Space Variant PSF – Deconvolution of Wide-Field Astronomical Images
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...
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| Format: | Article |
| Language: | English |
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CTU Central Library
2008-01-01
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| Series: | Acta Polytechnica |
| Subjects: | |
| Online Access: | https://ojs.cvut.cz/ojs/index.php/ap/article/view/1023 |
| _version_ | 1819043828310474752 |
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| author | M. Řeřábek |
| author_facet | M. Řeřábek |
| author_sort | M. Řeřábek |
| collection | DOAJ |
| description | 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. |
| first_indexed | 2024-12-21T10:02:59Z |
| format | Article |
| id | doaj.art-f24f92a236b84a298e158ce36b4a57db |
| institution | Directory Open Access Journal |
| issn | 1210-2709 1805-2363 |
| language | English |
| last_indexed | 2024-12-21T10:02:59Z |
| publishDate | 2008-01-01 |
| publisher | CTU Central Library |
| record_format | Article |
| series | Acta Polytechnica |
| spelling | doaj.art-f24f92a236b84a298e158ce36b4a57db2022-12-21T19:07:54ZengCTU Central LibraryActa Polytechnica1210-27091805-23632008-01-014831023Space Variant PSF – Deconvolution of Wide-Field Astronomical ImagesM. ŘeřábekThe 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.https://ojs.cvut.cz/ojs/index.php/ap/article/view/1023high order aberrationsPSFUWFCBOOTESZernikeSeidelLSILSVdeconvolutionimage processing |
| spellingShingle | M. Řeřábek Space Variant PSF – Deconvolution of Wide-Field Astronomical Images Acta Polytechnica high order aberrations PSF UWFC BOOTES Zernike Seidel LSI LSV deconvolution image processing |
| title | Space Variant PSF – Deconvolution of Wide-Field Astronomical Images |
| title_full | Space Variant PSF – Deconvolution of Wide-Field Astronomical Images |
| title_fullStr | Space Variant PSF – Deconvolution of Wide-Field Astronomical Images |
| title_full_unstemmed | Space Variant PSF – Deconvolution of Wide-Field Astronomical Images |
| title_short | Space Variant PSF – Deconvolution of Wide-Field Astronomical Images |
| title_sort | space variant psf deconvolution of wide field astronomical images |
| topic | high order aberrations PSF UWFC BOOTES Zernike Seidel LSI LSV deconvolution image processing |
| url | https://ojs.cvut.cz/ojs/index.php/ap/article/view/1023 |
| work_keys_str_mv | AT mrerabek spacevariantpsfdeconvolutionofwidefieldastronomicalimages |