with models of dark matter halo clustering evolution. Using models based on [@Mo_and_White:2002] we find a typical halo mass of $\sim 6\times10^{11} M_{\sun}$.

Applying the model of clustering evolution to the pBzKs we can qualitatively conclude that they are inhabitants of the most massive halos at their epoch (in excess of $10^{13} M_{\odot}$); halos which will eventually become massive groups and clusters by the present day. The evolutionary path that pBzKs take with redshift will also be the subject of future work, using further colour selection techniques.

Our conclusion based on the $r_0$ measurement is strengthened by their luminosity function. Even under the strict assumption of purely passive evolution, the descendants of pBzKs occupy the bright end of the luminosity function. Such galaxies are group and cluster dominant galaxies in the local universe. The brightest ($K < 21$) sBzKs have clustering scale lengths comparable to, or greater than, that which we have found for the pBzKs. This finding indicates that such galaxies will also become group and cluster dominant galaxies by $z=0$. The implication is that we are indeed witnessing the epoch at which the build up of the red sequence begins.

Acknowledgments {#acknowledgments .unnumbered}
===============

OA, IRS and RJM 