A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä

MAGIC detection of GRB 201216C at z = 1.1




TekijätAbe 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

KustantajaOxford University Press

Julkaisuvuosi2024

JournalMonthly Notices of the Royal Astronomical Society

Tietokannassa oleva lehden nimiMonthly Notices of the Royal Astronomical Society

Vuosikerta527

Numero3

Aloitussivu5856

Lopetussivu5867

eISSN1365-2966

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

Verkko-osoitehttps://academic.oup.com/mnras/article/527/3/5856/7326795

Rinnakkaistallenteen osoitehttps://research.utu.fi/converis/portal/detail/Publication/386835415

Preprintin osoitehttps://arxiv.org/abs/2310.06473


Tiivistelmä

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