that of [@Hayashi_etal:2007] and in addition we make fewer assumptions regarding their redshift distribution. Further surveys reaching depths of $K_{AB,lim} \sim 23$ are required to fully account the effects of cosmic variance, however.

We also confirm that the scale-length for the clustering of sBzK galaxies is dependent on apparent magnitude, consistent with the work of [@Hayashi_etal:2007] (figure \[sBzK\]). This dependence is far more significant at magnitudes below $K_{AB} \sim 22$ indicating a strong correlation between such galaxies and the mass of the hosting halo.

In addition to this luminosity dependence there is a clear enhancement at small scales in the sBzK clustering. This enhancement is indicative of multiple sBzK galaxies occupying a single dark matter halo. The scale at which this turn-off occurs can provide an indication of the size, and hence mass, of the hosting dark matter halos. The turn-off occurs at $\sim 0.01$ deg, which corresponds to $\sim 0.3$ Mpc at z$=1.65$. Halos of this size have masses between $10^{11}$ and $10^{12} M_{\sun}$ [@Mo_and_White:2002]. A full consideration of this enhancement within the halo occupation distribution framework will be presented in a future paper. The host halo mass can also be derived from comparing the de-projected clustering scale length 