  We present the first optimal power spectrum estimation and three dimensional
deprojections for the dark and luminous matter and their cross correlations.
The results are obtained using a new optimal fast estimator (Pen 2003)
deprojected using minimum variance and SVD techniques. We show the resulting
3-D power spectra for dark matter and galaxies, and their covariance for the
VIRMOS-DESCART weak lensing shear and galaxy data. The survey is most sensitive
to nonlinear scales k_NL ~ 1 h Mpc^-1. On these scales, our 3-D power spectrum
of dark matter is in good agreement with the RCS 3-D power spectrum found by
(Hoekstra et al 2002). Our galaxy power is similar to that found by the 2MASS
survey, and larger than that of SDSS, APM and RCS, consistent with the expected
difference in galaxy population.
  We find an average bias b=1.24+/-0.18 for the I selected galaxies, and a
cross correlation coefficient r=0.75+/-0.23. Together with the power spectra,
these results optimally encode the entire two point information about dark
matter and galaxies, including galaxy-galaxy lensing. We address some of the
implications regarding galaxy halos and mass-to-light ratios. The best fit
``halo'' parameter h=r/b=0.57+/-0.16, suggesting that dynamical masses
estimated using galaxies systematically underestimate total mass.
  Ongoing surveys, such as the Canada-France-Hawaii-Telescope-Legacy survey
will significantly improve on the dynamic range, and future photometric
redshift catalogs will allow tomography along the same principles.
