Measuring the Growth of Structure with Spectroscopically Identified Groups and Clusters

Details Measuring the Growth of Structure with Spectroscopically Identified Groups and Clusters Measuring the Growth of Structure with Spectroscopically Identified Groups and Clusters

2005-07-22

arxiv.org/abs/astro-ph/0507555v1

Astronomy and Astrophysics

Astrophysics

10 pages, including 5 figures. White paper submitted to the Dark Energy Task Force Committee

Scientific paper

Number counts of galaxy clusters offer a very promising probe of the Dark Energy (DE) equation-of-state parameter, $w$. The basic goal is to measure abundances of these objects as a function of redshift, compare this to a theoretical prediction, and infer the values of cosmological parameters. Various teams have proposed such a measurement, including the South Pole Telescope, the Dark Energy Survey and the Red-Sequence Cluster Survey. The specific study discussed here detects clusters and smaller galaxy groups in the three-dimensional distribution of galaxies inferred from a large spectroscopic redshift survey. This method allows the abundance, $N$, of groups and clusters to be measured as a function of \emph{velocity dispersion}, as well as of redshift, permitting a more sensitive test of cosmology.

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