S\'{e}rsic galaxy models in weak lensing shape measurement: model bias, noise bias and their interaction

TL;DR

This paper analyzes the combined impact of model bias, noise bias, and their interaction on galaxy shape measurements in weak lensing, providing analytical expressions and empirical quantification relevant for upcoming surveys.

Contribution

It introduces a comprehensive analytical framework for understanding and measuring the interplay between model bias and noise bias in galaxy shape estimation.

Findings

Interaction bias can be significant and comparable to model bias.

The interaction term is generally smaller than survey requirements.

Quantitative analysis using real COSMOS galaxy images.

Abstract

Cosmic shear is a powerful probe of cosmological parameters, but its potential can be fully utilised only if galaxy shapes are measured with great accuracy. Two major effects have been identified which are likely to account for most of the bias for maximum likelihood methods in recent shear measurement challenges. Model bias occurs when the true galaxy shape is not well represented by the fitted model. Noise bias occurs due to the non-linear relationship between image pixels and galaxy shape. In this paper we investigate the potential interplay between these two effects when an imperfect model is used in the presence of high noise. We present analytical expressions for this bias, which depends on the residual difference between the model and real data. They can lead to biases not accounted for in previous calibration schemes. By measuring the model bias, noise bias and their interaction, we provide a complete statistical framework for measuring galaxy shapes with model fitting methods from GRavitational lEnsing Accuracy Testing (GREAT) like images. We demonstrate the noise and model interaction bias using a simple toy model, which indicates that this effect can potentially be significant. Using real galaxy images from the Cosmological Evolution Survey (COSMOS) we quantify the strength of the model bias, noise bias and their interaction. We find that the interaction term is often a similar size to the model bias term, and is smaller than the requirements of the current and shortly upcoming galaxy surveys.