the difference in number counts in this case.

Clustering properties
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Angular clustering
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The 2-point angular correlation function, $w(\theta)$ is defined by the joint probability of finding two galaxies in solid angle elements $\delta\Omega_1$ and $\delta\Omega_2$ at a given separation [@Peebles:1980], $$\delta P = n^2 \delta\Omega_1 \delta\Omega_2 (1 + w(\theta_{12})).$$

![The angular correlation function for our BzK-selected galaxy samples. The best-fitting power laws are shown, with slopes fixed to the fiducial value of $\delta=0.8$. The pBzK galaxies are very strongly clustered, much more so than sBzKs, indicating that they occupy the most massive dark matter halos at their epoch.[]{data-label="wth"}](PSfiles/clustering_deconv_new_BzK.ps){width="240pt"}

To estimate the correlation function we use the estimator of [@Landy_and_Szalay:1993],

$$w(\theta) = \frac{DD - 2DR + RR}{RR}$$

where DD, DR and RR are the counts of data-data, data-random and random-random pairs respectively at angular separation $\theta$, normalised by the total number possible. Although this estimator is relatively robust against systematic errors, there remains a small bias due to the finite field size, which is corrected for an integral constraint by a constant, C. We follow the method of [@Roche_and_Eales:1999] by using the random–random counts to estimate the size of this bias:

$$C=\frac{\Sigma N_{RR}(\theta)\theta^{-0.8}}{\Sigma N_{RR}(\theta)},$$

where the sums extend to 