A Bayesian Hierarchical Approach to Galaxy-Galaxy Lensing

TL;DR

This paper introduces a Bayesian hierarchical method for galaxy-galaxy lensing analysis that improves the accuracy of scaling relation measurements by properly accounting for scatter and avoiding data stacking.

Contribution

The paper presents a novel Bayesian hierarchical inference formalism that enhances the analysis of weak lensing data, enabling unbiased constraints on galaxy-halo relations without stacking.

Findings

Accurately recovers mean halo mass and concentration with 0.1 dex precision.

Effectively constrains intrinsic scatter in halo mass with 0.05 dex accuracy.

Reduces bias caused by observational scatter in traditional stacking methods.

Abstract

We present a Bayesian hierarchical inference formalism to study the relation between the properties of dark matter halos and those of their central galaxies using weak gravitational lensing. Unlike traditional methods, this technique does not resort to stacking the weak lensing signal in bins, and thus allows for a more efficient use of the information content in the data. Our method is particularly useful for constraining scaling relations between two or more galaxy properties and dark matter halo mass, and can also be used to constrain the intrinsic scatter in these scaling relations. We show that, if observational scatter is not properly accounted for, the traditional stacking method can produce biased results when exploring correlations between multiple galaxy properties and halo mass. For example, this bias can affect studies of the joint correlation between galaxy mass, halo mass, and galaxy size, or galaxy color. In contrast, our method easily and efficiently handles the intrinsic and observational scatter in multiple galaxy properties and halo mass. We test our method on mocks with varying degrees of complexity. We find that we can recover the mean halo mass and concentration, each with a $0.1$ dex accuracy, and the intrinsic scatter in halo mass with a $0.05$ dex accuracy. In its current version, our method will be most useful for studying the weak lensing signal around central galaxies in groups and clusters, as well as massive galaxies samples with $\log{M_*} > 11$, which have low satellite fractions.