  Full space velocities are computed for a sample of 130 nearby RR Lyrae
variables using both ground-based and Hipparcos proper motions. In many cases
proper motions from multiple sources have been averaged to produce a
significant improvement in the transverse space velocity errors. In most cases,
this exceeds the accuracy of Hipparcos proper motions alone. The velocity
ellipsoids computed for halo and thick disk samples are in agreement with
previous studies. No distinct sample of thin disk RR Lyraes has been isolated
but there is kinematic evidence for some thin disk stars in our thick disk
samples. A sample of 21 stars with [Fe/H] < -1.0 and disk-like kinematics have
been isolated. It is concluded from their kinematics and spatial distribution
that these stars represent a sample of RR Lyraes in the metal weak tail of the
thick disk. In the halo samples the distribution of V velocities is not
gaussian, even when the metal weak thick disk stars are removed. Also, a plot
of U and W velocities as a function of V velocity for the kinematically
unbiased halo sample shows some curious structure. The cause of these kinematic
anomalies is not clear. In addition, systematic changes to the distance scale
within the range of currently accepted values of Mv(RR) are shown to
significantly change the calculated halo kinematics. Fainter values of Mv(RR),
such as those obtained by statistical parallax (~ 0.60 to 0.70 at [Fe/H]=-1.9),
result in local halo kinematics similar to those reported in independent
studies of halo kinematics, while brighter values of Mv(RR), such as those
obtained through recent analysis of Hipparcos subdwarf parallaxes (~ 0.30 to
0.40 at [Fe/H]=-1.9), result in a halo with retrograde rotation and
significantly enlarged velocity dispersions.
