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We present results on the clustering properties of galaxies as a function ofboth stellar mass and specific star formation rate (sSFR) using data from thePRIMUS and DEEP2 galaxy redshift surveys spanning 0.2 < z < 1.2. We usespectroscopic redshifts of over 100,000 galaxies covering an area of 7.2 deg^2over five separate fields on the sky, from which we calculate cosmic varianceerrors. We find that the galaxy clustering amplitude is as strong of a functionof sSFR as of stellar mass, and that at a given sSFR, it does not significantlydepend on stellar mass within the range probed here. We further find thatwithin the star-forming population and at a given stellar mass, galaxies abovethe main sequence of star formation with higher sSFR are less clustered thangalaxies below the main sequence with lower sSFR. We also find that within thequiescent population, galaxies with higher sSFR are less clustered thangalaxies with lower sSFR, at a given stellar mass. We show that the galaxyclustering amplitude smoothly increases with both increasing stellar mass anddecreasing sSFR, implying that galaxies likely evolve across the main sequence,not only along it, before galaxies eventually become quiescent. These resultsimply that the stellar mass to halo mass relation, which connects galaxies todark matter halos, likely depends on sSFR.

PRIMUS+DEEP2: The Dependence of Galaxy Clustering on Stellar Mass and Specific Star Formation Rate at 0.2 < z < 1.2