NEARLY SELF-CONSISTENT DISC-BULGE-HALO MODELS FOR GALAXIES

We describe methods for setting up self-consistent disc-bulge-halo gal axy models. The bulge and halo distribution functions (DFs) are functi ons of E and L(z) only. The halo's flattening and rotation can be spec ified. The disc DF is a function of E and L(z) and a third 'integral', E(z), the vertical energy, which is approximately conserved in a warm disc with vertical extent. The models also have finite extent, making them suitable for N-body simulation. A simulation of a sample model s hows that in practice the models are very close to equilibrium, making them ideal for experiments on instabilities in galactic discs. We als o present a sequence of models closely resembling the Milky Way mass d istribution with 5 exponential scale radii and varying halo mass and r adial extent.