The Supernova Remnant MSH 15-5 2 has been observed in very high energy ( VHE ) \gamma -rays using the H.E.S.S .
4-telescope array located in Namibia .
A \gamma -ray signal is detected at the 25 sigma level during an exposure of 22.1 hours live time .
The image reveals an elliptically shaped emission region around the pulsar PSR B1509–58 , with semi-major axis \sim 6 ^ { \prime } in the NW-SE direction and semi-minor axis \sim 2 ^ { \prime } .
This morphology coincides with the diffuse pulsar wind nebula as observed at X-ray energies by ROSAT .
The overall energy spectrum from 280 GeV up to 40 TeV can be fitted by a power law with photon index \Gamma = 2.27 \pm 0.03 _ { \textrm { \scriptsize stat } } \pm 0.20 _ { \textrm { \scriptsize syst } } .
The detected emission can be plausibly explained by inverse Compton scattering of accelerated relativistic electrons with soft photons .