Testing emission models on the extreme blazar 2WHSP J073326.7+515354 detected at very high energies with the MAGIC telescopes
Author:
, , Acciari V A12, Ansoldi S34567, Antonelli L A8, Arbet Engels A9, Baack D10, Babić A1112131415, Banerjee B16, Barres de Almeida U17, Barrio J A18, Becerra González J12, Bednarek W19, Bellizzi L20, Bernardini E2122, Berti A23, Besenrieder J24, Bhattacharyya W21, Bigongiari C8, Biland A9, Blanch O25, Bonnoli G20, Bošnjak Ž1112131415, Busetto G22, Carosi R26, Ceribella G24, Cerruti M27ORCID, Chai Y24, Chilingaryan A28, Cikota S1112131415, Colak S M25, Colin U24, Colombo E12, Contreras J L18, Cortina J29, Covino S8, D’Elia V8, Da Vela P26, Dazzi F8, De Angelis A22, De Lotto B3, Delfino M2530, Delgado J2530, Depaoli D23, Di Pierro F23, Di Venere L23, Do Souto Espiñeira E25, Dominis Prester D1112131415, Donini A3, Dorner D31, Doro M22, Elsaesser D10, Fallah Ramazani V3233, Fattorini A10, Ferrara G8, Fidalgo D18, Foffano L22ORCID, Fonseca M V18, Font L34, Fruck C24, Fukami S4567, García López R J1, Garczarczyk M21, Gasparyan S28, Gaug M34, Giglietto N23, Giordano F23, Godinović N1112131415, Green D24, Guberman D25, Hadasch D4567, Hahn A24, Herrera J12, Hoang J18, Hrupec D1112131415, Hütten M24, Inada T4567, Inoue S4567, Ishio K24, Iwamura Y4567, Jouvin L25, Kerszberg D25, Kubo H4567, Kushida J4567, Lamastra A8, Lelas D1112131415, Leone F8, Lindfors E3233, Lombardi S8, Longo F335, López M18, López-Coto R22, López-Oramas A12, Loporchio S23, Machado de Oliveira Fraga B17, Maggio C34, Majumdar P16, Makariev M36, Mallamaci M22, Maneva G36, Manganaro M1112131415, Mannheim K31, Maraschi L8, Mariotti M22, Martínez M25, Mazin D456724, Mićanović S1112131415, Miceli D3, Minev M36, Miranda J M20, Mirzoyan R24, Molina E27, Moralejo A25, Morcuende D18, Moreno V34, Moretti E25, Munar-Adrover P34, Neustroev V3233, Nigro C21, Nilsson K3233, Ninci D25, Nishijima K4567, Noda K4567, Nogués L25, Nozaki S4567, Paiano S22, Palacio J25, Palatiello M3, Paneque D24, Paoletti R20, Paredes J M27, Peñil P18, Peresano M3, Persic M337, Prada Moroni P G26, Prandini E22, Puljak I1112131415, Rhode W10, Ribó M27, Rico J25, Righi C8, Rugliancich A26, Saha L18, Sahakyan N28, Saito T4567, Sakurai S4567, Satalecka K21, Schmidt K10, Schweizer T24, Sitarek J19, Šnidarić I1112131415, Sobczynska D19, Somero A12, Stamerra A8, Strom D24, Strzys M24, Suda Y24, Surić T1112131415, Takahashi M4567, Tavecchio F8, Temnikov P36, Terzić T1112131415, Teshima M456724, Torres-Albà N27, Tosti L23, Vagelli V23, van Scherpenberg J24, Vanzo G12, Vazquez Acosta M12, Vigorito C F23, Vitale V23, Vovk I24, Will M24, Zarić D1112131415, Asano K4567, D’Ammando F38, Clavero R12
Affiliation:
1. Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain 2. Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain 3. Università di Udine, and INFN Trieste, I-33100 Udine, Italy 4. ICRR, The University of Tokyo, 277-8582 Chiba, Japan 5. Department of Physics, Kyoto University, 606-8502 Kyoto, Japan 6. Physics department, Tokai University, 259-1292 Kanagawa, Japan 7. RIKEN, 351-0198 Saitama, Japan 8. National Institute for Astrophysics (INAF), I-00136 Rome, Italy 9. ETH Zurich, CH-8093 Zurich, Switzerland 10. Physics department, Technische Universität Dortmund, D-44221 Dortmund, Germany 11. Department of Physics, University of Rijeka, 51000 Rijeka, Croatia 12. Physics department, University of Split - FESB, 21000 Split, Croatia 13. Physics department, University of Zagreb - FER, 10000 Zagreb, Croatia 14. Physics department, University of Osijek, 31000 Osijek, Croatia 15. Physics department, Rudjer Boskovic Institute, 10000 Zagreb, Croatia 16. Saha Institute of Nuclear Physics, HBNI, 1/AF Bidhannagar, Salt Lake, Sector-1, Kolkata 700064, India 17. Centro Brasileiro de Pesquisas Físicas (CBPF), 22290-180 URCA, Rio de Janeiro, RJ, Brazil 18. IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, E-28040 Madrid, Spain 19. Department of Astrophysics, University of Łódź, PL-90236 Łódź, Poland 20. Physics department, Università di Siena, and INFN Pisa, I-53100 Siena, Italy 21. Deutsches Elektronen-Synchrotron (DESY), D-15738 Zeuthen, Germany 22. Physics department, Università di Padova and INFN, I-35131 Padova, Italy 23. Istituto Nazionale Fisica Nucleare (INFN), I-00044 Frascati (Roma), Italy 24. Max-Planck-Institut für Physik, D-80805 München, Germany 25. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain 26. Physics department, Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy 27. ICCUB, Universitat de Barcelona, IEEC-UB, E-08028 Barcelona, Spain 28. ICRANet-Armenia at NAS RA, 0019 Yerevan, Armenia 29. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain 30. Port d’Informació Científica (PIC) E-08193 Bellaterra (Barcelona) Spain 31. Physics department, Universität Würzburg, D-97074 Würzburg, Germany 32. Finnish Centre of Astronomy with ESO (FINCA), University of Turku, FI-20014 Turku, Finland 33. Astronomy Research Unit, University of Oulu, FI-90014 Oulu, Finland 34. Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain 35. Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy 36. Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, BG-1784 Sofia, Bulgaria 37. INAF-Trieste and Department of Physics and Astronomy, University of Bologna, Italy 38. INAF Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna, Italy
Abstract
ABSTRACT
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 conventional blazars. Multiwavelength (MWL) observations constrain their synchrotron peak in the medium to hard X-ray band. Their gamma-ray SED peaks above the GeV band, and in some objects it extends up to several TeV. Up to now, only a few EHBLs have been detected in the TeV gamma-ray range. In this paper, we report the detection of the EHBL 2WHSP J073326.7+515354, observed and detected during 2018 in TeV gamma rays with the MAGIC telescopes. The broad-band SED is studied within an MWL context, including an analysis of the Fermi-LAT data over 10 yr of observation and with simultaneous Swift-XRT, Swift-UVOT, and KVA data. Our analysis results in a set of spectral parameters that confirms the classification of the source as an EHBL. In order to investigate the physical nature of this extreme emission, different theoretical frameworks were tested to model the broad-band SED. The hard TeV spectrum of 2WHSP J073326.7+515354 sets the SED far from the energy equipartition regime in the standard one-zone leptonic scenario of blazar emission. Conversely, more complex models of the jet, represented by either a two-zone spine-layer model or a hadronic emission model, better represent the broad-band SED.
Funder
BMBF MPG INFN INAF SNF ERDF MINECO Indian Department of Atomic Energy JSPS MEXT Bulgarian Ministry of Education and Science Academy of Finland Croatian Science Foundation DFG Polish National Research Centre MCTIC CNPq FAPERJ National Aeronautics and Space Administration U.S. Department of Energy Centre National de la Recherche Scientifique Institut National de Physique Nucléaire et de Physique des Particules Agenzia Spaziale Italiana Istituto Nazionale di Fisica Nucleare High Energy Accelerator Research Organization Japan Aerospace Exploration Agency Knut and Alice Wallenberg Foundation Swedish Research Council Swedish National Space Board Istituto Nazionale di Astrofisica Centre National d'Etudes Spatiales la Caixa Banking Foundation
Publisher
Oxford University Press (OUP)
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
21 articles.
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