2018/09/25 by B. Gillis, Bryan R. Gillis, A. N. Taylor
Mathematics · Physics and Astronomy · #Adaptive optics and wavefront sensing #Algorithm #Astronomy and Astrophysical Research #Calibration #Galaxies: Formation, Evolution, Phenomena #Mathematical analysis #Mathematics #Multiplicative function #Observational error #Optics #Physics #Residual #Statistics #astro-ph.CO
paper · pdf · doi:10.1093/mnras/sty2637
15 pages, 8 figures, 2 tables. Accepted for publication by MNRAS
arxiv created 2018/09/25 · openalex publication_date 2018/09/28 · arxiv updated 2018/10/17 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Forthcoming large-scale surveys will soon attempt to measure cosmic shear to an unprecedented level of accuracy, requiring a similarly high level of accuracy in the shear measurements of galaxies. Factors such as pixelization, imperfect point-spread function correction, and pixel noise can all directly or indirectly lead to biases in shear measurements, and so it can be necessary for shear measurement methods to be calibrated against internal, external, or simulated data to minimize bias. It is thus important to understand the nature of this calibration. In this paper, we show that a typical calibration procedure will on average leave no residual additive bias, but will leave a residual multiplicative bias. Additionally, the errors on the post-calibration bias parameters will be changed, and on average increased, from the errors on the pre-calibration measurements of these parameters, but that this is generally worth the benefit in decreasing the expected value of the multiplicative bias. We find that in most typical cases, it is worthwhile to apply a first-order bias correction, while a higher order bias correction is only worthwhile for methods with intrinsically high multiplicative bias (>10 per cent) or when the simulation size is very small (<106 simulated galaxies).