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摘要:
大口径巡天望远镜需要基于波前传感系统的反馈，进行主动光学闭环校正，以更好地发挥其极限探测能力。本文面向大口径巡天望远镜波前传感过程中，离焦星点像重合所导致的导星数量下降的问题，首先针对分区域曲率传感的基本理论表达进行了推导，之后，通过建立联合仿真模型，利用光学设计软件与数值计算软件之间的通讯交互，对分区域曲率传感的过程进行了仿真分析。最后，通过搭建桌面实验，分别就单目标与多目标的曲率传感进行了交叉比对，验证了算法的正确性。针对标准波前，本文所提出的方法与单导星曲率传感相比，误差为0.02个工作波长（RMS），误差在10%以内，可在传统主动光学技术的基础上，通过扩展可用导星，提升探测信噪比与采样速度，有效提升主动光学系统校正能力。
Abstract:The large aperture sky survey telescope needs closed-loop error correction based on the feedback of its wavefront sensing system, so as to give it a better conform to its limit detection ability. In this paper, firstly, the basic theoretical expression of sub region curvature sensing is derived. Then, a joint simulation model is established. The process of sub region curvature sensing is simulated and analyzed by using a combination of optical design software and numerical calculation software. Finally, by setting up a desktop experiment, the cross-comparison of single- and multi-target curvature sensors is carried out to verify the correctness of the algorithm. Compared to the traditional active optical technology, the method proposed in this paper can improve the detection signal-to-noise ratio and sampling speed by expanding the available guide stars. For the standard wavefront, compared with the single guide star curvature sensor, the error is 0.02 operating wavelengths (RMS), and the error is less than 10%, which can effectively improve the correction ability of the active optical system.
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Key words:
- large aperture survey telescope /
- active optics /
- curvature sensing /
- natural guide star
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图 2 导星重叠与离焦量之间的关系
Figure 2. Relationship between guide star overlap and defocus amount
图 5 小像差下的离焦星点像（a）重建波前与（b）原始波前
Figure 5. (a) Reconstructed wavefront and (b) original wavefront of stitching defocused star point image under small aberration
图 8 分割拼接的离焦星点像（大像差）。（a）焦前能量分布；（b）焦后能量分布；（c）光强分布差分
Figure 8. Segmented and spliced defocused star point image (large aberration). (a) Pre-focal energy distribution; (b) post-focal energy distribution; (c) light intensity distribution difference
图 4 分割拼接的离焦星点像（小像差）。（a）焦前能量分布；（b）焦后能量分布；（c）光强分布差分
Figure 4. Segmented and spliced defocused star point image (small aberration). (a) Pre-focal energy distribution; (b) post-focal energy distribution; (c) light intensity distribution difference
图 6 小像差下的离焦星点像拼接复原效果。（a）重建波前与原始波前相关函数；（b）泽尼克系数对比
Figure 6. Restoration effect of defocused star image stitching under small aberration. (a) Comparison of correlation function between reconstructed wavefront and original wavefront; (b) Zernike coefficient
图 7 大像差下的离焦星点像拼接结果。（a）重建波前与（b）原始波前
Figure 7. (a) Reconstructed wavefront and （b）original wavefront of stitching defocused star image under large aberration
图 10 5 cm相干长度下湍流对像差提取的影响。(a)焦前能量分布；（b）焦后能量分布；（c）光强分布差分；（d）短曝光重建波前（10 ms）；（e）长曝光重建波前（100 ms）；（f）原始波前
Figure 10. Influence of turbulence on aberration extraction at 5 cm coherence length. (a) Pre-focal energy distribution; (b) post-focal energy distribution; (c) light intensity distribution difference; (d) short exposure reconstruction wavefront (10 ms); (e) long exposure reconstruction wavefront (100 ms); (f) original wavefront
图 11 （a）模拟双星检测强度分布；（b）实验现场；（c）两种形式的波前传感结果对比
Figure 11. (a) Simulated binary detection intensity distribution; (b) experimental site; (c) comparison of two wavefront sensing results
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