  The kinematics of galactic C-Miras are discussed on the basis of the
bolometric magnitudes and radial velocities of Papers I and II of this series.
Differential galactic rotation is used to derive a zero-point for the
bolometric period-luminosity relation which is in satisfactory agreement with
that inferred from the LMC C-Miras. We find for the galactic Miras, Mbol =
-2.54logP + 2.06 (+/- 0.24), where the slope is taken from the LMC. The mean
velocity dispersion, together with the data of Nordstroem et al. and the Padova
models, leads to a mean age for our sample of C-Miras of 1.8 +/- 0.4 Gyr and a
mean initial mass of 1.8 +/-0.2 solar masses. Evidence for a variation of
velocity dispersion with period is found, indicating a dependence of period on
age and initial mass, the longer period stars being younger. We discuss the
relation between the O- and C-Miras and also their relative numbers in
different systems.
