one sixth of the UDS DR1 galaxies with photometric redshifts $> 1$.

We also confirm previous claims for a dependence of sBzK clustering on apparent magnitude [@Hayashi_etal:2007]. Figure \[sBzK\] and Table \[sBzKtab\] show the values for sBzKs with varying limiting magnitude. The dependence is much stronger at magnitudes of $K < 22$, indicating a strong correlation between halo mass and sBzK luminosity for these objects.

![The dependence of clustering strength of sBzK-selected galaxies on limiting K$_{AB}$-band magnitude. Our measurements (open squares) are shown together with literature values from [@Blanc_etal:2008] and [@Hayashi_etal:2007] (open triangle and asterisks respectively). Our values confirm the magnitude dependence of sBzK clustering strength.[]{data-label="sBzK"}](PSfiles/Lit_sBzK_K_deconv.ps){width="240pt"}

[|l|l|l|]{} K$_{AB,lim}$&N&r$_0$\
20.0&92&$39.0^{+11.8}_{-15.9}$\
20.5&250&$16.4^{+6.5}_{-10.0}$\
21.0&689&$12.6^{+2.7}_{-3.2}$\
21.5&1724&$8.71^{+1.49}_{-1.68}$\
22.0&3789&$5.00^{+0.49}_{-0.55}$\
22.5&7199&$6.23^{+0.64}_{-0.69}$\
23.0&11551&$6.75^{+0.34}_{-0.37}$\

\[sBzKtab\]

BzK galaxies selected at$1.4 < z < 2.5$ 
----------------------------------------

The BzK selection was defined by [@Daddi_etal:2004] to isolate galaxies in the redshift range $1.4 < z < 2.5$. Clearly from figure \[nz\], and as expected by [@Daddi_etal:2004], there are contaminating objects from outside of this range. Using our photometric redshifts we can asses how successful the BzK selection technique is in reproducing the clustering of objects within the desired range.

Following the same method outlined for the full samples, we compute clustering amplitudes find 