基于天文光子学的拼接主镜望远镜位相传感与对准  

Phasing sensing and alignment of telescopes with segmented primary mirrors based on astrophotonics

作　　者：安其昌[1,2,3] 刘欣悦 李洪文[1,2,3] 朱嘉康 AN Qichang;LIU Xinyue;LI Hongwen;ZHU Jiakang(Changchun Institute of Optics,Fine Mechanics and Physics,Chinese Academy of Sciences,Changchun 130033,China;University of Chinese Academy of Sciences,Beijing 100039,China;Jilin Provincial Key Laboratory of Intelligent Wavefront Sensing and Control,Changchun 130033,China)

机构地区：[1]中国科学院长春光学精密机械与物理研究所,吉林长春130033 [2]中国科学院大学,北京100039 [3]吉林省智能波前传感与控制重点实验室,吉林长春130033

出　　处：《宁波大学学报（理工版）》2024年第4期1-11,共11页Journal of Ningbo University：Natural Science and Engineering Edition

基　　金：国家自然科学基金(62235018,12373090);中国科学院青年创新促进会项目(2020221).

摘　　要：系统孔径的增加可以有效提高测量观察的灵敏度和分辨率,从而得到高质量的深场测量数据.然而孔径的增加不仅给系统尤其是具有拼接主镜的巡天望远镜系统引入了新的影响因素,从而使其变得更复杂,而且改变了现有组件的操作模式和效果.在这项研究中,我们将子孔径镜检测与曲率传感相结合,该策略可以利用焦平面前后的强度差异测量系统中的对齐倾斜和相位差,从而实现对齐调整和波前稳定性的维护.在子孔径之间使用波前信息来保持连续性,而在系统接口处使用条纹模式来调整对齐倾斜方向.最终实现了原始波前的相关系数大于0.8,子镜边缘区域的PV值减少了超过40%,并且实现了2″的共焦分辨率,以及在5μm范围内的0.08μm的共相位分辨率.此外,每个子镜的边缘干涉测量通道数量从6个减少到2个,吞吐量增加了3倍.为确保未来超大孔径拼接望远镜的最终条纹分辨率,必须有效地减小系统探测器的目标尺寸、体积和质量.而这种基于天文光子学器件的方法能够有效地增加系统的集成度,减少环境对地基系统的影响,降低天基系统的发射成本与风险.The sensitivity and resolution of survey observations can be effectively improved by increasing the aperture size of the system,resulting in high-quality deep-field survey data.However,an increase in aperture size not only increases the complexity of the system by introducing new influencing factors,but also alters the mode of operation and the effects of existing components,especially for survey telescopes with segmented primary mirrors.To address this problem,we combine subaperture mirror testing with curvature sensing.This strategy makes it possible to utilize the intensity difference before and after the focal plane.With this strategy,both the alignment tilt and phase differences in the system can be detected,enabling alignment adjustment and maintenance of wavefront stability.In addition,wavefront information across the subapertures was used to maintain continuity,and at the system interface,a fringe pattern was used to align the tilt adjustment direction.Eventually,the correlation coefficient with the original wavefront was>0.8,the decrease in PV value in the segment edge region was>40%,and a co-focus resolution of 2″was achieved,with a co-phasing resolution of 0.08μm over a 5μm range.The number of edge interferometric measurement channels(in each block)was reduced from 6 to 2,and the throughput was increased by a factor of 3.To ensure the final fringe resolution of future ultra-large-aperture splicing telescopes,the target size,volume,and weight of the system detector should be effectively reduced.In this regard,the use of astrophotonics devices can effectively increase the integration of the system,reducing the impact of the environment on ground-based systems,and reducing the launch costs and risks of space-based systems.

关 键 词：大型望远镜 主动光学 单次曲率传感 天文光子学 

分 类 号：P111[天文地球—天文学]