  Evidence for a bar at the center of the Milky Way triggered a renewed
enthusiasm for dynamical modelling of the Galactic bar-bulge. Our goal is to
compare the kinematics of a sample of tracers, planetary nebulae, widely
distributed over the bulge with the corresponding kinematics for a range of
models of the inner Galaxy. Three of these models are N-body barred systems
arising from the instabilities of a stellar disk (Sellwood, Fux and Kalnajs),
and one is a Schwarzschild system constructed to represent the 3D distribution
of the COBE/DIRBE near-IR light and then evolved as an N-body system for a few
dynamical times (Zhao). For the comparison of our data with the models, we use
a new technique developed by Saha (1998). The procedure finds the parameters of
each model, i.e. the solar galactocentric distance R_o in model units, the
orientation angle phi, the velocity scale (in km/s per model unit), and the
solar tangential velocity which best fit the data.
