the SDSS–2dF LRG survey, we hope to have redshifts for 10,000 LRGs over this intermediate redshifts range. When combined with the low redshift SDSS LRGs, we will be able to study the evolution in the properties and clustering of a single population of massive galaxies over half the age of the universe.

![The distribution in g–band luminosity and redshift for both the low redshift LRGs (solid points) and the SDSS–2dF LRGs (red crosses). The luminosities are k–corrected and corrected for passive evolution to $z=0$. The red lines show the expected selection boundaries for the SDSS-2dF survey, while the dashed line is the luminosity limit above which we expect the low redshift SDSS LRG sample to be complete. Plot courtesy of Daniel Eisenstein and my SDSS–2dF colleagues.[]{data-label="2df"}](lrg2dF_zz_Mg.eps){width="9cm"}

Galaxy Properties as a Function of Environment {#environ}
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Clusters and groups of galaxies play an important role in studying the effects of environment on the properties of galaxies. With the SDSS data, it is now possible to extend such studies well beyond the cores of clusters into lower density environments. Furthermore, the distance to the $N^{th}$ nearest neighbor can be used to provides an adaptive measure of the local density of galaxies (see 