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

We present results on the clustering properties of galaxies as afunction of both stellar mass and specific star formation rate (sSFR)using data from the PRIMUS and DEEP2 galaxy redshift surveys spanning0.2 z 1.2. We use spectroscopic redshifts of over 100,000galaxies covering an area of 7.2 deg² over five separatefields on the sky, from which we calculate cosmic variance errors. Wefind that the galaxy clustering amplitude is as strong of a function ofsSFR as of stellar mass, and that at a given sSFR, it does notsignificantly depend on stellar mass within the range probed here. Wefurther find that within the star-forming population and at a givenstellar mass, galaxies above the main sequence of star formation withhigher sSFR are less clustered than galaxies below the main sequencewith lower sSFR. We also find that within the quiescent population,galaxies with higher sSFR are less clustered than galaxies with lowersSFR, at a given stellar mass. We show that the galaxy clusteringamplitude smoothly increases with both increasing stellar mass anddecreasing sSFR, implying that galaxies likely evolve across the mainsequence, not only along it, before galaxies eventually becomequiescent. These results imply that the relation of stellar mass to halomass, which connects galaxies to dark matter halos, likely depends onsSFR.