Aleksic, J.Alvarez, E. A.Antonelli, L. A.Antoranz, P.Asensio, M.Backes, M.Barrio, J. A.Bastieri, D.Becerra González, J.Bednarek, W.Berdyugin, A.Zabalza, V.Ferenc, D.Zandanel, F.Zanin, R.Boller, A.Bonnoli, G.Borla Tridon, D.Braun, I.Bretz, T.Cañellas, A.Lombardi, S.Carmona, E.Carosi, A.Fonseca, M. V.Colin, P.Colombo, E.Contreras, J. L.Cortina, J.Cossio, L.Covino, S.Dazzi, F.Peruzzo, L.De Angelis, A.De Caneva, G.De Cea del Pozo, E.Font, L.Delgado Mendez, C.De Lotto, B.Diago Ortega, A.Doert, M.Domínguez, A.Dominis Prester, D.López, M.Dorner, D.Doro, M.Fruck, C.García López, R. J.Garczarczyk, M.Garrido, D.Giavitto, G.Perez-Torres, M. A.Godinovic, N.Hadasch, D.López-Oramas, A.Häfner, D.Herrero, A.Hildebrand, D.Hirotani, K.Höhne-Mönch, D.Hose, J.Hrupec, D.Jogler, T.Persic, M.Kellermann, H.Lorenz, E.Klepser, S.Krähenbühl, T.Krause, J.Kushida, J.La Barbera, A.Lelas, D.Leonardo, E.Lindfors, E.Makariev, M.Maneva, G.Mankuzhiyil, N.Mannheim, K.Maraschi, L.Sitarek, J.Marcote, B.Mariotti, M.Pilia, M.Martínez, M.Mazin, D.Meucci, M.Miranda, J. M.Mirzoyan, R.Moldón, J.Moralejo, A.Biland, A.Munar-Adrover, P.Nieto, D.Nilsson, K.Pochon, J.Orito, R.Otte, N.Oya, I.Paneque, D.Paoletti, R.Pardo, S.Snidaric, I.Paredes, J. M.Partini, S.Prada, F.Prada Moroni, P. G.Prandini, E.Puerto Gimenez, I.Puljak, I.Berger, K.Reichardt, I.Reinthal, R.Sobczynska, D.Rhode, W.Ribó, M.Rico, J.Rissi, M.Rügamer, S.Saggion, A.Saito, K.Saito, T. Y.Bernardini, E.Salvati, M.Spanier, F.Satalecka, K.Scalzotto, V.Scapin, V.Schultz, C.Schweizer, T.Shayduk, M.Shore, S. N.Sillanpää, A.Spiro, S.Stamatescu, V.Stamerra, A.Steinke, B.Storz, J.Eisenacher, D.Strah, N.Suric, T.Blanch, O.Takalo, L.Takami, H.Tavecchio, F.Temnikov, P.Terzic, T.Tescaro, D.Teshima, M.Elsaesser, D.Tibolla, O.Torres, D. F.Treves, A.Bock, R. K.Uellenbeck, M.Vankov, H.Vogler, P.Wagner, R. M.Weitzel, Q.2012-03-052012-03-052011-01-01http://hdl.handle.net/2003/2937010.17877/DE290R-4316We report on the observation of γ-rays above 25 GeV from the Crab pulsar (PSR B0532+21) using the MAGIC I telescope. Two data sets from observations during the winter period 2007/2008 and 2008/2009 are used. In order to discuss the spectral shape from 100 MeV to 100 GeV, one year of public Fermi Large Area Telescope (Fermi-LAT) data are also analyzed to complement the MAGIC data. The extrapolation of the exponential cutoff spectrum determined with the Fermi-LAT data is inconsistent with MAGIC measurements, which requires a modification of the standard pulsar emission models. In the energy region between 25 and 100 GeV, the emission in the P1 phase (from –0.06 to 0.04, location of the main pulse) and the P2 phase (from 0.32 to 0.43, location of the interpulse) can be described by power laws with spectral indices of –3.1 ± 1.0stat ± 0.3syst and –3.5 ± 0.5stat ± 0.3syst, respectively. Assuming an asymmetric Lorentzian for the pulse shape, the peak positions of the main pulse and the interpulse are estimated to be at phases –0.009 ± 0.007 and 0.393 ± 0.009, while the full widths at half-maximum are 0.025 ± 0.008 and 0.053 ± 0.015, respectively.enInstitute of PhysicsThe Astrophysical Journal ; Volume 727, Number 100410.1088/0004-637X/742/1/43article (journal)