correlation lengths of $11.1^{+1.7}_{-1.8}h^{-1}$ Mpc and $5.46^{+0.36}_{-0.37}h^{-1}$ Mpc for $1.4 < z < 2.5$ pBzKs and sBzKs respectively. These values are slightly lower than those for the full samples and indicate that the high redshift tails in the full sample are at least as highly clustered as those within the $1.4 < z < 2.5$ range. However, the conclusions drawn from the full sample are still valid, namely that the pBzK galaxies are significantly more strongly clustered than the sBzK galaxies.

Luminosity function
===================

![image](PSfiles/lumfun.eps){width="\textwidth"}

A luminosity function was constructed for our BzK-selected galaxies in the same way as detailed in [@Cirasuolo_etal:2007], by using the $1/V_{max}$ method [@Schmidt:1968]. Figure \[lum\] shows the luminosity function for the BzK galaxies with photometric redshifts in the range $1.4<z<2.5$ (points with error-bars), compared with all K-selected galaxies in the same range (solid line). Also plotted is the $z=0$ luminosity function from [@Kochanek_etal:2001]. It is clear that sBzK galaxies sample a wide range in luminosity, while the pBzK population are dominated by bright galaxies with $M_K>-23$. At this epoch, however, the bright end of the luminosity function is still dominated by star-forming objects, consistent with [@Cirasuolo_etal:2007] who found that the galaxy colour bimodality is weak 