Detecton of TeV Gamma-Rays from SN1006

Toru Tanimori

Tokyo Institute of Technology

In 1995, strong synchrotron X-ray emission from the rims in supernova remnant SN1006 was observed by ASCA, and its hard spectrum o is considered to be the evidence of the shock acceleration of high energy electrons up to $\sim$ 100 TeV. With this Motivation, the TeV gamma-rays emission form SN1006 was observed by CANGAROO Imaging air \v Cerenkov telescope, and successfully detected in the NE rim with the significance of about 5 sigma. Observed integral flux ($>$ 3 TeV) is $\sim 3\times 10^{-12} cm^{-2}s{-1}$. This result has been reconfirmed by the observation of 1997 with the re-detection of TeV gamma-ray emission of about 8 sigma significance. This is the first detection of the very high energy gamma-rays from a supernova remnant. The detected integral flux in 1997 ($>$ 1.2 TeV) is $\sim 8\times 10^{-12} cm^{-2}s{-1}$. The morphology of gamma-rays shows that the emission region of TeV gamma rays is well consistent of that of X-rays by ASCA, and extends along the ridge of the NE rims. The detected fluxes are consistent with the predictions based on the inverse compton radiation of very high energy electrons in SN1006 and 2.7K cosimc background, and the magnetic field strength in a SNR was determined directly to be about 6 micro gauss.