  We present the results of a BeppoSAX observation of the Supernova Remnant MSH
15-52, associated with the pulsar PSR B1509-58, and discuss its main
morphological and spectroscopic properties in the 1.6--200 keV energy range
(MECS and PDS instruments). The two main structures of the remnant, the
Southern Nebula, the plerion centered on the pulsar, and the Northern Nebula,
are clearly visible in the MECS, with the former showing a much a harder
spectrum. Furthermore, a diffuse extended emission surrounds the whole remnant
up to ~ 17' from the center. Non-thermal flux is detected in the PDS up to 200
keV as well, and it appears that also in this energy range the emission is not
concentrated in the central region around the pulsar. These data imply that the
plerion extends up to a few tens of parsecs from the pulsar.
