A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
MAGIC detection of GRB 201216C at z = 1.1
Tekijät: 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
Kustantaja: Oxford University Press
Julkaisuvuosi: 2024
Journal: Monthly Notices of the Royal Astronomical Society
Tietokannassa oleva lehden nimi: Monthly Notices of the Royal Astronomical Society
Vuosikerta: 527
Numero: 3
Aloitussivu: 5856
Lopetussivu: 5867
eISSN: 1365-2966
DOI: https://doi.org/10.1093/mnras/stad2958
Verkko-osoite: https://academic.oup.com/mnras/article/527/3/5856/7326795
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/386835415
Preprintin osoite: 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).
Ladattava julkaisu This is an electronic reprint of the original article. |