  We use the Jaffe model as a global mass distribution for the Galaxy and
determine the circular velocity $v_c$ and the Jaffe radius $r_j$ using the
satellites of the Galaxy, estimates of the local escape velocity of stars, the
constraints imposed by the known rotation curve of the disk, and the Local
Group timing model. The models include the systematic uncertainties in the
isotropy of the satellite orbits, the form of the stellar distribution function
near the escape velocity, and the ellipticity of the M31/Galaxy orbit. If we
include the Local Group timing constraint, then Leo I is bound,
$v_c=230\pm30\kms$, and $r_j=180$ kpc (110 kpc $\ltorder r_j \ltorder $ 300
kpc) at 90\% confidence. The satellite orbits are nearly isotropic with
$\beta=1-\sigma_\theta^2/\sigma_r^2=0.07$ ($-0.7 \ltorder \beta \ltorder 0.6$)
and the stellar distribution function near the escape velocity is
$f(\epsilon)\propto \epsilon^k$ with $k_r=3.7$ ($0.8 \ltorder k_r \ltorder
7.6$) where $k_r=k+5/2$. While not an accurate measurement of $k$, it is
consistent with models of violent relaxation ($k=3/2$). The mass inside 50 kpc
is $(5.4\pm1.3)\times 10^{11} M_\odot$. Higher mass models require that M31 is
on its second orbit and that the halo is larger than the classical tidal limit
of the binary. Such models must have a significant fraction of the Local Group
mass in an extended Local Group halo. Lower mass models require that both M31
and Leo I are unbound, but there is no plausible mechanism to produce the
observed deviations of M31 and Leo I from their expected velocities in an
unbound system. If we do not use the Local Group timing model, the median mass
of the Galaxy {\it increases} significantly, and the error bars broaden. Using
only the satellite, escape velocity, and disk rotation curve constraints, the
