It is an effective method to detect weak gravitational lensing (WL) in the universe by measuring ellipticities of galaxies via astronomical telescopes. Optical properties of telescopes are critical to WL detections. To ensure the used telescopes to be competent, it is necessary to measure point spread function (PSF) ellipticity of telescopes in labs. In this paper, a way based on simulated star target imaging is proposed to measure PSF ellipticity of an unobstructed off-axis space telescope. Related errors are identified and modeled carefully for the first time. Effects of detector noises, micro-vibration of optical platforms, defocusing of simulated star target, wavefront error (WFE) and central obstruction of collimators on PSF ellipticity measurements of the telescope are analyzed. Results show that the measurement error of PSF ellipticity decreases from 0.0105 to 0.0043 by adopting 10 iterations of the iterative weighted centroiding algorithm when the SNR is under 24dB. To ensure PSF ellipticity measurement error is not larger than 0.01, the micro-vibration angle of the optical platform should be less than 0.05". When focal length of the collimator is twice that of the telescope, the measurement error of PSF ellipticity is under 0.01 if the defocusing of simulated star target is controlled to be not larger than 0.1 mm. In addition, WFE and central obstruction of collimators change PSF ellipticity measurement errors to different degrees at different fields of view (FOVs). Due to 20nm RMS WFE of the collimator, the maximum value of PSF ellipticity measurement errors over full FOVs is 0.1 and the average value is 0.0269. If the radius of central obscuration of the collimator is 150 mm, the maximum measurement error of PSF ellipticity over full FOVs is 0.0091.According to the results shown in this paper, significant reference for high accuracy measurements of PSF ellipticity of telescopes can be provided.
INDEX TERMSWeak gravitational lensing, unobstructed off-axis space telescope, PSF ellipticity measurements, error analysis.
I. INTRODUCTION33 Weak gravitational lensing (WL) is a slight deflection of the 34 light from background galaxies through a gravitational field 35 formed by dark matter and ordinary matter [1]. WL is a good 36 probe to study dark matter and dark energy in the universe so 37 that it becomes one of the most powerful tools for 38 cosmologists. WL enables to map dark matter and detect dark 39 energy by statistically quantifying the shear distortions 40 encoded in the observed shapes of background galaxies, 41 namely, galaxy ellipticities [2]-[4]. Thus, precisely obtaining 42 ellipticities of galaxies via astronomical telescopes is critical 43 to WL detections [5]. 44 However, ellipticities of galaxies are typically distorted 45 only approximately 1% in size by WL [6], [7]. It is a big 46 challenge to measure such tiny WL signals. Currently, the 47 distortions and unbiased estimates of galaxy shapes are 48 accessed by statistically averaging a very large number of 49 samples [8], [9]. Several la...