Muraishi, H.Tanimori, T.Yanagita, S.Yoshida, Y.Moriya, M.Kifune, T.Dazeley, S.Edwards, P.Gunji, S.Hara, S.Hara, T.Kawachi, A.Kubo, H.Matsubara, Y.Mizumoto, Y.Mori, M.Muraki, Y.Naito, T.Nishijima, K.Patterson, J.et al.2007-06-022007-06-022000Astronomy and Astrophysics: a European journal, 2000; 354(1):57-610004-6361http://hdl.handle.net/2440/32200We report the results of TeV gamma-ray observations of the shell type SNR RXJ1713.7-3946 (G347.3-0.5). The discovery of strong non-thermal X-ray emission from the northwest part of the remnant strongly suggests the existence of electrons with energies up to 100 TeV in the remnant, making the SNR a good candidate TeV gamma-ray source. We observed RXJ1713.7-3946 from May to August 1998 with the CANGAROO 3.8m atmospheric imaging Cerenkov telescope and obtained evidence for TeV gamma-ray emission from the NW rim of the remnant with the significance of 5.6 sigma. The observed TeV gamma-ray flux from the NW rim region was estimated to be (5.3 +/- 0.9[statistical] +/- 1.6[systematic]) * 10^{-12} photons cm^{-2} s^{-1} at energies >= 1.8 +/- 0.9 TeV. The data indicate that the emitting region is much broader than the point spread function of our telescope. The extent of the emission is consistent with that of hard X-rays observed by ASCA. This TeV gamma-ray emission can be attributed to the Inverse Compton scattering of the Cosmic Microwave Background Radiation by shock accelerated ultra-relativistic electrons. Under this assumption, a rather low magnetic field of 11 micro gauss is deduced for the remnant from our observation.enCopyright © 2000. © European Southern Observatory (ESO) 2000. Submitted to Cornell University’s online archive www.arXiv.org in 2000 by Hiroshi Muraishi. Post-print can be sourced from www.arxiv.org.Journal article000100122700008595570001563332Rowell, G. [0000-0002-9516-1581]