Abstract
The principal aim of this paper is to present a general view of the special optical systems used for acquiring astronomical image data, commonly referred to as WFC or UWFC (Ultra Wide Field Camera), and of their transfer characteristics. UWFC image data analysis is very difficult in general, not only because the systems have so-called space variant (SV) properties. Images obtained from UWFC systems are usually incorrectly presented due to a wide range of optical aberrations and distortions. The influence of the optical aberrations increases towards the margins of the field of view. These aberrations distort the point spread function of the optical system and rapidly cut the accuracy of the measurements. This paper deals with simulation and modelling of the UWFC optical systems used in astronomy and their transfer characteristics.
Highlights
The properties of UWFC astronomical systems along with specific visual data in astronomical images contribute to complicated evaluation of acquired image data
These models based on Zernike polynomials serve us as suitable tools for understanding how to estimate and fit the wavefront aberration of a real optical system, and give us an idea of intrinsic point spread function (PSF)
The second focuses on using the PSF model in known deconvolution algorithms with which we can restore the original image
Summary
The properties of UWFC astronomical systems along with specific visual data in astronomical images contribute to complicated evaluation of acquired image data These systems contain many different kinds of optical aberrations, which have a negative impact on the image quality and imaging system transfer characteristics. For precise astronomical measurements (astrometry, photometry) over the entire field of view (FOV), it is very important to comprehend how the optical aberrations affect the transfer characteristics of the optical system. Optical aberrations models for linear space invariant and variant (LSI/LSV) systems are outlined in this paper. These models based on Zernike polynomials serve us as suitable tools for understanding how to estimate and fit the wavefront aberration of a real optical system, and give us an idea of intrinsic PSF. The second focuses on using the PSF model in known deconvolution algorithms with which we can restore the original image
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