Observation of VHE gamma-rays from Cassiopeia A with the MAGIC telescope RID B-5372-2009
- Albert J
- Aliu E
- Anderhub H
- Antoranz P
- Armada A
- Baixeras C
- Barrio JA
- Bartko H
- Bastieri D
- Becker JK
- Bednarek W
- Berger K
- Bigongiari C
- Biland A
- Bock RK
- Bordas P
- Bosch-Ramon V
- Bretz T
- Britvitch I
- Camara M
- Carmona E
- Chilingarian A
- Coarasa JA
- Commichau S
- Contreras JL
- Cortina J
- Costado MT
- Curtef V
- Danielyan V
- Dazzi F
- De Angelis A
- Delgado C
- de los Reyes R
- De Lotto B
- Domingo-Santamaria E
- Dorner D
- Doro M
- Errando M
- Fagiolini M
- Ferenc D
- Fernandez E
- Firpo R
- Flix J
- Fonseca MV
- Font L
- Fuchs M
- Galante N
- Garcia-Lopez R
- Garczarczyk M
- Gaug M
- Giller M
- Goebel F
- Hakobyan D
- Hayashida M
- Hengstebeck T
- Herrero A
- Hohne D
- Hose J
- Hsu CC
- Jacon P
- Jogler T
- Kosyra R
- Kranich D
- Kritzer R
- Laille A
- Lindfors E
- Lombardi S
- Longo F
- Lopez J
- Lopez M
- Lorenz E
- Majumdar P
- Maneva G
- Mannheim K
- Mansutti O
- Mariotti M
- Martinez M
- Mazin D
- Merck C
- Meucci M
- Meyer M
- Miranda JM
- Mirzoyan R
- Mizobuchi S
- Moralejo A
- Nilsson K
- Ninkovic J
- Ona-Wilhelmi E
- Otte N
- Oya I
- Paneque D
- Panniello M
- Paoletti R
- Paredes JM
- Pasanen M
- Pascoli D
- Pauss F
- Pegna R
- Persic M
- Peruzzo L
- Piccioli A
- Poller M
- Puchades N
- Prandini E
- Raymers A
- Rhode W
- Ribo M
- Rico J
- Rissi M
- Robert A
- Rugamer S
- Saggion A
- Sanchez A
- Sartori P
- Scalzotto V
- Scapin V
- Schmitt R
- Schweizer T
- Shayduk M
- Shinozaki K
- Shore S.N.
- Sidro N
- Sillanpaa A
- Sobczynska D
- Stamerra A
- Stark LS
- Takalo L
- Temnikov P
- Tescaro D
- Teshima M
- Tonello N
- Torres DF
- Turini N
- Vankov H
- Vitale V
- Wagner RM
- Wibig T
- Wittek W
- Zandanel F
- Zanin R
- Zapatero J
DOIAbstract
Aims. We searched for very high energy (VHE)gamma-ray emission from the supernova remnant Cassiopeia A Methods. The shell-type supernova remnant Cassiopeia A was observed with the 17 m MAGIC telescope between July 2006 and January 2007 for a total time of 47 h. Results. The source was detected above an energy of 250 GeV with a significance of 5.2s and a photon flux above 1 TeV of (7.3 +/- 0.7(stat) +/- 2.2(sys)) x 10(-13) cm(-2)s(-1). The photon spectrum is compatible with a power law dN/dE proportional to E-r with a photon index Gamma = 2.3 +/- 0.2(stat) +/- 0.2(sys). The source is point- like within the angular resolution of the telescope
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