# Practical Weak Lensing Shear Measurement with Metacalibration

## TL;DR

This paper advances the metacalibration method for weak lensing shear measurement by developing a formalism to correct for shear response, selection biases, and noise-induced biases, achieving high accuracy in realistic simulations.

## Contribution

It introduces a comprehensive formalism to correct for biases in metacalibration, including low signal-to-noise effects and selection biases, validated with extensive simulations.

## Key findings

- Achieved shear measurement accuracy better than 0.1% in simulations.
- Developed empirical correction for noise bias in low S/N images.
- Validated method with realistic galaxy and PSF simulations.

## Abstract

Metacalibration is a recently introduced method to accurately measure weak gravitational lensing shear using only the available imaging data, without need for prior information about galaxy properties or calibration from simulations. The method involves distorting the image with a small known shear, and calculating the response of a shear estimator to that applied shear. The method was shown to be accurate in moderate sized simulations with galaxy images that had relatively high signal-to-noise ratios, and without significant selection effects. In this work we introduce a formalism to correct for both shear response and selection biases. We also observe that, for images with relatively low signal-to-noise ratios, the correlated noise that arises during the metacalibration process results in significant bias, for which we develop a simple empirical correction. To test this formalism, we created large image simulations based on both parametric models and real galaxy images, including tests with realistic point-spread functions. We varied the point-spread function ellipticity at the five percent level. In each simulation we applied a small, few percent shear to the galaxy images. We introduced additional challenges that arise in real data, such as detection thresholds, stellar contamination, and missing data. We applied cuts on the measured galaxy properties to induce significant selection effects. Using our formalism, we recovered the input shear with an accuracy better than a part in a thousand in all cases.