VHE gamma-ray observation of the Crab Nebula and its pulsar with the MAGIC telescope
- ALBERT J
- ALIU E
- ANDERHUB H
- ANTORANZ P
- ARMADA A
- BAIXERAS C
- BARRIO JA
- BARTKO H
- 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
- 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
- LONGO F
- LOPEZ J
- LOPEZ M
- LORENZ E
- MAJUMDAR P
- MANEVA G
- MANNHEIM K
- MANSUTTI O
- MARTINEZ M
- MAZIN D
- MERCK C
- MEUCCI M
- MEYER M
- MIRANDA JM
- MIRZOYAN R
- MIZOBUCHI S
- MORALEJO A
- NIETO D
- NILSSON K
- NINKOVIC J
- ONA WILHELMI E
- OTTE N
- OYA I
- PANEQUE D
- PANNIELLO M
- PAOLETTI R
- PAREDES JM
- PASANEN M
- PAUSS F
- PEGNA R
- PERSIC M
- PERUZZO L
- PICCIOLI A
- POLLER M
- PUCHADES N
- RAYMERS A
- RHODE W
- RIBO M
- RICO J
- RISSI M
- ROBERT A
- RUGAMER S
- SANCHEZ A
- SCAPIN V
- SCHMITT R
- SCHWEIZER T
- SHAYDUK M
- SHINOZAKI K
- SHORE SN
- 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.
- BASTIERI, DENIS
- DORO, MICHELE
- LOMBARDI, SAVERIO
- MARIOTTI, MOSE'
- PASCOLI, DONATELLA
- PRANDINI, ELISA
- SAGGION, ANTONIO
- SARTORI, PAOLO
- SCALZOTTO, VILLI MARIO
DOIAbstract
We report about very high energy (VHE) gamma-ray observations of the Crab Nebula with the MAGIC telescope. The gamma-ray flux from the nebula was measured between 60 GeV and 9 TeV. The energy spectrum can be described by a curved power law dF/dE = f(0)(E/300 GeV)([a+b log)((E/300 GeV)])(10) with a flux normalization f(0) of (6.0 +/- 0.2(stat)) x 10(-10) cm(-2) s(-1) TeV-1, a = 2.31 +/- 0.06(stat), and b = 0.26 +/- 0.07(stat). The peak in the spectral energy distribution is estimated at 77 +/- 35 GeV. Within the observation time and the experimental resolution of the telescope, the gamma-ray emission is steady and pointlike. The emission's center of gravity coincides with the position of the pulsar. Pulsed gamma-ray emission from the pulsar ...
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