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We present measurements of the luminosity and color-dependence of galaxyclustering at 0.2<z<1.0 in the PRIsm MUlti-object Survey (PRIMUS). We quantifythe clustering with the redshift-space and projected two-point correlationfunctions, xi(rp,pi) and wp(rp), using volume-limited samples constructed froma parent sample of over 130,000 galaxies with robust redshifts in sevenindependent fields covering 9 sq. deg. of sky. We quantify how thescale-dependent clustering amplitude increases with increasing luminosity andredder color, with relatively small errors over large volumes. We find that redgalaxies have stronger small-scale (0.1<rp<1 Mpc/h) clustering and steepercorrelation functions compared to blue galaxies, as well as a strong colordependent clustering within the red sequence alone. We interpret our measuredclustering trends in terms of galaxy bias and obtain values betweenb_gal=0.9-2.5, quantifying how galaxies are biased tracers of dark matterdepending on their luminosity and color. We also interpret the color dependencewith mock catalogs, and find that the clustering of blue galaxies is nearlyconstant with color, while redder galaxies have stronger clustering in theone-halo term due to a higher satellite galaxy fraction. In addition, wemeasure the evolution of the clustering strength and bias, and we do not detectstatistically significant departures from passive evolution. We argue that theluminosity- and color-environment (or halo mass) relations of galaxies have notsignificantly evolved since z=1. Finally, using jackknife subsampling methods,we find that sampling fluctuations are important and that the COSMOS field isgenerally an outlier, due to having more overdense structures than otherfields; we find that 'cosmic variance' can be a significant source ofuncertainty for high-redshift clustering measurements.

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