of the galaxy colour bimodality occurs around $z\sim2$ (e.g. @Cirasuolo_etal:2007), but the precise evolutionary path from the distant Universe to the present day is still undetermined. The mechanism that terminates the major episode of star-formation is poorly understood [@Benson_etal:2005], and it is now clear that massive galaxies undergo significant size evolution from $z\sim2$ to the present day (e.g. @Cimatti_etal:2008 and references therein).

Galaxy clustering is an important tool for investigating these populations, since the amplitude of clustering on large scales ($>1$Mpc) can provide a measurement of the dark matter halo mass [@Mo_and_White:1996; @Sheth_and_Tormen:1999]. In principle, therefore, one can relate galaxy populations from the distant past to the present day by tracing the evolution of dark matter halos within the context of a framework for structure formation.

A full exploration of these issues will require large spectroscopic surveys of IR-selected galaxies over a representative volume of the distant Universe. Such surveys are currently at an early stage, so recent work has focused on the photometric colour selection of passive vs. star-forming galaxies at the crucial $z\sim 2$ epoch. The two key methods to date are the BM/BX selection [@Erb_etal:2003], which is an extension of the Lyman-break dropout technique, and the BzK 