynbo, A. S.Fruchter, J. Greiner, M. Gromadzki, K. E. Heintz, I. Heywood, A. J. van der Horst, Y.-D. Hu, C. Inserra, L. Izzo, V. Jaiswal, P. Jakobsson, J. Japelj, E. Kankare, D. A.Kann, C. Kouveliotou, S. Klose, A. J. Levan, X. Y. Li, S. Lotti, K. Maguire, D. B. Malesani, I. Manulis, M. Marongiu, S. Martin, A. Melandri, M. J.Michałowski, J. C. A. Miller-Jones, K. Misra, A. Moin, K. P. Mooley, S. Nasri, M. Nicholl, A. Noschese, G. Novara, S. B. Pandey, E. Peretti, C. J. Pérez del Pulgar, M. A. Pérez-Torres, D. A. Perley, L. Piro, F. Ragosta, L. Resmi, R. Ricci, A. Rossi, R. Sánchez-Ramírez, J. Selsing, S. Schulze, S. J. Smartt, I. A. Smith, V. V. Sokolov, J. Stevens, N. R. Tanvir, C. C. Thöne, A. Tiengo, E. Tremou, E. Troja, A. de Ugarte Postigo, A. F. Valeev, S. D. Vergani, M. Wieringa, P. A. Woudt, D. Xu, O. Yaron, D. R. Young, V. A. Acciari, S. Ansoldi, L. A. Antonelli, A. Arbet Engels, D. Baack, A. Babić, B. Banerjee, U. Barres de Almeida, J. A. Barrio, J. Becerra González, W. Bednarek, L. Bellizzi, E. Bernardini, A. Berti, J. Besenrieder, W. Bhattacharyya, C. Bigongiari, A. Biland, O. Blanch, G. Bonnoli, Ž. Bošnjak, G. Busetto, R. Carosi, G. Ceribella, Y. Chai, A. Chilingaryan, S. Cikota, S. M. Colak, U. Colin, E. Colombo, J. L. 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 Espiñeira, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, D. Elsaesser, V. Fallah Ramazani, A. Fattorini, G. Ferrara, D. Fidalgo, L. Foffano, M. V. Fonseca, L. Font, C. Fruck, S. Fukami, R. J. García López, M. Garczarczyk, S.Gasparyan, M. Gaug, N. Giglietto, F. Giordano, N. Godinović, D. Green, D. Guberman, D. Hadasch, A. Hahn, J. Herrera, J. Hoang, D. Hrupec, M. Hütten, 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. López, R. López-Coto, A. López-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. Martínez, D. Mazin, S. Mićanović, D. Miceli, M. Minev, J. M. 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. Nogués, S. Nozaki, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, P. Peñil, M. Peresano, M. Persic, P. G. Prada Moroni, E. Prandini, I. Puljak, W. Rhode, M. Ribó, J. Rico, C. Righi, A. Rugliancich, L. Saha, N. Sahakyan, T. Saito, S. Sakurai, K. Satalecka, K. Schmidt, T. Schweizer, J. Sitarek, I. Šnidarić, D. Sobczynska, A. Somero, A. Stamerra, D. Strom, M. Strzys, Y. Suda, T. Surić, M. Takahashi, F. Tavecchio, P. Temnikov, T. Terzić, M. Teshima, N. Torres-Albà, L. Tosti, V. Vagelli, J. van Scherpenberg, G. Vanzo, M. Vazquez Acosta, C. F. Vigorito, V. Vitale, I. Vovk, M. Will, D. Zarić, and L. Nava

Subjects
Space Sciences (General)
Abstract

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 emission. 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 bands. The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock. Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C. Here we report multifrequency 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 10^(12) 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.

Published
2019
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2. Observation of inverse Compton emission from a long γ-ray burst.

Author

Veres P, Bhat PN, Briggs MS, Cleveland WH, Hamburg R, Hui CM, Mailyan B, Preece RD, Roberts OJ, von Kienlin A, Wilson-Hodge CA, Kocevski D, Arimoto M, Tak D, Asano K, Axelsson M, Barbiellini G, Bissaldi E, Dirirsa FF, Gill R, Granot J, McEnery J, Omodei N, Razzaque S, Piron F, Racusin JL, Thompson DJ, Campana S, Bernardini MG, Kuin NPM, Siegel MH, Cenko SB, O'Brien P, Capalbi M, Daì A, De Pasquale M, Gropp J, Klingler N, Osborne JP, Perri M, Starling RLC, 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 GE, Anderson JP, Bernardi G, Bolmer J, Caballero-García MD, Carrasco IM, Castellón A, Segura NC, Castro-Tirado AJ, Cherukuri SV, Cockeram AM, D'Avanzo P, Di Dato A, Diretse R, Fender RP, Fernández-García E, Fynbo JPU, Fruchter AS, Greiner J, Gromadzki M, Heintz KE, Heywood I, van der Horst AJ, Hu YD, Inserra C, Izzo L, Jaiswal V, Jakobsson P, Japelj J, Kankare E, Kann DA, Kouveliotou C, Klose S, Levan AJ, Li XY, Lotti S, Maguire K, Malesani DB, Manulis I, Marongiu M, Martin S, Melandri A, Michałowski MJ, Miller-Jones JCA, Misra K, Moin A, Mooley KP, Nasri S, Nicholl M, Noschese A, Novara G, Pandey SB, Peretti E, Del Pulgar CJP, Pérez-Torres MA, Perley DA, Piro L, Ragosta F, Resmi L, Ricci R, Rossi A, Sánchez-Ramírez R, Selsing J, Schulze S, Smartt SJ, Smith IA, Sokolov VV, Stevens J, Tanvir NR, Thöne CC, Tiengo A, Tremou E, Troja E, de Ugarte Postigo A, Valeev AF, Vergani SD, Wieringa M, Woudt PA, Xu D, Yaron O, and Young DR

Abstract

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 emission 1,2 . 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 bands 1-6 . The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock 7-9 . Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C 10,11 . 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 10 12 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.

Published
2019
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3. A kilonova as the electromagnetic counterpart to a gravitational-wave source.

Author

Smartt SJ, Chen TW, Jerkstrand A, Coughlin M, Kankare E, Sim SA, Fraser M, Inserra C, Maguire K, Chambers KC, Huber ME, Krühler T, Leloudas G, Magee M, Shingles LJ, Smith KW, Young DR, Tonry J, Kotak R, Gal-Yam A, Lyman JD, Homan DS, Agliozzo C, Anderson JP, Angus CR, Ashall C, Barbarino C, Bauer FE, Berton M, Botticella MT, Bulla M, Bulger J, Cannizzaro G, Cano Z, Cartier R, Cikota A, Clark P, De Cia A, Della Valle M, Denneau L, Dennefeld M, Dessart L, Dimitriadis G, Elias-Rosa N, Firth RE, Flewelling H, Flörs A, Franckowiak A, Frohmaier C, Galbany L, González-Gaitán S, Greiner J, Gromadzki M, Guelbenzu AN, Gutiérrez CP, Hamanowicz A, Hanlon L, Harmanen J, Heintz KE, Heinze A, Hernandez MS, Hodgkin ST, Hook IM, Izzo L, James PA, Jonker PG, Kerzendorf WE, Klose S, Kostrzewa-Rutkowska Z, Kowalski M, Kromer M, Kuncarayakti H, Lawrence A, Lowe TB, Magnier EA, Manulis I, Martin-Carrillo A, Mattila S, McBrien O, Müller A, Nordin J, O'Neill D, Onori F, Palmerio JT, Pastorello A, Patat F, Pignata G, Podsiadlowski P, Pumo ML, Prentice SJ, Rau A, Razza A, Rest A, Reynolds T, Roy R, Ruiter AJ, Rybicki KA, Salmon L, Schady P, Schultz ASB, Schweyer T, Seitenzahl IR, Smith M, Sollerman J, Stalder B, Stubbs CW, Sullivan M, Szegedi H, Taddia F, Taubenberger S, Terreran G, van Soelen B, Vos J, Wainscoat RJ, Walton NA, Waters C, Weiland H, Willman M, Wiseman P, Wright DE, Wyrzykowski Ł, and Yaron O

Abstract

Gravitational waves were discovered with the detection of binary black-hole mergers and they should also be detectable from lower-mass neutron-star mergers. These are predicted to eject material rich in heavy radioactive isotopes that can power an electromagnetic signal. This signal is luminous at optical and infrared wavelengths and is called a kilonova. The gravitational-wave source GW170817 arose from a binary neutron-star merger in the nearby Universe with a relatively well confined sky position and distance estimate. Here we report observations and physical modelling of a rapidly fading electromagnetic transient in the galaxy NGC 4993, which is spatially coincident with GW170817 and with a weak, short γ-ray burst. The transient has physical parameters that broadly match the theoretical predictions of blue kilonovae from neutron-star mergers. The emitted electromagnetic radiation can be explained with an ejected mass of 0.04 ± 0.01 solar masses, with an opacity of less than 0.5 square centimetres per gram, at a velocity of 0.2 ± 0.1 times light speed. The power source is constrained to have a power-law slope of -1.2 ± 0.3, consistent with radioactive powering from r-process nuclides. (The r-process is a series of neutron capture reactions that synthesise many of the elements heavier than iron.) We identify line features in the spectra that are consistent with light r-process elements (atomic masses of 90-140). As it fades, the transient rapidly becomes red, and a higher-opacity, lanthanide-rich ejecta component may contribute to the emission. This indicates that neutron-star mergers produce gravitational waves and radioactively powered kilonovae, and are a nucleosynthetic source of the r-process elements.

Published
2017
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