Molecular gas interacting with the TeV gamma-ray SNR G347.3-0.5

Details Molecular gas interacting with the TeV gamma-ray SNR G347.3-0.5 Molecular gas interacting with the TeV gamma-ray SNR G347.3-0.5

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004asthe..97..287m&link_type=abstract

The Astronomical Herald (ISSN 0374-2466), Vol. 97, No. 5, p. 287 - 293 (2004)

Astronomy and Astrophysics

Astronomy

Supernova Remnants, Gamma Rays

Scientific paper

Supernova remanants (SNR) are believed to be major sites of acceleration of Galactic cosmic-rays whose energy is ~1015erg. In particular, it has been a big issue whether supernova remnants emitting TeV-gamma rays are sites of proton acceleration or not. We present new CO observations of molecular gas at 1 kpc distance interacting with the TeV gamma-ray SNR G347.3-0.5. Dense molecular gas toward the TeV-gamma SNR is a good predictor to verify the existence of cosmic-ray protons. One of the molecular clumps of ~200 solar mass coincides with the gamma-ray peak, providing strong evidence for proton acceleration. We have estimated the total energy of accelerated protons to be about 1048erg, which corresponds to an acceleration efficiency of about 0.001, posing an observational constraint on the proton acceleration.

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