R. Enomoto, K. Tsuchiya, Y. Adachi, S. Kabuki, P.G. Edwards, A. Asahara, G.V. Bicknell, R.W. Clay, Y. Doi, S. Gunji, S. Hara, T. Hara, T. Hattori, Sei. Hayashi, Y. Higashi, R. Inoue, C. Itoh, F. Kajino, H. Katagiri, A. Kawachi, S. Kawasaki, T. Kifune, R. Kiuchi, K. Konno, L.T. Ksenofontov, H. Kubo, J. Kushida, Y. Matsubara, Y. Mizumoto, M. Mori, H. Muraishi, Y. Muraki, T. Naito, T. Nakamori, D. Nishida, K. Nishijima, M. Ohishi, J.R. Patterson, R.J. Protheroe, Y. Sakamoto, M. Sato, S. Suzuki, T. Suzuki, D.L. Swaby, T. Tanimori, H. Tanimura, G.J. Thornton, S. Watanabe, T. Yamaoka, M. Yamazaki, S. Yanagita, T. Yoshida, T. Yoshikoshi, M. Yuasa, Y. Yukawa
We made stereoscopic observations of the Vela Pulsar region with two of the 10m diameter CANGAROO-III imaging atmospheric Cherenkov telescopes in January and February, 2004, in a search for sub-TeV gamma-rays from the pulsar and surrounding regions. We describe the observations, provide a detailed account of the calibration methods, and introduce the improved and bias-free analysis techniques employed for CANGAROO-III data. No evidence of gamma-ray emission is found from either the pulsar position or the previously reported position offset by 0.13 degree, and the resulting upper limits are a factor of five less than the previously reported flux from observations with the CANGAROO-I 3.8m telescope. Following the recent report by the H.E.S.S. group of TeV gamma-ray emission from the Pulsar Wind Nebula, which is 0.5 degree south of the pulsar position, we examined this region and found supporting evidence for emission extended over ~0.6 degree.