TeV Gamma-Ray Observations of the Supernova Remnant RCW86 with the CANGAROO-II Telescope

Details TeV Gamma-Ray Observations of the Supernova Remnant RCW86 with the CANGAROO-II Telescope TeV Gamma-Ray Observations of the Supernova Remnant RCW86 with the CANGAROO-II Telescope

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....4.2397w&link_type=abstract

Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I

Physics

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Scientific paper

The supernova remnant(SNR) RCW86(G315.4-2.3) has been observed as our third SNR in 2001 and 2002 with the CANGAROO-I I 10 m telescope from Wo omera, South Australia, to further test the hypothesis that SNR accelerate cosmic rays. RCW86 is a type I I and shell-like supernova remnant, and ASCA detected non-thermal X-ray emission from the southwest shell of RCW86, which is brighter than that from SN1006. The multiwavelength spectrum of RCW86 derived from radio and X-ray data indicates that the emission is due to the synchrotron radiation, and it is argued that high energy electrons emitting the detected synchrotron radiation are expected to be accelerated up to 20 TeV.

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