A Zeldovich reconstruction method for measuring redshift space distortions using cosmic voids

TL;DR

This paper introduces a Zeldovich reconstruction method to accurately measure redshift space distortions around cosmic voids, enabling better estimation of the growth rate of structure from observational data.

Contribution

It proposes a density-field reconstruction technique based on the Zeldovich approximation to recover real space void positions from redshift space data, improving RSD modeling.

Findings

Achieves 3.4% precision in growth rate measurement in simulations.

Recovers excellent agreement between theory and data after reconstruction.

Demonstrates effectiveness on mock galaxy and void catalogues.

Abstract

Redshift space distortions (RSD) in the void-galaxy correlation $\xi^s$ provide information on the linear growth rate of structure in low density environments. Accurate modelling of these RSD effects can also allow the use of voids in competitive Alcock-Paczynski measurements. Linear theory models of $\xi^s$ are able to provide extremely good descriptions of simulation data on all scales provided the real space void positions are known. However, by reference to simulation data we demonstrate the failure of the assumptions implicit in current models of $\xi^s$ for voids identified directly in redshift space, as would be simplest using real observational data. To overcome this problem we instead propose using a density-field reconstruction method based on the Zeldovich approximation to recover the real space void positions from redshift space data. We show that this recovers the excellent agreement between theory and data for $\xi^s$. Performing the reconstruction requires an input cosmological model so, to be self-consistent, we have to perform reconstruction for every model to be tested. We apply this method to mock galaxy and void catalogues in the Big MultiDark $N$-body simulation and consistently recover the fiducial growth rate to a precision of $3.4\%$ using the simulation volume of $(2.5\;h^{-1}\mathrm{Gpc})^3$.