B. Khélifi

VHE γ-ray emitting pulsar wind nebulae discovered by H.E.S.S.

Recent advances in very‐high‐energy (VHE) gamma‐ray astronomy have opened a new observational window on the physics of pulsars. The high sensitivity of current imaging atmospheric Cherenkov telescopes, and in particular of the H.E.S.S. array, has already led to the discovery of about a dozen VHE‐emitting pulsar wind nebulae (PWNe) and PWN candidates. These include the plerions in the composite supernova remnants MSH 15–52, G21.5–0.9, Kes 75, and Vela, two sources in the Kookaburra, and the nebula of PSR B1823–13. This VHE emission is generally interpreted as inverse Compton emission from the relativistic electrons and positrons accelerated by the pulsar and its wind; as such, it can yield a more direct spatial and spectral view of the accelerated particles than can be inferred from observations of their synchrotron emission. The VHE‐emitting PWNe detected by the H.E.S.S. telescopes are reviewed and the implications for pulsar physics discussed.