Studying the nature of the unidentified gamma-ray source HESS J1841−055 with the MAGIC telescopes
Author:
, Acciari V A1, Ansoldi S2, Antonelli L A3, Arbet Engels A4, Asano K5, Baack D6, Babić A7, Banerjee B8, Baquero A9, Barres de Almeida U10, Barrio J A9, Becerra González J111, Bednarek W12, Bellizzi L13, Bernardini E14, Bernardos M15, Berti A16, Besenrieder J17, Bhattacharyya W14, Bigongiari C3, Biland A4, Blanch O18, Bonnoli G13, Bošnjak Ž7, Busetto G19, Carosi R20, Ceribella G17, Cerruti M21, Chai Y17, Chilingarian A22, Cikota S7, Colak S M18, Colombo E1, Contreras J L9, Cortina J15, Covino S3, D’Amico G17, D’Elia V3, Da Vela P20, Dazzi F3, De Angelis A19, De Lotto B2, Delfino M18, Delgado J18, Delgado Mendez C15, Depaoli D16, Di Girolamo T16, Di Pierro F16, Di Venere L16, Do Souto Espiñeira E18, Dominis Prester D23, Donini A2, Dorner D24, Doro M19, Elsaesser D6, Fallah Ramazani V25, Fattorini A6, Ferrara G3, Foffano L19, Fonseca M V9, Font L26, Fruck C17, Fukami S5, García López R J111, Garczarczyk M14, Gasparyan S22, Gaug M26, Giglietto N16, Giordano F16, Gliwny P12, Godinović N27, Green D17, Hadasch D5, Hahn A17, Heckmann L17, Herrera J111, Hoang J9, Hrupec D28, Hütten M17, Inada T5, Inoue S5, Ishio K17, Iwamura Y5, Jouvin L18, Kajiwara Y29, Karjalainen M1, Kerszberg D18, Kobayashi Y5, Kubo H29, Kushida J30, Lamastra A3, Lelas D27, Leone F3, Lindfors E25, Lombardi S3, Longo F2, López M9, López-Coto R19, López-Oramas A111, Loporchio S16, Machado de Oliveira Fraga B10, Maggio C26, Majumdar P8, Makariev M31, Mallamaci M19, Maneva G31, Manganaro M23, Mannheim K24, Maraschi L3, Mariotti M19, Martínez M18, Mazin D5, Mender S6, Mićanović S23, Miceli D2, Miener T9, Minev M31, Miranda J M13, Mirzoyan R17, Molina E21, Moralejo A18, Morcuende D9, Moreno V26, Moretti E18, Munar-Adrover P26, Neustroev V32, Nigro C18, Nilsson K25, Ninci D18, Nishijima K30, Noda K5, Nozaki S29, Ohtani Y5, Oka T29, Otero-Santos J111, Palatiello M2, Paneque D17, Paoletti R13, Paredes J M21, Pavletić L23, Peñil P9, Perennes C19, Persic M2, Prada Moroni P G20, Prandini E19, Priyadarshi C18, Puljak I27, Rhode W6, Ribó M21, Rico J18, Righi C3, Rugliancich A20, Saha L9, Sahakyan N22, Saito T5, Sakurai S5, Satalecka K14, Schleicher B24, Schmidt K6, Schweizer T17, Sitarek J12, Šnidarić I33, Sobczynska D12, Spolon A19, Stamerra A3, Strom D17, Strzys M5, Suda Y17, Surić T33, Takahashi M5, Tavecchio F3, Temnikov P31, Terzić T23, Teshima M17, Torres-Albà N21, Tosti L16, Truzzi S13, van Scherpenberg J17, Vanzo G111, Vazquez Acosta M111, Ventura S13, Verguilov V31, Vigorito C F16, Vitale V16, Vovk I5, Will M17, Zarić D27
Affiliation:
1. Instituto de Astrofísica de Canarias, E-38200 La Laguna, Spain 2. Università di Udine, and INFN Trieste, I-33100 Udine, Italy 3. National Institute for Astrophysics (INAF), I-00136 Rome, Italy 4. ETH Zurich, CH-8093 Zurich, Switzerland 5. Japanese MAGIC Group: ICRR, The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan 6. Technische Universität Dortmund, D-44221 Dortmund, Germany 7. Croatian MAGIC Group: University of Zagreb, Faculty of Electrical Engineering and Computing (FER), 10000 Zagreb, Croatia 8. Saha Institute of Nuclear Physics, HBNI, 1/AF Bidhannagar, Salt Lake, Sector-1, Kolkata 700064, India 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. Departamento Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain 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. Centro de Investigaciones Energéticas, Meioambientales y Tecnológicas, E-28040 Madrid, Spain 16. Istituto Nazionale Fisica Nucleare (INFN), I-00044 Frascati (Roma), Italy 17. Max-Planck-Institut für Physik, D-80805 München, Germany 18. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain 19. Università di Padova and INFN, I-35131 Padova, Italy 20. Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy 21. Universitat de Barcelona, ICCUB, IEEC-UB, E-08028 Barcelona, Spain 22. Armenian MAGIC Group:ICRANet-Armenia at NAS RA, 0019, Yerevan, Armenia 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 of Astronomy with ESO, University of Turku, FI-20014 Turku, Finland 26. Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain 27. Croatian MAGIC Group: University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture (FESB), 21000 Split, Croatia 28. Croatian MAGIC Group: University of Osijek, 31000 Osijek, Croatia 29. Japanese MAGIC Group: Department of Physics, Kyoto University, 606-8502 Kyoto, Japan 30. Japanese MAGIC Group: Department of Physics, Tokai University, Hiratsuka, 259-1292 Kanagawa, Japan 31. Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, BG-1784 Sofia, Bulgaria 32. Finnish MAGIC Group: Astronomy Research Unit, University of Oulu, FI-90014 Oulu, Finland 33. Croatian MAGIC Group: Rudjer Boskovic Institute, 10000 Zagreb, Croatia
Abstract
ABSTRACT
We investigate the physical nature and origin of the gamma-ray emission from the extended source HESS J1841−055 observed at TeV and GeV energies. We observed HESS J1841−055 at TeV energies for a total effective time of 43 h with the MAGIC telescopes, in 2012 and 2013. Additionally, we analysed the GeV counterpart making use of about 10 yr of Fermi-LAT data. Using both Fermi-LAT and MAGIC, we study both the spectral and energy-dependent morphology of the source for almost four decades of energy. The origin of the gamma-ray emission from this region is investigated using multiwaveband information on sources present in this region, suggested to be associated with this unidentified gamma-ray source. We find that the extended emission at GeV–TeV energies is best described by more than one source model. We also perform the first energy-dependent analysis of the HESS J1841−055 region at GeV–TeV. We find that the emission at lower energies comes from a diffuse or extended component, while the major contribution of gamma rays above 1 TeV arises from the southern part of the source. Moreover, we find that a significant curvature is present in the combined observed spectrum of MAGIC and Fermi-LAT. The first multiwavelength spectral energy distribution of this unidentified source shows that the emission at GeV–TeV energies can be well explained with both leptonic and hadronic models. For the leptonic scenario, bremsstrahlung is the dominant emission compared to inverse Compton. On the other hand, for the hadronic model, gamma-ray resulting from the decay of neutral pions (π0) can explain the observed spectrum. The presence of dense molecular clouds overlapping with HESS J1841−055 makes both bremsstrahlung and π0-decay processes the dominant emission mechanisms for the source.
Funder
Bundesministerium für Bildung und Forschung Max-Planck-Gesellschaft Instituto Nazionale di Fisica Nucleare Institut sur la Nutrition et les Aliments Fonctionnels Statens Naturvidenskabelige Forskningsrad Ministerio de Economía y Competitividad Japan Society for the Promotion of Science Ministry of Education, Culture, Sports, Science and Technology Hrvatska Zaklada za Znanost Deutsche Forschungsgemeinschaft National Science Foundation
Publisher
Oxford University Press (OUP)
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
4 articles.
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