  We examine the vertical structure and equilibrium of the molecular gas layer
in the galactic disk, measuring its scale height and velocity dispersion as a
function of Galactic radius by modeling the CO emission at the tangent points.
The model takes into account emission from a large path length along the line
of sight, corresponding to an interval \Delta R ~ 200-400 pc; and is
parametrized by the scale height of the gas, the centroid in z, the rotation
velocity and the velocity dispersion. This model is then fit to the $^{12}CO$
survey of Knapp et al.(1985) to determine the best fit parameters. The reduced
\chi^2 from fitting the models (considering only the photon statistics) range
from 2 to 19. The main source of error is the `shot noise' due to the small
number of clouds. Simulations using discrete molecular clouds are carried out
to estimate the errors. The scale height of the molecular gas increases with
radius. The velocity dispersion varies from ~ 2 km/s to 11 km/s with a typical
uncertainty of ~3 km/s and shows a monotonic increase with galactic radius. The
midplane mass density of the disk calculated from the scale-height and velocity
dispersion is consistent with the local value \rho_0(R_0) of 0.2 \msun pc^{-3}.
