Bibcode
DOI
Albert, J.; Aliu, E.; Anderhub, H.; Antoranz, P.; Armada, A.; Baixeras, C.; Barrio, J. A.; Bartko, H.; Bastieri, D.; Becker, J. K.; Bednarek, W.; Berger, K.; Bigongiari, C.; Biland, A.; Bock, R. K.; Bordas, P.; Bosch-Ramon, V.; Bretz, T.; Britvitch, I.; Camara, M.; Carmona, E.; Chilingarian, A.; Coarasa, J. A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Costado, M. T.; Curtef, V.; Danielyan, V.; Dazzi, F.; De Angelis, A.; Delgado, C.; de los Reyes, R.; De Lotto, B.; Domingo-Santamaría, E.; Dorner, D.; Doro, M.; Errando, M.; Fagiolini, M.; Ferenc, D.; Fernández, E.; Firpo, R.; Flix, J.; Fonseca, M. V.; Font, L.; Fuchs, M.; Galante, N.; García-López, R.; Garczarczyk, M.; Gaug, M.; Giller, M.; Goebel, F.; Hakobyan, D.; Hayashida, M.; Hengstebeck, T.; Herrero, A.; Hirotani, K.; Höhne, D.; Hose, J.; Hsu, C.-C.; Jacon, P.; Jogler, T.; Kosyra, R.; Kranich, D.; Kritzer, R.; Laille, A.; Lindfors, E.; Lombardi, S.; Longo, F.; López, J.; López, M.; Lorenz, E.; Majumdar, P.; Maneva, G.; Mannheim, K.; Mansutti, O.; Mariotti, M.; Martínez, M.; Mazin, D.; Merck, C.; Meucci, M.; Meyer, M.; Miranda, J. M.; Mirzoyan, R.; Mizobuchi, S.; Moralejo, A.; Nieto, D.; Nilsson, K.; Ninković, J.; Oña-Wilhelmi, E.; Otte, N.; Oya, I.; Paneque, D.; Panniello, M.; Paoletti, R.; Paredes, J. M.; Pasanen, M.; Pascoli, D.; Pauss, F.; Pegna, R. et al.
Bibliographical reference
The Astrophysical Journal, Volume 669, Issue 2, pp. 1143-1149.
Advertised on:
11
2007
Journal
Citations
21
Refereed citations
15
Description
We report on very high energy γ-ray observations with the MAGIC
Telescope of the pulsar PSR B1951+32 and its associated nebula, CTB 80.
Our data constrain the cutoff energy of the pulsar to be less than 32
GeV, assuming the pulsed γ-ray emission to be exponentially cut
off. In the case that the cutoff follows a superexponential behavior,
the cutoff energy can be as high as ~60 GeV. The upper limit on the flux
of pulsed γ-ray emission above 75 GeV is
4.3×10-11 photons cm-2 s-1, and
the upper limit on the flux of steady emission above 140 GeV is
1.5×10-11 photons cm-2 s-1. We
discuss our results in the framework of recent model predictions and
other studies.