ABSTRACT
It is convenient to divide the discussion of gamma-ray observations of supernova remnants (SNRs) into two parts: plerions and shell-type SNRs. As we have seen in the previous chapter, there is no hard distinction between the two. VHE observations have been most pertinent to plerions and HE observations to shelltype SNRs. Neither set of observations have provided the smoking gun that would uniquely tie the origin of the cosmic radiation with SNRs.
