We measure the color and stellar mass dependence of clustering in spectroscopic galaxies at 0.6 < z < 0.65 using data from the Baryon Oscillation Spectroscopic Survey component of the Sloan Digital Sky Survey .
We greatly increase the statistical precision of our clustering measurements by using the cross-correlation of 66,657 spectroscopic galaxies to a sample of 6.6 million fainter photometric galaxies .
The clustering amplitude w ( R ) is measured as the ratio of the mean excess number of photometric galaxies found within a specified radius annulus around a spectroscopic galaxy to that from a random photometric galaxy distribution .
We recover many of the familiar trends at high signal-to-noise ratio .
We find the ratio of the clustering amplitudes of red and blue massive galaxies to be w _ { \text { red } } / w _ { \text { blue } } = 1.92 \pm 0.11 in our smallest annulus of 75–125 kpc .
At our largest radii ( 2–4 Mpc ) , we find w _ { \text { red } } / w _ { \text { blue } } = 1.24 \pm 0.05 .
Red galaxies therefore have denser environments than their blue counterparts at z \sim 0.625 , and this effect increases with decreasing radius .
Irrespective of color , we find that w ( R ) does not obey a simple power-law relation with radius , showing a dip around 1 Mpc .
Holding stellar mass fixed , we find a clear differentiation between clustering in red and blue galaxies , showing that clustering is not solely determined by stellar mass .
Holding color fixed , we find that clustering increases with stellar mass , especially for red galaxies at small scales ( more than a factor of 2 effect over 0.75 dex in stellar mass ) .