  VLA surface brightness and spectral index maps of the evolving extended
emission of the triple symbiotic star CH Cygni are presented. These are derived
from observations at 4.8, 8.4 and 14GHz between 1985 and 1999. The maps are
dominated by thermal emission around the central bright peak of the nebula, but
we also find unambiguous non-thermal emission associated with the extended
regions. Our observations confirm that this is a jet. The central region has
been associated with the stellar components through HST imaging. If the jets
are due to ejection events at outburst, expansion velocities are consistent
with those from other measurement methods. We propose that the non-thermal
emission is caused by material ejected in the bipolar jets interacting with the
circumstellar wind envelope. The resulting shocks lead to local enhancements in
the magnetic field from the compact component of the order 3mG.
