Résumé
The composite supernova remnant (SNR) MSH 15-52 comprises the bright X-ray
pulsar wind nebula (PWN) of PSR B1509-58, surrounded by a shell which is a
prominent object in the radio domain. H.E.S.S. had discovered extended
very-high-energy (VHE) gamma-ray emission coincident with the PWN. With
additional H.E.S.S. observations performed since the 2005 discovery paper, we
study the properties of the emission in greater detail. We compare the VHE
gamma-ray morphology of the PWN with that in synchrotron emission, obtained
from archival X-ray observations, and discuss the implications on the magnetic
field in the nebula. In particular, we discuss potential extended gamma-ray
emission beyond the X-ray PWN, which may allow for conclusions on scenarios of
PWNe as sources of cosmic ray electrons and positrons.