Cosmological density and power spectrum from peculiar velocities: Nonlinear corrections and principal component analysis

We allow for nonlinear effects in the likelihood analysis of galaxy peculia r velocities and obtain similar to 35% lower values for the cosmological de nsity parameter Omega (m) and for the amplitude of mass density fluctuation s sigma (8) Omega (0.6)(m). This result is obtained under the assumption th at the power spectrum in the linear regime is of the flat Lambda CDM model (h = 0.65, n = 1, COBE normalized) with only Omega (m) as a free parameter. Since the likelihood is driven by the nonlinear regime, we "break" the pow er spectrum at k(b) similar to 0.2 (h(-1) Mpc)(-1) and fit a power law at k > k(b). This allows for independent matching of the nonlinear behavior and an unbiased fit in the linear regime. The analysis assumes Gaussian fluctu ations and errors and a linear relation between velocity and density. Tests using mock catalogs that properly simulate nonlinear effects demonstrate t hat this procedure results in a reduced bias and a better fit. We find for the Mark III and SFI data Omega (m) = 0.32 +/- 0.06 and 0.37 +/- 0.09, resp ectively, with sigma (8) Omega (0.6)(m) = 0.49 +/- 0.06 and 0.63 +/- 0.08, in agreement with constraints from other data. The quoted 90% errors includ e distance errors and cosmic variance, for fixed values of the other parame ters. The improvement in the likelihood due to the nonlinear correction is very significant for Mark III and moderately significant for SFI. When allowing deviations from Lambda CDM, we find an indication for a wiggl e in the power spectrum: an excess near k similar to 0.05 (h(-1) Mpc)(-1) a nd a deficiency at k similar to 0.1 (h(-1) Mpc)(-1), or a "cold flow." This may be related to the wiggle seen in the power spectrum from redshift surv eys and the second peak in the cosmic microwave background (CMB) anisotropy . A chi (2) test applied to modes of a principal component analysis (PCA) sho ws that the nonlinear procedure improves the goodness of fit and reduces a spatial gradient that was of concern in the purely linear analysis. The PCA allows us to address spatial features of the data and to evaluate and fine -tune the theoretical and error models. It demonstrates in particular that the models used are appropriate for the cosmological parameter estimation p erformed. We address the potential for optimal data compression using PCA.