The formation of cosmic structure in a texture-seeded cold dark matter cosmogony

Details The formation of cosmic structure in a texture-seeded cold dark matter cosmogony The formation of cosmic structure in a texture-seeded cold dark matter cosmogony

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...393...42g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 393, no. 1, July 1, 1992, p. 42-58. Research supported by Alfred P. Sloan F

Mathematics

Probability

31

Astronomical Models, Background Radiation, Cosmology, Dark Matter, Power Spectra, Baryons, Galactic Clusters, Galactic Evolution, Infrared Astronomy Satellite, Probability Distribution Functions

Scientific paper

The growth of density fluctuations induced by global texture in an Omega = 1 cold dark matter (CDM) cosmogony is calculated. The resulting power spectra are in good agreement with each other, with more power on large scales than in the standard inflation plus CDM model. Calculation of related statistics (two-point correlation functions, mass variances, cosmic Mach number) indicates that the texture plus CDM model compares more favorably than standard CDM with observations of large-scale structure. Texture produces coherent velocity fields on large scales, as observed. Excessive small-scale velocity dispersions, and voids less empty than those observed may be remedied by including baryonic physics. The topology of the cosmic structure agrees well with observation. The non-Gaussian texture induced density fluctuations lead to earlier nonlinear object formation than in Gaussian models and may also be more compatible with recent evidence that the galaxy density field is non-Gaussian on large scales. On smaller scales the density field is strongly non-Gaussian, but this appears to be primarily due to nonlinear gravitational clustering. The velocity field on smaller scales is surprisingly Gaussian.

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