into account the shot noise and cosmic variance.

![Photometric redshift distributions for passive (left) and star-forming (right) BzK-selected galaxies (solid line histogram). The over-plotted dashed lines are distributions with photometric errors de-convolved (see text).[]{data-label="nz"}](PSfiles/BzK_nz_deconv.eps){width="240pt"}

The photometric redshifts are subject to errors ($\sigma/(1+z) = 0.095$ and $0.105$ for pBzKs and sBzKs respectively), however, and assuming that the true redshift distribution is highly peaked, these errors are likely to broaden the measured distribution. A broader distribution will result in a larger inferred clustering scale length. It is therefore important that we take such errors into account. We do so by assuming the errors are Gaussian, and then deconvolve the errors from the redshift distribution using a Fourier-based Wiener filter. A more detailed description of this method is provided in the appendix. The resulting de-convolved redshift distributions are shown in figure \[nz\].

The scaling lengths recovered using the corrected redshift distribution are as follows: $15.0^{+1.9}_{-2.2}h^{-1}$ Mpc and $6.75^{+0.34}_{-0.37}h^{-1}$ Mpc for pBzKs and sBzKs respectively.

However, we note that our photometric redshift code is largely untested for pBzK and sBzK galaxies. This work will be refined by the use of an ongoing ESO Large Programme using VIMOS and FORS2 on the VLT to target 