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We present new measurements of the clustering of stellar mass-completesamples of $\sim40,000$ SDSS galaxies at $z\sim0.03$ as a joint function ofstellar mass and specific star formation rate (sSFR). Our results confirm whatCoil et al. (2017) find at $z\sim0.7$: galaxy clustering is a stronger functionof sSFR at fixed stellar mass than of stellar mass at fixed sSFR. We also findthat galaxies above the star-forming main sequence (SFMS) with higher sSFR areless clustered than galaxies below the SFMS with lower sSFR, at a given stellarmass. A similar trend is present for quiescent galaxies. This confirms thatmain sequence scatter, and scatter within the quiescent sequence, is physicallyconnected to the large-scale cosmic density field. We compare the resultinggalaxy bias versus sSFR, and relative bias versus sSFR ratio, for differentgalaxy samples across ${0<z<1.2}$ to mock galaxy catalogs based on theempirical galaxy evolution model of Behroozi et al. (2019). This model fitsPRIMUS and DEEP2 clustering data well at intermediate redshift, but agreementwith SDSS is not as strong. We show that increasing the correlation betweengalaxy SFR and halo accretion rate at $z\sim0$ in the model substantiallyimproves agreement with SDSS data. Mock catalogs suggest that central galaxiescontribute substantially to the dependence of clustering on sSFR at a givenstellar mass and that the signal is not simply an effect of satellite galaxyfraction differences with sSFR. Our results are highly constraining for galaxyevolution models and show that the stellar-to-halo mass relation (SHMR) dependson sSFR.

Main Sequence Scatter is Real: The Joint Dependence of Galaxy Clustering on Star Formation and Stellar Mass