  We describe methods for setting up self-consistent disk-bulge-halo galaxy
models. The bulge and halo distribution functions (\df) are functions of $E$
and $L_z$ only. The halo's flattening and rotation can be specified. The disk
\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 disk with vertical
extent. The models also have finite extent making them suitable for N-body
simulation. A simulation of a sample model shows that in practice the models
are very close to equilibrium making them ideal for experiments on
instabilities in galactic disks. We also present a sequence of models closely
resembling the Milky Way mass distribution with 5 exponential scale radii and
varying halo mass and radial extent.
