  We measure the evolution in the virial mass-to-light ratio (M_{200}/L_B) and
virial-to-stellar mass ratio (M_{200}/M_\ast) for isolated ~ L* galaxies
between z~1 and z~0 by combining data from the DEEP2 Galaxy Redshift Survey and
the Sloan Digital Sky Survey. Utilizing the motions of satellite galaxies
around isolated galaxies, we measure line-of-sight velocity dispersions and
derive dark matter halo virial masses for these host galaxies. At both epochs
the velocity dispersion of satellites correlates with host galaxy stellar mass,
\sigma\propto M_\ast^{0.4+/-0.1}, while the relation between satellite velocity
dispersion and host galaxy B-band luminosity may grow somewhat shallower from
\sigma\propto L_B^{0.6+/-0.1} at z~1 to \sigma\propto L_B^{0.4+/-0.1} at z~0.
The evolution in M_200/M_\ast from z~1 to z~0 displays a bimodality insofar as
host galaxies with stellar mass below M_\ast ~10^{11} M_Sun/h maintain a
constant ratio (the intrinsic increase is constrained to a factor of 1.1+/-0.7)
while host galaxies above M_\ast ~10^{11} M_Sun/h experience a factor of 4+/-3
increase in their virial-to-stellar mass ratio. This result can be easily
understood if galaxies below this stellar mass scale continue to form stars
while star formation in galaxies above this scale is quenched and the dark
matter halos of galaxies both above and below this scale grow in accordance
with LCDM cosmological simulations. Host galaxies that are red in U-B color
have larger satellite dispersions and hence reside on average in more massive
halos than blue galaxies at both z~1 and z~0. The redshift and host galaxy
stellar mass dependence of M_200/M_\ast agrees qualitatively with the
Millennium Run semi-analytic model of galaxy formation. (ABRIDGED)
