The Cosmic Mach Number: Comparison from Observations, Numerical
  Simulations and Nonlinear Predictions
  We calculate the cosmic Mach number M - the ratio of the bulk flow of the
velocity field on scale R to the velocity dispersion within regions of scale R.
M is effectively a measure of the ratio of large-scale to small-scale power and
can be a useful tool to constrain the cosmological parameter space. Using a
compilation of existing peculiar velocity surveys, we calculate M and compare
it to that estimated from mock catalogues extracted from the LasDamas (a LCDM
cosmology) numerical simulations. We find agreement with expectations for the
LasDamas cosmology at ~ 1.5 sigma CL. We also show that our Mach estimates for
the mocks are not biased by selection function effects. To achieve this, we
extract dense and nearly-isotropic distributions using Gaussian selection
functions with the same width as the characteristic depth of the real surveys,
and show that the Mach numbers estimated from the mocks are very similar to the
values based on Gaussian profiles of the corresponding widths. We discuss the
importance of the survey window functions in estimating their effective depths.
We investigate the nonlinear matter power spectrum interpolator PkANN as an
alternative to numerical simulations, in the study of Mach number.
