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Lucie-Smith L, Peiris HV, Pontzen A. Explaining Dark Matter Halo Density Profiles with Neural Networks. PHYSICAL REVIEW LETTERS 2024; 132:031001. [PMID: 38307055 DOI: 10.1103/physrevlett.132.031001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/12/2023] [Revised: 09/04/2023] [Accepted: 12/20/2023] [Indexed: 02/04/2024]
Abstract
We use explainable neural networks to connect the evolutionary history of dark matter halos with their density profiles. The network captures independent factors of variation in the density profiles within a low-dimensional representation, which we physically interpret using mutual information. Without any prior knowledge of the halos' evolution, the network recovers the known relation between the early time assembly and the inner profile and discovers that the profile beyond the virial radius is described by a single parameter capturing the most recent mass accretion rate. The results illustrate the potential for machine-assisted scientific discovery in complicated astrophysical datasets.
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Affiliation(s)
- Luisa Lucie-Smith
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
| | - Hiranya V Peiris
- Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, United Kingdom
- The Oskar Klein Centre for Cosmoparticle Physics, Stockholm University, AlbaNova, Stockholm SE-106 91, Sweden
| | - Andrew Pontzen
- Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, United Kingdom
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Abe H, Abe S, Acciari VA, Aniello T, Ansoldi S, Antonelli LA, Arbet Engels A, Arcaro C, Artero M, Asano K, Baack D, Babić A, Baquero A, Barres de Almeida U, Barrio JA, Batković I, Baxter J, Becerra González J, Bednarek W, Bernardini E, Bernardos M, Berti A, Besenrieder J, Bhattacharyya W, Bigongiari C, Biland A, Blanch O, Bonnoli G, Bošnjak Ž, Burelli I, Busetto G, Carosi R, Carretero-Castrillo M, Ceribella G, Chai Y, Chilingarian A, Cikota S, Colombo E, Contreras JL, Cortina J, Covino S, D'Amico G, D'Elia V, Da Vela P, Dazzi F, De Angelis A, De Lotto B, Del Popolo A, Delfino M, Delgado J, Delgado Mendez C, Depaoli D, Di Pierro F, Di Venere L, Do Souto Espiñeira E, Dominis Prester D, Donini A, Dorner D, Doro M, Elsaesser D, Emery G, Fallah Ramazani V, Fariña L, Fattorini A, Font L, Fruck C, Fukami S, Fukazawa Y, García López RJ, Garczarczyk M, Gasparyan S, Gaug M, Giesbrecht Paiva JG, Giglietto N, Giordano F, Gliwny P, Godinović N, Green JG, Green D, Hadasch D, Hahn A, Hassan T, Heckmann L, Herrera J, Hrupec D, Hütten M, Imazawa R, Inada T, Iotov R, Ishio K, Jiménez Martínez I, Jormanainen J, Kerszberg D, Kobayashi Y, Kubo H, Kushida J, Lamastra A, Lelas D, Leone F, Lindfors E, Linhoff L, Lombardi S, Longo F, López-Coto R, López-Moya M, López-Oramas A, Loporchio S, Lorini A, Lyard E, Machado de Oliveira Fraga B, Majumdar P, Makariev M, Maneva G, Mang N, Manganaro M, Mangano S, Mannheim K, Mariotti M, Martínez M, Mas Aguilar A, Mazin D, Menchiari S, Mender S, Mićanović S, Miceli D, Miener T, Miranda JM, Mirzoyan R, Molina E, Mondal HA, Moralejo A, Morcuende D, Moreno V, Nakamori T, Nanci C, Nava L, Neustroev V, Nievas Rosillo M, Nigro C, Nilsson K, Nishijima K, Njoh Ekoume T, Noda K, Nozaki S, Ohtani Y, Oka T, Otero-Santos J, Paiano S, Palatiello M, Paneque D, Paoletti R, Paredes JM, Pavletić L, Persic M, Pihet M, Podobnik F, Prada Moroni PG, Prandini E, Principe G, Priyadarshi C, Puljak I, Rhode W, Ribó M, Rico J, Righi C, Rugliancich A, Sahakyan N, Saito T, Sakurai S, Satalecka K, Saturni FG, Schleicher B, Schmidt K, Schmuckermaier F, Schubert JL, Schweizer T, Sitarek J, Sliusar V, Sobczynska D, Spolon A, Stamerra A, Strišković J, Strom D, Strzys M, Suda Y, Surić T, Takahashi M, Takeishi R, Tavecchio F, Temnikov P, Terauchi K, Terzić T, Teshima M, Tosti L, Truzzi S, Tutone A, Ubach S, van Scherpenberg J, Vazquez Acosta M, Ventura S, Verguilov V, Viale I, Vigorito CF, Vitale V, Vovk I, Walter R, Will M, Wunderlich C, Yamamoto T, Zarić D, Hiroshima N, Kohri K. Search for Gamma-Ray Spectral Lines from Dark Matter Annihilation up to 100 TeV toward the Galactic Center with MAGIC. PHYSICAL REVIEW LETTERS 2023; 130:061002. [PMID: 36827578 DOI: 10.1103/physrevlett.130.061002] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/10/2022] [Revised: 11/02/2022] [Accepted: 12/15/2022] [Indexed: 06/18/2023]
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} cm^{3} s^{-1} at 1 TeV and ⟨σv⟩≲1×10^{-25} cm^{3} 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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Affiliation(s)
- H Abe
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - S Abe
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - V A Acciari
- Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
| | - T Aniello
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - S Ansoldi
- Università di Udine and INFN Trieste, I-33100 Udine, Italy
| | - L A Antonelli
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - A Arbet Engels
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - C Arcaro
- Università di Padova and INFN, I-35131 Padova, Italy
| | - M Artero
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - K Asano
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - D Baack
- Technische Universität Dortmund, D-44221 Dortmund, Germany
| | - A Babić
- Croatian MAGIC Group: University of Zagreb, Faculty of Electrical Engineering and Computing (FER), 10000 Zagreb, Croatia
| | - A Baquero
- IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, E-28040 Madrid, Spain
| | - U Barres de Almeida
- Centro Brasileiro de Pesquisas Físicas (CBPF), 22290-180 URCA, Rio de Janeiro (RJ), Brazil
| | - J A Barrio
- IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, E-28040 Madrid, Spain
| | - I Batković
- Università di Padova and INFN, I-35131 Padova, Italy
| | - J Baxter
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - J Becerra González
- Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
| | - W Bednarek
- University of Lodz, Faculty of Physics and Applied Informatics, Department of Astrophysics, 90-236 Lodz, Poland
| | - E Bernardini
- Università di Padova and INFN, I-35131 Padova, Italy
| | - M Bernardos
- Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - A Berti
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - J Besenrieder
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - W Bhattacharyya
- Deutsches Elektronen-Synchrotron (DESY), D-15738 Zeuthen, Germany
| | - C Bigongiari
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - A Biland
- ETH Zürich, CH-8093 Zürich, Switzerland
| | - O Blanch
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - G Bonnoli
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - Ž Bošnjak
- Croatian MAGIC Group: University of Zagreb, Faculty of Electrical Engineering and Computing (FER), 10000 Zagreb, Croatia
| | - I Burelli
- Università di Udine and INFN Trieste, I-33100 Udine, Italy
| | - G Busetto
- Università di Padova and INFN, I-35131 Padova, Italy
| | - R Carosi
- Università di Pisa and INFN Pisa, I-56126 Pisa, Italy
| | | | - G Ceribella
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - Y Chai
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - A Chilingarian
- Armenian MAGIC Group: A. Alikhanyan National Science Laboratory, 0036 Yerevan, Armenia
| | - S Cikota
- Croatian MAGIC Group: University of Zagreb, Faculty of Electrical Engineering and Computing (FER), 10000 Zagreb, Croatia
| | - E Colombo
- Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
| | - J L Contreras
- IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, E-28040 Madrid, Spain
| | - J Cortina
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain
| | - S Covino
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - G D'Amico
- Department for Physics and Technology, University of Bergen, Norway
| | - V D'Elia
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - P Da Vela
- Università di Pisa and INFN Pisa, I-56126 Pisa, Italy
| | - F Dazzi
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - A De Angelis
- Università di Padova and INFN, I-35131 Padova, Italy
| | - B De Lotto
- Università di Udine and INFN Trieste, I-33100 Udine, Italy
| | - A Del Popolo
- INFN MAGIC Group: INFN Sezione di Catania and Dipartimento di Fisica e Astronomia, University of Catania, I-95123 Catania, Italy
| | - M Delfino
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - J Delgado
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - C Delgado Mendez
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain
| | - D Depaoli
- INFN MAGIC Group: INFN Sezione di Torino and Università degli Studi di Torino, I-10125 Torino, Italy
| | - F Di Pierro
- INFN MAGIC Group: INFN Sezione di Torino and Università degli Studi di Torino, I-10125 Torino, Italy
| | - L Di Venere
- INFN MAGIC Group: INFN Sezione di Bari and Dipartimento Interateneo di Fisica dell'Università e del Politecnico di Bari, I-70125 Bari, Italy
| | - E Do Souto Espiñeira
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - D Dominis Prester
- Croatian MAGIC Group: University of Rijeka, Department of Physics, 51000 Rijeka, Croatia
| | - A Donini
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - D Dorner
- Universität Würzburg, D-97074 Würzburg, Germany
| | - M Doro
- Università di Padova and INFN, I-35131 Padova, Italy
| | - D Elsaesser
- Technische Universität Dortmund, D-44221 Dortmund, Germany
| | - G Emery
- University of Geneva, Chemin d'Ecogia 16, CH-1290 Versoix, Switzerland
| | - V Fallah Ramazani
- Finnish MAGIC Group: Finnish Centre for Astronomy with ESO, University of Turku, FI-20014 Turku, Finland
| | - L Fariña
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - A Fattorini
- Technische Universität Dortmund, D-44221 Dortmund, Germany
| | - L Font
- Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain
| | - C Fruck
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - S Fukami
- ETH Zürich, CH-8093 Zürich, Switzerland
| | - Y Fukazawa
- Japanese MAGIC Group: Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 739-8526 Hiroshima, Japan
| | - R J García López
- Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
| | - M Garczarczyk
- Deutsches Elektronen-Synchrotron (DESY), D-15738 Zeuthen, Germany
| | - S Gasparyan
- Armenian MAGIC Group: ICRANet-Armenia at NAS RA, 0019 Yerevan, Armenia
| | - M Gaug
- Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain
| | - J G Giesbrecht Paiva
- Centro Brasileiro de Pesquisas Físicas (CBPF), 22290-180 URCA, Rio de Janeiro (RJ), Brazil
| | - N Giglietto
- INFN MAGIC Group: INFN Sezione di Bari and Dipartimento Interateneo di Fisica dell'Università e del Politecnico di Bari, I-70125 Bari, Italy
| | - F Giordano
- INFN MAGIC Group: INFN Sezione di Bari and Dipartimento Interateneo di Fisica dell'Università e del Politecnico di Bari, I-70125 Bari, Italy
| | - P Gliwny
- University of Lodz, Faculty of Physics and Applied Informatics, Department of Astrophysics, 90-236 Lodz, Poland
| | - N Godinović
- Croatian MAGIC Group: University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture (FESB), 21000 Split, Croatia
| | - J G Green
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - D Green
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - D Hadasch
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - A Hahn
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - T Hassan
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain
| | - L Heckmann
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - J Herrera
- Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
| | - D Hrupec
- Croatian MAGIC Group: Josip Juraj Strossmayer University of Osijek, Department of Physics, 31000 Osijek, Croatia
| | - M Hütten
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - R Imazawa
- Japanese MAGIC Group: Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 739-8526 Hiroshima, Japan
| | - T Inada
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - R Iotov
- Universität Würzburg, D-97074 Würzburg, Germany
| | - K Ishio
- University of Lodz, Faculty of Physics and Applied Informatics, Department of Astrophysics, 90-236 Lodz, Poland
| | - I Jiménez Martínez
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain
| | - J Jormanainen
- Finnish MAGIC Group: Finnish Centre for Astronomy with ESO, University of Turku, FI-20014 Turku, Finland
| | - D Kerszberg
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - Y Kobayashi
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - H Kubo
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - J Kushida
- Japanese MAGIC Group: Department of Physics, Tokai University, Hiratsuka, 259-1292 Kanagawa, Japan
| | - A Lamastra
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - D Lelas
- Croatian MAGIC Group: University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture (FESB), 21000 Split, Croatia
| | - F Leone
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - E Lindfors
- Finnish MAGIC Group: Finnish Centre for Astronomy with ESO, University of Turku, FI-20014 Turku, Finland
| | - L Linhoff
- Technische Universität Dortmund, D-44221 Dortmund, Germany
| | - S Lombardi
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - F Longo
- Università di Udine and INFN Trieste, I-33100 Udine, Italy
| | - R López-Coto
- Università di Padova and INFN, I-35131 Padova, Italy
| | - M López-Moya
- IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, E-28040 Madrid, Spain
| | - A López-Oramas
- Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
| | - S Loporchio
- INFN MAGIC Group: INFN Sezione di Bari and Dipartimento Interateneo di Fisica dell'Università e del Politecnico di Bari, I-70125 Bari, Italy
| | - A Lorini
- Università di Siena and INFN Pisa, I-53100 Siena, Italy
| | - E Lyard
- University of Geneva, Chemin d'Ecogia 16, CH-1290 Versoix, Switzerland
| | | | - P Majumdar
- Saha Institute of Nuclear Physics, A CI of Homi Bhabha National Institute, Kolkata 700064, West Bengal, India
| | - M Makariev
- Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, BG-1784 Sofia, Bulgaria
| | - G Maneva
- Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, BG-1784 Sofia, Bulgaria
| | - N Mang
- Technische Universität Dortmund, D-44221 Dortmund, Germany
| | - M Manganaro
- Croatian MAGIC Group: University of Rijeka, Department of Physics, 51000 Rijeka, Croatia
| | - S Mangano
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, E-28040 Madrid, Spain
| | - K Mannheim
- Universität Würzburg, D-97074 Würzburg, Germany
| | - M Mariotti
- Università di Padova and INFN, I-35131 Padova, Italy
| | - M Martínez
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - A Mas Aguilar
- IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, E-28040 Madrid, Spain
| | - D Mazin
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - S Menchiari
- Università di Siena and INFN Pisa, I-53100 Siena, Italy
| | - S Mender
- Technische Universität Dortmund, D-44221 Dortmund, Germany
| | - S Mićanović
- Croatian MAGIC Group: University of Rijeka, Department of Physics, 51000 Rijeka, Croatia
| | - D Miceli
- Università di Padova and INFN, I-35131 Padova, Italy
| | - T Miener
- IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, E-28040 Madrid, Spain
| | - J M Miranda
- Università di Siena and INFN Pisa, I-53100 Siena, Italy
| | - R Mirzoyan
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - E Molina
- Universitat de Barcelona, ICCUB, IEEC-UB, E-08028 Barcelona, Spain
| | - H A Mondal
- Saha Institute of Nuclear Physics, A CI of Homi Bhabha National Institute, Kolkata 700064, West Bengal, India
| | - A Moralejo
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - D Morcuende
- IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid, E-28040 Madrid, Spain
| | - V Moreno
- Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain
| | - T Nakamori
- Japanese MAGIC Group: Department of Physics, Yamagata University, Yamagata 990-8560, Japan
| | - C Nanci
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - L Nava
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - V Neustroev
- Finnish MAGIC Group: Space Physics and Astronomy Research Unit, University of Oulu, FI-90014 Oulu, Finland
| | - M Nievas Rosillo
- Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
| | - C Nigro
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - K Nilsson
- Finnish MAGIC Group: Finnish Centre for Astronomy with ESO, University of Turku, FI-20014 Turku, Finland
| | - K Nishijima
- Japanese MAGIC Group: Department of Physics, Tokai University, Hiratsuka, 259-1292 Kanagawa, Japan
| | - T Njoh Ekoume
- Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
| | - K Noda
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - S Nozaki
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - Y Ohtani
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - T Oka
- Japanese MAGIC Group: Department of Physics, Kyoto University, 606-8502 Kyoto, Japan
| | - J Otero-Santos
- Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
| | - S Paiano
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - M Palatiello
- Università di Udine and INFN Trieste, I-33100 Udine, Italy
| | - D Paneque
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - R Paoletti
- Università di Siena and INFN Pisa, I-53100 Siena, Italy
| | - J M Paredes
- Universitat de Barcelona, ICCUB, IEEC-UB, E-08028 Barcelona, Spain
| | - L Pavletić
- Croatian MAGIC Group: University of Rijeka, Department of Physics, 51000 Rijeka, Croatia
| | - M Persic
- Università di Udine and INFN Trieste, I-33100 Udine, Italy
| | - M Pihet
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - F Podobnik
- Università di Siena and INFN Pisa, I-53100 Siena, Italy
| | | | - E Prandini
- Università di Padova and INFN, I-35131 Padova, Italy
| | - G Principe
- Università di Udine and INFN Trieste, I-33100 Udine, Italy
| | - C Priyadarshi
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - I Puljak
- Croatian MAGIC Group: University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture (FESB), 21000 Split, Croatia
| | - W Rhode
- Technische Universität Dortmund, D-44221 Dortmund, Germany
| | - M Ribó
- Universitat de Barcelona, ICCUB, IEEC-UB, E-08028 Barcelona, Spain
| | - J Rico
- Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology (BIST), E-08193 Bellaterra (Barcelona), Spain
| | - C Righi
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - A Rugliancich
- Università di Pisa and INFN Pisa, I-56126 Pisa, Italy
| | - N Sahakyan
- Armenian MAGIC Group: ICRANet-Armenia at NAS RA, 0019 Yerevan, Armenia
| | - T Saito
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - S Sakurai
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - K Satalecka
- Finnish MAGIC Group: Finnish Centre for Astronomy with ESO, University of Turku, FI-20014 Turku, Finland
| | - F G Saturni
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | | | - K Schmidt
- Technische Universität Dortmund, D-44221 Dortmund, Germany
| | | | - J L Schubert
- Technische Universität Dortmund, D-44221 Dortmund, Germany
| | - T Schweizer
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - J Sitarek
- University of Lodz, Faculty of Physics and Applied Informatics, Department of Astrophysics, 90-236 Lodz, Poland
| | - V Sliusar
- University of Geneva, Chemin d'Ecogia 16, CH-1290 Versoix, Switzerland
| | - D Sobczynska
- University of Lodz, Faculty of Physics and Applied Informatics, Department of Astrophysics, 90-236 Lodz, Poland
| | - A Spolon
- Università di Padova and INFN, I-35131 Padova, Italy
| | - A Stamerra
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - J Strišković
- Croatian MAGIC Group: Josip Juraj Strossmayer University of Osijek, Department of Physics, 31000 Osijek, Croatia
| | - D Strom
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - M Strzys
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - Y Suda
- Japanese MAGIC Group: Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 739-8526 Hiroshima, Japan
| | - T Surić
- Croatian MAGIC Group: Ruđer Bošković Institute, 10000 Zagreb, Croatia
| | - M Takahashi
- Japanese 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
| | - R Takeishi
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - F Tavecchio
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - P Temnikov
- Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, BG-1784 Sofia, Bulgaria
| | - K Terauchi
- Japanese MAGIC Group: Department of Physics, Kyoto University, 606-8502 Kyoto, Japan
| | - T Terzić
- Croatian MAGIC Group: University of Rijeka, Department of Physics, 51000 Rijeka, Croatia
| | - M Teshima
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - L Tosti
- INFN MAGIC Group: INFN Sezione di Perugia, I-06123 Perugia, Italy
| | - S Truzzi
- Università di Siena and INFN Pisa, I-53100 Siena, Italy
| | - A Tutone
- National Institute for Astrophysics (INAF), I-00136 Rome, Italy
| | - S Ubach
- Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain
| | | | - M Vazquez Acosta
- Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain
| | - S Ventura
- Università di Siena and INFN Pisa, I-53100 Siena, Italy
| | - V Verguilov
- Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, BG-1784 Sofia, Bulgaria
| | - I Viale
- Università di Padova and INFN, I-35131 Padova, Italy
| | - C F Vigorito
- INFN MAGIC Group: INFN Sezione di Torino and Università degli Studi di Torino, I-10125 Torino, Italy
| | - V Vitale
- INFN MAGIC Group: INFN Roma Tor Vergata, I-00133 Roma, Italy
| | - I Vovk
- Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR), The University of Tokyo, Kashiwa, 277-8582 Chiba, Japan
| | - R Walter
- University of Geneva, Chemin d'Ecogia 16, CH-1290 Versoix, Switzerland
| | - M Will
- Max-Planck-Institut für Physik, D-80805 München, Germany
| | - C Wunderlich
- Università di Siena and INFN Pisa, I-53100 Siena, Italy
| | - T Yamamoto
- Japanese MAGIC Group: Department of Physics, Konan University, Kobe, Hyogo 658-8501, Japan
| | - D Zarić
- Croatian MAGIC Group: University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture (FESB), 21000 Split, Croatia
| | - N Hiroshima
- Department of Physics, University of Toyama, 3190 Gofuku, Toyama 930-8555, Japan
- RIKEN iTHEMS, Wako, Saitama 351-0198, Japan
| | - K Kohri
- Theory Center, IPNS, KEK, Tsukuba, Ibaraki 305-0801, Japan
- The Graduate University for Advanced Studies (SOKENDAI), 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan
- Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
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3
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Abstract
This review deals with the inconsistency of inner dark matter density profiles in dwarf galaxies, known as the cusp–core problem. In particular, we aim to focus on gas-poor dwarf galaxies. One of the most promising solutions to this cold dark matter small-scale issue is the stellar feedback, but it seems to be only designed for gas-rich dwarfs. However, in the regime of classical dwarfs, this core mechanism becomes negligible. Therefore, it is required to find solutions without invoking these baryonic processes as dark matter cores tend to persist even for these dwarfs, which are rather dark-matter-dominated. Here, we have presented two categories of solutions. One consists of creating dark matter cores from cusps within cold dark matter by altering the dark matter potential via perturbers. The second category gathers solutions that depict the natural emergence of dark matter cores in alternative theories. Given the wide variety of solutions, it becomes necessary to identify which mechanism dominates in the central region of galaxies by finding observational signatures left by them in order to highlight the true nature of dark matter.
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4
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Abstract
This review aims at proposing to the field an overview of the Cusp-core problem, including a discussion of its advocated solutions, assessing how each can satisfactorily provide a description of central densities. Whether the Cusp-core problem reflects our insufficient grasp on the nature of dark matter, of gravity, on the impact of baryonic interactions with dark matter at those scales, as included in semi-analytical models or fully numerical codes, the solutions to it can point either to the need for a paradigm change in cosmology, or to to our lack of success in ironing out the finer details of the ΛCDM paradigm.
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5
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Fundamental Properties of the Dark and the Luminous Matter from the Low Surface Brightness Discs. UNIVERSE 2021. [DOI: 10.3390/universe7090344] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
Dark matter (DM) is one of the biggest mystery in the Universe. In this review, we start reporting the evidences for this elusive component and discussing about the proposed particle candidates and scenarios for such phenomenon. Then, we focus on recent results obtained for rotating disc galaxies, in particular for low surface brightness (LSB) galaxies. The main observational properties related to the baryonic matter in LSBs, investigated over the last decades, are briefly recalled. Next, these galaxies are analyzed by means of the mass modelling of their rotation curves both individual and stacked. The latter analysis, via the universal rotation curve (URC) method, results really powerful in giving a global or universal description of the properties of these objects. We report the presence in LSBs of scaling relations among their structural properties that result comparable with those found in galaxies of different morphologies. All this confirms, in disc systems, the existence of a strong entanglement between the luminous matter (LM) and the dark matter (DM). Moreover, we report how in LSBs the tight relationship between their radial gravitational accelerations g and their baryonic components gb results to depend also on the stellar disk length scale and the radius at which the two accelerations have been measured. LSB galaxies strongly challenge the ΛCDM scenario with the relative collisionless dark particle and, alongside with the non-detection of the latter, contribute to guide us towards a new scenario for the DM phenomenon.
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6
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Rogers KK, Peiris HV. Strong Bound on Canonical Ultralight Axion Dark Matter from the Lyman-Alpha Forest. PHYSICAL REVIEW LETTERS 2021; 126:071302. [PMID: 33666479 DOI: 10.1103/physrevlett.126.071302] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/07/2020] [Revised: 11/18/2020] [Accepted: 12/22/2020] [Indexed: 06/12/2023]
Abstract
We present a new bound on the ultralight axion (ULA) dark matter mass m_{a}, using the Lyman-alpha forest to look for suppressed cosmic structure growth: a 95% lower limit m_{a}>2×10^{-20} eV. This strongly disfavors (>99.7% credibility) the canonical ULA with 10^{-22} eV<m_{a}<10^{-21} eV, motivated by the string axiverse and solutions to possible tensions in the cold dark matter model. We strengthen previous equivalent bounds by about an order of magnitude. We demonstrate the robustness of our results using an optimized emulator of improved hydrodynamical simulations.
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Affiliation(s)
- Keir K Rogers
- Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova University Center, Stockholm 10691, Sweden
| | - Hiranya V Peiris
- Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova University Center, Stockholm 10691, Sweden
- Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, United Kingdom
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7
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Chavanis PH. Predictive model of BEC dark matter halos with a solitonic core and an isothermal atmosphere. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.100.083022] [Citation(s) in RCA: 27] [Impact Index Per Article: 5.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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8
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Mocz P, Fialkov A, Vogelsberger M, Becerra F, Amin MA, Bose S, Boylan-Kolchin M, Chavanis PH, Hernquist L, Lancaster L, Marinacci F, Robles VH, Zavala J. First Star-Forming Structures in Fuzzy Cosmic Filaments. PHYSICAL REVIEW LETTERS 2019; 123:141301. [PMID: 31702225 DOI: 10.1103/physrevlett.123.141301] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/16/2019] [Revised: 08/07/2019] [Indexed: 06/10/2023]
Abstract
In hierarchical models of structure formation, the first galaxies form in low-mass dark matter potential wells, probing the behavior of dark matter on kiloparsec scales. Even though these objects are below the detection threshold of current telescopes, future missions will open an observational window into this emergent world. In this Letter, we investigate how the first galaxies are assembled in a "fuzzy" dark matter (FDM) cosmology where dark matter is an ultralight ∼10^{-22} eV boson and the primordial stars are expected to form along dense dark matter filaments. Using a first-of-its-kind cosmological hydrodynamical simulation, we explore the interplay between baryonic physics and unique wavelike features inherent to FDM. In our simulation, the dark matter filaments show coherent interference patterns on the boson de Broglie scale and develop cylindrical solitonlike cores, which are unstable under gravity and collapse into kiloparsec-scale spherical solitons. Features of the dark matter distribution are largely unaffected by the baryonic feedback. On the contrary, the distributions of gas and stars, which do form along the entire filament, exhibit central cores imprinted by dark matter-a smoking gun signature of FDM.
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Affiliation(s)
- Philip Mocz
- Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, New Jersey 08544, USA
| | - Anastasia Fialkov
- Department of Physics and Astronomy, University of Sussex, Falmer, Brighton BN1 9QH, United Kingdom
| | - Mark Vogelsberger
- Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA
| | - Fernando Becerra
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA
| | - Mustafa A Amin
- Physics and Astronomy Department, Rice University, Houston, Texas 77005-1827, USA
| | - Sownak Bose
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA
| | - Michael Boylan-Kolchin
- Department of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, Texas 78712-1205, USA
| | - Pierre-Henri Chavanis
- Laboratoire de Physique Théorique, Université Paul Sabatier, 118 route de Narbonne 31062 Toulouse, France
| | - Lars Hernquist
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA
| | - Lachlan Lancaster
- Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, New Jersey 08544, USA
| | - Federico Marinacci
- Department of Physics and Astronomy, University of Bologna, via Gobetti 93/2, 40129 Bologna, Italy
| | - Victor H Robles
- Department of Physics and Astronomy, University of California, Irvine, California 92697, USA
| | - Jesús Zavala
- Center for Astrophysics and Cosmology, Science Institute, University of Iceland, Dunhagi 5, 107 Reykjavik, Iceland
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9
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Chan MH. A universal constant for dark matter-baryon interplay. Sci Rep 2019; 9:3570. [PMID: 30837521 PMCID: PMC6400959 DOI: 10.1038/s41598-019-39717-x] [Citation(s) in RCA: 10] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/23/2018] [Accepted: 02/01/2019] [Indexed: 11/09/2022] Open
Abstract
Recent studies point out that there exists some rough scaling relations for dark matter and some tight connections between dark matter and baryons. However, most of the relations and tight connections can only be found in galaxies, but not in galaxy clusters. In this article, we consider a new expression that can characterize the properties of dark matter-baryon interplay for both galactic and galaxy cluster scales. By using the archival observational data of galaxies and galaxy clusters, we show that the value [Formula: see text] is almost a constant and scale independent within the optical radius ro, where [Formula: see text] is the average dark matter number density, [Formula: see text] is the average baryon number density, v is the characteristic velocity and V is the interacting volume. This would be the first universal relation between dark matter and baryons on both galactic and galaxy cluster scales. We anticipate this result to be a starting point to explain the small-scale problem and the scaling relations for dark matter in galaxies. The constant K discovered may reveal some underlying global interaction between dark matter and baryons.
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Affiliation(s)
- Man Ho Chan
- Department of Science and Environmental Studies, The Education University of Hong Kong Tai Po, New Territories, Hong Kong, China.
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10
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El-Badry K, Bland-Hawthorn J, Wetzel A, Quataert E, Weisz DR, Boylan-Kolchin M, Hopkins PF, Faucher-Giguère CA, Kereš D, Garrison-Kimmel S. Where are the most ancient stars in the Milky Way? MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2018; 480:652-668. [PMID: 30581239 PMCID: PMC6301095 DOI: 10.1093/mnras/sty1864] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
The oldest stars in the Milky Way (MW) bear imprints of the Galaxy's early assembly history. We use FIRE cosmological zoom-in simulations of three MW-mass disc galaxies to study the spatial distribution, chemistry, and kinematics of the oldest surviving stars (z form ≳ 5) in MW-like galaxies. We predict the oldest stars to be less centrally concentrated at z = 0 than stars formed at later times as a result of two processes. First, the majority of the oldest stars are not formed in situ but are accreted during hierarchical assembly. These ex situ stars are deposited on dispersion-supported, halo-like orbits but dominate over old stars formed in situ in the solar neighbourhood, and in some simulations, even in the galactic centre. Secondly, old stars formed in situ are driven outwards by bursty star formation and energetic feedback processes that create a time-varying gravitational potential at z ≳ 2, similar to the process that creates dark matter cores and expands stellar orbits in bursty dwarf galaxies. The total fraction of stars that are ancient is more than an order of magnitude higher for sight lines away from the bulge and inner halo than for inward-looking sight lines. Although the task of identifying specific stars as ancient remains challenging, we anticipate that million-star spectral surveys and photometric surveys targeting metal-poor stars already include hundreds of stars formed before z = 5. We predict most of these targets to have higher metallicity (-3 < [Fe/H] < -2) than the most extreme metal-poor stars.
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Affiliation(s)
- Kareem El-Badry
- Department of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720, USA
| | - Joss Bland-Hawthorn
- Miller Institute, University of California Berkeley, Berkeley, CA 94720, USA
- Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO-3D), Sydney, NSW 2006, Australia
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | - Andrew Wetzel
- Department of Physics, University of California, Davis, CA 95616, USA
| | - Eliot Quataert
- Department of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720, USA
| | - Daniel R. Weisz
- Department of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720, USA
| | | | - Philip F. Hopkins
- TAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USA
| | | | - Dušan Kereš
- Department of Physics, Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093, USA
| | - Shea Garrison-Kimmel
- TAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USA
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11
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Chan TK, Kereš D, Wetzel A, Hopkins PF, Faucher-Giguère CA, El-Badry K, Garrison-Kimmel S, Boylan-Kolchin M. The origin of ultra diffuse galaxies: stellar feedback and quenching. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2018; 478:906-925. [PMID: 30573924 PMCID: PMC6295926 DOI: 10.1093/mnras/sty1153] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
We test if the cosmological zoom-in simulations of isolated galaxies from the FIRE project reproduce the properties of ultra diffuse galaxies (UDGs). We show that outflows that dynamically heat galactic stars, together with a passively aging stellar population after imposed quenching, naturally reproduce the observed population of red UDGs, without the need for high spin haloes, or dynamical influence from their host cluster. We reproduce the range of surface brightness, radius, and absolute magnitude of the observed red UDGs by quenching simulated galaxies at a range of different times. They represent a mostly uniform population of dark matter-dominated dwarf galaxies with M * ~ 108 M☉, low metallicity, and a broad range of ages; the more massive the UDGs, the older they are. The most massive red UDG in our sample(M * ~ 3 × 108 M☉) requires quenching at z ~ 3 when its halo reached M h ~ 1011M☉. Our simulated UDGs form with normal stellar-to-halo ratios and match the central enclosed masses and the velocity dispersions of the observed UDGs. Enclosed masses remain largely fixed across a broad range of quenching times because the central regions of their dark matter haloes complete their growth early. If our simulated dwarfs are not quenched, they evolve into bluer low surface brightness galaxies with M/L similar to observed field dwarfs. While our simulation sample covers a limited range of formation histories and halo masses, we predict that UDG is a common, and perhaps even dominant, galaxy type around M * ~ 108 M☉, both in the field and in clusters.
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Affiliation(s)
- T K Chan
- Department of Physics, Center for Astrophysics and Space Sciences, University of California at San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USA
| | - D Kereš
- Department of Physics, Center for Astrophysics and Space Sciences, University of California at San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USA
| | - A Wetzel
- TAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USA
- The Observatories of the Carnegie Institution for Science, Pasadena, CA 91101, USA
- Department of Physics, University of California, Davis, CA 95616, USA
| | - P F Hopkins
- TAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USA
| | - C-A Faucher-Giguère
- Department of Physics and Astronomy and CIERA, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA
| | - K El-Badry
- Department of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720, USA
| | - S Garrison-Kimmel
- TAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USA
| | - M Boylan-Kolchin
- Department of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712-1205, USA
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12
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El-Badry K, Bradford J, Quataert E, Geha M, Boylan-Kolchin M, Weisz DR, Wetzel A, Hopkins PF, Chan TK, Fitts A, Kereš D, Faucher-Giguére CA. Gas kinematics in FIRE simulated galaxies compared to spatially unresolved HI observations. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2018; 477:1536-1548. [PMID: 30713356 PMCID: PMC6350816 DOI: 10.1093/mnras/sty730] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
The shape of a galaxy's spatially unresolved, globally integrated 21-cm emission line depends on its internal gas kinematics: galaxies with rotationally supported gas discs produce double-horned profiles with steep wings, while galaxies with dispersion-supported gas produce Gaussian-like profiles with sloped wings. Using mock observations of simulated galaxies from the FIRE project, we show that one can therefore constrain a galaxy's gas kinematics from its unresolved 21-cm line profile. In particular, we find that the kurtosis of the 21-cm line increases with decreasing V/σ and that this trend is robust across a wide range of masses, signal-to-noise ratios, and inclinations. We then quantify the shapes of 21-cm line profiles from a morphologically unbiased sample of ~2000 low-redshift, HI-detected galaxies with Mstar = 107-11 M☉ and compare to the simulated galaxies. At Mstar ≳ 1010 M☉, both the observed and simulated galaxies produce double-horned profiles with low kurtosis and steep wings, consistent with rotationally supported discs. Both the observed and simulated line profiles become more Gaussian like (higher kurtosis and less-steep wings) at lower masses, indicating increased dispersion support. However, the simulated galaxies transition from rotational to dispersion support more strongly: at Mstar 108-10 M, most of the simulations produce more Gaussian-like profiles than typical observed galaxies with similar mass, indicating that gas in the low-mass simulated galaxies is, on average, overly dispersion supported. Most of the lower-mass-simulated galaxies also have somewhat lower gas fractions than the median of the observed population. The simulations nevertheless reproduce the observed line-width baryonic Tully-Fisher relation, which is insensitive to rotational versus dispersion support.
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Affiliation(s)
- Kareem El-Badry
- Department of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720, USA
| | - Jeremy Bradford
- Department of Astronomy, Yale University, New Haven, CT 06520, USA
| | - Eliot Quataert
- Department of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720, USA
| | - Marla Geha
- Department of Astronomy, Yale University, New Haven, CT 06520, USA
| | | | - Daniel R. Weisz
- Department of Astronomy and Theoretical Astrophysics Center, University of California Berkeley, Berkeley, CA 94720, USA
| | - Andrew Wetzel
- Department of Physics, University of California, Davis, CA 95616, USA
| | - Philip F. Hopkins
- TAPIR, Mailcode 350-17, California Institute of Technology, Pasadena, CA 91125, USA
| | - T. K. Chan
- Department of Physics, Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093, USA
| | - Alex Fitts
- Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA
| | - Dušan Kereš
- Department of Physics, Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093, USA
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13
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Calore F, De Romeri V, Di Mauro M, Donato F, Marinacci F. Realistic estimation for the detectability of dark matter subhalos using Fermi-LAT catalogs. Int J Clin Exp Med 2017. [DOI: 10.1103/physrevd.96.063009] [Citation(s) in RCA: 22] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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14
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15
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16
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Brook CB, Santos-Santos I, Stinson G. The different baryonic Tully-Fisher relations at low masses. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2016; 459:638-645. [PMID: 27274704 DOI: 10.1093/mnras/stw650] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/16/2015] [Revised: 03/14/2016] [Accepted: 03/14/2016] [Indexed: 06/06/2023]
Abstract
We compare the Baryonic Tully-Fisher relation (BTFR) of simulations and observations of galaxies ranging from dwarfs to spirals, using various measures of rotational velocity Vrot. We explore the BTFR when measuring Vrot at the flat part of the rotation curve, Vflat, at the extent of H i gas, Vlast, and using 20 per cent (W20) and 50 per cent (W50) of the width of H i line profiles. We also compare with the maximum circular velocity of the parent halo, [Formula: see text], within dark matter only simulations. The different BTFRs increasingly diverge as galaxy mass decreases. Using Vlast one obtains a power law over four orders of magnitude in baryonic mass, with slope similar to the observed BTFR. Measuring Vflat gives similar results as Vlast when galaxies with rising rotation curves are excluded. However, higher rotation velocities would be found for low-mass galaxies if the cold gas extended far enough for Vrot to reach a maximum. W20 gives a similar slope as Vlast but with slightly lower values of Vrot for low-mass galaxies, although this may depend on the extent of the gas in your galaxy sample. W50 bends away from these other relations towards low velocities at low masses. By contrast, [Formula: see text] bends towards high velocities for low-mass galaxies, as cold gas does not extend out to the radius at which haloes reach [Formula: see text]. Our study highlights the need for careful comparisons between observations and models: one needs to be consistent about the particular method of measuring Vrot, and precise about the radius at which velocities are measured.
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Affiliation(s)
- Chris B Brook
- Departamento de Física Teórica, Universidad Autónoma de Madrid, E-28049 Cantoblanco, Madrid, Spain; Astro-UAM, UAM, Unidad Asociada CSIC, E-28049, Madrid, Spain
| | - Isabel Santos-Santos
- Departamento de Física Teórica, Universidad Autónoma de Madrid, E-28049 Cantoblanco, Madrid, Spain
| | - Greg Stinson
- Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
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17
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18
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Evslin J. What canGaia(with Thirty Meter Telescope) say about the Sculptor Dwarf's Core? ACTA ACUST UNITED AC 2015. [DOI: 10.1093/mnrasl/slv083] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022]
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Menon H, Wesolowski L, Zheng G, Jetley P, Kale L, Quinn T, Governato F. Adaptive techniques for clustered N-body cosmological simulations. ACTA ACUST UNITED AC 2015. [DOI: 10.1186/s40668-015-0007-9] [Citation(s) in RCA: 76] [Impact Index Per Article: 8.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Abstract
AbstractChaNGa is an N-body cosmology simulation application implemented using Charm++. In this paper, we present the parallel design of ChaNGa and address many challenges arising due to the high dynamic ranges of clustered datasets. We propose optimizations based on adaptive techniques. We evaluate the performance of ChaNGa on highly clustered datasets: a $z \sim0$
z
∼
0
snapshot of a 2 billion particle realization of a 25 Mpc volume, and a 52 million particle multi-resolution realization of a dwarf galaxy. For the 25 Mpc volume, we show strong scaling on up to 128K cores of Blue Waters. We also demonstrate scaling up to 128K cores of a multi-stepping run of the 2 billion particle simulation. While the scaling of the multi-stepping run is not as good as single stepping, the throughput at 128K cores is greater by a factor of 2. We also demonstrate strong scaling on up to 512K cores of Blue Waters for two large, uniform datasets with 12 and 24 billion particles.
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Harvey D, Massey R, Kitching T, Taylor A, Tittley E. The nongravitational interactions of dark matter in colliding galaxy clusters. Science 2015; 347:1462-5. [PMID: 25814581 DOI: 10.1126/science.1261381] [Citation(s) in RCA: 327] [Impact Index Per Article: 36.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Collisions between galaxy clusters provide a test of the nongravitational forces acting on dark matter. Dark matter's lack of deceleration in the "bullet cluster" collision constrained its self-interaction cross section σ(DM)/m < 1.25 square centimeters per gram (cm(2)/g) [68% confidence limit (CL)] (σ(DM), self-interaction cross section; m, unit mass of dark matter) for long-ranged forces. Using the Chandra and Hubble Space Telescopes, we have now observed 72 collisions, including both major and minor mergers. Combining these measurements statistically, we detect the existence of dark mass at 7.6σ significance. The position of the dark mass has remained closely aligned within 5.8 ± 8.2 kiloparsecs of associated stars, implying a self-interaction cross section σ(DM)/m < 0.47 cm(2)/g (95% CL) and disfavoring some proposed extensions to the standard model.
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Affiliation(s)
- David Harvey
- Laboratoire d'Astrophysique, École Polytechnique Fédérale de Lausanne, Observatoire de Sauverny, 1290 Versoix, Switzerland. Royal Observatory, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK.
| | - Richard Massey
- Institute for Computational Cosmology, Durham University, South Road, Durham DH1 3LE, UK
| | - Thomas Kitching
- Mullard Space Science Laboratory, University College London, Dorking, Surrey RH5 6NT, UK
| | - Andy Taylor
- Royal Observatory, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK
| | - Eric Tittley
- Royal Observatory, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK
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Abramowski A, Aharonian F, Ait Benkhali F, Akhperjanian AG, Angüner EO, Backes M, Balenderan S, Balzer A, Barnacka A, Becherini Y, Becker Tjus J, Berge D, Bernhard S, Bernlöhr K, Birsin E, Biteau J, Böttcher M, Boisson C, Bolmont J, Bordas P, Bregeon J, Brun F, Brun P, Bryan M, Bulik T, Carrigan S, Casanova S, Chadwick PM, Chakraborty N, Chalme-Calvet R, Chaves RCG, Chrétien M, Colafrancesco S, Cologna G, Conrad J, Couturier C, Cui Y, Davids ID, Degrange B, Deil C, deWilt P, Djannati-Ataï A, Domainko W, Donath A, Drury LO, Dubus G, Dutson K, Dyks J, Dyrda M, Edwards T, Egberts K, Eger P, Espigat P, Farnier C, Fegan S, Feinstein F, Fernandes MV, Fernandez D, Fiasson A, Fontaine G, Förster A, Füßling M, Gabici S, Gajdus M, Gallant YA, Garrigoux T, Giavitto G, Giebels B, Glicenstein JF, Gottschall D, Grondin MH, Grudzińska M, Hadasch D, Häffner S, Hahn J, Harris J, Heinzelmann G, Henri G, Hermann G, Hervet O, Hillert A, Hinton JA, Hofmann W, Hofverberg P, Holler M, Horns D, Ivascenko A, Jacholkowska A, Jahn C, Jamrozy M, Janiak M, Jankowsky F, Jung-Richardt I, Kastendieck MA, Katarzyński K, Katz U, Kaufmann S, Khélifi B, Kieffer M, Klepser S, Klochkov D, Kluźniak W, Kolitzus D, Komin N, Kosack K, Krakau S, Krayzel F, Krüger PP, Laffon H, Lamanna G, Lefaucheur J, Lefranc V, Lemière A, Lemoine-Goumard M, Lenain JP, Lohse T, Lopatin A, Lu CC, Marandon V, Marcowith A, Marx R, Maurin G, Maxted N, Mayer M, McComb TJL, Méhault J, Meintjes PJ, Menzler U, Meyer M, Mitchell AMW, Moderski R, Mohamed M, Morå K, Moulin E, Murach T, de Naurois M, Niemiec J, Nolan SJ, Oakes L, Odaka H, Ohm S, Opitz B, Ostrowski M, Oya I, Panter M, Parsons RD, Paz Arribas M, Pekeur NW, Pelletier G, Petrucci PO, Peyaud B, Pita S, Poon H, Pühlhofer G, Punch M, Quirrenbach A, Raab S, Reichardt I, Reimer A, Reimer O, Renaud M, de Los Reyes R, Rieger F, Romoli C, Rosier-Lees S, Rowell G, Rudak B, Rulten CB, Sahakian V, Salek D, Sanchez DA, Santangelo A, Schlickeiser R, Schüssler F, Schulz A, Schwanke U, Schwarzburg S, Schwemmer S, Sol H, Spanier F, Spengler G, Spies F, Stawarz Ł, Steenkamp R, Stegmann C, Stinzing F, Stycz K, Sushch I, Tavernet JP, Tavernier T, Taylor AM, Terrier R, Tluczykont M, Trichard C, Valerius K, van Eldik C, van Soelen B, Vasileiadis G, Veh J, Venter C, Viana A, Vincent P, Vink J, Völk HJ, Volpe F, Vorster M, Vuillaume T, Wagner SJ, Wagner P, Wagner RM, Ward M, Weidinger M, Weitzel Q, White R, Wierzcholska A, Willmann P, Wörnlein A, Wouters D, Yang R, Zabalza V, Zaborov D, Zacharias M, Zdziarski AA, Zech A, Zechlin HS. Constraints on an annihilation signal from a core of constant dark matter density around the milky way center with H.E.S.S. PHYSICAL REVIEW LETTERS 2015; 114:081301. [PMID: 25768750 DOI: 10.1103/physrevlett.114.081301] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/12/2014] [Indexed: 06/04/2023]
Abstract
An annihilation signal of dark matter is searched for from the central region of the Milky Way. Data acquired in dedicated on-off observations of the Galactic center region with H.E.S.S. are analyzed for this purpose. No significant signal is found in a total of ∼9 h of on-off observations. Upper limits on the velocity averaged cross section, ⟨σv⟩, for the annihilation of dark matter particles with masses in the range of ∼300 GeV to ∼10 TeV are derived. In contrast to previous constraints derived from observations of the Galactic center region, the constraints that are derived here apply also under the assumption of a central core of constant dark matter density around the center of the Galaxy. Values of ⟨σv⟩ that are larger than 3×10^{-24} cm^{3}/s are excluded for dark matter particles with masses between ∼1 and ∼4 TeV at 95% C.L. if the radius of the central dark matter density core does not exceed 500 pc. This is the strongest constraint that is derived on ⟨σv⟩ for annihilating TeV mass dark matter without the assumption of a centrally cusped dark matter density distribution in the search region.
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Affiliation(s)
- A Abramowski
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
| | - F Aharonian
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
- Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
- National Academy of Sciences of the Republic of Armenia, Marshall Baghramian Avenue, 24, 0019 Yerevan, Republic of Armenia
| | - F Ait Benkhali
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - A G Akhperjanian
- National Academy of Sciences of the Republic of Armenia, Marshall Baghramian Avenue, 24, 0019 Yerevan, Republic of Armenia
- Yerevan Physics Institute, 2 Alikhanian Brothers St., 375036 Yerevan, Armenia
| | - E O Angüner
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - M Backes
- University of Namibia, Department of Physics, Private Bag 13301, Windhoek, Namibia
| | - S Balenderan
- University of Durham, Department of Physics, South Road, Durham DH1 3LE, United Kingdom
| | - A Balzer
- GRAPPA, Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, Netherlands
| | - A Barnacka
- Obserwatorium Astronomiczne, Uniwersytet Jagielloński, ul. Orla 171, 30-244 Kraków, Poland
- Now at Harvard-Smithsonian Center for Astrophysics, 60 Garden St, MS-20, Cambridge, Massachusetts 02138, USA
| | - Y Becherini
- Department of Physics and Electrical Engineering, Linnaeus University, 351 95 Växjö, Sweden
| | - J Becker Tjus
- Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, D 44780 Bochum, Germany
| | - D Berge
- GRAPPA, Anton Pannekoek Institute for Astronomy and Institute of High-Energy Physics, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, Netherlands
| | - S Bernhard
- Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria
| | - K Bernlöhr
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - E Birsin
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - J Biteau
- Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France
- Now at Santa Cruz Institute for Particle Physics, Department of Physics, University of California at Santa Cruz, Santa Cruz, California 95064, USA
| | - M Böttcher
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - C Boisson
- LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France
| | - J Bolmont
- LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252 Paris Cedex 5, France
| | - P Bordas
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - J Bregeon
- Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - F Brun
- DSM/Irfu, CEA Saclay, F-91191 Gif-Sur-Yvette Cedex, France
| | - P Brun
- DSM/Irfu, CEA Saclay, F-91191 Gif-Sur-Yvette Cedex, France
| | - M Bryan
- GRAPPA, Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, Netherlands
| | - T Bulik
- Astronomical Observatory, The University of Warsaw, Al. Ujazdowskie 4, 00-478 Warsaw, Poland
| | - S Carrigan
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - S Casanova
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
- Instytut Fizyki Ja˛drowej PAN, ul. Radzikowskiego 152, 31-342 Kraków, Poland
| | - P M Chadwick
- University of Durham, Department of Physics, South Road, Durham DH1 3LE, United Kingdom
| | - N Chakraborty
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - R Chalme-Calvet
- LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252 Paris Cedex 5, France
| | - R C G Chaves
- Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - M Chrétien
- LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252 Paris Cedex 5, France
| | - S Colafrancesco
- School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein, Johannesburg 2050, South Africa
| | - G Cologna
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - J Conrad
- Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, SE-10691 Stockholm, Sweden
- Wallenberg Academy Fellow
| | - C Couturier
- LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252 Paris Cedex 5, France
| | - Y Cui
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - I D Davids
- University of Namibia, Department of Physics, Private Bag 13301, Windhoek, Namibia
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - B Degrange
- Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France
| | - C Deil
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - P deWilt
- School of Chemistry & Physics, University of Adelaide, Adelaide 5005, Australia
| | - A Djannati-Ataï
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - W Domainko
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - A Donath
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - L O'C Drury
- Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
| | - G Dubus
- Univ. Grenoble Alpes, IPAG, F-38000 Grenoble, France and CNRS, IPAG, F-38000 Grenoble, France
| | - K Dutson
- Department of Physics and Astronomy, The University of Leicester, University Road, Leicester LE1 7RH, United Kingdom
| | - J Dyks
- Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland
| | - M Dyrda
- Instytut Fizyki Ja˛drowej PAN, ul. Radzikowskiego 152, 31-342 Kraków, Poland
| | - T Edwards
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - K Egberts
- Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, D 14476 Potsdam, Germany
| | - P Eger
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - P Espigat
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - C Farnier
- Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, SE-10691 Stockholm, Sweden
| | - S Fegan
- Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France
| | - F Feinstein
- Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - M V Fernandes
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
| | - D Fernandez
- Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - A Fiasson
- Laboratoire d'Annecy-le-Vieux de Physique des Particules, Université de Savoie, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France
| | - G Fontaine
- Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France
| | - A Förster
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | | | - S Gabici
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - M Gajdus
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - Y A Gallant
- Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - T Garrigoux
- LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252 Paris Cedex 5, France
| | | | - B Giebels
- Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France
| | | | - D Gottschall
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - M-H Grondin
- Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - M Grudzińska
- Astronomical Observatory, The University of Warsaw, Al. Ujazdowskie 4, 00-478 Warsaw, Poland
| | - D Hadasch
- Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria
| | - S Häffner
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - J Hahn
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - J Harris
- Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
| | - G Heinzelmann
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
| | - G Henri
- Univ. Grenoble Alpes, IPAG, F-38000 Grenoble, France and CNRS, IPAG, F-38000 Grenoble, France
| | - G Hermann
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - O Hervet
- LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France
| | - A Hillert
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - J A Hinton
- Department of Physics and Astronomy, The University of Leicester, University Road, Leicester LE1 7RH, United Kingdom
| | - W Hofmann
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - P Hofverberg
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - M Holler
- Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, D 14476 Potsdam, Germany
| | - D Horns
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
| | - A Ivascenko
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - A Jacholkowska
- LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France
| | - C Jahn
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - M Jamrozy
- Obserwatorium Astronomiczne, Uniwersytet Jagielloński, ul. Orla 171, 30-244 Kraków, Poland
| | - M Janiak
- Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland
| | - F Jankowsky
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - I Jung-Richardt
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - M A Kastendieck
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
| | - K Katarzyński
- Centre for Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziadzka 5, 87-100 Torun, Poland
| | - U Katz
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - S Kaufmann
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - B Khélifi
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - M Kieffer
- LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252 Paris Cedex 5, France
| | | | - D Klochkov
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - W Kluźniak
- Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland
| | - D Kolitzus
- Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria
| | - Nu Komin
- School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein, Johannesburg 2050, South Africa
| | - K Kosack
- DSM/Irfu, CEA Saclay, F-91191 Gif-Sur-Yvette Cedex, France
| | - S Krakau
- Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, D 44780 Bochum, Germany
| | - F Krayzel
- Laboratoire d'Annecy-le-Vieux de Physique des Particules, Université de Savoie, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France
| | - P P Krüger
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - H Laffon
- Université Bordeaux 1, CNRS/IN2P3, Centre d'Études Nucléaires de Bordeaux Gradignan, 33175 Gradignan, France
| | - G Lamanna
- Laboratoire d'Annecy-le-Vieux de Physique des Particules, Université de Savoie, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France
| | - J Lefaucheur
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - V Lefranc
- DSM/Irfu, CEA Saclay, F-91191 Gif-Sur-Yvette Cedex, France
| | - A Lemière
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - M Lemoine-Goumard
- Université Bordeaux 1, CNRS/IN2P3, Centre d'Études Nucléaires de Bordeaux Gradignan, 33175 Gradignan, France
| | - J-P Lenain
- LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252 Paris Cedex 5, France
| | - T Lohse
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - A Lopatin
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - C-C Lu
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - V Marandon
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - A Marcowith
- Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - R Marx
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - G Maurin
- Laboratoire d'Annecy-le-Vieux de Physique des Particules, Université de Savoie, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France
| | - N Maxted
- Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - M Mayer
- Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, D 14476 Potsdam, Germany
| | - T J L McComb
- University of Durham, Department of Physics, South Road, Durham DH1 3LE, United Kingdom
| | - J Méhault
- Université Bordeaux 1, CNRS/IN2P3, Centre d'Études Nucléaires de Bordeaux Gradignan, 33175 Gradignan, France
| | - P J Meintjes
- Department of Physics, University of the Free State, PO Box 339, Bloemfontein 9300, South Africa
| | - U Menzler
- Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, D 44780 Bochum, Germany
| | - M Meyer
- Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, SE-10691 Stockholm, Sweden
| | - A M W Mitchell
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - R Moderski
- Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland
| | - M Mohamed
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - K Morå
- Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, SE-10691 Stockholm, Sweden
| | - E Moulin
- DSM/Irfu, CEA Saclay, F-91191 Gif-Sur-Yvette Cedex, France
| | - T Murach
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - M de Naurois
- Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France
| | - J Niemiec
- Instytut Fizyki Ja˛drowej PAN, ul. Radzikowskiego 152, 31-342 Kraków, Poland
| | - S J Nolan
- University of Durham, Department of Physics, South Road, Durham DH1 3LE, United Kingdom
| | - L Oakes
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - H Odaka
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - S Ohm
- DESY, D-15738 Zeuthen, Germany
| | - B Opitz
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
| | - M Ostrowski
- Obserwatorium Astronomiczne, Uniwersytet Jagielloński, ul. Orla 171, 30-244 Kraków, Poland
| | - I Oya
- DESY, D-15738 Zeuthen, Germany
| | - M Panter
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - R D Parsons
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - M Paz Arribas
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - N W Pekeur
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - G Pelletier
- Univ. Grenoble Alpes, IPAG, F-38000 Grenoble, France and CNRS, IPAG, F-38000 Grenoble, France
| | - P-O Petrucci
- Univ. Grenoble Alpes, IPAG, F-38000 Grenoble, France and CNRS, IPAG, F-38000 Grenoble, France
| | - B Peyaud
- DSM/Irfu, CEA Saclay, F-91191 Gif-Sur-Yvette Cedex, France
| | - S Pita
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - H Poon
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - G Pühlhofer
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - M Punch
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - A Quirrenbach
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - S Raab
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - I Reichardt
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - A Reimer
- Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria
| | - O Reimer
- Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria
| | - M Renaud
- Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - R de Los Reyes
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - F Rieger
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - C Romoli
- Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
| | - S Rosier-Lees
- Laboratoire d'Annecy-le-Vieux de Physique des Particules, Université de Savoie, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France
| | - G Rowell
- School of Chemistry & Physics, University of Adelaide, Adelaide 5005, Australia
| | - B Rudak
- Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland
| | - C B Rulten
- LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France
| | - V Sahakian
- National Academy of Sciences of the Republic of Armenia, Marshall Baghramian Avenue, 24, 0019 Yerevan, Republic of Armenia
- Yerevan Physics Institute, 2 Alikhanian Brothers St., 375036 Yerevan, Armenia
| | - D Salek
- GRAPPA, Institute of High-Energy Physics, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, Netherlands
| | - D A Sanchez
- Laboratoire d'Annecy-le-Vieux de Physique des Particules, Université de Savoie, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France
| | - A Santangelo
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - R Schlickeiser
- Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, D 44780 Bochum, Germany
| | - F Schüssler
- DSM/Irfu, CEA Saclay, F-91191 Gif-Sur-Yvette Cedex, France
| | | | - U Schwanke
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - S Schwarzburg
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - S Schwemmer
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - H Sol
- LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France
| | - F Spanier
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - G Spengler
- Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, SE-10691 Stockholm, Sweden
| | - F Spies
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
| | - Ł Stawarz
- Obserwatorium Astronomiczne, Uniwersytet Jagielloński, ul. Orla 171, 30-244 Kraków, Poland
| | - R Steenkamp
- University of Namibia, Department of Physics, Private Bag 13301, Windhoek, Namibia
| | - C Stegmann
- Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, D 14476 Potsdam, Germany
- DESY, D-15738 Zeuthen, Germany
| | - F Stinzing
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - K Stycz
- DESY, D-15738 Zeuthen, Germany
| | - I Sushch
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - J-P Tavernet
- LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252 Paris Cedex 5, France
| | - T Tavernier
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - A M Taylor
- Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
| | - R Terrier
- APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
| | - M Tluczykont
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
| | - C Trichard
- Laboratoire d'Annecy-le-Vieux de Physique des Particules, Université de Savoie, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France
| | - K Valerius
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - C van Eldik
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - B van Soelen
- Department of Physics, University of the Free State, PO Box 339, Bloemfontein 9300, South Africa
| | - G Vasileiadis
- Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - J Veh
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - C Venter
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - A Viana
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - P Vincent
- LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252 Paris Cedex 5, France
| | - J Vink
- GRAPPA, Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, Netherlands
| | - H J Völk
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - F Volpe
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - M Vorster
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - T Vuillaume
- Univ. Grenoble Alpes, IPAG, F-38000 Grenoble, France and CNRS, IPAG, F-38000 Grenoble, France
| | - S J Wagner
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - P Wagner
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - R M Wagner
- Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, SE-10691 Stockholm, Sweden
| | - M Ward
- University of Durham, Department of Physics, South Road, Durham DH1 3LE, United Kingdom
| | - M Weidinger
- Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, D 44780 Bochum, Germany
| | - Q Weitzel
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - R White
- Department of Physics and Astronomy, The University of Leicester, University Road, Leicester LE1 7RH, United Kingdom
| | - A Wierzcholska
- Instytut Fizyki Ja˛drowej PAN, ul. Radzikowskiego 152, 31-342 Kraków, Poland
| | - P Willmann
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - A Wörnlein
- Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - D Wouters
- DSM/Irfu, CEA Saclay, F-91191 Gif-Sur-Yvette Cedex, France
| | - R Yang
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - V Zabalza
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
- Department of Physics and Astronomy, The University of Leicester, University Road, Leicester LE1 7RH, United Kingdom
| | - D Zaborov
- Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France
| | - M Zacharias
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - A A Zdziarski
- Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland
| | - A Zech
- LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France
| | - H-S Zechlin
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
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Schive HY, Liao MH, Woo TP, Wong SK, Chiueh T, Broadhurst T, Hwang WYP. Understanding the core-halo relation of quantum wave dark matter from 3D simulations. PHYSICAL REVIEW LETTERS 2014; 113:261302. [PMID: 25615301 DOI: 10.1103/physrevlett.113.261302] [Citation(s) in RCA: 25] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/29/2014] [Indexed: 06/04/2023]
Abstract
We examine the nonlinear structure of gravitationally collapsed objects that form in our simulations of wavelike cold dark matter, described by the Schrödinger-Poisson (SP) equation with a particle mass ∼10(-22) eV. A distinct gravitationally self-bound solitonic core is found at the center of every halo, with a profile quite different from cores modeled in the warm or self-interacting dark matter scenarios. Furthermore, we show that each solitonic core is surrounded by an extended halo composed of large fluctuating dark matter granules which modulate the halo density on a scale comparable to the diameter of the solitonic core. The scaling symmetry of the SP equation and the uncertainty principle tightly relate the core mass to the halo specific energy, which, in the context of cosmological structure formation, leads to a simple scaling between core mass (Mc) and halo mass (Mh), Mc∝a(-1/2)Mh(1/3), where a is the cosmic scale factor. We verify this scaling relation by (i) examining the internal structure of a statistical sample of virialized halos that form in our 3D cosmological simulations and by (ii) merging multiple solitons to create individual virialized objects. Sufficient simulation resolution is achieved by adaptive mesh refinement and graphic processing units acceleration. From this scaling relation, present dwarf satellite galaxies are predicted to have kiloparsec-sized cores and a minimum mass of ∼10(8)M⊙, capable of solving the small-scale controversies in the cold dark matter model. Moreover, galaxies of 2×10(12)M⊙ at z=8 should have massive solitonic cores of ∼2×10(9)M⊙ within ∼60 pc. Such cores can provide a favorable local environment for funneling the gas that leads to the prompt formation of early stellar spheroids and quasars.
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Affiliation(s)
- Hsi-Yu Schive
- Department of Physics, National Taiwan University, Taipei 10617, Taiwan
| | - Ming-Hsuan Liao
- Department of Physics, National Taiwan University, Taipei 10617, Taiwan
| | - Tak-Pong Woo
- Department of Physics, National Taiwan University, Taipei 10617, Taiwan
| | - Shing-Kwong Wong
- Department of Physics, National Taiwan University, Taipei 10617, Taiwan
| | - Tzihong Chiueh
- Department of Physics, National Taiwan University, Taipei 10617, Taiwan and National Center for Theoretical Sciences, National Taiwan University, Taipei 10617, Taiwan
| | - Tom Broadhurst
- Department of Theoretical Physics, University of the Basque Country UPV/EHU, E-48080 Bilbao, Spain and Ikerbasque, Basque Foundation for Science, E-48011 Bilbao, Spain
| | - W-Y Pauchy Hwang
- Department of Physics, National Taiwan University, Taipei 10617, Taiwan and National Center for Theoretical Sciences, National Taiwan University, Taipei 10617, Taiwan
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Fields BD, Shapiro SL, Shelton J. Galactic center gamma-ray excess from dark matter annihilation: is there a black hole spike? PHYSICAL REVIEW LETTERS 2014; 113:151302. [PMID: 25375700 DOI: 10.1103/physrevlett.113.151302] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/18/2014] [Indexed: 06/04/2023]
Abstract
If the supermassive black hole Sgr A* at the center of the Milky Way grew adiabatically from an initial seed embedded in a Navarro-Frenk-White dark matter (DM) halo, then the DM profile near the hole has steepened into a spike. We calculate the dramatic enhancement to the gamma-ray flux from the Galactic center (GC) from such a spike if the 1-3 GeV excess observed in Fermi data is due to DM annihilations. We find that for the parameter values favored in recent fits, the point-source-like flux from the spike is 35 times greater than the flux from the inner 1° of the halo, far exceeding all Fermi point source detections near the GC. We consider the dependence of the spike signal on astrophysical and particle parameters and conclude that if the GC excess is due to DM, then a canonical adiabatic spike is disfavored by the data. We discuss alternative Galactic histories that predict different spike signals, including (i) the nonadiabatic growth of the black hole, possibly associated with halo and/or black hole mergers, (ii) gravitational interaction of DM with baryons in the dense core, such as heating by stars, or (iii) DM self-interactions. We emphasize that the spike signal is sensitive to a different combination of particle parameters than the halo signal and that the inclusion of a spike component to any DM signal in future analyses would provide novel information about both the history of the GC and the particle physics of DM annihilations.
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Affiliation(s)
- Brian D Fields
- Departments of Physics and of Astronomy, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Departments of Physics and of Astronomy, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Jessie Shelton
- Departments of Physics and of Astronomy, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
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