Observation of the shell-type supernova remnant RXJ0852.0-4622 with H.E.S.S.

Shell-type supernova remnants are prime candidates for the acceleration of galactic cosmic rays. The detection of TeV γ-ray emission from the shells is believed to be a key to unravelling the underlying acceleration mechanisms. In 2004 and 2005, the shell-type supernova remnant RXJ0852.0-4622 (also called G266.2-1.2)was observed and detected with H.E.S.S., an array of four Imaging Atmospheric Cherenkov Telescopes located in Namibia, dedicated to observations of γ-rays above 100 GeV. The energy spectrum of the source can be described by a power law and the integral flux is similar to the flux from the Crab nebula. The emission region is found to be clearly extended, making RX J0852.0-4622 the second shell-type supernova remnant which has been spatially resolved in TeV energies [1]. The morphology of the TeV emission is well correlated with the X-ray morphology. The results of the observations will be presented and possible implications will be discussed