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

  • Author(s): Davis, M
  • Gerke, BF
  • Coil, AL
  • Cooper, MC
  • Yan, R
  • Newman, JA
  • Faber, SM
  • Koo, D
  • Guhathakurta, P
  • et al.

Published Web Location

https://arxiv.org/pdf/astro-ph/0507555v1.pdf
No data is associated with this publication.
Abstract

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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