Dynamical Models for the Milky Way

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The only way to map the Galaxy's gravitational potential Φ(x) and the distribution of matter that produces it is by modelling the dynamics of stars and gas. Observations of the kinematics of gas provide key information about gradients of Φ within the plane, but little information about the structure of Φ out of the plane. Traditional Galaxy models assume, for each of the Galaxy's components, arbitrary flattenings, which together with the components' relative masses yield the model's equipotentials. However, the Galaxy's isopotential surfaces should be determined directly from the motions of stars that move far from the plane. Moreover, from the kinematics of samples of such stars that have well defined selection criteria, one should be able not only to map Φ at all positions, but to determine the distribution function fᵢ(x, v) of each stellar population i studied. These distribution functions will contain a wealth of information relevant to the formation and evolution of the Galaxy. An approach to fitting a wide class of dynamical models to the very heterogeneous body of available data is described and illustrated.