Summary
A percolation cluster analysis is performed on equivalent regions of the CFA redshift survey of galaxies and the 4000 body simulations of gravitational clustering made by Aarseth, Gott & Turner (1979). The observed and simulated percolation properties are compared and, unlike correlation and multiplicity function analyses, favour high density (Ω = 1) models with n = −1 initial data. Our results show that the three-dimensional data are consistent with the degree of filamentary structure present in isothermal models of galaxy formation at the level of percolation analysis. We also find that the percolation structure of the CFA data is a function of depth. Percolation structure does not appear to be a sensitive probe of intrinsic filamentary structure.
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© 1984 D. Reidel Publishing Company
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Bhavsar, S.P., Barrow, J.D. (1984). Percolation Studies of Galaxy Clustering. In: Mardirossian, F., Giuricin, G., Mezzetti, M. (eds) Clusters and Groups of Galaxies. Astrophysics and Space Science Library, vol 111. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-6412-9_77
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DOI: https://doi.org/10.1007/978-94-009-6412-9_77
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