Defining a weak lensing experiment in space

被引：78

作者：

Cropper, Mark ^{[1
]}

Hoekstra, Henk ^{[2
]}

Kitching, Thomas ^{[1
,3
]}

Massey, Richard ^{[3
,4
]}

Amiaux, Jerome ^{[5
]}

Miller, Lance ^{[6
]}

Mellier, Yannick ^{[5
,7
]}

Rhodes, Jason ^{[8
,9
]}

Rowe, Barnaby ^{[9
,10
]}

Pires, Sandrine ^{[5
]}

Saxton, Curtis ^{[1
]}

Scaramella, Roberto ^{[11
]}

机构：

[1] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[2] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

[3] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland

[4] Univ Durham, Dept Phys, Durham DH1 3LE, England

[5] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France

[6] Univ Oxford, Dept Phys, Oxford OX1 3RH, England

[7] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France

[8] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[9] CALTECH, Pasadena, CA 91125 USA

[10] UCL, Dept Phys & Astron, London WC1E 6BT, England

[11] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2013年 / 431卷 / 04期

基金：

欧洲研究理事会;

关键词：

gravitational lensing: weak; methods: statistical; space vehicles: instruments; cosmological parameters; cosmology: observations; POINT-SPREAD FUNCTION; GALAXY SHAPE MEASUREMENT; CHARGE-TRANSFER INEFFICIENCY; PIXEL-BASED CORRECTION; COSMIC SHEAR; ADVANCED CAMERA; DARK ENERGY; SYSTEMATIC-ERRORS; IMAGE-ANALYSIS; TELESCOPE;

D O I：

10.1093/mnras/stt384

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页码：3103 / 3126

页数：24

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