Origins of weak lensing systematics, and requirements on future instrumentation (or knowledge of instrumentation)

TL;DR

This paper investigates the origins of systematic biases in weak lensing measurements, emphasizing the importance of instrument stability and calibration, and sets stringent requirements for future surveys like Euclid to achieve precise cosmological constraints.

Contribution

It expands the understanding of weak lensing systematics by including detector non-idealities and shape measurement biases, providing a comprehensive framework for instrument calibration and performance requirements.

Findings

Performance depends on telescope/camera quality and knowledge about it.

Current software meets requirements for bright galaxies in space-based surveys.

Calibration on simulations is necessary for fainter galaxies and 3D tomography.

Abstract

The first half of this paper explores the origin of systematic biases in the measurement of weak gravitational lensing. Compared to previous work, we expand the investigation of PSF instability and fold in for the first time the effects of non-idealities in electronic imaging detectors and imperfect galaxy shape measurement algorithms. Together, these now explain the additive A(l) and multiplicative M(l) systematics typically reported in current lensing measurements. We find that overall performance is driven by a product of a telescope/camera's *absolute performance*, and our *knowledge about its performance*. The second half of this paper propagates any residual shear measurement biases through to their effect on cosmological parameter constraints. Fully exploiting the statistical power of Stage IV weak lensing surveys will require additive biases A<1.8e-12 and multiplicative biases M<4.0e-3. These can be allocated between individual budgets in hardware, calibration data and software, using results from the first half of the paper. If instrumentation is stable and well-calibrated, we find extant shear measurement software from GREAT10 already meet requirements on galaxies detected at S/N=40. Averaging over a population of galaxies with a realistic distribution of sizes, it also meets requirements for a 2D cosmic shear analysis from space. If used on fainter galaxies or for 3D cosmic shear tomography, existing algorithms would need calibration on simulations to avoid introducing bias at a level similar to the statistical error. Requirements on hardware and calibration data are discussed in more detail in a companion paper. Our analysis is intentionally general, but is specifically being used to drive the hardware and ground segment performance budget for the design of the European Space Agency's recently-selected Euclid mission.