The difference between the galaxy and cluster correlation functions - A manifestation of tails of galaxy clusters

Details The difference between the galaxy and cluster correlation functions - A manifestation of tails of galaxy clusters The difference between the galaxy and cluster correlation functions - A manifestation of tails of galaxy clusters

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...302l..41b&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 302, March 15, 1986, p. L41-L44.

Mathematics

Logic

27

Astronomical Models, Galactic Clusters, Correlation, Galactic Structure, Spatial Distribution

Scientific paper

A phenomenological model is presented that explains the observed difference between the galaxy and rich cluster correlation functions, based on the fraction of galaxies that participate in the clustering. The model also explains the observed trend of increasing correlation strength with richness. It is shown that if about 25 percent of all galaxies are associated with rich (richness equal to or greater than 1) clusters, and the other galaxies are only weakly correlated, the galaxy correlation function will be, as observed, about 18 times weaker than the cluster correlations. The model suggests that the fraction of galaxies associated with rich clusters is larger than previously expected; most of these galaxies are distributed in the outer tails of the clusters which may extend to at least about 30/h Mpc. The weak (or negligible) correlation observed among Ly-alpha clouds in QSO spectra may reflect the noncluster component of galaxies. The model can be tested by measuring with redshift surveys the number of galaxies that lie beyond one Abell radius in rich clusters and by recalculating the galaxy correlation function excluding all areas within 20 Abell radii of rich clusters.

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