ACKERMANN, Markus; AJELLO, Marco; B. ATWOOD, W.; BALDINI, Luca; BARBIELLINI, Guido; BASTIERI, D.; BECHTOL, K.; BELLAZZINI, R.; D. BLANDFORD, R.; D. BLOOM, E.; BONAMENTE, E.; W. BORGLAND, A.; BOTTACINI, E.; J. BRANDT, T.; BREGEON, J.; BRIGIDA, M.; BRUEL, Pascal; BUEHLER, R.; BUSON, S.; A. CALIANDRO, G.; A. CAMERON, R.; CARAVEO, P. A.; M. CASANDJIAN, J.; CECCHI, C.; CHARLES, E.; CHEKHTMAN, A.; CHIANG, J.; CIPRINI, S.; CLAUS, R.; COHEN-TANUGI, J.; CONRAD, J.; CUOCO, A.; CUTINI, S.; D'AMMANDO, F.; DE ANGELIS, A.; DE PALMA, F.; D. DERMER, C.; DO COUTO E SILVA, E.; S. DRELL, P.; DRLICA-WAGNER, A.; FALLETTI, L.; FAVUZZI, C.; J. FEGAN, S.; B. FOCKE, W.; FUKAZAWA, Y.; FUNK, S.; FUSCO, P.; GARGANO, F.; GASPARRINI, D.; GERMANI, S.; GIGLIETTO, N.; GIORDANO, F.; GIROLETTI, M.; GLANZMAN, T.; GODFREY, G.; A. GRENIER, I.; GUIRIEC, S.; GUSTAFSSON, M.; HADASCH, D.; HAYASHIDA, M.; HORAN, D.; E. HUGHES, R.; S. JACKSON, M.; JOGLER, T.; JÓHANNESSON, G.; S. JOHNSON, A.; KAMAE, T.; KNÖDLSEDER, Jürgen; KUSS, M.; LANDE, J.; LATRONICO, L.; M. LIONETTO, A.; LLENA GARDE, M.; LONGO, F.; LOPARCO, F.; LOTT, B.; N. LOVELLETTE, M.; LUBRANO, P.; N. MAZZIOTTA, M.; E. MCENERY, J.; MEHAULT, J.; F. MICHELSON, P.; MITTHUMSIRI, W.; MIZUNO, T.; A. MOISEEV, A.; MONTE, C.; E. MONZANI, M.; MORSELLI, A.; V. MOSKALENKO, I.; MURGIA, S.; NAUMANN-GODO, M.; P. NORRIS, J.; NUSS, E.; OHSUGI, T.; ORIENTI, M.; ORLANDO, E.; F. ORMES, J.; PANEQUE, D.; H. PANETTA, J.; PESCE-ROLLINS, M.; PIERBATTISTA, M.; PIRON, F.; PIVATO, G.; POON, H.; RAINÒ, S.; RANDO, R.; RAZZANO, M.; RAZZAQUE, S.; REIMER, A.; REIMER, O.; ROMOLI, C.; SBARRA, C.; D. SCARGLE, J.; SGRÒ, C.; J. SISKIND, E.; SPANDRE, G.; SPINELLI, P.; STAWARZ, Łukasz; W. STRONG, A.; J. SUSON, D.; TAJIMA, H.; TAKAHASHI, H.; TANAKA, T.; G. THAYER, J.; B. THAYER, J.; TIBALDO, L.; TINIVELLA, M.; TOSTI, G.; TROJA, E.; L. USHER, T.; VANDENBROUCKE, J.; VASILEIOU, V.; VIANELLO, G.; VITALE, V.; P. WAITE, A.; WALLACE, E.; S. WOOD, K.; WOOD, M.; YANG, Z.; ZAHARIJAS, G.; ZIMMER, S.

doi:10.1088/0004-637X/761/2/91

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The Astrophysical Journal. 2012, vol. 761, p. 91

American Astronomical Society

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We have performed an analysis of the diffuse gamma-ray emission with the Fermi Large Area Telescope (LAT) in the Milky Way halo region, searching for a signal from dark matter annihilation or decay. In the absence of a robust dark matter signal, constraints are presented. We consider both gamma rays produced directly in the dark matter annihilation/decay and produced by inverse Compton scattering of the e +/e - produced in the annihilation/decay. Conservative limits are derived requiring that the dark matter signal does not exceed the observed diffuse gamma-ray emission. A second set of more stringent limits is derived based on modeling the foreground astrophysical diffuse emission using the GALPROP code. Uncertainties in the height of the diffusive cosmic-ray halo, the distribution of the cosmic-ray sources in the Galaxy, the index of the injection cosmic-ray electron spectrum, and the column density of the interstellar gas are taken into account using a profile likelihood formalism, while the parameters governing the cosmic-ray propagation have been derived from fits to local cosmic-ray data. The resulting limits impact the range of particle masses over which dark matter thermal production in the early universe is possible, and challenge the interpretation of the PAMELA/Fermi-LAT cosmic ray anomalies as the annihilation of dark matter.< Réduire

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dark matter

Galaxy: halo

gamma rays: diffuse background

methods: statistical

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Constraints on the Galactic Halo Dark Matter from Fermi-LAT Diffuse Measurements

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