Transition scale to a homogeneous universe

Details Transition scale to a homogeneous universe Transition scale to a homogeneous universe

Apr 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...407..443e&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 407, no. 2, p. 443-447.

Statistics

Computation

34

Computational Astrophysics, Galactic Clusters, Relic Radiation, Universe, Astronomical Observatories, Spatial Distribution, Transfer Functions

Scientific paper

We analyze observed and simulated galaxy and cluster samples to find the transition scale to homogeneity in the real space, r(t), and in the Fourier space, lambda(t). The correlation transition scale is determined by the minimum of the second derivative of the correlation function, the spectral scale by the transition from a negative to a positive spectral index. Available data suggest values r(t) = 130 +/- 10/h and lambda(t)t = 175 + 15/h Mpc. These values are in good agreement with the amplitude of fluctuations of the cosmic microwave background radiation. The comparison of potential fields of model samples of identical transition scale but different spectral index on large scales demonstrates that long-wavelength fluctuations influence significantly the potential field. Consequently the fair sample size must be larger than the spectral transition scale.

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