Optimal PSF modeling for weak lensing: complexity and sparsity

TL;DR

This paper explores how the complexity and sparsity of PSF models affect weak lensing measurements, providing optimized strategies to calibrate PSF with limited stars for current and future surveys.

Contribution

It introduces a framework linking PSF model complexity and sparsity to calibration requirements, optimizing bias and error trade-offs in weak lensing.

Findings

Optimal PSF modeling reduces biases in cosmic shear measurements.

Future surveys need strict sparsity constraints for effective PSF calibration.

Relation between number of calibration stars and model sparsity is established.

Abstract

We investigate the impact of point spread function (PSF) fitting errors on cosmic shear measurements using the concepts of complexity and sparsity. Complexity, introduced in a previous paper, characterizes the number of degrees of freedom of the PSF. For instance, fitting an underlying PSF with a model with low complexity will lead to small statistical errors on the model parameters, however these parameters could suffer from large biases. Alternatively, fitting with a large number of parameters will tend to reduce biases at the expense of statistical errors. We perform an optimisation of scatters and biases by studying the mean squared error of a PSF model. We also characterize a model sparsity, which describes how efficiently the model is able to represent the underlying PSF using a limited number of free parameters. We present the general case and illustrate it for a realistic example of PSF fitted with shapelet basis sets. We derive the relation between complexity and sparsity of the PSF model, signal-to-noise ratio of stars and systematic errors on cosmological parameters. With the constraint of maintaining the systematics below the statistical uncertainties, this lead to a relation between the required number of stars to calibrate the PSF and the sparsity. We discuss the impact of our results for current and future cosmic shear surveys. In the typical case where the biases can be represented as a power law of the complexity, we show that current weak lensing surveys can calibrate the PSF with few stars, while future surveys will require hard constraints on the sparsity in order to calibrate the PSF with 50 stars.