@article{oai:ir.soken.ac.jp:00003294,
 author = {池内, 了 and FUKUI, Yasuo and MORIGUCHI, Yoshiaki and TAMURA, Keisuke and YAMAMOTO, Hiroaki and TAWARA, Yuzuru and MIZUNO, Norikazu and ONISHI, Toshikazu and MIZUNO, Akira and UCHIYAMA, Yasunobu and HIRAGA, Junko and TAKAHASHI, Tadayuki and YAMASHITA, Koujin and IKEUCHI, Satoru},
 issue = {5},
 journal = {Publications of the Astronomical Society of Japan, Publications of the Astronomical Society of Japan},
 month = {Oct},
 note = {application/pdf, Supernova remnants ( = SNR) are suggested to be sites of cosmic-ray acceleration. In particular, it has been an issue of keen interest whether cosmic ray protons are being accelerated in a SNR which emits TeV γ-rays. A crucial observational test for this is to find dense molecular gas towards the SNR, because such molecular gas can best verify the existence of cosmic-ray protons via pion decay to γ-rays. Here, we show that new high-resolution mm-wave observations of interstellar CO molecule have revealed molecular gas at 1kpc distance interacting with the TeV γ-ray SNR G 347.3 - 0.5, and that a molecular cloud of ˜ 200 solar masses is clearly associated with the TeV γ-ray peak, providing strong evidence for proton acceleration. We have estimated the total energy of accelerated protons to be ˜ 1048 erg, which corresponds to an acceleration efficiency of ˜ 0.001, posing an observational constraint on the proton acceleration.},
 pages = {L61--L64},
 title = {Discovery of Interacting Molecular Gas toward the TeV Gamma-Ray Peak of the SNR G 347.3-0.5},
 volume = {55},
 year = {2003}
}