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Abramowski, A; Acero, F; Aharonian, F; Akhperjanian, A G; Anton, G; Balenderan, S; Balzer, A; Barnacka, A; Becherini, Y; Becker Tjus, J; Bernlöhr, K; Birsin, E; Biteau, J; Bochow, A; Boisson, C; Bolmont, J; Bordas, P; Brucker, J; Brun, F; Brun, P; Bulik, T; Carrigan, S; Casanova, S; Cerruti, M; Chadwick, P M; Chaves, R C G; Cheesebrough, A; Colafrancesco, S; Cologna, G; Conrad, J; Couturier, C; Dalton, M; Daniel, M K; Davids, I D; Degrange, B; Deil, C; deWilt, P; Dickinson, H J; Djannati-Ataï, A; Domainko, W; Drury, L O'C; Dubus, G; Dutson, K; Dyks, J; Dyrda, M; Egberts, K; Eger, P; Espigat, P; Fallon, L; Farnier, C.
Affiliation
  • Abramowski A; Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany.
  • Acero F; Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France.
  • Aharonian F; Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany and Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland and National Academy of Sciences of the Republic of Armenia, Armenia, Yerevan.
  • Akhperjanian AG; National Academy of Sciences of the Republic of Armenia, Armenia, Yerevan and Yerevan Physics Institute, 2 Alikhanian Brothers Street, 375036 Yerevan, Armenia.
  • Anton G; Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Strasse 1, D 91058 Erlangen, Germany.
  • Balenderan S; University of Durham, Department of Physics, South Road, Durham DH1 3LE, United Kingdom.
  • Balzer A; DESY, D-15735 Zeuthen, Germany and Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, D 14476 Potsdam, Germany.
  • Barnacka A; Nicolaus Copernicus Astronomical Center, ulica Bartycka 18, 00-716 Warsaw, Poland and CEA Saclay, DSM/Irfu, F-91191 Gif-Sur-Yvette Cedex, France.
  • Becherini Y; 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, and Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France.
  • Becker Tjus J; Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, D 44780 Bochum, Germany.
  • Bernlöhr K; Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany and Institut für Physik, Humboldt-Universität zu Berlin, Newtonstrasse 15, D 12489 Berlin, Germany.
  • Birsin E; Institut für Physik, Humboldt-Universität zu Berlin, Newtonstrasse 15, D 12489 Berlin, Germany.
  • Biteau J; Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France.
  • Bochow A; Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany.
  • Boisson C; LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France.
  • Bolmont J; LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252, Paris Cedex 5, France.
  • Bordas P; Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany.
  • Brucker J; Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Strasse 1, D 91058 Erlangen, Germany.
  • Brun F; Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France.
  • Brun P; CEA Saclay, DSM/Irfu, F-91191 Gif-Sur-Yvette Cedex, France.
  • Bulik T; Astronomical Observatory, The University of Warsaw, Aleje Ujazdowskie 4, 00-478 Warsaw, Poland.
  • Carrigan S; Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany.
  • Casanova S; Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany and Unit for Space Physics, North-West University, Potchefstroom 2520, South Africa.
  • Cerruti M; LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France.
  • Chadwick PM; University of Durham, Department of Physics, South Road, Durham DH1 3LE, United Kingdom.
  • Chaves RC; Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany and CEA Saclay, DSM/Irfu, F-91191 Gif-Sur-Yvette Cedex, France.
  • Cheesebrough A; University of Durham, Department of Physics, South Road, Durham DH1 3LE, United Kingdom.
  • Colafrancesco S; School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein, Johannesburg, 2050 South Africa.
  • Cologna G; Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany.
  • Conrad J; Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, SE-10691 Stockholm, Sweden.
  • Couturier C; LPNHE, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, CNRS/IN2P3, 4 Place Jussieu, F-75252, Paris Cedex 5, France.
  • Dalton M; Institut für Physik, Humboldt-Universität zu Berlin, Newtonstrasse 15, D 12489 Berlin, Germany and Université Bordeaux 1, CNRS/IN2P3, Centre d'Études Nucléaires de Bordeaux Gradignan, 33175 Gradignan, France.
  • Daniel MK; University of Durham, Department of Physics, South Road, Durham DH1 3LE, United Kingdom.
  • Davids ID; University of Namibia, Department of Physics, Private Bag 13301, Windhoek, Namibia.
  • Degrange B; Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France.
  • Deil C; Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany.
  • deWilt P; School of Chemistry and Physics, University of Adelaide, Adelaide 5005, Australia.
  • Dickinson HJ; Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, SE-10691 Stockholm, Sweden.
  • Djannati-Ataï A; 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.
  • Domainko W; Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany.
  • Drury LO; Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland.
  • Dubus G; UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG) UMR 5274, Grenoble, F-38041, France.
  • Dutson K; Department of Physics and Astronomy, The University of Leicester, University Road, Leicester, LE1 7RH, United Kingdom.
  • Dyks J; Nicolaus Copernicus Astronomical Center, ulica Bartycka 18, 00-716 Warsaw, Poland.
  • Dyrda M; Instytut Fizyki Ja̧drowej PAN, ulica Radzikowskiego 152, 31-342 Kraków, Poland.
  • Egberts K; Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria.
  • Eger P; Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Strasse 1, D 91058 Erlangen, Germany.
  • Espigat P; 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.
  • Fallon L; Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland.
  • Farnier C; Oskar Klein Centre, Department of Physics, Stockholm University, Albanova University Center, SE-10691 Stockholm, Sweden.
Phys Rev Lett ; 110(4): 041301, 2013 Jan 25.
Article de En | MEDLINE | ID: mdl-25166149
ABSTRACT
Gamma-ray line signatures can be expected in the very-high-energy (E(γ)>100 GeV) domain due to self-annihilation or decay of dark matter (DM) particles in space. Such a signal would be readily distinguishable from astrophysical γ-ray sources that in most cases produce continuous spectra that span over several orders of magnitude in energy. Using data collected with the H.E.S.S. γ-ray instrument, upper limits on linelike emission are obtained in the energy range between ∼ 500 GeV and ∼ 25 TeV for the central part of the Milky Way halo and for extragalactic observations, complementing recent limits obtained with the Fermi-LAT instrument at lower energies. No statistically significant signal could be found. For monochromatic γ-ray line emission, flux limits of (2 × 10(-7) -2 × 10(-5)) m(-2) s(-1) sr(-1) and (1 × 10(-8) -2 × 10(-6)) m(-2) s(-1)sr(-1) are obtained for the central part of the Milky Way halo and extragalactic observations, respectively. For a DM particle mass of 1 TeV, limits on the velocity-averaged DM annihilation cross section ⟨σv⟩(χχ → γγ) reach ∼ 10(-27) cm(3)s(-1), based on the Einasto parametrization of the Galactic DM halo density profile.
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Collection: 01-internacional Base de données: MEDLINE Langue: En Journal: Phys Rev Lett Année: 2013 Type de document: Article Pays d'affiliation: Allemagne
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Collection: 01-internacional Base de données: MEDLINE Langue: En Journal: Phys Rev Lett Année: 2013 Type de document: Article Pays d'affiliation: Allemagne