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In this work, we use measurements of galaxy stellar mass and two-pointangular correlation functions to constrain the stellar-to-halo mass ratios(SHMRs) of passive and \np\ galaxies at $z\sim2-3$, as identified in the\emph{Spitzer} Matching Survey of the UltraVISTA ultra-deep Stripes (SMUVS). Weadopt a sophisticated halo modeling approach to statistically divide our twopopulations into central and satellite galaxies. For central galaxies, we findthat the normalization of the SHMR is greater for our passive population.Through the modeling of $\Lambda$ cold dark matter halo mass accretionhistories, we show that this can only arise if the conversion of baryons intostars was more efficient at higher redshifts and additionally that passivegalaxies can be plausibly explained as residing in halos with the highestformation redshifts (i.e., those with the lowest accretion rates) at a givenhalo mass. At a fixed stellar mass, satellite galaxies occupy host halos with agreater mass than central galaxies, and we find further that the fraction ofpassive galaxies that are satellites is higher than for the combinedpopulation. This, and our derived satellite quenching timescales, combined withearlier estimates from the literature, support dynamical/environmentalmechanisms as the dominant process for satellite quenching at $z\lesssim3$.

The Stellar-to-Halo Mass Ratios of Passive and Star-Forming Galaxies at z~2-3 from the SMUVS survey