702 respectively at $K_{AB} < 23.0$.

Number counts
-------------

![$(z - K)_{AB}$ colour versus K-band magnitude. The dashed line is our completeness limit of $K_{AB} = 23.5$ for the full sample, while the solid line shows how the completeness limit in z affects $(z - K)$ colour. We begin to be incomplete above $(z - K) > 2.94$. The impact of this incompleteness is discussed in the text.[]{data-label="kzk"}](PSfiles/Kvszk.ps){width="240pt"}

[|l|l|l|l|l|]{} K bin&all&sBzK&pBzK&Worst\
centre&sources& & &case pBzK\
17.41&2.832&0.198&-&-\
17.91&2.803&0.676&-&-\
18.41&2.957&0.198&-&-\
18.91&3.203&0.500&-&-\
19.41&3.380&1.403&0.676&0.676\
19.91&3.556&2.025&1.429&1.429\
20.41&3.720&2.504&1.914&1.923\
20.91&3.872&2.982&2.181&2.185\
21.41&3.998&3.315&2.386&2.394\
21.91&4.121&3.592&2.386&2.394\
22.41&4.229&3.778&2.377&2.431\
22.91&4.285&3.849&2.158&2.394\
23.41&4.258&3.536&1.560&2.158\
23.91&3.942&0.801&-&-\

\[tab-counts\]

The differential K-band number counts are illustrated in Figure \[counts\], and tabulated in Table 1, for both the full sample of galaxies and those selected as passive and star-forming BzKs. We find a steep rise in the counts of star-forming sBzKs toward fainter magnitudes. In contrast, pBzK number counts exhibit an apparent flattening at $K\sim 21$, consistent with the findings of K06 and L07. Since these galaxies are sampled over a relatively narrow redshift range, this may imply that the passive population consists largely of luminous galaxies at this early epoch (see Section 4).

To investigate the reality of the turn-over, we note that the galaxies around and beyond this 