2026-03-10T00:16:48Z https://ir.soken.ac.jp/oai

oai:ir.soken.ac.jp:00003294 2023-06-20T14:11:59Z 1:274

Discovery of Interacting Molecular Gas toward the TeV Gamma-Ray Peak of the SNR G 347.3-0.5 Discovery of Interacting Molecular Gas toward the TeV Gamma-Ray Peak of the SNR G 347.3-0.5 池内, 了 FUKUI, Yasuo MORIGUCHI, Yoshiaki TAMURA, Keisuke YAMAMOTO, Hiroaki TAWARA, Yuzuru MIZUNO, Norikazu ONISHI, Toshikazu MIZUNO, Akira UCHIYAMA, Yasunobu HIRAGA, Junko TAKAHASHI, Tadayuki YAMASHITA, Koujin IKEUCHI, Satoru 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. journal article The Astronomical Society of Japan 2003-10 VoR application/pdf Publications of the Astronomical Society of Japan 5 55 L61 L64 Publications of the Astronomical Society of Japan 00046264 https://ir.soken.ac.jp/record/3294/files/55052495.pdf https://ir.soken.ac.jp/records/3294 eng 10.1093/pasj/55.5.L61 https://doi.org/10.1093/pasj/55.5.L61 Copyright http://pasj.asj.or.jp/info/subscription.html © 2003. The Astronomical Society of Japan.