Astronomical Image Co-adding Method based on Wide-field Image Deconvolution |
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| Institution: | 1. College of Physics and Optoelectronics, Taiyuan University of Technology, Taiyuan 030024;2. Department of Physics, Durham University, Durham DH13LE;3. Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008;1. Key Laboratory foe Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033;2. University of Chinese Academy of Sciences, Beijing 100049;3. School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026;1. Pulkovo Observatory, 196140, St.Peterburg, Pulkovskoje shosse, 65, Russia;2. Astronomical Observatory, DSFTA - University of Siena, K54, Italy;3. Balzaretto Observatory, Rome, A81, Italy;4. Private Observatory, 1155, Hartford St, Elgin, OR 97827, USA;5. Ngileah Observatory, 144 Kilkern Road, RD 1. Bulls 4894, New Zealand;6. Special Astrophysical Observatory (SAO RAS), 369167 Nizhnij, Arkhyz, Russia;7. Baronnies Provençales Observatory, Hautes Alpes - Parc Naturel Régional des Baronnies Provençales, 05150 Moydans, France;1. Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008;2. Key Laboratory of Planetary Science, Chinese Academy of Sciences, Nanjing 210008;3. China University of Geoscience (Beijing), Beijing 100083;4. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012;5. Space Science Institute, Marco University of Science and Technology, Marco 999078;1. Depart. of Mathematics and Computer Science, Royal Military College of Canada, Kingston, ON, K7K 7B4, Canada;2. Dpto. Electromagnetismo y Electrónica, Universidad de Murcia, Murcia, E 30100, Spain;1. Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049;2. Department of Astronomy, Beijing Normal University, Beijing 100875 |
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| Abstract: | Due to the atmospheric turbulence, the static aberration, tracking and pointing errors of telescopes, the point spread functions (PSFs) in different fields of view are different. Meanwhile, there are different PSFs in the images obtained by different telescopes. The quality of co-adding image is limited by the image with the poorest quality, and finally the resolution and sensitivity of the quad-channel telescope will also be affected. Dividing the image into some regions with the same type of PSF, and deconvolving these regions can improve the quality of the co-adding image. According to this theory, an image restoration algorithm based on the PSF clustering is proposed. Firstly, this paper makes the PSF clustering analysis by using Self-Organizing Maps, and makes the image segmentation based on the result of the PSF clustering analysis, then using the clustered PSFs to make deconvolutions on the sub-images. Then, the restored sub-images after deconvolution are joined together. Finally, by through the image registration and co-adding, the image with a high signal to noise ratio can be obtained. The result shows that the signal to noise ratio of the astronomical images are improved with our method, and the detection capability on faint stars is also improved. |
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| Keywords: | Techniques: Image processing Telescopes Atmospheric effects |
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