Gamma Rays From Dark Matter Subhalos Revisited: Refining the Predictions and Constraints

Utilizing data from the ELVIS and Via Lactea-II simulations, we characterize the local dark matter subhalo population, and use this information to refine the predictions for the gamma-ray fluxes arising from annihilating dark matter in this class of objects. We find that the shapes of nearby subhalos are significantly altered by tidal effects, and are generally not well described by NFW density profiles, instead prefering power-law profiles with an exponential cutoff. From the subhalo candidates detected by the Fermi Gamma-Ray Space Telescope, we place limits on the dark matter annihilation cross section that are only modestly weaker than those based on observations of dwarf galaxies. We also calculate the fraction of observable subhalos that are predicted to be spatially extended at a level potentially discernible to Fermi.

Comments: 20 pages, 13 figures

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2017Feb
Authors: MAGIC Collaboration, M. L. Ahnen1, S. Ansoldi2, L. A. Antonelli3, P. Antoranz4, C. Arcaro5, A. Babic6, B. Banerjee7, P. Bangale8, U. Barres de Almeida9, J. A. Barrio10, J. Becerra González11, W. Bednarek12, E. Bernardini13, A. Berti14, B. Biasuzzi15, A. Biland16, O. Blanch17, S. Bonnefoy18, G. Bonnoli19, F. Borracci20, T. Bretz21, R. Carosi22, A. Carosi23, A. Chatterjee24, P. Colin25, E. Colombo26, J. L. Contreras27, J. Cortina28, S. Covino29, P. Cumani30, P. Da Vela31, F. Dazzi32, A. De Angelis33, B. De Lotto34, E. de Oña Wilhelmi35, F. Di Pierro36, M. Doert37, A. Domínguez38, D. Dominis Prester39, D. Dorner40, M. Doro41, S. Einecke42, D. Eisenacher Glawion43, D. Elsaesser44, M. Engelkemeier45, V. Fallah Ramazani46, A. Fernández-Barral47, D. Fidalgo48, M. V. Fonseca49, L. Font50, K. Frantzen51, C. Fruck52, D. Galindo53, R. J. García López54, M. Garczarczyk55, D. Garrido Terrats56, M. Gaug57, P. Giammaria58, N. Godinović59, D. Gora60, D. Guberman61, D. Hadasch62, A. Hahn63, M. Hayashida64, J. Herrera65, J. Hose66, D. Hrupec67, G. Hughes68, W. Idec69, K. Kodani70, Y. Konno71, H. Kubo72, J. Kushida73, A. La Barbera74, D. Lelas75, E. Lindfors76, S. Lombardi77, F. Longo78, M. López79, R. López-Coto80, P. Majumdar81, M. Makariev82, K. Mallot83, G. Maneva84, M. Manganaro85, K. Mannheim86, L. Maraschi87, B. Marcote88, M. Mariotti89, M. Martínez90, D. Mazin91, U. Menzel92, J. M. Miranda93, R. Mirzoyan94, A. Moralejo95, E. Moretti96, D. Nakajima97, V. Neustroev98, A. Niedzwiecki99, M. Nievas Rosillo100, K. Nilsson101, K. Nishijima102, K. Noda103, L. Nogués104, S. Paiano105, J. Palacio106, M. Palatiello107, D. Paneque108, R. Paoletti109, J. M. Paredes110, X. Paredes-Fortuny111, G. Pedaletti112, M. Peresano113, L. Perri114, M. Persic115, J. Poutanen116, P. G. Prada Moroni117, E. Prandini118, I. Puljak119, J. R. Garcia120, I. Reichardt121, W. Rhode122, M. Ribó123, J. Rico124, T. Saito125, K. Satalecka126, S. Schroeder127, T. Schweizer128, A. Sillanpää129, J. Sitarek130, I. Snidaric131, D. Sobczynska132, A. Stamerra133, M. Strzys134, T. Surić135, L. Takalo136, F. Tavecchio137, P. Temnikov138, T. Terzić139, D. Tescaro140, M. Teshima141, D. F. Torres142, T. Toyama143, A. Treves144, G. Vanzo145, M. Vazquez Acosta146, I. Vovk147, J. E. Ward148, M. Will149, M. H. Wu150, R. Zanin151
Affiliations: 1ETH Zurich, CH-8093 Zurich, Switzerland, 2Università di Udine, and INFN Trieste, I-33100 Udine, Italy, 3INAF National Institute for Astrophysics, I-00136 Rome, Italy, 4Università di Siena, and INFN Pisa, I-53100 Siena, Italy, 5Università di Padova and INFN, I-35131 Padova, Italy, 6Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka, University of Split and University of Zagreb, Croatia, 7Saha Institute of Nuclear Physics, 1/AF Bidhannagar, Salt Lake, Sector-1, Kolkata 700064, India, 8Max-Planck-Institut für Physik, D-80805 München, Germany, 9Max-Planck-Institut für Physik, D-80805 München, Germany, 10Universidad Complutense, E-28040 Madrid, Spain, 11Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain, 12University of Łódź, PL-90236 Lodz, Poland, 13Deutsches Elektronen-Synchrotron, 14Università di Udine, and INFN Trieste, I-33100 Udine, Italy, 15Università di Udine, and INFN Trieste, I-33100 Udine, Italy, 16ETH Zurich, CH-8093 Zurich, Switzerland, 17Institut de Fisica d'Altes Energies, 18Universidad Complutense, E-28040 Madrid, Spain, 19Università di Siena, and INFN Pisa, I-53100 Siena, Italy, 20Max-Planck-Institut für Physik, D-80805 München, Germany, 21Universität Würzburg, D-97074 Würzburg, Germany, 22Università di Siena, and INFN Pisa, I-53100 Siena, Italy, 23INAF National Institute for Astrophysics, I-00136 Rome, Italy, 24Saha Institute of Nuclear Physics, 1/AF Bidhannagar, Salt Lake, Sector-1, Kolkata 700064, India, 25Max-Planck-Institut für Physik, D-80805 München, Germany, 26Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain, 27Universidad Complutense, E-28040 Madrid, Spain, 28Institut de Fisica d'Altes Energies, 29INAF National Institute for Astrophysics, I-00136 Rome, Italy, 30Institut de Fisica d'Altes Energies, 31Università di Siena, and INFN Pisa, I-53100 Siena, Italy, 32Max-Planck-Institut für Physik, D-80805 München, Germany, 33Università di Padova and INFN, I-35131 Padova, Italy, 34Università di Udine, and INFN Trieste, I-33100 Udine, Italy, 35Institute for Space Sciences, 36INAF National Institute for Astrophysics, I-00136 Rome, Italy, 37Technische Universität Dortmund, D-44221 Dortmund, Germany, 38Universidad Complutense, E-28040 Madrid, Spain, 39Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka, University of Split and University of Zagreb, Croatia, 40Universität Würzburg, D-97074 Würzburg, Germany, 41Università di Padova and INFN, I-35131 Padova, Italy, 42Technische Universität Dortmund, D-44221 Dortmund, Germany, 43Universität Würzburg, D-97074 Würzburg, Germany, 44Technische Universität Dortmund, D-44221 Dortmund, Germany, 45Technische Universität Dortmund, D-44221 Dortmund, Germany, 46Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Astronomy Division, University of Oulu, Finland, 47Institut de Fisica d'Altes Energies, 48Universidad Complutense, E-28040 Madrid, Spain, 49Universidad Complutense, E-28040 Madrid, Spain, 50Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain, 51Technische Universität Dortmund, D-44221 Dortmund, Germany, 52Max-Planck-Institut für Physik, D-80805 München, Germany, 53Universitat de Barcelona, ICC, IEEC-UB, E-08028 Barcelona, Spain, 54Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain, 55Deutsches Elektronen-Synchrotron, 56Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain, 57Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Spain, 58INAF National Institute for Astrophysics, I-00136 Rome, Italy, 59Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka, University of Split and University of Zagreb, Croatia, 60Deutsches Elektronen-Synchrotron, 61Institut de Fisica d'Altes Energies, 62Japanese MAGIC Consortium, ICRR, The University of Tokyo, Department of Physics and Hakubi Center, Kyoto University, Tokai University, The University of Tokushima, Japan, 63Max-Planck-Institut für Physik, D-80805 München, Germany, 64Japanese MAGIC Consortium, ICRR, The University of Tokyo, Department of Physics and Hakubi Center, Kyoto University, Tokai University, The University of Tokushima, Japan, 65Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain, 66Max-Planck-Institut für Physik, D-80805 München, Germany, 67Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka, University of Split and University of Zagreb, Croatia, 68ETH Zurich, CH-8093 Zurich, Switzerland, 69University of Łódź, PL-90236 Lodz, Poland, 70Japanese MAGIC Consortium, ICRR, The University of Tokyo, Department of Physics and Hakubi Center, Kyoto University, Tokai University, The University of Tokushima, Japan, 71Japanese MAGIC Consortium, ICRR, The University of Tokyo, Department of Physics and Hakubi Center, Kyoto University, Tokai University, The University of Tokushima, Japan, 72Japanese MAGIC Consortium, ICRR, The University of Tokyo, Department of Physics and Hakubi Center, Kyoto University, Tokai University, The University of Tokushima, Japan, 73Japanese MAGIC Consortium, ICRR, The University of Tokyo, Department of Physics and Hakubi Center, Kyoto University, Tokai University, The University of Tokushima, Japan, 74INAF National Institute for Astrophysics, I-00136 Rome, Italy, 75Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka, University of Split and University of Zagreb, Croatia, 76Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Astronomy Division, University of Oulu, Finland, 77INAF National Institute for Astrophysics, I-00136 Rome, Italy, 78Università di Udine, and INFN Trieste, I-33100 Udine, Italy, 79Universidad Complutense, E-28040 Madrid, Spain, 80Institut de Fisica d'Altes Energies, 81Saha Institute of Nuclear Physics, 1/AF Bidhannagar, Salt Lake, Sector-1, Kolkata 700064, India, 82Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria, 83Deutsches Elektronen-Synchrotron, 84Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria, 85Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain, 86Universität Würzburg, D-97074 Würzburg, Germany, 87INAF National Institute for Astrophysics, I-00136 Rome, Italy, 88Universitat de Barcelona, ICC, IEEC-UB, E-08028 Barcelona, Spain, 89Università di Padova and INFN, I-35131 Padova, Italy, 90Institut de Fisica d'Altes Energies, 91Max-Planck-Institut für Physik, D-80805 München, Germany, 92Max-Planck-Institut für Physik, D-80805 München, Germany, 93Università di Siena, and INFN Pisa, I-53100 Siena, Italy, 94Max-Planck-Institut für Physik, D-80805 München, Germany, 95Institut de Fisica d'Altes Energies, 96Max-Planck-Institut für Physik, D-80805 München, Germany, 97Japanese MAGIC Consortium, ICRR, The University of Tokyo, Department of Physics and Hakubi Center, Kyoto University, Tokai University, The University of Tokushima, Japan, 98Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Astronomy Division, University of Oulu, Finland, 99University of Łódź, PL-90236 Lodz, Poland, 100Universidad Complutense, E-28040 Madrid, Spain, 101Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Astronomy Division, University of Oulu, Finland, 102Japanese MAGIC Consortium, ICRR, The University of Tokyo, Department of Physics and Hakubi Center, Kyoto University, Tokai University, The University of Tokushima, Japan, 103Max-Planck-Institut für Physik, D-80805 München, Germany, 104Institut de Fisica d'Altes Energies, 105Università di Padova and INFN, I-35131 Padova, Italy, 106Institut de Fisica d'Altes Energies, 107Università di Udine, and INFN Trieste, I-33100 Udine, Italy, 108Max-Planck-Institut für Physik, D-80805 München, Germany, 109Università di Siena, and INFN Pisa, I-53100 Siena, Italy, 110Universitat de Barcelona, ICC, IEEC-UB, E-08028 Barcelona, Spain, 111Universitat de Barcelona, ICC, IEEC-UB, E-08028 Barcelona, Spain, 112Deutsches Elektronen-Synchrotron, 113Università di Udine, and INFN Trieste, I-33100 Udine, Italy, 114INAF National Institute for Astrophysics, I-00136 Rome, Italy, 115Università di Udine, and INFN Trieste, I-33100 Udine, Italy, 116Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Astronomy Division, University of Oulu, Finland, 117Università di Pisa, and INFN Pisa, I-56126 Pisa, Italy, 118ETH Zurich, CH-8093 Zurich, Switzerland, 119Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka, University of Split and University of Zagreb, Croatia, 120Max-Planck-Institut für Physik, D-80805 München, Germany, 121Università di Padova and INFN, I-35131 Padova, Italy, 122Technische Universität Dortmund, D-44221 Dortmund, Germany, 123Universitat de Barcelona, ICC, IEEC-UB, E-08028 Barcelona, Spain, 124Institut de Fisica d'Altes Energies, 125Japanese MAGIC Consortium, ICRR, The University of Tokyo, Department of Physics and Hakubi Center, Kyoto University, Tokai University, The University of Tokushima, Japan, 126Deutsches Elektronen-Synchrotron, 127Technische Universität Dortmund, D-44221 Dortmund, Germany, 128Max-Planck-Institut für Physik, D-80805 München, Germany, 129Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Astronomy Division, University of Oulu, Finland, 130University of Łódź, PL-90236 Lodz, Poland, 131Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka, University of Split and University of Zagreb, Croatia, 132University of Łódź, PL-90236 Lodz, Poland, 133INAF National Institute for Astrophysics, I-00136 Rome, Italy, 134Max-Planck-Institut für Physik, D-80805 München, Germany, 135Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka, University of Split and University of Zagreb, Croatia, 136Finnish MAGIC Consortium, Tuorla Observatory, University of Turku and Astronomy Division, University of Oulu, Finland, 137INAF National Institute for Astrophysics, I-00136 Rome, Italy, 138Inst. for Nucl. Research and Nucl. Energy, BG-1784 Sofia, Bulgaria, 139Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka, University of Split and University of Zagreb, Croatia, 140Università di Padova and INFN, I-35131 Padova, Italy, 141Max-Planck-Institut für Physik, D-80805 München, Germany, 142ICREA and Institute for Space Sciences, 143Max-Planck-Institut für Physik, D-80805 München, Germany, 144Università di Udine, and INFN Trieste, I-33100 Udine, Italy, 145Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain, 146Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain, 147Max-Planck-Institut für Physik, D-80805 München, Germany, 148Institut de Fisica d'Altes Energies, 149Inst. de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain, 150Institute for Space Sciences, 151Universitat de Barcelona, ICC, IEEC-UB, E-08028 Barcelona, Spain

In this work we present data from observations with the MAGIC telescopes of SN 2014J detected in January 21 2014, the closest Type Ia supernova since Imaging Air Cherenkov Telescopes started to operate. We probe the possibility of very-high-energy (VHE; $E\geq100$ GeV) gamma rays produced in the early stages of Type Ia supernova explosions. We performed follow-up observations after this supernova explosion for 5 days, between January 27 and February 2 in 2014. Read More


The data from all observations of RX J0720.4-3125 conducted by XMM-Newton EPIC-pn with the same instrumental setup in 2000-2012 were reprocessed to form a homogenous data set of solar barycenter corrected photon arrival times registered from RX J0720.4-3125. Read More


Muon pairs can be produced in the annihilation of ultra-high energy (UHE, $E \gtrsim 10^{18} \,\mathrm{eV}$) photons with low energy cosmic background radiation in the intergalactic space, giving birth to neutrinos. Although the branching ratio of muon pair production is low, products of other channels, which are mainly electron/positron pairs, will probably transfer most of their energies into the new generated UHE photon in the subsequent interaction with the cosmic background radiation via Compton scattering in deep Klein-Nishina regime. The regeneration of these new UHE photons then provides a second chance to produce the muon pairs, enhancing the neutrino flux. Read More


2017Feb
Affiliations: 1Leiden Observatory, 2Leiden Observatory, 3Leiden Observatory

The low mass X-ray binary 2A 1822-371 is an eclipsing system with an accretion disc corona and with an orbital period of 5.57 hr. The primary is an 0. Read More


The luminosity ratio of electrons to protons as it is produced in stochastic acceleration processes in cosmic ray sources is an important quantity relevant for several aspects of the modeling of the sources themselves. It is usually assumed to be around 1:100 in the case of Galactic sources, while a value of 1:10 is typically assumed when describing extragalactic sources. It is supported by observations that the average ratios should be close to these values. Read More


Anomalies in the abundance measurements of short lived radionuclides in meteorites indicate that the protosolar nebulae was irradiated by a high amount of energetic particles (E$\gtrsim$10 MeV). The particle flux of the contemporary Sun cannot explain these anomalies. However, similar to T Tauri stars the young Sun was more active and probably produced enough high energy particles to explain those anomalies. Read More


The formation mechanism of CO clouds observed with NANTEN2 and Mopra telescope toward the stellar cluster Westerlund 2 is studied by three-dimensional magnetohydrodynamic (MHD) simulations taking into account the interstellar cooling. These molecular clouds show a peculiar shape composing of an arc-shaped cloud in one side of a TeV-ray source HESS J1023-575 and a linear distribution of clouds (jet clouds) in another side. We propose that these clouds are formed by the interaction of a jet with interstellar neutral hydrogen (HI) clumps. Read More


In this paper we treat the pre-ionisation problem in shocks over the velocity range $10 < v_{\rm s} < 1500$\,km/s in a self-consistent manner. We identify four distinct classes of solution controlled by the value of the shock precursor parameter, $\Psi = {\cal Q}/v_s$, where ${\cal Q}$ is the ionization parameter of the UV photons escaping upstream. This parameter determines both the temperature and the degree of ionisation of the gas entering the shock. Read More


The radio evolution of, so far the youngest known, Galactic supernova remnant (SNR) G1.9+0.3 is investigated by using three-dimensional (3D) hydrodynamic modeling and non-linear kinetic theory of cosmic ray (CR) acceleration in SNRs. Read More


(abridged) The dominant thermal mechanisms in the neutral interstellar medium, which acts as a star-forming gas reservoir, are uncertain in extremely metal-poor galaxies. Our objective is to identify the heating mechanisms in one such galaxy, IZw18, and assess the diagnostic value of fine-structure cooling lines. We also seek to constrain the mass of H$_2$, which, despite being an important catalyst and tracer of star formation, remains elusive in this object. Read More