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.

Scale-Invariant Clustering and Primordial Biasing

LUCCHIN, FRANCESCO;MATARRESE, SABINO;
1988

Abstract

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.
1988
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11577/135461
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