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The Perseus galaxy cluster was observed by the MAGIC Cherenkov telescope for a total effective time of 24.4 hr during 2008 November and December. The resulting upper limits on the gamma-ray emission above 100 GeV are in the range of 4.6-7.5 x 10(-12) cm(-2) s(-1) for spectral indices from -1.5 to -2.5, thereby constraining the emission produced by cosmic rays, dark matter annihilations, and the central radio galaxy NGC 1275. Results are compatible with cosmological cluster simulations for the cosmic-ray-induced gamma-ray emission, constraining the average cosmic ray-to-thermal pressure to < 4% for the cluster core region (< 8% for the entire cluster).

MAGIC GAMMA-RAY TELESCOPE OBSERVATION OF THE PERSEUS CLUSTER OF GALAXIES: IMPLICATIONS FOR COSMIC RAYS, DARK MATTER, AND NGC 1275

SHORE, STEVEN NEIL;
2010-01-01

Abstract

The Perseus galaxy cluster was observed by the MAGIC Cherenkov telescope for a total effective time of 24.4 hr during 2008 November and December. The resulting upper limits on the gamma-ray emission above 100 GeV are in the range of 4.6-7.5 x 10(-12) cm(-2) s(-1) for spectral indices from -1.5 to -2.5, thereby constraining the emission produced by cosmic rays, dark matter annihilations, and the central radio galaxy NGC 1275. Results are compatible with cosmological cluster simulations for the cosmic-ray-induced gamma-ray emission, constraining the average cosmic ray-to-thermal pressure to < 4% for the cluster core region (< 8% for the entire cluster).
2010
Aleksic, J; Antonelli, La; Antoranz, P; Backes, M; Baixeras, C; Balestra, S; Barrio, Ja; Bastieri, D; Gonzalez, Jb; Bednarek, W; Berdyugin, A; Berger, K; Bernardini, E; Biland, A; Bock, Rk; Bonnoli, G; Bordas, P; Tridon, Db; Bosch Ramon, V; Bose, D; Braun, I; Bretz, T; Britzger, D; Camara, M; Carmona, E; Carosi, A; Colin, P; Commichau, S; Contreras, Jl; Cortina, J; Costado, Mt; Covino, S; Dazzi, F; De Angelis, A; del Pozo, Ed; Reyes, Rd; De Lotto, B; De Maria, M; De Sabata, F; Mendez, Cd; Doert, M; Dominguez, A; Prester, Dd; Dorner, D; Doro, M; Elsaesser, D; Errando, M; Ferenc, D; Fonseca, Mv; Font, L; Galante, N; Lopez, Rjg; Garczarczyk, M; Gaug, M; Godinovic, N; Hadasch, D; Herrero, A; Hildebrand, D; Hohne Monch, D; Hose, J; Hrupec, D; Hsu, Cc; Jogler, T; Klepser, S; Krahenbuhl, T; Kranich, D; La Barbera, A; Laille, A; Leonardo, E; Lindfors, E; Lombardi, S; Longo, F; Lopez, M; Lorenz, E; Majumdar, P; Maneva, G; Mankuzhiyil, N; Mannheim, K; Maraschi, L; Mariotti, M; Martinez, M; Mazin, D; Meucci, M; Miranda, Jm; Mirzoyan, R; Miyamoto, H; Moldon, J; Moles, M; Moralejo, A; Nieto, D; Nilsson, K; Ninkovic, J; Orito, R; Oya, I; Paiano, S; Paoletti, R; Paredes, Jm; Partini, S; Pasanen, M; Pascoli, D; Pauss, F; Pegna, Rg; Perez Torres, Ma; Persic, M; Peruzzo, L; Prada, F; Prandini, E; Puchades, N; Puljak, I; Reichardt, I; Rhode, W; Ribo, M; Rico, J; Rissi, M; Rugamer, S; Saggion, A; Saito, Ty; Salvati, M; Sanchez Conde, Ma; Satalecka, K; Scalzotto, V; Scapin, V; Schultz, C; Schweizer, T; Shayduk, M; Shore, STEVEN NEIL; Sierpowska Bartosik, A; Sillanpaa, A; Sitarek, J; Sobczynska, D; Spanier, F; Spiro, S; Stamerra, A; Steinke, B; Struebig, Jc; Suric, T; Takalo, L; Tavecchio, F; Temnikov, P; Terzic, T; Tescaro, D; Teshima, M; Torres, Df; Vankov, H; Wagner, Rm; Zabalza, V; Zandanel, F; Zanin, R; Zapatero, J; Pfrommer, C; Pinzke, A; Enlin, Ta; Inoue, S; Ghisellini, G.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11568/142892
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