Broadband characterisation of the very intense TeV flares of the blazar 1ES 1959+650 in 2016
Creators: name: MAGIC Collaboration
name: Acciari, V. A.
name: Ansoldi, S.
name: Antonelli, L. A.
name: Engels, A. Arbet
name: Baack, D.
name: Babić, A.
name: Banerjee, B.
name: de Almeida, U. Barres
name: Barrio, J. A.
name: González, J. Becerra
name: Bednarek, W.
name: Bellizzi, L.
name: Bernardini, E.
name: Berti, A.
name: Besenrieder, J.
name: Bhattacharyya, W.
name: Bigongiari, C.
name: Biland, A.
name: Blanch, O.
name: Bonnoli, G.
name: Bosnjak, Z.
name: Busetto, G.
name: Carosi, R.
name: Ceribella, G.
name: Chai, Y.
name: Cikota, S.
name: Colak, S. M.
name: Colin, U.
name: Colombo, E.
name: Contreras, J. L.
name: Cortina, J.
name: Covino, S.
name: D'Elia, V.
name: Da Vela, P.
name: Dazzi, F.
name: De Angelis, A.
name: De Lotto, B.
name: Delfino, M.
name: Delgado, J.
name: Di Pierro, F.
name: Espiñeira, E. Do Souto
name: Prester, D. Dominis
name: Donini, A.
name: Dorner, D.
name: Doro, M.
name: Elsaesser, D.
name: Ramazani, V. Fallah
name: Fattorini, A.
name: Fernández-Barral, A.
name: Ferrara, G.
name: Fidalgo, D.
name: Foffano, L.
name: Fonseca, M. V.
name: Font, L.
name: Fruck, C.
name: Fukami, S.
name: Gallozzi, S.
name: López, R. J. García
name: Garczarczyk, M.
name: Gasparyan, S.
name: Gaug, M.
name: Godinović, N.
name: Green, D.
name: Guberman, D.
name: Hadasch, D.
name: Hahn, A.
name: Herrera, J.
name: Hoang, J.
name: Hrupec, D.
name: Inada, T.
name: Inoue, S.
name: Ishio, K.
name: Iwamura, Y.
name: Jouvin, L.
name: Kubo, H.
name: Kushida, J.
name: Lamastra, A.
name: Lelas, D.
name: Leone, F.
name: Lindfors, E.
name: Lombardi, S.
name: Longo, F.
name: López, M.
name: López-Coto, R.
name: López-Oramas, A.
name: Fraga, B. Machado de Oliveira
name: Maggio, C.
name: Majumdar, P.
name: Makariev, M.
name: Mallamaci, M.
name: Maneva, G.
name: Manganaro, M.
name: Mannheim, K.
name: Maraschi, L.
name: Mariotti, M.
name: Martínez, M.
name: Masuda, S.
name: Mazin, D.
name: Mićanović, S.
name: Miceli, D.
name: Minev, M.
name: Miranda, J. M.
name: Mirzoyan, R.
name: Molina, E.
name: Moralejo, A.
name: Morcuende, D.
name: Moreno, V.
name: Moretti, E.
name: Munar-Adrover, P.
name: Neustroev, V.
name: Niedzwiecki, A.
name: Nigro, C.
name: Nilsson, K.
name: Ninci, D.
name: Nishijima, K.
name: Noda, K.
name: Nogués, L.
name: Nöthe, M.
name: Nozaki, S.
name: Paiano, S.
name: Palacio, J.
name: Palatiello, M.
name: Paneque, D.
name: Paoletti, R.
name: Paredes, J. M.
name: Peñil, P.
name: Peresano, M.
name: Persic, M.
name: Moroni, P. G. Prada
name: Prandini, E.
name: Puljak, I.
name: Rhode, W.
name: Ribó, M.
name: Rico, J.
name: Righi, C.
name: Rugliancich, A.
name: Saha, L.
name: Sahakyan, N.
name: Saito, T.
name: Sakurai, S.
name: Satalecka, K.
name: Schweizer, T.
name: Sitarek, J.
name: Šnidarić, I.
name: Sobczynska, D.
name: Somero, A.
name: Stamerra, A.
name: Strom, D.
name: Strzys, M.
name: Surić, T.
name: Takahashi, M.
name: Tavecchio, F.
name: Temnikov, P.
name: Terzić, T.
name: Teshima, M.
name: Torres-Albà, N.
name: Tsujimoto, S.
name: van Scherpenberg, J.
name: Vanzo, G.
name: Acosta, M. Vazquez
name: Vovk, I.
name: Will, M.
name: Zarić, D.
name: Collaboration, Fermi-LAT
name: :
name: Hayashida, M.
Publisher: name: arXiv
Year: 2020
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: 1ES 1959+650 is a bright TeV high-frequency-peaked BL Lac object exhibiting interesting features like "orphan" TeV flares and a broad emission in the high-energy regime, that are difficult to interpret using conventional one-zone Synchrotron Self-Compton (SSC) scenarios. We report the results from the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) observations in 2016 along with the multi-wavelength data from the Fermi Large Area Telescope (LAT) and Swift instruments. MAGIC observed 1ES 1959+650 with different emission levels in the very-high-energy (VHE, E &gt;100 GeV) gamma-ray band during 2016. In the long-term data, the X-ray spectrum becomes harder with increasing flux and a hint of a similar trend is also visible in the VHE band. An exceptionally high VHE flux reaching ~ 3 times the Crab Nebula flux was measured by MAGIC on the 13th, 14th of June and 1st July 2016 (the highest flux observed since 2002). During these flares, the high-energy peak of the spectral energy distribution (SED) lies in the VHE domain and extends up to several TeV. The spectrum in the gamma-ray (both Fermi-LAT and VHE bands) and the X-ray bands are quite hard. On 13th June and 1st July 2016, the source showed rapid variations of the VHE flux within timescales of less than an hour. A simple one-zone SSC model can describe the data during the flares requiring moderate to high values of the Doppler factors (&gt;=30-60). Alternatively, the high-energy peak of the SED can be explained by a purely hadronic model attributed to proton-synchrotron radiation with jet power L_{jet}~10^{46} erg/s and under high values of the magnetic field strength (~100 G) and maximum proton energy (~few EeV). Mixed lepto-hadronic models require super-Eddington values of the jet power. We conclude that it is difficult to get detectable neutrino emission from the source during the extreme VHE flaring period of 2016.
description: 18 pages, 9 figures, accepted to A&amp;A