Predictions of a non-Gaussian model for large scale structure

Details Predictions of a non-Gaussian model for large scale structure Predictions of a non-Gaussian model for large scale structure

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992stin...9330528f&link_type=abstract

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Physics

Background Radiation, Cosmology, Dark Matter, Universe, Cosmic Background Explorer Satellite, Galactic Clusters, Mass Distribution, Microwaves, Scalars

Scientific paper

A modified CDM model for the origin of structure in the universe based on an inflation model with two interacting scalar fields, is analyzed to make predictions for the statistical properties of the density and velocity fields and the microwave background anisotropy. The initial gauge-invariant potential zeta which is defined as zeta = (delta)rho/(rho + p) + 3(var phi), where (var phi) is the curvature perturbation amplitude and p is the pressure, is the sum of a Gaussian field phi1, and the square of a Gaussian field phi2. A Harrison-Zel'dovich scale-invariant power spectrum is assumed for phi1; and a log-normal 'peak' power spectrum for phi2. The location and the width of the peak are described by parameters kc and a. respectively. The model is motivated to some extent by inflation models with two interacting scalar fields, but is mainly interesting as an example of a model whose statistical properties change with scale. On small scales, it is almost identical to a standard scale-invariant Gaussian CDM model. On scales near the location of the peak of the non-Gaussian field, the distributions have long tails in high positive values of the density and velocity fields. Thus, it is easier to get large-scale streaming velocities than the standard CDM model. The quadrupole amplitude of fluctuations of the cosmic microwave background radiation and the rms variation of the temperature field smoothed with a 10 deg FWHM Gaussian are calculated; a reasonable agreement is found with the new COBE results.

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