The three-point function as a probe of models for large-scale structure

Details The three-point function as a probe of models for large-scale structure The three-point function as a probe of models for large-scale structure

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993stin...9411153f&link_type=abstract

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Mathematics

Logic

Bias, Dark Matter, Galactic Clusters, Galactic Evolution, Galactic Structure, Mathematical Models, Astronomical Models, Density Distribution, Extraterrestrial Matter

Scientific paper

The consequences of models of structure formation for higher-order (n-point) galaxy correlation functions in the mildly non-linear regime are analyzed. Several variations of the standard Omega = 1 cold dark matter model with scale-invariant primordial perturbations were recently introduced to obtain more power on large scales, Rp is approximately 20 h-1 Mpc, e.g., low-matter-density (non-zero cosmological constant) models, 'tilted' primordial spectra, and scenarios with a mixture of cold and hot dark matter. They also include models with an effective scale-dependent bias, such as the cooperative galaxy formation scenario of Bower, etal. It is shown that higher-order (n-point) galaxy correlation functions can provide a useful test of such models and can discriminate between models with true large-scale power in the density field and those where the galaxy power arises from scale-dependent bias: a bias with rapid scale-dependence leads to a dramatic decrease of the hierarchical amplitudes QJ at large scales, r is approximately greater than Rp. Current observational constraints on the three-point amplitudes Q3 and S3 can place limits on the bias parameter(s) and appear to disfavor, but not yet rule out, the hypothesis that scale-dependent bias is responsible for the extra power observed on large scales.

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