A1 Refereed original research article in a scientific journal

MAGIC detection of GRB 201216C at z = 1.1




AuthorsAbe 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

PublisherOxford University Press

Publication year2024

JournalMonthly Notices of the Royal Astronomical Society

Journal name in sourceMonthly Notices of the Royal Astronomical Society

Volume527

Issue3

First page 5856

Last page5867

eISSN1365-2966

DOIhttps://doi.org/10.1093/mnras/stad2958

Web address https://academic.oup.com/mnras/article/527/3/5856/7326795

Self-archived copy’s web addresshttps://research.utu.fi/converis/portal/detail/Publication/386835415

Preprint addresshttps://arxiv.org/abs/2310.06473


Abstract

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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Last updated on 2024-26-11 at 16:45