Phase-resolved energy spectra of the Crab Pulsar in the range of 50-400 GeV measured with the MAGIC Telescopes
Creators: name: MAGIC Collaboration
name: Aleksić, J.
name: Alvarez, E. A.
name: Antonelli, L. A.
name: Antoranz, P.
name: Asensio, M.
name: Backes, M.
name: Barrio, J. A.
name: Bastieri, D.
name: González, J. Becerra
name: Bednarek, W.
name: Berdyugin, A.
name: Berger, K.
name: Bernardini, E.
name: Biland, A.
name: Blanch, O.
name: Bock, R. K.
name: Boller, A.
name: Bonnoli, G.
name: Tridon, D. Borla
name: Braun, I.
name: Bretz, T.
name: Cañellas, A.
name: Carmona, E.
name: Carosi, A.
name: Colin, P.
name: Colombo, E.
name: Contreras, J. L.
name: Cortina, J.
name: Cossio, L.
name: Covino, S.
name: Dazzi, F.
name: De Angelis, A.
name: De Caneva, G.
name: del Pozo, E. De Cea
name: De Lotto, B.
name: Mendez, C. Delgado
name: Ortega, A. Diago
name: Doert, M.
name: Domínguez, A.
name: Prester, D. Dominis
name: Dorner, D.
name: Doro, M.
name: Eisenacher, D.
name: Elsaesser, D.
name: Ferenc, D.
name: Fonseca, M. V.
name: Font, L.
name: Fruck, C.
name: López, R. J. García
name: Garczarczyk, M.
name: Garrido, D.
name: Giavitto, G.
name: Godinović, N.
name: Hadasch, D.
name: Häfner, D.
name: Herrero, A.
name: Hildebrand, D.
name: Höhne-Mönch, D.
name: Hose, J.
name: Hrupec, D.
name: Jogler, T.
name: Kellermann, H.
name: Klepser, S.
name: Krähenbühl, T.
name: Krause, J.
name: Kushida, J.
name: La Barbera, A.
name: Lelas, D.
name: Leonardo, E.
name: Lewandowska, N.
name: Lindfors, E.
name: Lombardi, S.
name: López, M.
name: López-Oramas, A.
name: Lorenz, E.
name: Makariev, M.
name: Maneva, G.
name: Mankuzhiyil, N.
name: Mannheim, K.
name: Maraschi, L.
name: Mariotti, M.
name: Martínez, M.
name: Mazin, D.
name: Meucci, M.
name: Miranda, J. M.
name: Mirzoyan, R.
name: Moldón, J.
name: Moralejo, A.
name: Munar-Adrover, P.
name: Niedzwiecki, A.
name: Nieto, D.
name: Nilsson, K.
name: Nowak, N.
name: Orito, R.
name: Paneque, D.
name: Paoletti, R.
name: Pardo, S.
name: Paredes, J. M.
name: Partini, S.
name: Perez-Torres, M. A.
name: Persic, M.
name: Peruzzo, L.
name: Pilia, M.
name: Pochon, J.
name: Prada, F.
name: Moroni, P. G. Prada
name: Prandini, E.
name: Gimenez, I. Puerto
name: Puljak, I.
name: Reichardt, I.
name: Reinthal, R.
name: Rhode, W.
name: Ribó, M.
name: Rico, J.
name: Rügamer, S.
name: Saggion, A.
name: Saito, K.
name: Saito, T. Y.
name: Salvati, M.
name: Satalecka, K.
name: Scalzotto, V.
name: Scapin, V.
name: Schultz, C.
name: Schweizer, T.
name: Shayduk, M.
name: Shore, S. N.
name: Sillanpää, A.
name: Sitarek, J.
name: Snidaric, I.
name: Sobczynska, D.
name: Spanier, F.
name: Spiro, S.
name: Stamatescu, V.
name: Stamerra, A.
name: Steinke, B.
name: Storz, J.
name: Strah, N.
name: Surić, T.
name: Takalo, L.
name: Takami, H.
name: Tavecchio, F.
name: Temnikov, P.
name: Terzić, T.
name: Tescaro, D.
name: Teshima, M.
name: Tibolla, O.
name: Torres, D. F.
name: Treves, A.
name: Uellenbeck, M.
name: Vankov, H.
name: Vogler, P.
name: Wagner, R. M.
name: Weitzel, Q.
name: Zabalza, V.
name: Zandanel, F.
name: Zanin, R.
name: Hirotani, K.
Publisher: name: arXiv
Year: 2011
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We use 73 h of stereoscopic data taken with the MAGIC telescopes to investigate the very high-energy (VHE) gamma-ray emission of the Crab pulsar. Our data show a highly significant pulsed signal in the energy range from 50 to 400 GeV in both the main pulse (P1) and the interpulse (P2) phase regions. We provide the widest spectra to date of the VHE components of both peaks, and these spectra extend to the energy range of satellite-borne observatories. The good resolution and background rejection of the stereoscopic MAGIC system allows us to cross-check the correctness of each spectral point of the pulsar by comparison with the corresponding (strong and well-known) Crab nebula flux. The spectra of both P1 and P2 are compatible with power laws with photon indices of 4.0 \pm 0.8 (P1) and 3.42 \pm 0.26 (P2), respectively, and the ratio P1/P2 between the photon counts of the two pulses is 0.54 \pm 0.12. The VHE emission can be understood as an additional component produced by the inverse Compton scattering of secondary and tertiary e\pm pairs on IR-UV photons.
description: 6 pages, 4 figures. Accepted for publication in A&amp;A on 16 February 2012