1. Michael Brown (going to Princeton) Buell Jannuzi (PI) Arjun Dey (PI) Glenn Tiede (now @ Bowling Green) Tod Lauer Kate Brand Frank Valdes Alyson Ford (going to Swinburne) Lissa Miller (going to Yale) NDWFS Survey Team The Clustering of Galaxies in Bootes AAS, Denver, June 2004

2. Clustering Strength Luminosity (B J ) L* Bright Redshift Clumpy Spatial clustering

4. Clustering is a function of mass and colour. Clustering could be a function of redshift. Angular scale Clustering strength  (1')=0.024  =1.81

5. How does galaxy clustering evolve? Trace the same galaxy population with redshift. Accurate redshifts and restframe selected galaxies. Red galaxies. Two preliminary studies using the first data release. Red galaxies at z<0.9 (Brown et al. 2003). EROs at 0.8<z<1.4 (Brown et al 2004).

6. Luminosity Spatial Clustering Red galaxies at z<0.9

7. Red galaxies and EROs Redshift Spatial Clustering

8. Completed preliminary studies of galaxy clustering. Red galaxies at z<0.9 (Brown et al. 2003). EROs at z~1.1 (Brown et al. 2004). Galaxy clustering is a function of luminosity. Galaxy clustering does not evolve rapidly with redshift. Preliminary studies are consistent with  CDM. Full survey area will be used for robust tests of  CDM.