Cosmic Strings, Loops, and Large-Scale Structure

Details Cosmic Strings, Loops, and Large-Scale Structure Cosmic Strings, Loops, and Large-Scale Structure

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998tx19.confe.200w&link_type=abstract

Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.:

Astronomy and Astrophysics

Astrophysics

Scientific paper

We describe the results of high-resolution numerical simulations of cosmic-string-seeded structure formation in open universes and those with a non-zero cosmological constant. For models with Gamma = Omega h = 0.1-0.2 and a CDM background, the linear density perturbation power spectrum {cal P}(k) has both an amplitude at 8 h^{-1}Mpc, sigma_8, and an overall shape which are consistent within uncertainties with those currently inferred from galaxy surveys. We also show that cosmic string loops behave like part of the long-string network on large scales and can therefore contribute significantly to {cal P}(k) if they live long enough. This will potentially improve the large-scale bias problem previously seen in cosmic string models. The non-Gaussian scales revealed in the linear regime are 1.5(Omega h^2)^{-1}Mpc and below. The cosmic string scenario with HDM requires a strongly scale-dependent bias in order to agree with observations.

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