Left panel: projected clustering of CMASS galaxies binned by stellar mass above the completeness limit of the CMASS selection algorithm. The solid black curve shows the nonlinear clustering of dark matter. Middle panel: clustering of CMASS galaxies at and below the completeness limit of the sample. Right panel: cross-correlation function of the SPARSE sample, binned by stellar mass, with the full CMASS sample. In each panel, the numbers on the right side indicate the center of the bin in ﹩\mathrm{log}{M}_{* }﹩.