Gamma-ray observations of MAXI J1820+070 during the 2018 outburst
Creators: name: Abe, H.
name: Abe, S.
name: Acciari, V. A.
name: Aniello, T.
name: Ansoldi, S.
name: Antonelli, L. A.
name: Engels, A. Arbet
name: Arcaro, C.
name: Artero, M.
name: Asano, K.
name: Baack, D.
name: Babić, A.
name: Baquero, A.
name: de Almeida, U. Barres
name: Barrio, J. A.
name: Batković, I.
name: Baxter, J.
name: González, J. Becerra
name: Bednarek, W.
name: Bernardini, E.
name: Bernardos, M.
name: Berti, A.
name: Besenrieder, J.
name: Bhattacharyya, W.
name: Bigongiari, C.
name: Biland, A.
name: Blanch, O.
name: Bonnoli, G.
name: Bošnjak, Ž.
name: Burelli, I.
name: Busetto, G.
name: Carosi, R.
name: Carretero-Castrillo, M.
name: Ceribella, G.
name: Chai, Y.
name: Chilingarian, A.
name: Cikota, S.
name: Colombo, E.
name: Contreras, J. L.
name: Cortina, J.
name: Covino, S.
name: D'Amico, G.
name: D'Elia, V.
name: Da Vela, P.
name: Dazzi, F.
name: De Angelis, A.
name: De Lotto, B.
name: Del Popolo, A.
name: Delfino, M.
name: Delgado, J.
name: Mendez, C. Delgado
name: Depaoli, D.
name: Di Pierro, F.
name: Di Venere, L.
name: Prester, D. Dominis
name: Donini, A.
name: Dorner, D.
name: Doro, M.
name: Elsaesser, D.
name: Emery, G.
name: Ramazani, V. Fallah
name: Fariña, L.
name: Fattorini, A.
name: Font, L.
name: Fruck, C.
name: Fukami, S.
name: Fukazawa, Y.
name: López, R. J. García
name: Garczarczyk, M.
name: Gasparyan, S.
name: Gaug, M.
name: Paiva, J. G. Giesbrecht
name: Giglietto, N.
name: Giordano, F.
name: Gliwny, P.
name: Godinović, N.
name: Grau, R.
name: Green, D.
name: Green, J. G.
name: Hadasch, D.
name: Hahn, A.
name: Hassan, T.
name: Heckmann, L.
name: Herrera, J.
name: Hoang, J.
name: Hrupec, D.
name: Hütten, M.
name: Imazawa, R.
name: Inada, T.
name: Iotov, R.
name: Ishio, K.
name: Martínez, I. Jiménez
name: Jormanainen, J.
name: Kerszberg, D.
name: Kobayashi, Y.
name: Kubo, H.
name: Kushida, J.
name: Lamastra, A.
name: Lelas, D.
name: Leone, F.
name: Lindfors, E.
name: Linhoff, L.
name: Lombardi, S.
name: Longo, F.
name: López-Coto, R.
name: López-Moya, M.
name: López-Oramas, A.
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name: Lorini, A.
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name: Fraga, B. Machado de Oliveira
name: Majumdar, P.
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name: Roache, E.
name: Ryan, J. L.
name: Sadeh, I.
name: Saha, L.
name: Santander, M.
name: Sembroski, G. H.
name: Shang, R.
name: Splettstoesser, M.
name: Tak, D.
name: Tucci, J. V.
name: Weinstein, A.
name: Williams, D. A.
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name: Sala, G.
Publisher: name: arXiv
Year: 2022
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: MAXI J1820+070 is a low-mass X-ray binary with a black hole as a compact object. This binary underwent an exceptionally bright X-ray outburst from March to October 2018, showing evidence of a non-thermal particle population through its radio emission during this whole period. The combined results of 59.5 hours 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 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 high-energy and very-high-energy gamma-ray emitting region should be located at a distance from the black hole ranging between 10^11 and 10^13 cm. Similar outbursts from low-mass X-ray binaries might be detectable in the near future with upcoming instruments such as CTA.
description: 15 pages, 5 figures. Accepted for publication in MNRAS