Non-self-similar clustering of galaxies

Details Non-self-similar clustering of galaxies Non-self-similar clustering of galaxies

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...401...19g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 401, no. 1, p. 19-27.

Astronomy and Astrophysics

Astrophysics

12

Cosmology, Galactic Clusters, Many Body Problem, Computerized Simulation, Power Spectra, Relic Radiation, Spatial Distribution

Scientific paper

The influence of large-scale density fluctuations on the evolution of small-scale clustering of galaxies is examined. To investigate the fully nonlinear regime we ran N-body simulations. Numerical results show that the evolution of clustering of galaxies strongly depends on the transition scale of the power spectrum. For a 2D power spectrum with n = -1, the wavelength on which density fluctuations go nonlinear is determined by the value of (/lambdat//lambda sub delta/) exp 1/2, where lambdat is the transition scale of the power spectrum, and lambdadelta is the length scale on which the rms amplitude of the density becomes equal to unity. We analyze the variance of the power spectrum and potential field in different subsamples of the simulations. To investigate the potential field using observational data, the sample size must be at least of the order of the transition scale in the power spectrum.

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