  The surface brightness fluctuation (SBF) method is a robust and efficient way
of measuring distances to galaxies containing evolved stellar populations.
Although many recent applications of the method have used space-based imaging,
SBF remains a powerful technique for ground-based telescopes. Deep, wide-field
imaging surveys with subarsecond seeing enable SBF measurements for numerous
nearby galaxies. Using a preliminary calibration, Cantiello et al. (2018)
presented SBF distances for 89 bright, mainly early-type galaxies observed in
the Next Generation Virgo Cluster Survey (NGVS). Here, we present a refined
calibration and SBF distances for 278 galaxies extending several magnitudes
fainter than in previous work. The derived distances have uncertainties of
5-12\% depending on the properties of the individual galaxies, and our sample
is more than three times larger than any previous SBF study of this region.
Virgo has a famously complex structure with numerous subclusters, clouds and
groups; we associate individual galaxies with the various substructures and map
their three-dimensional spatial distribution. Curiously, subcluster A, centered
around M87, appears to have two peaks in distance: the main peak at $\sim$16.5
Mpc and a smaller one at $\sim$19.4 Mpc. Subclusters B and C have distances of
$\sim$15.8 Mpc. The W and W' groups form a filament-like structure, extending
more than 15~Mpc behind the cluster with a commensurate velocity increase of
$\sim$1000 \kms\ along its length. These measurements are a valuable resource
for future studies of the relationship between galaxy properties and local
environment within a dynamic and evolving region.
