Expansion schemes for gravitational clustering: computing two-point and three-point functions

Abstract

We describe various expansion schemes that can be used to study gravitational clustering. Obtained from the equations of motion or their path-integral formulation, they provide several perturbative expansions that are organized in different fashion or involve different partial resummations. We focus on the two-point and three-point correlation functions, but these methods also apply to all higher-order correlation and response functions. We present the general formalism, which holds for the gravitational dynamics as well as for similar models, such as the Zeldovich dynamics, that obey similar hydrodynamical equations of motion with a quadratic nonlinearity. We give our explicit analytical results up to one-loop order for the simpler Zeldovich dynamics. For the gravitational dynamics, we compare our one-loop numerical results with numerical simulations. We check that the standard perturbation theory is recovered from the path integral by expanding over Feynman's diagrams. However, the latter expansion is organized in a different fashion and it contains some UV divergences that cancel out as we sum all diagrams of a given order. Resummation schemes modify the scaling of tree and one-loop diagrams, which exhibit the same scaling over the linear power spectrum (contrary to the standard expansion). However, they do not significantly improve over standard perturbation theory for the bispectrum, unless one uses accurate two-point functions (e.g. a fit to the nonlinear power spectrum from simulations). Extending the range of validity to smaller scales, to reach the range described by phenomenological models, seems to require at least two-loop diagrams.

24 pages, published in A&A

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• Combining perturbation theories with halo models
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• Impact on the power spectrum of Screening in Modified Gravity Scenarios
• Structure Formation in Modified Gravity Scenarios
• Angular averaged consistency relations of large-scale structures
• Matter power spectrum from a Lagrangian-space regularization of perturbation theory
• Power spectra in the eikonal approximation with adiabatic and non-adiabatic modes
• Impact of shell crossing and scope of perturbative approaches in real and redshift space
• How to generate a significant effective temperature for cold dark matter, from first principles
• Combining perturbation theories with halo models for the matter bispectrum
• Kinematic consistency relations of large-scale structures
• Large-scale structure perturbation theory without losing stream crossing
• Modeling of weak lensing statistics. I. Power spectrum and bispectrum
• Accuracy of analytical models of the large-scale matter distribution
• Eulerian and Lagrangian propagators for the adhesion model (Burgers dynamics)
• Evolution of dark matter velocity dispersion
• Redshift-space equal-time angular-averaged consistency relations of the gravitational dynamics
• Impact of a Warm Dark Matter late-time velocity dispersion on large-scale structures
• Dark matter vorticity and velocity dispersion from truncated Dyson$\unicode{x2013}$Schwinger equations
• Exact Results for Propagators in the Geometrical Adhesion Model
• Estimating power spectrum of discrete cosmic momentum field with fast Fourier transform
• Projection of the gravitational dynamics on a subspace of probability distributions: curl-free Gaussian ansatz
• Cosmological functional renormalisation group, extended Galilean invariance and the sweeping effect
• A redshift distortion free correlation function at third order in the nonlinear regime