Detection of bridge emission above 50 GeV from the Crab pulsar with the MAGIC telescopes
: Aleksic J, Ansoldi S, Antonelli LA, Antoranz P, Babic A, Bangale P, de Almeida UB, Barrio JA, Gonzalez JB, Bednarek W, Bernardini E, Biasuzzi B, Biland A, Blanch O, Bonnefoy S, Bonnoli G, Borracci F, Bretz T, Carmona E, Carosi A, Colin P, Colombos E, Contreras JL, Cortina J, Covino S, Da Vela P, Dazzi E, De Angelis A, De Caneva G, De Lotto B, Mendez CCD, Doert M, Prester DD, Dorner D, Doro M, Einecke S, Eisenacher D, Elsaesser D, Farina E, Ferenc D, Fidalgo D, Fonseca MV, Font L, Frantzen K, Fruck C, Lopez RJG, Garczarczyk M, Terrats DG, Gaug M, Godinovic N, Munoz AG, Gozzini SR, Hadasch D, Hayashida M, Herrera J, Herrero A, Hildebrand D, Hirotani K, Hose J, Hrupec D, Idec W, Kadenius V, Kellermann H, Kodani K, Konno Y, Krause J, Kubo H, Kushida J, La Barbera A, Lelas D, Lewandowska N, Lindfors E, Lombardi S, Lopez M, Lopez-Coto R, Lopez-Oramas A, Lorenz E, Lozano I, Makariev M, Mallot K, Maneva G, Mankuzhiyil N, Mannheim K, Maraschi L, Marcote B, Mariotti M, Martinez M, Mazin D, Menzel U, Miranda JM, Mirzoyan R, Moralejo A, Munar-Adrover P, Nakajima D, Niedzwiecki A, Nilsson K, Nishijima K, Noda K, Nowak N, Orito R, Overkemping A, Paiano S, Palatiello M, Paneque D, Paoletti R, Paredes JM, Paredes-Fortuny X, Partini S, Persic M, Moroni PGP, Prandini E, Preziuso S, Puljak I, Reinthal R, Rhode W, Ribo M, Rico J, Garcia JR, Rugamer S, Saggion A, Saito TY, Saito K, Satalecka K, Scalzotto V, Scapin V, Schultz C, Schweizer T, Shore SN, Sillanpaa A, Sitarek J, Snidaric I, Sobczynska D, Spanier E, Stamatescu V, Stamerra A, Steinbring T, Storz M, Strzys M, Sun S, Suric T, Takalo L, Takami H, Tavecchio F, Temnikov P, Terzic T, Tescaro D, Teshima M, Thaele J, Tibolla O, Forres DE, Toyama T, Treves A, Uellenbeck M, Vogler P, Wagner RM, Zanin R
Publisher: EDP Sciences S A
: 2014
: Astronomy and Astrophysics
: ASTRONOMY & ASTROPHYSICS
: Astron astrophys
: L12
: 565
: 5
: 0004-6361
DOI: https://doi.org/10.1051/0004-6361/201423664
Conclusions. We discovered the bridge emission above 50 GeV between the two main pulses. This emission can not be explained with the existing theories. These data can be used for testing new theoretical models.