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

Journal Article · · Monthly Notices of the Royal Astronomical Society
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  1. Università di Udine, and INFN Trieste, I-33100 Udine, Italy; Japanese MAGIC Consortium: ICRR, The University of Tokyo, 277-8582 Chiba, Japan, Department of Physics, Kyoto University, 606-8502 Kyoto, Japan, Tokai University, 259-1292 Kanagawa, Japan, RIKEN, 351-0198 Saitama, Japan
  2. National Institute for Astrophysics (INAF), I-00136 Rome, Italy
  3. Università di Padova and INFN, I-35131 Padova, Italy
  4. Technische Universität Dortmund, D-44221 Dortmund, Germany
  5. Croatian MAGIC Consortium: University of Rijeka, 51000 Rijeka, University of Split – FESB, 21000 Split, University of Zagreb – FER, 10000 Zagreb, University of Osijek, 31000 Osijek, and Rudjer Boskovic Institute, 10000 Zagreb, Croatia
  6. Saha Institute of Nuclear Physics, HBNI, 1/AF Bidhannagar, Salt Lake, Sector-1, Kolkata 700064, India
  7. Max-Planck-Institut für Physik, D-80805 München, Germany
  8. Max-Planck-Institut für Physik, D-80805 München, Germany; now at Centro Brasileiro de Pesquisas Físicas (CBPF), 22290-180 URCA, Rio de Janeiro (RJ), Brazil
  9. Unidad de Partículas y Cosmología (UPARCOS), Universidad Complutense, E-28040 Madrid, Spain
  10. Inst. de Astrofísica de Canarias, E-38200 La Laguna, and Universidad de La Laguna, Dpto. Astrofísica, E-38206 La Laguna, Tenerife, Spain
  11. Department of Astrophysics, University of Łódź, PL-90236 Łódź, Poland
  12. Deutsches Elektronen-Synchrotron (DESY), D-15738 Zeuthen, Germany; Institut für Physik, Humboldt University of Berlin, D-12489 Berlin, Germany
  13. Università di Udine, and INFN Trieste, I-33100 Udine, Italy; also at Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy
  14. Deutsches Elektronen-Synchrotron (DESY), D-15738 Zeuthen, Germany
  15. ETH Zurich, CH-8093 Zurich, Switzerland
  16. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
  17. Università di Siena and INFN Pisa, I-53100 Siena, Italy
  18. Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy
  19. Università di Udine, and INFN Trieste, I-33100 Udine, Italy
  20. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain; also at Port d’Informació Científica (PIC), E-08193 Bellaterra (Barcelona), Spain
  21. Universität Würzburg, D-97074 Würzburg, Germany
  22. Finnish MAGIC Consortium: Tuorla Observatory (Department of Physics and Astronomy) and Finnish Centre of Astronomy with ESO (FINCA), University of Turku, FIN-20014 Turku, Finland, Astronomy Division, University of Oulu, FIN-90014 Oulu, Finland
  23. Departament de Física, and CERES-IEEC, Universitat Autónoma de Barcelona, E-08193 Bellaterra, Spain
  24. Japanese MAGIC Consortium: ICRR, The University of Tokyo, 277-8582 Chiba, Japan, Department of Physics, Kyoto University, 606-8502 Kyoto, Japan, Tokai University, 259-1292 Kanagawa, Japan, RIKEN, 351-0198 Saitama, Japan
  25. Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, BG-1784 Sofia, Bulgaria
  26. Japanese MAGIC Consortium: ICRR, The University of Tokyo, 277-8582 Chiba, Japan, Department of Physics, Kyoto University, 606-8502 Kyoto, Japan, Tokai University, 259-1292 Kanagawa, Japan, RIKEN, 351-0198 Saitama, Japan; Max-Planck-Institut für Physik, D-80805 München, Germany
  27. Universitat de Barcelona, ICC, IEEC-UB, E-08028 Barcelona, Spain
  28. Università di Udine, and INFN Trieste, I-33100 Udine, Italy; INAF-Trieste and Department of Physics and Astronomy, University of Bologna, 40126 Bologna, Italy
  29. Agenzia Spaziale Italiana (ASI), Space Science Data Center, I-00133 Roma, Italy; Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Perugia, I-06123 Perugia, Italy
  30. Tuorla Observatory, Department of Physics and Astronomy, University of Turku, FIN-20014 Turku, Finland
  31. Astrophysical Sciences Division, BARC, Mumbai-400085, India
  32. Metsähovi Radio Observatory, Aalto University, Metsähovintie 114, FI-02540 Kylmälä, Finland; Department of Electronics and Nanoengineering, Aalto University, PO Box 15500, FI-00076 Aalto, Finland; Tartu Observatory, Observatooriumi 1, 61602 Tõravere, Estonia
  33. Metsähovi Radio Observatory, Aalto University, Metsähovintie 114, FI-02540 Kylmälä, Finland
  34. Metsähovi Radio Observatory, Aalto University, Metsähovintie 114, FI-02540 Kylmälä, Finland; Department of Electronics and Nanoengineering, Aalto University, PO Box 15500, FI-00076 Aalto, Finland
  35. Owens Valley Radio Observatory, California Institute of Technology, Pasadena, CA 91125, USA
  36. Departmento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile
+ Show Author Affiliations

Here, 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 compare the source long-term behaviour to other VHE gamma-ray emitting (TeV) blazars. We performed a temporal and spectral analysis of the data centred around the MAGIC interval of observation (MJD 57225–57231). Long-term radio and optical data have also been investigated using the discrete correlation function. The redshift of the source is estimated through optical host-galaxy imaging and also using the amount of VHE gamma-ray absorption. The quasi-simultaneous multifrequency spectral energy distribution (SED) is modelled with the conventional one-zone synchrotron self-Compton (SSC) model. MAGIC observations resulted in the detection of the source at a significance level of 5.3σ. The VHE gamma-ray emission of S2 0109+22 is variable on a daily time scale. VHE gamma-ray luminosity of the source is lower than the average of TeV BL Lacs. The optical polarization and long-term optical/radio behaviour of the source are different from the general population of TeV blazars. All these findings agree with the classification of the source as an ISP BL Lac object. As a result, we estimate the source redshift as z = 0.36 ± 0.07. The SSC parameters describing the SED are rather typical for blazars.

Research Organization:
SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Organization:
USDOE
Contributing Organization:
MAGIC Collaboration
Grant/Contract Number:
AC02-76SF00515
OSTI ID:
1475024
Journal Information:
Monthly Notices of the Royal Astronomical Society, Vol. 480, Issue 1; ISSN 0035-8711
Publisher:
Royal Astronomical SocietyCopyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 6 works
Citation information provided by
Web of Science

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Cited By (6)

High-energy neutrino flux from individual blazar flares journal September 2019
Testing emission models on the extreme blazar 2WHSP J073326.7+515354 detected at very high energies with the MAGIC telescopes journal September 2019
Signature of Stochastic Acceleration and Cooling Processes in an Outburst Phase of the TeV Blazar ON 231 journal July 2019
Testing emission models on the extreme blazar 2WHSP J073326.7+515354 detected at very high energies with the MAGIC telescopes text January 2019
High energy neutrino flux from individual blazar flares text January 2019
Signature of stochastic acceleration and cooling processes in an outburst phase of the TeV blazar ON 231 text January 2019

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Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
galaxies: active
BL Lacertae objects: individual: S2 0109+22
galaxies: jets
gamma-rays: galaxies