Weakly Nonlinear Density-Velocity Relation

Details Weakly Nonlinear Density-Velocity Relation Weakly Nonlinear Density-Velocity Relation

1996-06-14

arxiv.org/abs/astro-ph/9606088v2

Astronomy and Astrophysics

Astrophysics

34 pages, figures included, minor changes, a few references added, accepted for publication in MNRAS

Scientific paper

We rigorously derive weakly nonlinear relation between cosmic density and velocity fields up to third order in perturbation theory. The density field is described by the mass density contrast, $\de$. The velocity field is described by the variable $\te$ proportional to the velocity divergence, $\te = - f(\Omega)^{-1} H_0^{-1} \nabla\cdot\bfv$, where $f(\Omega) \simeq \Omega^{0.6}$, $\Omega$ is the cosmological density parameter and $H_0$ is the Hubble constant. Our calculations show that mean $\de$ given $\te$ is a third order polynomial in $\te$, $\lan \de \ran|_{\te} = a_1 \te + a_2 (\te^2 - \s_\te^2) + a_3 \te^3$. This result constitutes an extension of the formula $\lan \de \ran|_{\te} = \te + a_2 (\te^2 - \s_\te^2)$, found by Bernardeau~(1992) which involved second order perturbative solutions. Third order perturbative corrections introduce the cubic term. They also, however, cause the coefficient $a_1$ to depart from unity, in contrast with the linear theory prediction. We compute the values of the coefficients $a_p$ for scale-free power spectra, as well as for standard CDM, for Gaussian smoothing. The coefficients obey a hierarchy $a_3 \ll a_2 \ll a_1$, meaning that the perturbative series converges very fast. Their dependence on $\Omega$ is expected to be very weak. The values of the coefficients for CDM spectrum are in qualitative agreement with the results of N-body simulations by Ganon et al. (1996). The results provide a method for breaking the $\Omega$-bias degeneracy in comparisons of cosmic density and velocity fields such as IRAS-POTENT.

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