  We explore the connections between stellar age, chemistry, and kinematics
across a Galactocentric distance of $7.5 < R\,(\mathrm{kpc}) < 9.0$, using a
sample of $\sim 12\,000$ intermediate-mass (FGK) turnoff stars observed with
the RAdial Velocity Experiment (RAVE) survey. The kinematics of this sample are
determined using radial velocity measurements from RAVE, and parallax and
proper motion measurements from the Tycho-Gaia Astrometric Solution (TGAS). In
addition, ages for RAVE stars are determined using a Bayesian method, taking
TGAS parallaxes as a prior. We divide our sample into young ($0 < \tau < 3$
Gyr) and old ($8 < \tau < 13$ Gyr) populations, and then consider different
metallicity bins for each of these age groups. We find significant differences
in kinematic trends of young and old, metal-poor and metal-rich, stellar
populations. In particular, we find a strong metallicity dependence in the mean
Galactocentric radial velocity as a function of radius ($\partial {V_{\rm
R}}/\partial R$) for young stars, with metal-rich stars having a much steeper
gradient than metal-poor stars. For $\partial {V_{\phi}}/\partial R$, young,
metal-rich stars significantly lag the LSR with a slightly positive gradient,
while metal-poor stars show a negative gradient above the LSR. We interpret
these findings as correlations between metallicity and the relative
contributions of the non-axisymmetries in the Galactic gravitational potential
(the spiral arms and the bar) to perturb stellar orbits.
