Gamma-ray observations of MAXI J1820+070 during the 2018 outburst
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dc.contributor.author | Abe, S. | |
dc.contributor.author | Acciari, V.A. | |
dc.contributor.author | Aniello, T. | |
dc.contributor.author | Ansoldi, S. | |
dc.contributor.author | Antonelli, L.A. | |
dc.contributor.author | Arbet Engels, Engels | |
dc.contributor.author | Arcaro, C. | |
dc.contributor.author | Artero, M. | |
dc.contributor.author | Asano, K. | |
dc.contributor.author | Baack, D. | |
dc.contributor.author | Babić, A. | |
dc.contributor.author | Baquero, A. | |
dc.contributor.author | De Almeida, U. Barres | |
dc.contributor.author | Barrio, J.A. | |
dc.contributor.author | Batković, I. | |
dc.contributor.author | Baxter, J. | |
dc.contributor.author | Becerra González, Gonzalez | |
dc.contributor.author | Bednarek, W. | |
dc.contributor.author | Bernardini, E. | |
dc.contributor.author | Bernardos, M. | |
dc.contributor.author | Berti, A. | |
dc.contributor.author | Besenrieder, J. | |
dc.contributor.author | Bhattacharyya, W. | |
dc.contributor.author | Bigongiari, C. | |
dc.contributor.author | Biland, A. | |
dc.contributor.author | Blanch, O. | |
dc.contributor.author | Bonnoli, G. | |
dc.contributor.author | Bošnjak, Z. | |
dc.contributor.author | Burelli, I. | |
dc.contributor.author | Busetto, G. | |
dc.contributor.author | Carosi, R. | |
dc.contributor.author | Carretero-Castrillo, M. | |
dc.contributor.author | Ceribella, G. | |
dc.contributor.author | Chai, Y. | |
dc.contributor.author | Chilingarian, A. | |
dc.contributor.author | Cikota, S. | |
dc.contributor.author | Colombo, E. | |
dc.contributor.author | Contreras, J.L. | |
dc.contributor.author | Cortina, J. | |
dc.contributor.author | Covino, S. | |
dc.contributor.author | D'Amico, Giacomo | |
dc.contributor.author | D'Elia, V. | |
dc.contributor.author | Da Vela, Vela | |
dc.contributor.author | Dazzi, F. | |
dc.contributor.author | De Angelis, Angelis | |
dc.contributor.author | De Lotto, Lotto | |
dc.contributor.author | Del Popolo, Popolo | |
dc.contributor.author | Delfino, M. | |
dc.contributor.author | Delgado, J. | |
dc.contributor.author | Delgado Mendez, Mendez | |
dc.contributor.author | Depaoli, D. | |
dc.contributor.author | Di Pierro, Pierro | |
dc.contributor.author | Di Venere, Venere | |
dc.contributor.author | Dominis Prester, Prester | |
dc.contributor.author | Donini, A. | |
dc.contributor.author | Dorner, D. | |
dc.contributor.author | Doro, M. | |
dc.contributor.author | Elsaesser, D. | |
dc.contributor.author | Emery, G. | |
dc.contributor.author | Fallah Ramazani, Ramazani | |
dc.contributor.author | Farina, L. | |
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dc.contributor.author | Font, L. | |
dc.contributor.author | Fruck, C. | |
dc.contributor.author | Fukami, S. | |
dc.contributor.author | Fukazawa, Y. | |
dc.contributor.author | García López, Lopez | |
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dc.contributor.author | Gliwny, P. | |
dc.contributor.author | Godinović, N. | |
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dc.contributor.author | Jimenez Martínez, Martinez | |
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dc.contributor.author | Kobayashi, Y. | |
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dc.contributor.author | López-Oramas, A. | |
dc.contributor.author | Loporchio, S. | |
dc.contributor.author | Lorini, A. | |
dc.contributor.author | Lyard, E. | |
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dc.contributor.author | Makariev, M. | |
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dc.contributor.author | Manganaro, M. | |
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dc.contributor.author | Mukherjee, R. | |
dc.contributor.author | O'Brien, S. | |
dc.contributor.author | Ong, R.A. | |
dc.contributor.author | Park, N. | |
dc.contributor.author | Patel, S.R. | |
dc.contributor.author | Pfrang, K. | |
dc.contributor.author | Pohl, M. | |
dc.contributor.author | Pueschel, E. | |
dc.contributor.author | Quinn, J. | |
dc.contributor.author | Ragan, K. | |
dc.contributor.author | Reynolds, P.T. | |
dc.contributor.author | Ribeiro, D. | |
dc.contributor.author | Roache, E. | |
dc.contributor.author | Ryan, J.L. | |
dc.contributor.author | Sadeh, I. | |
dc.contributor.author | Saha, L. | |
dc.contributor.author | Santander, M. | |
dc.contributor.author | Sembroski, G.H. | |
dc.contributor.author | Shang, R. | |
dc.contributor.author | Splettstoesser, M. | |
dc.contributor.author | Tak, D. | |
dc.contributor.author | Tucci, J.V. | |
dc.contributor.author | Weinstein, A. | |
dc.contributor.author | Williams, D.A. | |
dc.contributor.author | Williamson, T.J. | |
dc.contributor.author | Bosch-Ramon, V. | |
dc.contributor.author | Celma, C. | |
dc.contributor.author | Linares, Manuel | |
dc.contributor.author | Russell, D.M. | |
dc.contributor.author | Sala, G. | |
dc.date.accessioned | 2023-01-20T09:28:05Z | |
dc.date.available | 2023-01-20T09:28:05Z | |
dc.date.created | 2023-01-13T09:14:31Z | |
dc.date.issued | 2022 | |
dc.identifier.citation | Monthly notices of the Royal Astronomical Society. 2022, 517 (4), 4736-4751. | en_US |
dc.identifier.issn | 0035-8711 | |
dc.identifier.uri | https://hdl.handle.net/11250/3044868 | |
dc.description.abstract | MAXI J1820+070 is a low-mass X-ray binary with a black hole (BH) as a compact object. This binary underwent an exceptionally bright X-ray outburst from 2018 March to October, showing evidence of a non-thermal particle population through its radio emission during this whole period. The combined results of 59.5 h of observations of the MAXI J1820+070 outburst with the H.E.S.S., MAGIC and VERITAS experiments at energies above 200 GeV are presented, together with Fermi-LAT data between 0.1 and 500 GeV, and multiwavelength observations from radio to X-rays. Gamma-ray emission is not detected from MAXI J1820+070, but the obtained upper limits and the multiwavelength data allow us to put meaningful constraints on the source properties under reasonable assumptions regarding the non-thermal particle population and the jet synchrotron spectrum. In particular, it is possible to show that, if a high-energy (HE) gamma-ray emitting region is present during the hard state of the source, its predicted flux should be at most a factor of 20 below the obtained Fermi-LAT upper limits, and closer to them for magnetic fields significantly below equipartition. During the state transitions, under the plausible assumption that electrons are accelerated up to ∼500 GeV, the multiwavelength data and the gamma-ray upper limits lead consistently to the conclusion that a potential HE and very-HE gamma-ray emitting region should be located at a distance from the BH ranging between 1011 and 1013 cm. Similar outbursts from low-mass X-ray binaries might be detectable in the near future with upcoming instruments such as CTA. | en_US |
dc.language.iso | eng | en_US |
dc.publisher | Oxford University Press | en_US |
dc.title | Gamma-ray observations of MAXI J1820+070 during the 2018 outburst | en_US |
dc.title.alternative | Gamma-ray observations of MAXI J1820+070 during the 2018 outburst | en_US |
dc.type | Peer reviewed | en_US |
dc.type | Journal article | en_US |
dc.description.version | publishedVersion | en_US |
dc.source.pagenumber | 4736-4751 | en_US |
dc.source.volume | 517 | en_US |
dc.source.journal | Monthly notices of the Royal Astronomical Society | en_US |
dc.source.issue | 4 | en_US |
dc.identifier.doi | 10.1093/mnras/stac2686 | |
dc.identifier.cristin | 2106162 | |
cristin.ispublished | true | |
cristin.fulltext | original | |
cristin.qualitycode | 1 |
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