  We use measurements of the stellar mass function, galaxy clustering, and
galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo
mass relation (SHMR) of star forming and quiescent galaxies over the redshift
range z=[0.2,1.0]. For massive galaxies, M*>~10^10.6 Msol, our results indicate
that star-forming galaxies grow proportionately as fast as their dark matter
halos while quiescent galaxies are outpaced by dark matter growth. At lower
masses, there is minimal difference in the SHMRs, implying that the majority
low-mass quiescent galaxies have only recently been quenched of their star
formation. Our analysis also affords a breakdown of all COSMOS galaxies into
the relative numbers of central and satellite galaxies for both populations. At
z=1, satellite galaxies dominate the red sequence below the knee in the stellar
mass function. But the number of quiescent satellites exhibits minimal redshift
evolution; all evolution in the red sequence is due to low-mass central
galaxies being quenched of their star formation. At M*~10^10 Msol, the fraction
of central galaxies on the red sequence increases by a factor of ten over our
redshift baseline, while the fraction of quenched satellite galaxies at that
mass is constant with redshift. We define a "migration rate" to the red
sequence as the time derivative of the passive galaxy abundances. We find that
the migration rate of central galaxies to the red sequence increases by nearly
an order of magnitude from z=1 to z=0. These results imply that the efficiency
of quenching star formation for centrals is increasing with cosmic time, while
the mechanisms that quench the star formation of satellite galaxies in groups
and clusters is losing efficiency.
