Broadband characterisation of the very intense TeV flares of the blazar 1ES 1959+650 in 2016. (arXiv:2002.00129v1 [astro-ph.HE])

Broadband characterisation of the very intense TeV flares of the blazar 1ES 1959+650 in 2016. (arXiv:2002.00129v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_MAGIC/0/1/0/all/0/1">MAGIC Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Acciari_V/0/1/0/all/0/1">V. A. Acciari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ansoldi_S/0/1/0/all/0/1">S. Ansoldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antonelli_L/0/1/0/all/0/1">L. A. Antonelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Engels_A/0/1/0/all/0/1">A. Arbet Engels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baack_D/0/1/0/all/0/1">D. Baack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Babic_A/0/1/0/all/0/1">A. Babić</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banerjee_B/0/1/0/all/0/1">B. Banerjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Almeida_U/0/1/0/all/0/1">U. Barres de Almeida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barrio_J/0/1/0/all/0/1">J. A. Barrio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_J/0/1/0/all/0/1">J. Becerra González</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bednarek_W/0/1/0/all/0/1">W. Bednarek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellizzi_L/0/1/0/all/0/1">L. Bellizzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardini_E/0/1/0/all/0/1">E. Bernardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berti_A/0/1/0/all/0/1">A. Berti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Besenrieder_J/0/1/0/all/0/1">J. Besenrieder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhattacharyya_W/0/1/0/all/0/1">W. Bhattacharyya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bigongiari_C/0/1/0/all/0/1">C. Bigongiari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biland_A/0/1/0/all/0/1">A. Biland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanch_O/0/1/0/all/0/1">O. Blanch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonnoli_G/0/1/0/all/0/1">G. Bonnoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bosnjak_Z/0/1/0/all/0/1">Z. Bosnjak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Busetto_G/0/1/0/all/0/1">G. Busetto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carosi_R/0/1/0/all/0/1">R. Carosi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ceribella_G/0/1/0/all/0/1">G. Ceribella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chai_Y/0/1/0/all/0/1">Y. Chai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cikota_S/0/1/0/all/0/1">S. Cikota</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colak_S/0/1/0/all/0/1">S. M. Colak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colin_U/0/1/0/all/0/1">U. Colin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colombo_E/0/1/0/all/0/1">E. Colombo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Contreras_J/0/1/0/all/0/1">J. L. Contreras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cortina_J/0/1/0/all/0/1">J. Cortina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Covino_S/0/1/0/all/0/1">S. Covino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DElia_V/0/1/0/all/0/1">V. D'Elia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vela_P/0/1/0/all/0/1">P. Da Vela</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dazzi_F/0/1/0/all/0/1">F. Dazzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angelis_A/0/1/0/all/0/1">A. De Angelis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lotto_B/0/1/0/all/0/1">B. De Lotto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delfino_M/0/1/0/all/0/1">M. Delfino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delgado_J/0/1/0/all/0/1">J. Delgado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pierro_F/0/1/0/all/0/1">F. Di Pierro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Espineira_E/0/1/0/all/0/1">E. Do Souto Espiñeira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prester_D/0/1/0/all/0/1">D. Dominis Prester</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Donini_A/0/1/0/all/0/1">A. Donini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dorner_D/0/1/0/all/0/1">D. Dorner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doro_M/0/1/0/all/0/1">M. Doro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elsaesser_D/0/1/0/all/0/1">D. Elsaesser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramazani_V/0/1/0/all/0/1">V. Fallah Ramazani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fattorini_A/0/1/0/all/0/1">A. Fattorini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_Barral_A/0/1/0/all/0/1">A. Fernández-Barral</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrara_G/0/1/0/all/0/1">G. Ferrara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fidalgo_D/0/1/0/all/0/1">D. Fidalgo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Foffano_L/0/1/0/all/0/1">L. Foffano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fonseca_M/0/1/0/all/0/1">M. V. Fonseca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Font_L/0/1/0/all/0/1">L. Font</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fruck_C/0/1/0/all/0/1">C. Fruck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fukami_S/0/1/0/all/0/1">S. Fukami</a>, et al. (109 additional authors not shown)

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 >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
(>=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.

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