PRIMUS: Galaxy Clustering as a Function of Luminosity and Color at 0.2 < z < 1

We present measurements of the luminosity and color-dependence of galaxyclustering at 0.2 z 1.0 in the Prism Multi-object Survey. Wequantify the clustering with the redshift-space and projected two-pointcorrelation functions, ξ(r_p , π) and w_p(r_p ), using volume-limited samples constructed from a parentsample of over ~130, 000 galaxies with robust redshifts in sevenindependent fields covering 9 deg² of sky. We quantify howthe scale-dependent clustering amplitude increases with increasingluminosity and redder color, with relatively small errors over largevolumes. We find that red galaxies have stronger small-scale (0.1 Mpc h^-1 r_p 1 Mpc h ^-1)clustering and steeper correlation functions compared to blue galaxies,as well as a strong color dependent clustering within the red sequencealone. We interpret our measured clustering trends in terms of galaxybias and obtain values of b _gal ≈ 0.9-2.5, quantifying howgalaxies are biased tracers of dark matter depending on their luminosityand color. We also interpret the color dependence with mock catalogs,and find that the clustering of blue galaxies is nearly constant withcolor, while redder galaxies have stronger clustering in the one-haloterm due to a higher satellite galaxy fraction. In addition, we measurethe evolution of the clustering strength and bias, and we do not detectstatistically significant departures from passive evolution. We arguethat the luminosity- and color-environment (or halo mass) relations ofgalaxies have not significantly evolved since z ~ 1. Finally, usingjackknife subsampling methods, we find that sampling fluctuations areimportant and that the COSMOS field is generally an outlier, due tohaving more overdense structures than other fields; we find that "cosmicvariance" can be a significant source of uncertainty for high-redshiftclustering measurements.