  At redshifts around 0.1 the CFHT Legacy Survey Deep fields contain some
6x10^4 galaxies spanning the mass range from 10^5 to 10^12 Msun. We measure the
stellar mass dependence of the two point correlation using angular measurements
to largely bypass the errors, approximately 0.02 in the median, of the
photometric redshifts. Inverting the power-law fits with Limber's equation we
find that the auto-correlation length increases from a very low 0.4hMpc at
10^5.5 Msun to the conventional 4.5hMpc at 10^10.5 Msun. The power law fit to
the correlation function has a slope which increases from gamma approximately
1.6 at high mass to gamma approximately 2.3 at low mass. The spatial
cross-correlation of dwarf galaxies with more massive galaxies shows fairly
similar trends, with a steeper radial dependence at low mass than predicted in
numerical simulations of sub-halos within galaxy halos. To examine the issue of
missing satellites we combine the cross-correlation measurements with our
estimates of the low mass galaxy number density. We find on the average there
are 60+/-20 dwarfs in sub-halos with M(total) > 10^7 Msun for a typical Local
Group M(total)/M(stars)=30, corresponding to M/L_V approximately 100 for a
galaxy with no recent star formation. The number of dwarfs per galaxy is about
a factor of two larger than currently found for the Milky Way. Nevertheless,
the average dwarf counts are about a factor of 30 below LCDM simulation
results. The divergence from LCDM predictions is one of slope of the relation,
approximately dN/dlnM approximately -0.5 rather than the predicted -0.9, not
sudden onset at some characteristic scale. The dwarf galaxy star formation
rates span the range from passive to bursting, which suggests that there are
few completely dark halos.
