2012/10/31 by M. Cropper, Mark Cropper, Henk Hoekstra +18
Physics and Astronomy · #Adaptive optics and wavefront sensing #Astrophysical Phenomena and Observations #Astrophysics #Computer science #Detector #Galaxies: Formation, Evolution, Phenomena #Galaxy #Optics #Physics #Point spread function #Redshift #Set (abstract data type) #Weak gravitational lensing #Weighting #astro-ph.CO #astro-ph.IM
paper · pdf · doi:10.1093/mnras/stt384
published as MNRAS 431 (2013), 3103 · 26 pages, 12 figures. Version 2 contains changes from the refereeing with a useful clarification of points in section 2.2, leading to an added section 2.3, while section 3.1 has been slightly expanded. There are no changes to the results. Other minor edits have been made, and the author list slightly amended. Accepted by MNRAS. See companion (theory) paper Massey et al (2013) MNRAS, 429, 661
openalex publication_date 2013/04/09 · arxiv created 2013/05/19 · arxiv updated 2015/06/11 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
This paper describes the definition of a typical next-generation space-based weak gravitational lensing experiment. We first adopt a set of top-level science requirements from the literature, based on the scale and depth of the galaxy sample, and the avoidance of systematic effects in the measurements which would bias the derived shear values. We then identify and categorize the contributing factors to the systematic effects, combining them with the correct weighting, in such a way as to fit within the top-level requirements. We present techniques which permit the performance to be evaluated and explore the limits at which the contributing factors can be managed. Besides the modelling biases resulting from the use of weighted moments, the main contributing factors are the reconstruction of the instrument point spread function, which is derived from the stellar images on the image, and the correction of the charge transfer inefficiency in the CCD detectors caused by radiation damage.