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Defining a weak lensing experiment in space

M. CropperMullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UKHenk HoekstraLeiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the NetherlandsT. KitchingMullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UKR. MasseyDepartment of Physics, Durham University, South Road, Durham DH1 3LE, UKJ. AmiauxService dAstrophysique, CEA Saclay, F-91191 Gif sur Yvette, FranceL. MillerDepartment of Physics, University of Oxford, The Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UKY. MellierInstitut dAstrophysique de Paris, UMR7095 CNRS, Université Pierre et Marie Curie, 98 bis Boulevard Arago, F-75014 Paris, FranceJason RhodesJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USABarnaby RoweCalifornia Institute of Technology, 1200 E California Blvd., Pasadena, CA 91125, USAS. PiresService dAstrophysique, CEA Saclay, F-91191 Gif sur Yvette, FranceC. J. SaxtonMullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UKR. ScaramellaINAF, Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monteporzio Catone, Italy

2013en

ABI

Annotatsiya

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.

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Identifikatorlar

DOI: 10.1093/mnras/stt384

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