  We present the stellar and gaseous kinematics of an Sb galaxy, NGC 3223, with
the aim of determining the vertical and radial stellar velocity dispersion as a
function of radius, which can help to constrain disk heating theories. Together
with the observed NIR photometry, the vertical velocity dispersion is also used
to determine the stellar mass-to-light (M/L) ratio, typically one of the
largest uncertainties when deriving the dark matter distribution from the
observed rotation curve. We find a vertical-to-radial velocity dispersion ratio
of sigma_z/sigma_R=1.21+-0.14, significantly higher than expectations from
known correlations, and a weakly-constrained Ks-band stellar M/L ratio in the
range 0.5-1.7, at the high end of (but consistent with) the predictions of
stellar population synthesis models. Such a weak constraint on the stellar M/L
ratio, however, does not allow us to securely determine the dark matter density
distribution. To achieve this, either a statistical approach or additional data
(e.g. integral-field unit) are needed.
