Abstract
The properties of UWFC (Ultra Wide-Field Camera) astronomical systems along with specific visual data in astronomical images contribute to a comprehensive evaluation of the acquired image data. These systems contain many different kinds of optical aberrations which have a negatively effect on image quality and imaging system transfer characteristics, and reduce the precision of astronomical measurement. It is very important to figure two main questions out. At first: In which astrometric depend on optical aberrations? And at second: How optical aberrations affect the transfer characteristics of the whole optical system. If we define the PSF (Point Spread Function) [2] of an optical system, we can use some suitable methods for restoring the original image. Optical aberration models for LSI/LSV (Linear Space Invariant/Variant) [2] systems are presented in this paper. These models are based on Seidel and Zernike approximating polynomials [1]. Optical aberration models serve as suitable tool for estimating and fitting the wavefront aberration of a real optical system. Real data from the BOOTES (Burst Observer and Optical Transient Exploring System) experiment is used for our simulations. Problems related to UWFC imaging systems, especially a restoration method in the presence of space variant PSF are described in this paper. A model of the space variant imaging system and partially of the space variant optical system has been implemented in MATLAB. The “brute force” method has been used for restoration of the testing images. The results of different deconvolution algorithms are demonstrated in this paper. This approach could help to improve the precision of astronomic measurements.
Highlights
A wide range of applications use lenses with a wide angle of view (WFC, UWFC) for sky monitoring
The objects in ultra wide-field images are very small. Optical aberrations have their greatest impact toward the margins of the FOV (Field of View), it means that aberration error growing with increasing angular distance from optical axis of the system
When the impulse response of the optical imaging system depends on the coordinates of the object (x, h), we speak about Linear Shift Variant (LSV) systems
Summary
A wide range of applications use lenses with a wide angle of view (WFC, UWFC) for sky monitoring. Real image data from the BOOTES experiment and from double-station video observation of meteors is analyzed. The main goal of double-station video observation of meteors to acquire and analyse video records of meteors. The images from these systems contain survey data with huge numbers of objects of small size. The objects in ultra wide-field images are very small (a few pixels per object dimension) Optical aberrations have their greatest impact toward the margins of the FOV (Field of View), it means that aberration error growing with increasing angular distance from optical axis of the system. Optical aberrations are dependent on three-dimensional coordinates This relation affects the transfer characteristics of optical systems and makes them spatially variant. The influence of spatially variant optical aberrations on the transfer function of optical imaging systems is outlined in this paper
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