\times 10^{-3}$ (deg.$^{0.8}$). The clustering amplitude of the pBzKs is inconsistent with the clustering of sBzK galaxies at the 3-sigma level. Figure \[wth\] shows the clustering measurements corrected for the integral constraint for the sBzK and pBzK galaxies.

De-projected clustering amplitude
---------------------------------

The real space clustering and projected clustering are linked by the relativistic Limber equation [@Limber:1954]. If the redshift distribution of a sample is known, the Limber equation can be inverted and the correlation length, $r_0$, can be calculated in a robust manner [@Peebles:1980; @Magliocchetti_and_Maddox:1999]

To estimate the redshift distribution we use photometric redshifts based on the Subaru and UDS bands previously introduced, with the addition of Spitzer data taken as part of the SWIRE survey [@Lonsdale_etal:2003]. The method is described fully in [@Cirasuolo_etal:2007], and consists of minimising the $\chi^2$ of synthetic galaxy templates. The distributions are shown in figure \[nz\]. The photometric redshift distribution was then used directly in the inverted Limber’s equation during the calculation of $r_0$. The values obtained in this manner are r$_0 = 15.8^{+2.0}_{-2.2}h^{-1}$ Mpc and $7.69^{+0.40}_{-0.41}h^{-1}$ Mpc for $K < 23$ pBzKs and sBzKs respectively. The quoted errors are due to the error in the fit to the clustering amplitude and therefore take 