Discovery of Very High Energy Gamma Rays from 1ES 1218+30.4

Albert, J.; Aliu, E.; Anderhub, H.; Antoranz, P.; Armada, A.; Asensio, M.; Baixeras, C.; Barrio, J. A.; Bartelt, M.; Bartko, H.; Bastieri, D.; Bavikadi, S. R.; Bednarek, W.; Berger, K.; Bigongiari, C.; Biland, A.; Bisesi, E.; Bock, R. K.; Bretz, T.; Britvitch, I.; Camara, M.; Chilingarian, A.; Ciprini, S.; Coarasa, J. A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Curtef, V.; Danielyan, V.; Dazzi, F.; De Angelis, A.; 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.; Galante, N.; Garczarczyk, M.; Gaug, M.; Giller, M.; Goebel, F.; Hakobyan, D.; Hayashida, M.; Hengstebeck, T.; Höhne, D.; Hose, J.; Jacon, P.; Kalekin, O.; Kranich, D.; Laille, A.; Lenisa, T.; Liebing, P.; Lindfors, E.; Longo, F.; López, J.; López, M.; Lorenz, E.; Lucarelli, F.; Majumdar, P.; Maneva, G.; Mannheim, K.; Mariotti, M.; Martínez, M.; Mase, K.; Mazin, D.; Meucci, M.; Meyer, M.; Miranda, J. M.; Mirzoyan, R.; Mizobuchi, S.; Moralejo, A.; Nilsson, K.; Oña-Wilhelmi, E.; Orduña, R.; Otte, N.; Oya, I.; Paneque, D.; Paoletti, R.; Pasanen, M.; Pascoli, D.; Pauss, F.; Pavel, N.; Pegna, R.; Persic, M.; Peruzzo, L.; Piccioli, A.; Poller, M.; Prandini, E.; Rhode, W.; Rico, J.; Riegel, B.; Rissi, M. et al.
Referencia bibliográfica

The Astrophysical Journal, Volume 642, Issue 2, pp. L119-L122.

Fecha de publicación:
5
2006
Número de autores
131
Número de autores del IAC
0
Número de citas
109
Número de citas referidas
82
Descripción
The MAGIC collaboration has studied the high-frequency-peaked BL Lac object 1ES 1218+30.4, at a redshift z=0.182, using the MAGIC imaging air Cerenkov telescope located on the Canary Island of La Palma. A gamma-ray signal was observed with 6.4 σ significance. The differential energy spectrum for an energy threshold of 120 GeV can be fitted by a simple power law, yielding FE(E)=(8.1+/-2.1)×10-7[E/(250 GeV)]-3.0+/-0.4 TeV-1 m-2 s-1. During the 6 days of observation in 2005 January, no time variability on timescales of days was found within the statistical errors. The observed integral flux above 350 GeV is nearly a factor of 2 below the upper limit reported by the Whipple collaboration in 2003.