  A and F stars can be used as probes of outer Galactic disk kinematics: here
we extend the work of Harris et al. (2018) by crossmatching their A/F sample
with Gaia DR2 to bring in proper motions. These are combined with the already
measured radial velocities and spectro-photometric distances to obtain full
space motions. We use this sample of 1173 stars, located in two pencil-beam
sightlines (l=178deg and l=118deg), to sample the Galactocentric velocity field
out to almost R_G=15 kpc. We find there are significant differences in all
three (radial, azimuthal and vertical) kinematic components between the two
directions. The rotation curve is roughly flat in the anticentre direction,
confirming and extending the result of Kawata et al. (2018a) thanks to the
greater reach of our spectro-photometric distance scale. However at l=118deg
the circular velocity rises outwards from R_G=10.5 kpc and there is a more
pronounced gradient in radial motion than is seen at l=178deg. Furthermore, the
A star radial motion differs from the F stars by ~10 km/s. We discuss our
findings in the context of perturbers potentially responsible for the trends,
such as the central bar, spiral arms, the warp and external satellites. Our
results at l=178deg are broadly consistent with previous work on K giants in
the anticentre, but the kinematics at l=118deg in the Perseus region do not yet
reconcile easily with bar or spiral arm perturbation.
