Scale-invariant clustering and primordial biasing

Details Scale-invariant clustering and primordial biasing Scale-invariant clustering and primordial biasing

Jul 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...330l..21l&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 330, July 1, 1988, p. L21-L23.

Statistics

Computation

20

Galactic Clusters, Galactic Evolution, Normal Density Functions, Space Density, Computational Astrophysics, Power Spectra

Scientific paper

If cosmic objects formed around the maxima of a scale-invariant (either Gaussian or non-Gaussian) density perturbation field, their correlation length and mean distance are proportional as suggested by the observations. Since the typical density contrast of a peak is v times greater than the field rms value, a size-independent, primordial threshold v is obtained whose magnitude depends only on the statistics; late nonlinear evolution would mainly affect the clustering properties of objects like galaxies. In this framework a simple, phenomenological model for the power-spectrum and a 'minimal,' isocurvature perturbation model are discussed.

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