WFST Astrometric Calibration -- I. Modeling Global Geometric Distortion with Zernike Polynomials
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arXiv
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2026
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| _version_ | 1866910033679220736 |
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| author | Yang, Chao Fang, Min Zheng, Xian Zhong Li, Guoliang Liu, Binyang Lou, Zheng Wan, Zhen Zhang, Miaomiao Sun, Tian-Rui Fan, Lulu Zhang, Xiaoling Kong, Xu Xue, Yongquan Zhao, Wen Li, Bin Luo, Wentao Li, Feng Liu, Wei Wang, Jian Zhang, Hongfei Liu, Hao Zhu, Qinfeng Wang, Hairen Yao, Dazhi |
| author_facet | Yang, Chao Fang, Min Zheng, Xian Zhong Li, Guoliang Liu, Binyang Lou, Zheng Wan, Zhen Zhang, Miaomiao Sun, Tian-Rui Fan, Lulu Zhang, Xiaoling Kong, Xu Xue, Yongquan Zhao, Wen Li, Bin Luo, Wentao Li, Feng Liu, Wei Wang, Jian Zhang, Hongfei Liu, Hao Zhu, Qinfeng Wang, Hairen Yao, Dazhi |
| contents | Accurate modeling of geometric distortion is essential for precise astrometric calibration in wide-field imaging surveys. We present a self-calibration method based on Zernike polynomials, applied to imaging data from the Wide Field Survey Telescope (WFST). Our approach constructs a global geometric distortion (GD) model from the position offsets of stars in the WFST r-band relative to Gaia DR3, achieving a median systematic uncertainty of below 10 mas for individual exposures. The correspondence between Zernike polynomials and optical aberrations reveals that the global GD of WFST is dominated by coma, inherent to the optical design, while rapid variations are likely attributed to the atmospheric dispersion corrector. Applying this method to 82 exposures from a single night (20250218), we find that the relative positions of the WFST CCDs remain stable, with standard deviations of less than 0.1 pixel in translation and 1.8 arcsec in rotation. The corrected WFST astrometric system is thereby tied to the Gaia DR3 coordinate frame, with further refinements to be presented in future work. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2602_22569 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | WFST Astrometric Calibration -- I. Modeling Global Geometric Distortion with Zernike Polynomials Yang, Chao Fang, Min Zheng, Xian Zhong Li, Guoliang Liu, Binyang Lou, Zheng Wan, Zhen Zhang, Miaomiao Sun, Tian-Rui Fan, Lulu Zhang, Xiaoling Kong, Xu Xue, Yongquan Zhao, Wen Li, Bin Luo, Wentao Li, Feng Liu, Wei Wang, Jian Zhang, Hongfei Liu, Hao Zhu, Qinfeng Wang, Hairen Yao, Dazhi Instrumentation and Methods for Astrophysics Accurate modeling of geometric distortion is essential for precise astrometric calibration in wide-field imaging surveys. We present a self-calibration method based on Zernike polynomials, applied to imaging data from the Wide Field Survey Telescope (WFST). Our approach constructs a global geometric distortion (GD) model from the position offsets of stars in the WFST r-band relative to Gaia DR3, achieving a median systematic uncertainty of below 10 mas for individual exposures. The correspondence between Zernike polynomials and optical aberrations reveals that the global GD of WFST is dominated by coma, inherent to the optical design, while rapid variations are likely attributed to the atmospheric dispersion corrector. Applying this method to 82 exposures from a single night (20250218), we find that the relative positions of the WFST CCDs remain stable, with standard deviations of less than 0.1 pixel in translation and 1.8 arcsec in rotation. The corrected WFST astrometric system is thereby tied to the Gaia DR3 coordinate frame, with further refinements to be presented in future work. |
| title | WFST Astrometric Calibration -- I. Modeling Global Geometric Distortion with Zernike Polynomials |
| topic | Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2602.22569 |