  The idea that the shocks from supernova remnants (SNR) expanding into the
interstellar medium (ISM) accelerate CR is still popular one but a number of
authors have drawn attention to the fact that the experimental evidence for the
presence of gamma rays from the expected interaction of CR with gas in the
remnant is poor. Indeed, it is claimed that many SNR are not `seen' in GeV or
TeV gamma rays, whereas `they should have been'.
  We have looked at this problem and we conclude that the idea of CR production
in SNR cannot be faulted in this way, if the evacuation of ambient gas by the
stellar wind of the progenitor star and, frequently, by associated earlier
close-by SN, is taken into account; such phenomena are expected for the
important Type II SN which result from very massive stars.
  Other SNR have, apparently, been seen and the interaction of SNR-accelerated
particles with adjacent molecular clouds has been deemed responsible. However,
we worry about this interpretation because of the slow progress of the SNR
shock through such clouds, although electron-effects may, indeed, contribute.
  This paper is devoted mainly to the visibility of nearby SNR in gamma rays
although many of the arguments also relate to remote SNR. For the nearby SNR
another problem enters the scene: the large angular spread of the remnant. It
is especially important for the old SNR, where cosmic rays have already
diffused to a large distance from the SNR center. We have also examined the
effect of the 'anomalous diffusion' of CR propagation in the non-homogeneous
interstellar medium on the visibility of SNR for gamma rays of different
energies.
