the largest separations within the field.

The sBzK and pBzK samples were selected to a limit of $K_{AB} <
23$. We adopted this conservative magnitude limit to ensure the minimum contamination by spurious sources. We fit a single power law of the form $w(\theta) = A(\theta^{-\delta} - C)$ to the corrected data over the separation range $0.01 - 0.1$ degrees, fixing the slope to the fiducial $\delta=0.8$ and minimising the $\chi^2$. The errors on the measurements are a combination of those due to shot noise (estimated by bootstrap resampling) and an estimate of those due to cosmic variance. The estimates for cosmic variance were found by splitting the field into 4 and computing the variance of $w(\theta)$.

In order to fit the clustering reliably, we wish to avoid small-scale excesses due to multiple galaxy occupation of a single halo. The lower bound was chosen to correspond to $\sim 0.9$Mpc (co-moving) at z$\sim 2$ for this reason. The upper bound is a conservative estimate of the limit to which our data have enough signal for a reliable fit to be obtained.

For sBzK galaxies the amplitude was found to be $A=1.79^{+0.17}_{-0.17} \times 10^{-3}$ (deg.$^{0.8}$)and for the pBzK population $A = 6.37^{+1.58}_{-1.54} 