Very High Energy Gamma Rays from the Vela Pulsar/Nebula
Yoshikoshi, T. · Kifune, T. · Dazeley, S. A. · Edwards, P. G. · Hara, T. · Hayami, Y. · Kamei, S. · Kita, R. · Konishi, T. · Masaike, A. · Matsubara, Y. · Mizumoto, Y. · Mori, M. · Muraishi, H. · Muraki, Y. · Naito, T. · Nishijima, K. · Ogio, S. · Patterson, J. R. · Roberts, M. D. · Rowell, G. P. · Sako, T. · Sakurazawa, K. · Susukita, R. · Suzuki, A. · Suzuki, R. · Tamura, T. · Tanimori, T. · Thornton, G. J. · Yanagita, S. · Yoshida, T.
Original · EN
We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Cherenkov telescope near Woomera, South Australia every year since 1992. This is the first concerted search for pulsed and unpulsed emission from the Vela region, and the imaging technique also allows the location of the emission within the field of view to be examined. A significant excess of gamma-ray-like events is found offset from the Vela pulsar to the southeast by about 0.13deg. The excess shows the behavior expected of gamma-ray images when the asymmetry cut is applied to the data. There is no evidence for the emission being modulated with the pulsar period -- in contrast to earlier claims of signals from the Vela pulsar direction.
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