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    Search for Gamma-Ray Spectral Lines from Dark Matter Annihilation up to 100 TeV toward the Galactic Center with MAGIC

    H. Abe1, S. Abe1, V. A. Acciari2, T. Aniello3, S. Ansoldi4,†, L. A. Antonelli3, A. Arbet Engels5, C. Arcaro6, M. Artero7 et al. (MAGIC Collaboration)

    M. Artero7, K. Asano1, D. Baack8, A. Babić9, A. Baquero10, U. Barres de Almeida11, J. A. Barrio10, I. Batković6, J. Baxter1, J. Becerra González2, W. Bednarek12, E. Bernardini6, M. Bernardos13, A. Berti5, J. Besenrieder5, W. Bhattacharyya14, C. Bigongiari3, A. Biland15, O. Blanch7, G. Bonnoli3, Ž. Bošnjak9, I. Burelli4, G. Busetto6, R. Carosi16, M. Carretero-Castrillo17, G. Ceribella1, Y. Chai5, A. Chilingarian18, S. Cikota9, E. Colombo2, J. L. Contreras10, J. Cortina19, S. Covino3, G. D’Amico20, V. D’Elia3, P. Da Vela16,‡, F. Dazzi3, A. De Angelis6, B. De Lotto4, A. Del Popolo21, M. Delfino7,§, J. Delgado7,§, C. Delgado Mendez19, D. Depaoli22, F. Di Pierro22, L. Di Venere23, E. Do Souto Espiñeira7, D. Dominis Prester24, A. Donini3, D. Dorner25, M. Doro6, D. Elsaesser8, G. Emery26, V. Fallah Ramazani27,∥, L. Fariña7, A. Fattorini8, L. Font28, C. Fruck5, S. Fukami15, Y. Fukazawa29, R. J. García López2, M. Garczarczyk14, S. Gasparyan30, M. Gaug28, J. G. Giesbrecht Paiva11, N. Giglietto23, F. Giordano23, P. Gliwny12, N. Godinović31, J. G. Green5, D. Green5, D. Hadasch1, A. Hahn5, T. Hassan19, L. Heckmann5,¶, J. Herrera2, D. Hrupec32, M. Hütten1,*, R. Imazawa29, T. Inada1,*, R. Iotov25, K. Ishio12, I. Jiménez Martínez19, J. Jormanainen27, D. Kerszberg7,*, Y. Kobayashi1, H. Kubo1, J. Kushida33, A. Lamastra3, D. Lelas31, F. Leone3, E. Lindfors27, L. Linhoff8, S. Lombardi3, F. Longo4,**, R. López-Coto6, M. López-Moya10, A. López-Oramas2, S. Loporchio23, A. Lorini34, E. Lyard26, B. Machado de Oliveira Fraga11, P. Majumdar35,††, M. Makariev36, G. Maneva36, N. Mang8, M. Manganaro24, S. Mangano19, K. Mannheim25, M. Mariotti6, M. Martínez7, A. Mas Aguilar10, D. Mazin1,5, S. Menchiari34, S. Mender8, S. Mićanović24, D. Miceli6, T. Miener10, J. M. Miranda34, R. Mirzoyan5, E. Molina17, H. A. Mondal35, A. Moralejo7, D. Morcuende10, V. Moreno28, T. Nakamori37, C. Nanci3, L. Nava3, V. Neustroev38, M. Nievas Rosillo2, C. Nigro7, K. Nilsson27, K. Nishijima33, T. Njoh Ekoume2, K. Noda1, S. Nozaki5, Y. Ohtani1, T. Oka39, J. Otero-Santos2, S. Paiano3, M. Palatiello4, D. Paneque5, R. Paoletti34, J. M. Paredes17, L. Pavletić24, M. Persic4,‡‡, M. Pihet5, F. Podobnik34, P. G. Prada Moroni16, E. Prandini6, G. Principe4, C. Priyadarshi7, I. Puljak31, W. Rhode8, M. Ribó17, J. Rico7, C. Righi3, A. Rugliancich16, N. Sahakyan30, T. Saito1, S. Sakurai1, K. Satalecka27, F. G. Saturni3, B. Schleicher25, K. Schmidt8, F. Schmuckermaier5, J. L. Schubert8, T. Schweizer5, J. Sitarek12, V. Sliusar26, D. Sobczynska12, A. Spolon6, A. Stamerra3, J. Strišković32, D. Strom5, M. Strzys1, Y. Suda29, T. Surić40, M. Takahashi41, R. Takeishi1, F. Tavecchio3, P. Temnikov36, K. Terauchi39, T. Terzić24, M. Teshima5,1, L. Tosti42, S. Truzzi34, A. Tutone3, S. Ubach28, J. van Scherpenberg5, M. Vazquez Acosta2, S. Ventura34, V. Verguilov36, I. Viale6, C. F. Vigorito22, V. Vitale43, I. Vovk1, R. Walter26, M. Will5, C. Wunderlich34, T. Yamamoto44, D. Zarić31, N. Hiroshima45,46, and K. Kohri47,48,49 (MAGIC Collaboration)

    • 1Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
    • 2Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
    • 3National Institute for Astrophysics (INAF), I-00136 Rome, Italy
    • 4Università di Udine and INFN Trieste, I-33100 Udine, Italy
    • 5Max-Planck-Institut für Physik, D-80805 München, Germany
    • 6Università di Padova and INFN, I-35131 Padova, Italy
    • 7Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
    • 8Technische Universität Dortmund, D-44221 Dortmund, Germany
    • 9Croatian MAGIC Group: University of Zagreb, Faculty of Electrical Engineering and Computing (FER), 10000 Zagreb, Croatia
    • 10IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, E-28040 Madrid, Spain
    • 11Centro Brasileiro de Pesquisas Físicas (CBPF), 22290-180 URCA, Rio de Janeiro (RJ), Brazil
    • 12University of Lodz, Faculty of Physics and Applied Informatics, Department of Astrophysics, 90-236 Lodz, Poland
    • 13Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
    • 14Deutsches Elektronen-Synchrotron (DESY), D-15738 Zeuthen, Germany
    • 15ETH Zürich, CH-8093 Zürich, Switzerland
    • 16Università di Pisa and INFN Pisa, I-56126 Pisa, Italy
    • 17Universitat de Barcelona, ICCUB, IEEC-UB, E-08028 Barcelona, Spain
    • 18Armenian MAGIC Group: A. Alikhanyan National Science Laboratory, 0036 Yerevan, Armenia
    • 19Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain
    • 20Department for Physics and Technology, University of Bergen, Norway
    • 21INFN MAGIC Group: INFN Sezione di Catania and Dipartimento di Fisica e Astronomia, University of Catania, I-95123 Catania, Italy
    • 22INFN MAGIC Group: INFN Sezione di Torino and Università degli Studi di Torino, I-10125 Torino, Italy
    • 23INFN MAGIC Group: INFN Sezione di Bari and Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari, I-70125 Bari, Italy
    • 24Croatian MAGIC Group: University of Rijeka, Department of Physics, 51000 Rijeka, Croatia
    • 25Universität Würzburg, D-97074 Würzburg, Germany
    • 26University of Geneva, Chemin d’Ecogia 16, CH-1290 Versoix, Switzerland
    • 27Finnish MAGIC Group: Finnish Centre for Astronomy with ESO, University of Turku, FI-20014 Turku, Finland
    • 28Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain
    • 29Japanese MAGIC Group: Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 739-8526 Hiroshima, Japan
    • 30Armenian MAGIC Group: ICRANet-Armenia at NAS RA, 0019 Yerevan, Armenia
    • 31Croatian MAGIC Group: University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture (FESB), 21000 Split, Croatia
    • 32Croatian MAGIC Group: Josip Juraj Strossmayer University of Osijek, Department of Physics, 31000 Osijek, Croatia
    • 33Japanese MAGIC Group: Department of Physics, Tokai University, Hiratsuka, 259-1292 Kanagawa, Japan
    • 34Università di Siena and INFN Pisa, I-53100 Siena, Italy
    • 35Saha Institute of Nuclear Physics, A CI of Homi Bhabha National Institute, Kolkata 700064, West Bengal, India
    • 36Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, BG-1784 Sofia, Bulgaria
    • 37Japanese MAGIC Group: Department of Physics, Yamagata University, Yamagata 990-8560, Japan
    • 38Finnish MAGIC Group: Space Physics and Astronomy Research Unit, University of Oulu, FI-90014 Oulu, Finland
    • 39Japanese MAGIC Group: Department of Physics, Kyoto University, 606-8502 Kyoto, Japan
    • 40Croatian MAGIC Group: Ruđer Bošković Institute, 10000 Zagreb, Croatia
    • 41Japanese MAGIC Group: Institute for Space-Earth Environmental Research and Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, 464-6801 Nagoya, Japan
    • 42INFN MAGIC Group: INFN Sezione di Perugia, I-06123 Perugia, Italy
    • 43INFN MAGIC Group: INFN Roma Tor Vergata, I-00133 Roma, Italy
    • 44Japanese MAGIC Group: Department of Physics, Konan University, Kobe, Hyogo 658-8501, Japan
    • 45Department of Physics, University of Toyama, 3190 Gofuku, Toyama 930-8555, Japan
    • 46RIKEN iTHEMS, Wako, Saitama 351-0198, Japan
    • 47Theory Center, IPNS, KEK, Tsukuba, Ibaraki 305-0801, Japan
    • 48The Graduate University for Advanced Studies (SOKENDAI), 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan
    • 49Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan

    • *Corresponding authors. (T. Inada, D. Kerszberg, M. Hütten) contact.magic@mpp.mpg.de
    • †Also at International Center for Relativistic Astrophysics (ICRA), Rome, Italy.
    • ‡Present address: University of Innsbruck, Institute for Astro and Particle Physics.
    • §Also at Port d’Informació Científica (PIC), E-08193 Bellaterra (Barcelona), Spain.
    • ∥Present address: Ruhr-Universität Bochum, Fakultät für Physik und Astronomie, Astronomisches Institut (AIRUB), 44801 Bochum, Germany.
    • Also at University of Innsbruck, Institute for Astro- and Particle Physics.
    • **Also at Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy.
    • ††Also at University of Lodz, Faculty of Physics and Applied Informatics, Department of Astrophysics, 90-236 Lodz, Poland.
    • ‡‡Also at INAF-Padova, Padova, Italy.
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    Phys. Rev. Lett. 130, 061002 – Published 10 February, 2023

    DOI: https://doi.org/10.1103/PhysRevLett.130.061002

    Abstract

    Linelike features in TeV γ rays constitute a “smoking gun” for TeV-scale particle dark matter and new physics. Probing the Galactic Center region with ground-based Cherenkov telescopes enables the search for TeV spectral features in immediate association with a dense dark matter reservoir at a sensitivity out of reach for satellite γ-ray detectors, and direct detection and collider experiments. We report on 223 hours of observations of the Galactic Center region with the MAGIC stereoscopic telescope system reaching γ-ray energies up to 100 TeV. We improved the sensitivity to spectral lines at high energies using large-zenith-angle observations and a novel background modeling method within a maximum-likelihood analysis in the energy domain. No linelike spectral feature is found in our analysis. Therefore, we constrain the cross section for dark matter annihilation into two photons to ⟨σv⟩≲5×10−28  cm3 s−1 at 1 TeV and ⟨σv⟩≲1×10−25  cm3 s−1 at 100 TeV, achieving the best limits to date for a dark matter mass above 20 TeV and a cuspy dark matter profile at the Galactic Center. Finally, we use the derived limits for both cuspy and cored dark matter profiles to constrain supersymmetric wino models.

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    Phys. Rev. Lett. 130, 061002– Published 10 February, 2023
    • Received 10 June 2022
    • Revised 2 November 2022
    • Accepted 15 December 2022
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