  We present faint galaxy counts from deep $VRI$ images obtained with the Keck
Telescope. These images reach $R\sim27$ in median seeing FWHM $\sim 0.5$--0.6
arcsec and we detect a integrated galaxy number density of $7\times 10^{5}$
degree$^{-2}$, equivalent to $3\times 10^{10}$ galaxies in the observable
Universe. In addition we present median galaxy colors as a function of
magnitude; bluing trends are visible in all colors to $R\sim 24.5$. Fainter
than $R\sim24.5$, however, the typical \VR\ color becomes redder again, \VI\
remains constant, and \RI\ becomes yet bluer. These trends are consistent with
the $VRI$ count slopes, implying a decrease in the $V$ slope at the faintest
levels, which our data supports. Taking advantage of our good seeing we also
present median half-light radii for faint galaxies, these show a steady decline
at fainter magnitudes, leading to an intrinsic half-light radius of $\sim 0.2$
arcsec for a typical $R\sim25.5$--26 galaxy. Irrespective of the redshift
distribution, the extremely high galaxy surface densities and their small
intrinsic sizes are consistent with a scenario in which the majority of the
very faint field population are dwarf galaxies or sub-galactic units.
