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.

Michael Brown (going to Princeton)Buell Jannuzi (PI)

Arjun Dey (PI)Glenn Tiede (now @ Bowling Green)

Tod LauerKate Brand

Frank ValdesAlyson Ford (going to Swinburne)

Lissa Miller (going to Yale)NDWFS Survey Team

The Clustering of Galaxies in Bootes

AAS, Denver, June 2004

Clu

ster

ing

Str

engt

h

Luminosity (BJ)

L* Bright

Redshift

Clumpy

Spatial clustering

Clustering is a function of mass and colour.

Clustering could be a function of redshift.

Angular scale

Clu

ster

ing

stre

ngthw(1')=0.024g=1.81

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).

Luminosity

Spa

tial

Clu

ster

ing

Red galaxies at z<0.9

Red galaxies and EROs

Redshift

Spa

tial

Clu

ster

ing

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 LCDM.

Full survey area will be used for robust tests of LCDM.