Enomoto, R.Tsuchiya, K.Adachi, Y.Kabuki, S.Edwards, P.Asahara, A.Bicknell, G.Clay, R.Doi, Y.Gunji, S.Hara, S.Hara, T.Hattori, T.Hayashi, S.Higashi, T.Inoue, R.Itoh, C.Kajino, F.Katagiri, H.Kawachi, A.et al.2007-01-162007-01-162006The Astrophysical Journal (ApJ), 2006; 638(1):397-4080004-637X1538-4357http://hdl.handle.net/2440/23584© 2006 The American Astronomical Society. All rights reserved. Submitted to Cornell University’s online archive www.arXiv.org in 2006 by Ryoji Enomoto. Post-print sourced from www.arxiv.org.We made stereoscopic observations of the Vela pulsar region with two of the 10 m diameter CANGAROO-III imaging atmospheric Cerenkov telescopes in 2004 January and February 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, and the resulting upper limits are a factor of 5 less than the previously reported flux from observations with the CANGAROO-I 3.8 m 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 south of the pulsar position, we examined this region and found supporting evidence for emission extended over ~0°.6.enJournal article002006001510.1086/4988580002351321000352-s2.0-3364455769953306Clay, R. [0000-0002-9040-9648]