An analytic model for the bispectrum of galaxies in redshift space

TL;DR

This paper presents an analytic halo model for the galaxy bispectrum in redshift space, accurately capturing non-linear effects and redshift distortions across various scales, and validated against simulations.

Contribution

The paper introduces a comprehensive analytic halo model for the redshift space bispectrum that improves upon perturbation theory, especially on smaller, non-linear scales.

Findings

Good agreement with simulations on large scales (k=0.05 h/Mpc)

Model accuracy improves over perturbation theory on smaller scales

Breakdown of PT on scales larger than 0.1 h/Mpc

Abstract

We develop an analytic theory for the redshift space bispectrum of dark matter, haloes and galaxies. This is done within the context of the halo model of structure formation, as this allows for the self-consistent inclusion of linear and non-linear redshift space distortions and also for the non-linearity of the halo bias. The model is applicable over a wide range of scales: on the largest scales the predictions reduce to those of the standard perturbation theory (PT); on smaller scales they are determined primarily by the nonlinear virial velocities of galaxies within haloes, and this gives rise to the U-shaped anisotropy in the reduced bispectrum -- a finger print of the Finger-Of-God distortions. We then confront the predictions with bispectrum measurements from an ensemble of numerical simulations. On very large scales, k=0.05 h/Mpc, we find reasonably good agreement between our Halo Model, PT and the data, to within the errors. On smaller scales, k=0.1 h/Mpc, the measured bispectra differ from the PT at the level of 10-20%, especially for colinear triangle configurations. The Halo Model predictions improve over PT, but are accurate to no better than 10%. On smaller scales k=0.5-1.0 h/Mpc, our model provides a significant improvement over PT, which breaks down. This implies that studies which use the lowest order PT to extract galaxy bias information are not robust on scales k>0.1 h/Mpc. The analytic and simulation results also indicate that there is no observable scale for which the configuration dependence of the reduced bispectrum is constant--hierarchical models for the higher order correlation functions in redshift space are unlikely to be useful. It is hoped that our model will facilitate extraction of information from large-scale structure surveys of the Universe.