First detection of VHE gamma-ray emission from TXS 1515–273, study of its X-ray variability and spectral energy distribution
Author:
, Acciari V A1, Ansoldi S2, Antonelli L A3, Arbet Engels A4, Artero M5, Asano K6, Baack D7, Babić A8, Baquero A9, Barres de Almeida U10, Barrio J A9, Batković I11, Becerra González J1, Bednarek W12, Bellizzi L13, Bernardini E14, Bernardos M11, Berti A15, Besenrieder J16, Bhattacharyya W14, Bigongiari C3, Biland A4, Blanch O5, Bošnjak Ž8, Busetto G11, Carosi R17, Ceribella G16, Cerruti M18, Chai Y16, Chilingarian A19, Cikota S8, Colak S M5, Colombo E1, Contreras J L9, Cortina J20, Covino S3, D’Amico G16, D’Elia V3, Da Vela P17, Dazzi F3, De Angelis A11, De Lotto B2, Delfino M521, Delgado J521, Delgado Mendez C20, Depaoli D15, Pierro F Di15, Venere L Di22, Do Souto Espiñeira E5, Dominis Prester D23, Donini A2, Dorner D24, Doro M11, Elsaesser D7, Fallah Ramazani V2526ORCID, Fattorini A7, Ferrara G3, Fonseca M V9, Font L27, Fruck C16, Fukami S6, García López R J1, Garczarczyk M14, Gasparyan S28, Gaug M27, Giglietto N22, Giordano F22, Gliwny P12, Godinović N29, Green J G3, Green D16, Hadasch D6, Hahn A16, Heckmann L16, Herrera J1, Hoang J9, Hrupec D30, Hütten M16, Inada T6, Inoue S31, Ishio K16, Iwamura Y6, Jiménez I20, Jormanainen J25, Jouvin L5, Kajiwara Y32, Karjalainen M1, Kerszberg D5, Kobayashi Y6, Kubo H32, Kushida J33, Lamastra A3, Lelas D29, Leone F3, Lindfors E25, Lombardi S3, Longo F234, López-Coto R11, López-Moya M9, López-Oramas A1, Loporchio S22ORCID, Machado de Oliveira Fraga B10, Maggio C27, Majumdar P35, Makariev M36, Mallamaci M11, Maneva G36, Manganaro M23, Mannheim K24, Maraschi L3, Mariotti M11, Martínez M5, Mazin D616, Menchiari S13, Mender S7, Mićanović S23, Miceli D2, Miener T9, Minev M36, Miranda J M13, Mirzoyan R16, Molina E18, Moralejo A5, Morcuende D9, Moreno V27, Moretti E5, Neustroev V37, Nigro C5, Nilsson K25, Nishijima K33, Noda K6, Nozaki S32, Ohtani Y6, Oka T32, Otero-Santos J1, Paiano S3, Palatiello M2, Paneque D16, Paoletti R13, Paredes J M18, Pavletić L23, Peñil P9, Perennes C11, Persic M238, Prada Moroni P G17, Prandini E11, Priyadarshi C5, Puljak I29, Rhode W7, Ribó M18, Rico J5, Righi C3, Rugliancich A17, Saha L9, Sahakyan N28, Saito T6, Sakurai S6, Satalecka K14, Saturni F G3, Schleicher B24, Schmidt K7, Schweizer T16, Sitarek J12, Šnidarić I39, Sobczynska D12, Spolon A11, Stamerra A3, Strom D16, Strzys M6, Suda Y16, Surić T39, Takahashi M6, Tavecchio F3, Temnikov P36, Terzić T23, Teshima M616, Tosti L40, Truzzi S13, Tutone A3, Ubach S27, van Scherpenberg J16, Vanzo G1, Vazquez Acosta M1, Ventura S13, Verguilov V36, Vigorito C F15, Vitale V41, Vovk I6, Will M16, Wunderlich C13, Zarić D29, Bissaldi E42, Bonnoli G1343, Cutini S44, D’Ammando F45, Nabizadeh A46, Marchini A47, Orienti M45
Affiliation:
1. Inst. de Astrofísica de Canarias and Dpto. Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain 2. Università di Udine and INFN Trieste, I-33100 Udine, Italy 3. National Institute for Astrophysics (INAF), I-00136 Rome, Italy 4. ETH Zürich, CH-8093 Zürich, Switzerland 5. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain 6. Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan 7. Technische Universität Dortmund, D-44221 Dortmund, Germany 8. Croatian MAGIC Group: Faculty of Electrical Engineering and Computing (FER), University of Zagreb, 10000 Zagreb, Croatia 9. IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, E-28040 Madrid, Spain 10. Centro Brasileiro de Pesquisas Físicas (CBPF), 22290-180 URCA, Rio de Janeiro (RJ), Brazil 11. Università di Padova and INFN, I-35131 Padova, Italy 12. Faculty of Physics and Applied Informatics, Department of Astrophysics, University of Lodz, PL-90-236 Lodz, Poland 13. Università di Siena and INFN Pisa, I-53100 Siena, Italy 14. Deutsches Elektronen-Synchrotron (DESY), D-15738 Zeuthen, Germany 15. INFN MAGIC Group: INFN Sezione di Torino and Università degli Studi di Torino, I-10125 Torino, Italy 16. Max-Planck-Institut für Physik, D-80805 München, Germany 17. Università di Pisa and INFN Pisa, I-56126 Pisa, Italy 18. ICCUB, IEEC-UB, Universitat de Barcelona, E-08028 Barcelona, Spain 19. Armenian MAGIC Group: A. Alikhanyan National Science Laboratory , 0036 Yerevan, Armenia 20. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain 21. Port d’Informació Científica (PIC), E-08193 Bellaterra (Barcelona), Spain 22. INFN MAGIC Group: INFN Sezione di Bari and Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari, I-70125 Bari, Italy 23. Croatian MAGIC Group: Department of Physics, University of Rijeka, 51000 Rijeka, Croatia 24. Universität Würzburg, D-97074 Würzburg, Germany 25. Finnish MAGIC Group: Finnish Centre for Astronomy with ESO, University of Turku, FI-20014 Turku, Finland 26. Ruhr-Universität Bochum, Fakultät fur Physik und Astronomie, AstronomischesInstitut (AIRUB), 44801 Bochum, Germany 27. Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain 28. Armenian MAGIC Group: ICRANet-Armenia at NAS RA , 0019 Yerevan, Armenia 29. Croatian MAGIC Group: Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture (FESB), University of Split, 21000 Split, Croatia 30. Croatian MAGIC Group: Department of Physics, Josip Juraj Strossmayer University of Osijek, 31000 Osijek, Croatia 31. Japanese MAGIC Group: RIKEN, Wako, Saitama 351-0198, Japan 32. Japanese MAGIC Group: Department of Physics, Kyoto University, 606-8502 Kyoto, Japan 33. Japanese MAGIC Group: Department of Physics, Tokai University, Hiratsuka, 259-1292 Kanagawa, Japan 34. Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy 35. Saha Institute of Nuclear Physics, HBNI, 1/AF Bidhannagar, Salt Lake, Sector-1, Kolkata 700064, India 36. Inst. for Nucl. Research and Nucl. Energy, Bulgarian Academy of Sciences, BG-1784 Sofia, Bulgaria 37. Finnish MAGIC Group: Astronomy Research Unit, University of Oulu, FI-90014 Oulu, Finland 38. INAF Trieste and Dept. of Physics and Astronomy, University of Bologna 39. Croatian MAGIC Group: Ruđer Bošković Institute, 10000 Zagreb, Croatia 40. INFN MAGIC Group: INFN Sezione di Perugia, I-06123 Perugia, Italy 41. INFN MAGIC Group: INFN Roma Tor Vergata, I-00133 Roma, Italy 42. Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari, I-70125 Bari, Italy 43. Instituto de Astrofísica de Andalucía (CSIC), Apartado 3004, E-18080 Granada, Spain 44. INFN Sezione di Perugia, I-06123 Perugia, Italy 45. INAF – Istituto di Radioastronomia, Via Gobetti 101, I-40129 Bologna, Italy 46. Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland 47. Università di Siena, I-53100, Siena, Italy
Abstract
ABSTRACT
We report here on the first multiwavelength (MWL) campaign on the blazar TXS 1515–273, undertaken in 2019 and extending from radio to very-high-energy gamma-rays (VHE). Up until now, this blazar had not been the subject of any detailed MWL observations. It has a rather hard photon index at GeV energies and was considered a candidate extreme high-synchrotron-peaked source. MAGIC observations resulted in the first-time detection of the source in VHE with a statistical significance of 7.6σ. The average integral VHE flux of the source is 6 ± 1 per cent of the Crab nebula flux above 400 GeV. X-ray coverage was provided by Swift-XRT, XMM–Newton, and NuSTAR. The long continuous X-ray observations were separated by ∼9 h, both showing clear hour scale flares. In the XMM–Newton data, both the rise and decay time-scales are longer in the soft X-ray than in the hard X-ray band, indicating the presence of a particle cooling regime. The X-ray variability time-scales were used to constrain the size of the emission region and the strength of the magnetic field. The data allowed us to determine the synchrotron peak frequency and classify the source as a flaring high, but not extreme synchrotron-peaked object. Considering the constraints and variability patterns from the X-ray data, we model the broad-band spectral energy distribution. We applied a simple one-zone model, which could not reproduce the radio emission and the shape of the optical emission, and a two-component leptonic model with two interacting components, enabling us to reproduce the emission from radio to VHE band.
Funder
BMBF MPG HGF INFN INAF SNF ERDF MICINN University of Tokyo JSPS MEXT Ministry of Education and Science Academy of Finland DFG National Research Centre MCTIC CNPq FAPERJ National Aeronautics and Space Administration Department of Energy Centre National de la Recherche Scientifique Institut National de Physique Nucléaire et de Physique des Particules Istituto Nazionale di Fisica Nucleare Ministry of Education, Culture, Sports, Science and Technology High Energy Accelerator Research Organization Japan Aerospace Exploration Agency Swedish Research Council Istituto Nazionale di Astrofisica Centre National d’Etudes Spatiales Astrophysics Science Division NASA GSFC
Publisher
Oxford University Press (OUP)
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
4 articles.
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