  Using the HST STIS spectrograph we have obtained a grid of [O III] and H-beta
emission-line spectra at 0"05x0"19 and 60 km/s (FWHM) resolution that covers
much of the NLR of NGC 1068. We find emitting knots that have blueshifted
radial velocities up to 3200 km/s relative to galaxy systemic, are 70-150 pc NE
of the nucleus and up to 40 pc from the radio jet, emit several percent of the
NLR line flux but no significant continuum, span velocity extents of up to 1250
km/s but a small fraction of the sky seen from the nucleus, coincide with a
region of enhanced IR coronal-line emission, and have ionized masses $\sim$200
Msun/ne4 (ne4=10^4 cm^{-3}). We argue that the blueshifted knots are ablata
from disintegrating molecular clouds that are being photoionized by the AGN,
and are being accelerated readiatively by the AGN or mechanically by the radio
jet. In their kinematic properties, the knots resemble the associated absorbers
seen projected on the UV continua of some AGN. Between 2"5-4"5 from the
nucleus, emission is redshifted relative to systemic, a pattern that we
interpret as gas in the galaxy disk being pushed away from us by the NE radio
lobe.
