A1 Refereed original research article in a scientific journal
MAGIC detection of GRB 201216C at z = 1.1
Authors: Abe H, Abe S, Acciari V, Agudo I, Aniello T, Ansoldi S, Antonelli L, Arbet Engels A, Arcaro C, Artero M, Asano K, Baack D, Babić A, Baquero A, Almeida U, Barrio J, Batković I, Baxter J, Becerra González J, Bednarek W, Bernardini E, Bernete J, Berti A, Besenrieder J, Bigongiari C, Biland A, Blanch O, Bonnoli G, Bošnjak Ž, Burelli I, Busetto G, Campoy-Ordaz A, Carosi A, Carosi R, Carretero-Castrillo M, Castro-Tirado A, Ceribella G, Chai Y, Cifuentes A, Cikota S, Colombo E, Contreras J, Cortina J, Covino S, D’Amico G, D’Elia V, Da Vela P, Dazzi F, De Angelis A, De Lotto B, Del Popolo A, Delfino M, Delgado J, Delgado Mendez C, Depaoli D, Di Pierro F, Di Venere L, Dominis Prester D, Donini A, Dorner D, Doro M, Elsaesser D, Emery G, Escudero J, Fariña L, Fattorini A, Foffano L, Font L, Fukami S, Fukazawa Y, García López R, Garczarczyk M, Gasparyan S, Gaug M, Giesbrecht Paiva J, Giglietto N, Giordano F, Gliwny P, Godinović N, Grau R, Green D, Green J, Hadasch D, Hahn A, Hassan T, Heckmann L, Herrera J, Hrupec D, Hütten M, Imazawa R, Inada T, Iotov R, Ishio K, Jiménez Martínez I, Jormanainen J, Kerszberg D, Kluge G, Kobayashi Y, Kouch P, Kubo H, Kushida J, Láinez Lezáun M, Lamastra A, Leone F, Lindfors E, Linhoff L, Lombardi S, Longo F, López-Coto R, López-Moya M, López-Oramas A, Loporchio S, Lorini A, Lyard E, Oliveira Fraga B, Majumdar P, Makariev M, Maneva G, Mang N, Manganaro M, Mangano S, Mannheim K, Mariotti M, Martínez M, Mas-Aguilar A, Mazin D, Menchiari S, Mender S, Mićanović S, Miceli D, Miener T, Miranda J, Mirzoyan R, Molero González M, Molina E, Mondal H, Moralejo A, Morcuende D, Nanci C, Nava L, Neustroev V, Nievas Rosillo M, Nigro C, Nikolić L, Nilsson K, Nishijima K, Njoh Ekoume T, Noda K, Nozaki S, Ohtani Y, Okumura A, Otero-Santos J, Paiano S, Palatiello M, Paneque D, Paoletti R, Paredes J, Pavletić L, Pavlović D, Persic M, Pihet M, Pirola G, Podobnik F, Prada Moroni P, Prandini E, Principe G, Priyadarshi C, Rhode W, Ribó M, Rico J, Righi C, Sahakyan N, Saito T, Satalecka K, Saturni F, Schleicher B, Schmidt K, Schmuckermaier F, Schubert J, Schweizer T, Sciaccaluga A, Sitarek J, Sliusar V, Sobczynska D, Spolon A, Stamerra A, Strišković J, Strom D, Strzys M, Suda Y, Suutarinen S, Tajima H, Takahashi M, Takeishi R, Tavecchio F, Temnikov P, Terauchi K, Terzić T, Teshima M, Tosti L, Truzzi S, Tutone A, Ubach S, Scherpenberg J, Vazquez Acosta M, Ventura S, Verguilov V, Viale I, Vigorito C, Vitale V, Vovk I, Walter R, Will M, Yamamoto T, Gomboc A, Jordana-Mitjans N, Melandri A, Mundell C, Shrestha M, Steele I
Publisher: Oxford University Press
Publication year: 2024
Journal: Monthly Notices of the Royal Astronomical Society
Journal name in source: Monthly Notices of the Royal Astronomical Society
Volume: 527
Issue: 3
First page : 5856
Last page: 5867
eISSN: 1365-2966
DOI: https://doi.org/10.1093/mnras/stad2958
Web address : https://academic.oup.com/mnras/article/527/3/5856/7326795
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/386835415
Preprint address: https://arxiv.org/abs/2310.06473
Gamma-ray bursts (GRBs) are explosive transient events occurring at cosmological distances, releasing a large amount of energy as electromagnetic radiation over several energy bands. We report the detection of the long GRB 201216C by the MAGIC telescopes. The source is located at z = 1.1 and thus it is the farthest one detected at very high energies. The emission above 70 GeV of GRB 201216C is modelled together with multiwavelength data within a synchrotron and synchrotron self-Compton (SSC) scenario. We find that SSC can explain the broad-band data well from the optical to the very-high-energy band. For the late-time radio data, a different component is needed to account for the observed emission. Differently from previous GRBs detected in the very-high-energy range, the model for GRB 201216C strongly favours a wind-like medium. The model parameters have values similar to those found in past studies of the afterglows of GRBs detected up to GeV energies. © 2023 The Author(s).
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