Search for Very High Energy $\gamma$-Rays from the SNR 1006 with the HEGRA CT1 Air Imaging Cherenkov Telescope

Abstract.

The observation of $\gamma$-rays from SuperNova Remnants (SNRs) allows one to study the acceleration of charged particles ([1,2]) by SuperNova blast waves. The remnant of SN 1006 is a candidate for such studies: its 2 rims (NE and SW) have been detected as X-ray non-thermal sources by ASCA [3] and ROSAT [4] satellites, while TeV $\gamma$-ray emission has been observed from NE rim by the CANGAROO collaboration [5]. Both KeV and TeV radiation can be explained by synchrotron and inverse Compton emission of the same electron population (energy $\sim$50 TeV [6]. The HEGRA Collaboration searched for TeV emission from SNR 1006 from 1999 to the 2002. A preliminary analysis of these data is presented. From the experimental location one can observe SN1006 only at large Zenith angle (ZA), for this the data analysis requires substantial modifications. The analysis shows evidence for 5.5 $\sigma$ excess at NE rim.