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slides
Clusters in Various Cosmological Models: Abundance and Evolution
Authors
Stefano Borgani
Marisa Girardi
+3Â more
Michael A. K. Gross
Joel R. Primack
Rachel S. Somerville
Publication date
4 November 1997
Publisher
View
on
arXiv
Abstract
The combination of measurements of the local abundance of rich clusters of galaxies and its evolution to higher redshift offers the possibility of a direct measurement of
Ω
0
\Omega_0
Ω
0
​
with little contribution from other cosmological parameters. We investigate the significance of recent claims that this evolution indicates that
Ω
0
\Omega_0
Ω
0
​
must be small. The most recent cluster velocity dispersion function from a compilation including the ESO Northern Abell Cluster Survey (ENACS) results in a significantly higher normalization for models, corresponding to
σ
8
≈
0.6
\sigma_8\approx 0.6
σ
8
​
≈
0.6
for
Ω
0
=
1
\Omega_0=1
Ω
0
​
=
1
, compared to the Eke, Cole, & Frenk result of
σ
8
=
0.52
±
0.04
\sigma_8=0.52\pm 0.04
σ
8
​
=
0.52
±
0.04
. Using the ENACS data for a
z
=
0
z=0
z
=
0
calibration results in strong evolution in the abundance of clusters, and we find that the velocity dispersion function is consistent with
Ω
0
=
1
\Omega_0=1
Ω
0
​
=
1
. The results are dependent upon the choice and analysis of low-redshift and high-redshift data, so at present, the data is not good enough to determine
Ω
0
\Omega_0
Ω
0
​
unambiguously.Comment: 4 pages Latex using sprocl.sty, 1 figure. To appear in Proceedings of 12th Potsdam Cosmology Workshop, "Large-Scale Structure: Tracks and Traces" Sept. 15-19, 199
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Last time updated on 12/11/2016