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 ( ) , 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 } \sim 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 ( ) .
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 \pm 0.18 for the I selected galaxies , and a cross correlation coefficient r = 0.75 \pm 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 \equiv r / b = 0.57 \pm 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 .