Luminosity distance in Swiss cheese cosmology with randomized voids. II. Magnification probability distributions

TL;DR

This paper models the impact of large-scale voids on luminosity distance fluctuations in a Swiss cheese cosmology, quantifying the resulting magnification distributions and their dependence on void properties.

Contribution

It introduces a simplified model incorporating lensing shear effects in Swiss cheese cosmology to quantify luminosity distance fluctuations due to voids.

Findings

Standard deviation of magnitude shifts ~ 0.027 magnitudes for 35 Mpc voids at z=1.0

Void size, redshift, and shell mass fraction significantly affect the dispersion

Corrections to weak lensing theory are within a few percent for typical voids.

Abstract

We study the fluctuations in luminosity distances due to gravitational lensing by large scale (> 35 Mpc) structures, specifically voids and sheets. We use a simplified "Swiss cheese" model consisting of a \Lambda -CDM Friedman-Robertson-Walker background in which a number of randomly distributed non-overlapping spherical regions are replaced by mass compensating comoving voids, each with a uniform density interior and a thin shell of matter on the surface. We compute the distribution of magnitude shifts using a variant of the method of Holz & Wald (1998), which includes the effect of lensing shear. The standard deviation of this distribution is ~ 0.027 magnitudes and the mean is ~ 0.003 magnitudes for voids of radius 35 Mpc, sources at redshift z_s=1.0, with the voids chosen so that 90% of the mass is on the shell today. The standard deviation varies from 0.005 to 0.06 magnitudes as we vary the void size, source redshift, and fraction of mass on the shells today. If the shell walls are given a finite thickness of ~ 1 Mpc, the standard deviation is reduced to ~ 0.013 magnitudes. This standard deviation due to voids is a factor ~ 3 smaller than that due to galaxy scale structures. We summarize our results in terms of a fitting formula that is accurate to ~ 20%, and also build a simplified analytic model that reproduces our results to within ~ 30%. Our model also allows us to explore the domain of validity of weak lensing theory for voids. We find that for 35 Mpc voids, corrections to the dispersion due to lens-lens coupling are of order ~ 4%, and corrections to due shear are ~ 3%. Finally, we estimate the bias due to source-lens clustering in our model to be negligible.