The broad-band properties of the intermediate synchrotron peaked BL Lac S2 0109+22 from radio to VHE gamma-rays

@article{Ansoldi2018TheBP,
  title={The broad-band properties of the intermediate synchrotron peaked BL Lac S2 0109+22 from radio to VHE gamma-rays},
  author={Magic Collaboration S. Ansoldi and Lucio Angelo Antonelli and C. Arcaro and D. Baack and A. Babi'c and B Banerjee and Priyadarshini Bangale and Ulisses Barres DE Almeida and J. A. Barrio and J. Becerra Gonz'alez and W. Bednarek and Elisa Bernardini and R. Ch. Berse and Alessio Berti and J{\"u}rgen Besenrieder and W. Bhattacharyya and Ciro Bigongiari and Adrian Biland and O. Blanch and G. Bonnoli and R. Carosi and G. Ceribella and Arka Chatterjee and S. M. Colak and Pierre Colin and E. Colombo and J. L. Contreras and J. Cortina and Stefano Covino and Paolo Cumani and V. D’Elia and P. Da Vela and Francesco Dazzi and Alessandro De Angelis and Barbara De Lotto and M. Delfino and J. Delgado and F. Di Pierro and Alberto Dom{\'i}nguez and D. Dominis Prester and Daniela Dorner and Michele Doro and Sabrina Einecke and D. Elsaesser and Vandad Fallah Ramazani and A. Fattorini and Alba Fern'andez-Barral and Giuseppe Ferrara and David Carreto Fidalgo and L. Foffano and M. Victoria Fonseca and Ll. Font and Christian Fruck and Stefano Gallozzi and R. J. Garc'ia L'opez and Markus Garczarczyk and Markus Gaug and Paola Giammaria and Nikola Godinovi'c and Daniel Guberman and D. Hadasch and A. Hahn and Tarek Hassan and Morihiro Hayashida and J. Herrera and John Hoang and D. Hrupec and Susumu Inoue and K. Ishio and Yukio Iwamura and Yusuke Konno and Hidetoshi Kubo and J. Kushida and A. Lamastra and Damir Lelas and Francesco Leone and Eila Lindfors and S. Lombardi and Francesco Longo and M. A. L'opez and C. Maggio and Pratik Majumdar and M. Makariev and Galina Maneva and Marina Manganaro and Karl Mannheim and Laura Maraschi and Mose Mariotti and M. C. Mart'inez and Satoshi Masuda and D. Mazin and K. Mielke and Milen Minev and J. M. Miranda and Razmik Mirzoyan and A. Moralejo and V. Moreno and E. Moretti and V. V. Neustroev and Andrzej Niedźwiecki and M. Nievas Rosillo and C. Nigro and Kari Nilsson and Daniele Ninci and K. Nishijima and K. Noda and L. Nogu'es and Simona Paiano and Joaquim Palacio and D. Paneque and Riccardo Paoletti and Josep Maria Paredes and Giovanna Pedaletti and Pablo Pe{\~n}il and Michele Peresano and Massimo Persic and K. Pfrang and P. G. Prada Moroni and E. Prandini and Ivica Puljak and J. Rodriguez Garcia and Wolfgang Rhode and Marc Rib'o and Javier Rico and Chiara Righi and A. Rugliancich and L. Saha and T. Saito and Konstancja Satalecka and Thomas Schweizer and Julian Sitarek and I. vSnidari'c and D. Sobczynska and A. Stamerra and M. Strzys and T. Suri'c and Fabrizio Tavecchio and P. Temnikov and Tomislav Terzi'c and Masahiro Teshima and N. Torres-Alb{\`a} and Shimpei Tsujimoto and G. Vanzo and M. Vazquez Acosta and I. Vovk and John E. Ward and Martin Will and Darko Zari'c and for the Fermi-LAT Collaboration S. Ciprini and R. Desiante and Mwl Collaborators S. Barcewicz and Talvikki Hovatta and J. Jormanainen and Leo O. Takalo and Riho Reinthal and Folkert Wierda and Anne Lahteenmaki and Joni Tammi and Merja Tornikoski and Rafael J. C. Vera and Sebastian Kiehlmann and Walter Max-Moerbeck and A. C. S. Readhead Universita di Udine and Infn Sezione di Trieste and I-33100 Udine and Italy. and National Centre for Radio Astrophysics and I-00136 Rome and Universit̀a di Padova and Infn and Technische Universitat Dortmund and H Germany and Croatian Magic Consortium University of Rijeka and 51000 Rijeka and University of Split - Fesb and 21000 Split and University of Zagreb - Fer and University of Osijek and 31000 Osijek and Rudjer Boskovic Institute and 10000 Zagreb and Croatia. and Saha Institute of Nuclear Physics and Hbni and 1AF Bidhannagar and Salt Lake and Sector-1 and Kolkata 700064 and India. and Max-Planck-Institut fur extraterrestrische Physik and D-80805 Munchen and Now at Centro Brasileiro de Pesquisas F'isicas and 22290-180 Urca and R. D. Janeiro and Brasil and Unidad de Part'iculas y Cosmolog'ia and Universidad Complutense and E-28040 Madrid and Spain. and Instituto de Astrof'isica de Canarias and E-38200 La Laguna and Universidad de la Laguna and Dpto. Astrof'isica and E-38200 La Laguna and Tenerife and University of L'od'z and Department of Theoretical Astrophysics and PL-90236 L'od'z and Poland and Deutsches Elektronen-Synchrotron and D-15738 Zeuthen and Eth Zurich and CH-8093 Zurich and Switzerland. and Institut de F'isica d'Altes Energies and The Barcelona Institute of Science and Technology and E-08193 Bellaterra and Universit'a di Siena and Infn sez. di Pisa and Italy Universita di Siena and Universita' di Pisa and Infn sez. di Pisa and Universitat Wurzburg and D-97074 Wurzburg and Finnish Magic Consortium Tuorla Observatory and Finnish Magic Consortium Finnish Centre of Astronomy with Eso and University of Turku and 20 Vaisalantie and FI-21500 Piikkio and Astronomy Division and University of Oulu and FIN-90014 University of Oulu and Finland. and Departament de F'isica and CERES-IEEC and Universitat Aut'onoma de Barcelona and Japanese Magic Consortium Icrr and The University of Tokyo and 277-8582 Chiba and Japan. and Dep. of Physics and Kyoto University and 606-8502 Kyoto and Tokai University and 259-1292 Kanagawa and Riken and 351-0198 Saitama and Inst. for Nucl. Research and Nucl. Energy and Bulgarian academy of Sciences and BG-1784 Sofia and Bulgaria. and Universitat Aut'onoma de Barcelona and Icc and IEEC-UB and E-08028 Barcelona and Humboldt University of Berlin and Institut fur Physik D-12489 Berlin Germany and also at Dipartimento di Fisica and Universita di UdineI.N.F.N. Trieste and Infn Sezione di Trieste and also at Port d'Informaci'o Cient'ifica E-08193 Bellater Spain and also at INAF-Trieste and Dept. of Physics and Astronomy and University of Bologna and Agenzia Spaziale Italiana Science Data Center and I. Roma and Istituto Nazionale Fisica Nucleare and Sezione di Perugia and Infn Sezione di Perugia and Departamento de Astronom'ia and Universidad Catolica de Chile and Camino El Observatorio 1515 and L. F. Cond{\'e}s and Santiago and Chile. and Tuorla Astronomical Observatory and Aalto University Metsahovi Radio Observatory and Metsahovintie 114 and 02540 Kylmala and Aalto University Department of Electronics and Nanoengineering and P. O. Box 15500 and FI-00076 Aalto and Tartu Observatory and 1 Observatooriumi and 61602 Toravere and Estonia. and Owens Valley Radio Observatory and California Institute of Technology. and Pasadena and CA 91125 and Usa},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2018}
}
The Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes observed S2 0109+22 in 2015 July during its flaring activity in high-energy gamma-rays observed by Fermi-Large Area Telescope. We analyse the MAGIC data to characterize the very high energy (VHE) gamma-ray emission of S2 0109+22, which belongs to the subclass of intermediate synchrotron peak (ISP) BL Lacertae (BL Lac) objects. We study the multifrequency emission in order to investigate the source classification. Finally, we… 
Testing emission models on the extreme blazar 2WHSP J073326.7+515354 detected at very high energies with the MAGIC telescopes
Extreme high-energy-peaked BL Lac objects (EHBLs) are an emerging class of blazars. Their typical two-hump-structured spectral energy distribution (SED) peaks at higher energies with respect to
Testing two-component models on very high-energy gamma-ray-emitting BL Lac objects
Context. It has become evident that one-zone synchrotron self-Compton models are not always adequate for very high-energy (VHE) gamma-ray-emitting blazars. While two-component models perform better,
Signature of Stochastic Acceleration and Cooling Processes in an Outburst Phase of the TeV Blazar ON 231
We present a detailed spectral and temporal study of the intermediate-type blazar ON 231 during the TeV outburst phase in 2008 June with observations performed by Swift and XMM-Newton. The X-ray flux
Constraints on the AGN flares as sources of ultra-high energy cosmic rays from the Fermi-LAT observations
It is well known that if the most energetic cosmic rays (E>1020 eV) were protons then their acceleration sites should possess some extreme properties, including gigantic luminosity. As no stationary
High-energy neutrino flux from individual blazar flares
Motivated by the recently reported evidence of an association between a high-energy neutrino and a γ-ray flare from the blazar TXS 0506+056, we calculate the expected high-energy neutrino signal
J C A P 0 3 ( 2 0 2 0 ) 0 6 0 ournal of C osmology and A stroparticle P hysics
  • 2020

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