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The Effect of Detector Nonlinearity on WFIRSTPSF Profiles for Weak Gravitational Lensing Measurements

Plazas, A. A. and Shapiro, C. and Kannawadi, A. and Mandelbaum, R. and Rhodes, J. and Smith, R. (2016) The Effect of Detector Nonlinearity on WFIRSTPSF Profiles for Weak Gravitational Lensing Measurements. Publications of the Astronomical Society of the Pacific, 128 (968). Art. No. 104001. ISSN 0004-6280. doi:10.1088/1538-3873/128/968/104001. https://resolver.caltech.edu/CaltechAUTHORS:20160913-091303272

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Abstract

Weak gravitational lensing (WL) is one of the most powerful techniques to learn about the dark sector of the universe. To extract the WL signal from astronomical observations, galaxy shapes must be measured and corrected for the point-spread function (PSF) of the imaging system with extreme accuracy. Future WL missions—such as NASA's Wide-Field Infrared Survey Telescope (WFIRST)—will use a family of hybrid near-infrared complementary metal-oxide-semiconductor detectors (HAWAII-4RG) that are untested for accurate WL measurements. Like all image sensors, these devices are subject to conversion gain nonlinearities (voltage response to collected photo-charge) that bias the shape and size of bright objects such as reference stars that are used in PSF determination. We study this type of detector nonlinearity (NL) and show how to derive requirements on it from WFIRST PSF size and ellipticity requirements. We simulate the PSF optical profiles expected for WFIRST and measure the fractional error in the PSF size (ΔR/R) and the absolute error in the PSF ellipticity (Δe) as a function of star magnitude and the NL model. For our nominal NL model (a quadratic correction), we find that, uncalibrated, NL can induce an error of ΔR/R = 1 × 10^(−2) and Δe_2 = 1.75 × 10^(−3) in the H158 bandpass for the brightest unsaturated stars in WFIRST. In addition, our simulations show that to limit the bias of ΔR/R and Δe in the H158 band to ~10% of the estimated WFIRST error budget, the quadratic NL model parameter β must be calibrated to ~1% and ~2.4%, respectively. We present a fitting formula that can be used to estimate WFIRST detector NL requirements once a true PSF error budget is established.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/1538-3873/128/968/104001DOIArticle
http://iopscience.iop.org/article/10.1088/1538-3873/128/968/104001/metaPublisherArticle
https://arxiv.org/abs/1605.01001arXivDiscussion Paper
ORCID:
AuthorORCID
Plazas, A. A.0000-0002-2598-0514
Mandelbaum, R.0000-0003-2271-1527
Additional Information:© 2016 The Astronomical Society of the Pacific. Received 2016 April 26; accepted 2016 June 10; published 2016 September 12. We thank Chris Hirata, Jeff Kruk, Dave Content, and the WFIRST detector requirements working group for useful discussions. AAP is supported by the Jet Propulsion Laboratory. CS and JR are being supported in part by the Jet Propulsion Laboratory. The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:cosmology: observations, dark energy, instrumentation: detectors
Issue or Number:968
DOI:10.1088/1538-3873/128/968/104001
Record Number:CaltechAUTHORS:20160913-091303272
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20160913-091303272
Official Citation:A. A. Plazas et al 2016 PASP 128 104001
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:70298
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:13 Sep 2016 23:52
Last Modified:11 Nov 2021 04:27

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