Y. Sakamoto, K. Nishijima, T. Mizukami, E. Yamazaki, J. Kushida, R. Enomoto, M. Ohishi, G. V. Bicknell, R. W. Clay, P. G. Edwards, S. Gunji, S. Hara, T. Hattori, S. Hayashi, Y. Higashi, K. Inoue, S. Kabuki, F. Kajino, H. Katagiri, A. Kawachi, T. Kifune, R. Kiuchi, H. Kubo, R. Mizuniwa, M. Mori, H. Muraishi, T. Naito, T. Nakamori, S. Nakano, D. Nishida, A. Seki, V. Stamatescu, T. Suzuki, D. L. Swaby, T. Tanimori, G. Thornton, F. Tokanai, K. Tsuchiya, S. Watanabe, Y. Yamada, S. Yanagita, T. Yoshida, T. Yoshikoshi, and Y. Yukawa
PKS2155-304 between 2006 July 28 (MJD 53944) and August 2, triggered by the H.E.S.S. report that the source was in a high state of TeV gamma-ray emission. A signal was detected at the 4.8σ level in an e ective live time of 25.1 hours during the outburst period. The fluxof Very High Energy gammarays from the CANGAROO-III observations shows the variability on the time scale of less than a few hours. The averaged integral ux above 660 GeV is (1.6+-0.3stat+-0.5syst)×10-11cm-2sec-1 which corresponds to ∼45% of the flux observed from the Crab nebula. Follow-up observations between August 17 (MJD 53964) and 25 indicate the source activity had decreased.