Very High Energy Gamma Rays from the Vela Pulsar Direction
Abstract
We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Cherenkov telescope near Woomera, South Australia between January 1993 and March 1995. Evidence of an unpulsed gamma-ray signal has been detected at the 5.8 sigma level. The detected gamma-ray flux is (2.9 +/- 0.5 +/- 0.4) x 10^-12 photons cm^-2 sec^-1 above 2.5 +/- 1.0 TeV and the signal is consistent with steady emission over the two years. The gamma-ray emission region is offset from the Vela pulsar position to the southeast by about 0.13 deg. No pulsed emission modulated with the pulsar period has been detected and the 95 % confidence flux upper limit to the pulsed emission from the pulsar is (3.7 +/- 0.7) x 10^-13 photons cm^-2 sec^-1 above 2.5 +/- 1.0 TeV.
Keywords
Cite
@article{arxiv.astro-ph/9707203,
title = {Very High Energy Gamma Rays from the Vela Pulsar Direction},
author = {T. Yoshikoshi and T. Kifune and S. A. Dazeley and P. G. Edwards and T. Hara and Y. Hayami and F. Kakimoto and T. Konishi and A. Masaike and Y. Matsubara and T. Matsuoka and Y. Mizumoto and M. Mori and H. Muraishi and Y. Muraki and T. Naito and K. Nishijima and S. Oda and S. Ogio and T. Ohsaki and J. R. Patterson and M. D. Roberts and G. P. Rowell and T. Sako and K. Sakurazawa and R. Susukita and A. Suzuki and T. Tamura and T. Tanimori and G. J. Thornton and S. Yanagita and T. Yoshida},
journal= {arXiv preprint arXiv:astro-ph/9707203},
year = {2011}
}
Comments
18 pages, 3 figures, LaTeX with AASTeX, accepted for publication in ApJ Letters