C. S. Kochanek et al. 2003 ApJ 585 161 doi:10.1086/345896
Clusters of Galaxies in the Local Universe
FREEC. S. Kochanek1, Martin White2, J. Huchra1, L. Macri1, T. H. Jarrett3, S. E. Schneider4 and J. Mader5
Show affiliationsWe use a matched filter algorithm to find and study clusters in both N-body simulations artificially populated with galaxies and the Two Micron All Sky Survey (2MASS). In addition to numerous checks of the matched filter algorithm, we present results on the halo multiplicity function and the cluster number function. For a subset of our identified clusters we have information on X-ray temperatures and luminosities that we cross-correlate with optical richness and galaxy velocity dispersions. With all quantities normalized by the spherical radius corresponding to a mass overdensity of ΔM = 200 or the equivalent galaxy number overdensity of ΔN = 200Ω
666, we find that the number of L > L* galaxies in a cluster of mass M200 is log N*666 = (1.44 ± 0.17) + (1.10 ± 0.09) log(M200h/1015 M
), where the uncertainties are dominated by the scatter created by three choices for relating the observed quantities to the cluster mass. The region inside the virial radius has a K-band cluster mass-to-light ratio of (M/L)K = (116 ± 46)h, which is essentially independent of cluster mass. Integrating over all clusters more massive than M200 = 1014 h-1 M, the virialized regions of clusters contain 7% of the local stellar luminosity, quite comparable to the mass fraction in such objects in currently popular ΛCDM models.
- Subject headings
cosmology: theory; galaxies: clusters: general; large-scale structure of universe
- Dates
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Issue 1 (2003 March 1)
Received 2002 August 8, accepted for publication 2002 November 1
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Clusters of Galaxies in the Local Universe
C. S. Kochanek et al. 2003 ApJ 585 161
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