michael brown (going to princeton) buell jannuzi (pi) arjun dey (pi) glenn tiede (now @ bowling...
TRANSCRIPT
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.