Observational Constraints for Power-law spectra of Density Perturbations

Details Observational Constraints for Power-law spectra of Density Perturbations Observational Constraints for Power-law spectra of Density Perturbations

1998-03-30

arxiv.org/abs/astro-ph/9803328v1

Grav.Cosmol.5:159,1999

Astronomy and Astrophysics

Astrophysics

6 pages, 4 figures, to appear in Proceedings of the 3rd International Conference on Cosmoparticle Physics "Cosmion-97", Moscow

Scientific paper

We present an analysis of cosmological models with mixed dark matter (spectrum slope of density perturbations $n_S \in [0.6, 1.6]$, hot dark matter abundance $\Omega_\nu \in [0.0, 0.6]$) in spatially flat Universe, based on Press-Schechter formalism (P\&S). We found that the models with $n_S > 1$ and $\Omega_\nu < 0.5$ are preferable. Additionally, for all considered models we simulated $\Delta T/T\vert_{10^0}$ and compared it with the COBE measured amplitude of CMB anisotropy. We found that the models favourable for galaxy cluster abundance need large amount of cosmological gravitational waves (T/S $> 1$).

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