  The ACS Virgo Cluster Survey consists of HST ACS imaging for 100 early-type
galaxies in the Virgo Cluster, observed in the F475W and F850LP filters. We
derive distances for 84 of these galaxies using the method of surface
brightness fluctuations (SBFs), present the SBF distance catalog, and use this
database to examine the three-dimensional distribution of early-type galaxies
in the Virgo Cluster. The SBF distance moduli have a mean (random) measurement
error of 0.07 mag (0.5 Mpc), or roughly 3 times better than previous SBF
measurements for Virgo Cluster galaxies. Five galaxies lie at a distance of ~23
Mpc and are members of the W' cloud. The remaining 79 galaxies have a narrow
distribution around our adopted mean distance of 16.5+/-0.1 (random mean error)
+/-1.1 Mpc (systematic). The rms distance scatter of this sample is 0.6+/-0.1
Mpc, with little dependence on morphological type or luminosity class (i.e.,
0.7+/-0.1 and 0.5+/-0.1 Mpc for the giants and dwarfs, respectively). The
back-to-front depth of the cluster measured from our sample of galaxies is
2.4+/-0.4 Mpc (i.e., +/-2sigma of the intrinsic distance distribution). The M87
(cluster A) and M49 (cluster B) subclusters are found to lie at distances of
16.7+/-0.2 and 16.4+/-0.2 Mpc, respectively. There may be a third subcluster
associated with M86. A weak correlation between velocity and line-of-sight
distance may be a faint echo of the cluster velocity distribution not having
yet completely virialized. In three dimensions, Virgo's early-type galaxies
appear to define a slightly triaxial distribution, with axis ratios of
(1:0.7:0.5). The principal axis of the best-fit ellipsoid is inclined ~20-40
deg. from the line of sight, while the galaxies belonging to the W' cloud lie
on an axis inclined by ~10-15 deg.
