  We model three dSph galaxies, Draco, Ursa Minor and Fornax, as axisymmetric
stellar systems embedded in spherical dark-matter potentials, which are in
dynamical equilibrium without significant external tidal forces. We construct
non-parametric two- and three-integral models that match the observed
surface-density profiles and the current kinematic samples of $\sim150-200$
stars per galaxy; these models naturally produce the so-called ``extra-tidal
extensions", which had previously been suggested as evidence of tidal
stripping. Isochrone, NFW and power-law models fit the data, but we strongly
rule out any centrally condensed mass distribution like a dominant central
black hole, as well as constant-density and (for Draco and Fornax) constant
mass-to-light ratio models. The average V-band mass-to-light ratio is
$400\pm80$ \ml within 0.75 kpc for Draco, $580^{+140}_{-100}$ \ml within 1.1
kpc for Ursa Minor and $25^{+7}_{-5}$ \ml within 2.5 kpc for Fornax.
Two-integral models fit the data almost as well as three-integral models; in
contrast to previous suggestions we do not find that anisotropy contributes
substantially to the high mass-to-light ratios in these dSph galaxies.
