passive galaxies in the redshift range $1.4 < z < 2.5$ by using the B-, z- and K$_s$-band broadband filters. Recent work has shown that the number counts of these populations differ markedly [@Kong_etal:2006; @Lane_etal:2007], with star-forming galaxies being far more abundant at all magnitudes. The abundance of sBzK galaxies allowed [@Kong_etal:2006] (henceforth K06) to perform a detailed clustering analysis, segregated by limiting K-band luminosity in the range $18.5 < K_{vega} < 20$. They found that the clustering of sBzKs is strongly dependent on $K$-band luminosity. [@Hayashi_etal:2007] studied the clustering of sBzKs over a smaller area (180 arcmin$^{2}$) but to much greater depth (K$_{AB} < 23.2$) and confirmed this strong luminosity dependence. The sBzK population therefore appear to inhabit a range of halo masses, and are therefore likely to be the progenitors of a wide range of present day galaxies.

There have been fewer studies of [*passive*]{} galaxy clustering at high redshift, in part because of their relatively low surface density. K06 found early evidence that pBzKs are more strongly clustered than sBzKs, although the limited depth and area of this survey ($320 {\rm arcmin}^2$ to K$_{Vega}=20$) gives rise to significant statistical uncertainly, particularly given the relatively low surface density 