Evidence for TeV gamma ray emission from Cassiopeia A

Details Evidence for TeV gamma ray emission from Cassiopeia A Evidence for TeV gamma ray emission from Cassiopeia A

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icrc....6.2451p&link_type=abstract

Proceedings of the 27th International Cosmic Ray Conference. 07-15 August, 2001. Hamburg, Germany. Under the auspices of the Int

Physics

1

Scientific paper

With the HEGRA stereoscopic system of imaging atmospheric Cherenkov telescopes, TeV γ-ray emission was detected from the Supernova remnant Cassiopeia A for the first time. The detection has a statistical significance of 5 σ. A flux of (5.8 ± 1.2stat ± 1.2syst) × 10-9 ph m-2 s-1 above 1 TeV is derived. The spectral distribution is consistent with a power law with a differential spectral index -2.5 ± 0.4stat ± 0.1syst between 1 and 10 TeV. The signal has a Crab-like spectrum, but only 3% of its flux. With this detection, the HEGRA system has demonstrated its currently unique ability to detect TeV γ-ray emission at the "centiCrab" scale. The detection of TeV γ-rays indicates that Cassiopeia A is a site of CR acceleration for particles - either nucleons or electrons - with multi-TeV energies. However, the assignment of the γ-ray emission to either or both particle populations relies on modeling. We discuss some important aspects in this paper.

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