  We present dynamical distribution functions for evolved stars in the inner
galactic plane. We use an axisymmetric, two-component Stackel potential that
satisfies recent constraints on the galactic potential, amongst others a
slightly declining local rotation curve. We show that this potential is
adequate to model stellar-kinematic samples with radial extent ranging from
\~100 pc to ~5 kpc in the Galaxy. The two-integral model that gives the best
fit to the first three projected moments provides a very good global
representation of the data but fails to reproduce the central dispersion, the
central apparent scaleheight and the cylindrical rotation at intermediate
longitudes. All these features are fitted well by a three--integral model. We
discuss various properties of the 2I- and 3I models and the implications for
galactic structure. A somewhat thicker disk component is needed to explain the
distribution of older AGB stars in the plane; this component also fits the
kinematics at higher latitudes better. We find that the Disk and the Bulge, as
traced by AGB stars, are very similar dynamically and could well be one and the
same component. There is a dynamically distinct component in the inner 100 pc
of the Bulge, however.
