Discovery of Interacting Molecular Gas toward the TeV Gamma-Ray Peak of the SNR G 347.3--0.5

Details 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

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003pasj...55l..61f&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.55, No.5, pp. L61-L64

Astronomy and Astrophysics

Astronomy

58

Cosmic Rays, Ism: Cloud, Molecules, Supernova Remnants

Scientific paper

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.

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