望远镜光路实时对准方法研究
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摘要
随着望远镜口径日益增大和光学系统复杂度的提升，工作过程中动态对准误源也变得越来越多。为了使望远镜能够长时间保持最佳工作状态，需实时修正其动态对准误差。本文对望远镜光路实时对准方法进行了深入研究，并针对其中的核心问题提出了具体的实现方案。
通过对望远镜光路静态对准方法进行深入研究，并结合实时对准的需求，提出了望远镜光路实时对准的基本方法。其基本步骤为：量化对准误差，设计对准检测光路，检测信息处理，对准误差求解，对准状态评价，对准误差修正。其中，对准状态评价是指根据工作光路的探测结果来量化评价其工作状态；对准误差修正过程需要迅速、平稳，以保证工作光路的稳定性。该基本方法明晰了实时对准的基本要求和工作内容，具有一定的指导意义。
对准误差求解是望远镜光路实时对准技术中的核心部分，主要研究对准误差的精确求解方法或量化判断条件及其边界条件。本文分别对基于图像信息和基于波前信息的对准误差求解方法进行了深入研究。
在利用图像信息求解对准误差方面，本文利用动态光学模型深入研究了离散阵列光源、离焦星点图和次镜回转机构等在对准误差求解中的应用。采用离散阵列光源的对准误差求解算法是利用离散阵列光源产生参考光，然后通过离焦位置探测器上各光斑的变化计算出主次镜的对准误差，仿真表明该方法可以实现37μm和50″的对准精度；利用离焦星点图的对准误差求解算法则是利用次镜对入射光线的遮拦，根据离焦星点图内外环的信息计算出对准误差，利用该对准误差求解算法进行了RC地平式望远镜的主次镜对准实验，实现了最佳2.4″的角分辨率；利用次镜回转的对准误差求解算法则是使用一个线光源产生参考光，然后利用次镜回转时光斑的移动轨迹计算出主次镜的对准误差。
在利用波前信息求解对准误差方面，本文深入研究了采用线性拟合的对准误差求解算法和利用像散分解的对准误差求解算法。线性拟合算法是指先通过分析对准误差和出瞳波前误差的各项泽尼克系数之间的关系，从而建立线性映射关系，在测出出瞳波前误差后，便可根据线性方程组求出对准误差，仿真表明该方法可以实现优于1μm和1″的对准精度；利用像散分解的对准误差求解算法是指通过像散项分解求出两组对准误差单独作用时产生的像散的大小，然后结合慧差项求解对准误差，仿真结果表明该算法可以实现优于5μm和0.5″的对准精度。
工作光与探测器模块的对准问题主要体现在工作光与探测器模块的相对位置的稳定性上。针对量子通信后光路多光路探测、探测视场小等特点，使用共光轴的方法实现各探测光路的工作光与探测器模块的实时对准。室内测试和外场实验结果均达到了预期目标，证明了该方法的有效性。
本文通过对望远镜光路实时对准技术的研究，提出了实时对准的基本方法，并深入研究了对准误差求解方法。对望远镜光路实时对准技术在实际工程中的应用有一定参考价值。
As the telescope aperture is increasing and the optical system complexity is upgrading, dynamic alignment errors of the telescope in work process also increase. In order to make the telescope keeping best working state for a long time, the dynamic alignment error of the telescope must be corrected in the real time. In this paper, the real-time alignment method of the telescope optical path was studied, and a concrete implementing scheme was proposed about the core problem.
Through in-depth study of the static alignment technology of telescope optical path, combining the demand of real-time alignment, the basic method of the real-time alignment of telescope optical path was put forward. The basic steps were as follows:quantifying the alignment error, designing the alignment detection optical path, testing information processing, solving the alignment error, the evaluation of the alignment state, and the correction of the alignment error. Among them, alignment state evaluation referred to quantitatively evaluating working condition according to the detection results of telescope working optical path. The correction process of the alignment error should be quick and smooth to ensure the stability of the working optical path. The basic method clarified the basic requirements and the work content of the real-time alignment, and it had a certain guiding significance.
The algorithm for solving the alignment error was the core part of the real-time alignment of telescope optical path. The accurate solution of the alignment error or quantification of the judgment conditions and boundary conditions were mainly studied. The algorithms for solving the alignment error based on image information and based on wave front information were studied respectively.
In terms of using image information to solve the alignment error, dynamic optical model was used to study the discrete array light source, out-of-focus stellar images and the slewing mechanism of the secondary mirror to solve the alignment error. Alignment error algorithm based on discrete array light source was using the discrete array reference light source to produce reference light, and then calculating the primary and secondary mirror alignment error through the change of light spot in the detector from the focal position. The result indicated that this method could obtain the alignment accuracy of37μm and50". The algorithm for solving the alignment error based on out-of-focus stellar images was using the secondary mirror to block the incident light, and calculating the primary and secondary mirror alignment error of the telescope according to the information inside and outside the ring of the out-of-focus stellar images. This algorithm for solving the alignment error was used for the alignment experiment of the primary and secondary mirrors of the RC horizon telescope, the best angular resolution of2.4" had been obtained. The algorithm for solving the alignment error based on the secondary mirror rotation was using a linear light source to generate a reference light. Then, the movement trajectory of the spot during the secondary mirror rotating was used to calculate the alignment error of the primary and secondary mirrors.
In using the wave front information to solve the alignment error, the algorithms for solving the alignment error based on linear fit and astigmatic decomposition were studied. Linear fit algorithm referred as follows:firstly, a linear mapping relationship was established by analyzing the relationship of the Zernike coefficient between the pupil front wave error and the alignment error. Then the alignment error could be obtained according to the linear equations after the pupil wave front error was obtained. The results indicated that this method could achieve the alignment accuracy better than1μm and1". The algorithm for solving the alignment error based on astigmatic decomposition firstly obtained the size of the astigmatism with only two alignment error by astigmatic decomposition, and then solved the alignment error by the coma items. The results indicated that this method could achieve the alignment accuracy better than5μm and0.5"
The alignment problems of the telescope work light and the detector module were mainly reflected in the stability of the relative position. To address the issue of multi-light path detection of quantum communication, small detection field of view, the real-time alignment of the work light and the detector module were achieved by the common optical axis detection method. The results of indoor test and outdoor experiment both achieved the expected goal and this method proved to be effective.
Through the study on the real-time alignment of telescope optical path, a basic method to align the optical path in real time was proposed, and the solution for alignment error was in-depth studied. The research had some reference value on practical applications of engineering.
通过对望远镜光路静态对准方法进行深入研究，并结合实时对准的需求，提出了望远镜光路实时对准的基本方法。其基本步骤为：量化对准误差，设计对准检测光路，检测信息处理，对准误差求解，对准状态评价，对准误差修正。其中，对准状态评价是指根据工作光路的探测结果来量化评价其工作状态；对准误差修正过程需要迅速、平稳，以保证工作光路的稳定性。该基本方法明晰了实时对准的基本要求和工作内容，具有一定的指导意义。
对准误差求解是望远镜光路实时对准技术中的核心部分，主要研究对准误差的精确求解方法或量化判断条件及其边界条件。本文分别对基于图像信息和基于波前信息的对准误差求解方法进行了深入研究。
在利用图像信息求解对准误差方面，本文利用动态光学模型深入研究了离散阵列光源、离焦星点图和次镜回转机构等在对准误差求解中的应用。采用离散阵列光源的对准误差求解算法是利用离散阵列光源产生参考光，然后通过离焦位置探测器上各光斑的变化计算出主次镜的对准误差，仿真表明该方法可以实现37μm和50″的对准精度；利用离焦星点图的对准误差求解算法则是利用次镜对入射光线的遮拦，根据离焦星点图内外环的信息计算出对准误差，利用该对准误差求解算法进行了RC地平式望远镜的主次镜对准实验，实现了最佳2.4″的角分辨率；利用次镜回转的对准误差求解算法则是使用一个线光源产生参考光，然后利用次镜回转时光斑的移动轨迹计算出主次镜的对准误差。
在利用波前信息求解对准误差方面，本文深入研究了采用线性拟合的对准误差求解算法和利用像散分解的对准误差求解算法。线性拟合算法是指先通过分析对准误差和出瞳波前误差的各项泽尼克系数之间的关系，从而建立线性映射关系，在测出出瞳波前误差后，便可根据线性方程组求出对准误差，仿真表明该方法可以实现优于1μm和1″的对准精度；利用像散分解的对准误差求解算法是指通过像散项分解求出两组对准误差单独作用时产生的像散的大小，然后结合慧差项求解对准误差，仿真结果表明该算法可以实现优于5μm和0.5″的对准精度。
工作光与探测器模块的对准问题主要体现在工作光与探测器模块的相对位置的稳定性上。针对量子通信后光路多光路探测、探测视场小等特点，使用共光轴的方法实现各探测光路的工作光与探测器模块的实时对准。室内测试和外场实验结果均达到了预期目标，证明了该方法的有效性。
本文通过对望远镜光路实时对准技术的研究，提出了实时对准的基本方法，并深入研究了对准误差求解方法。对望远镜光路实时对准技术在实际工程中的应用有一定参考价值。
As the telescope aperture is increasing and the optical system complexity is upgrading, dynamic alignment errors of the telescope in work process also increase. In order to make the telescope keeping best working state for a long time, the dynamic alignment error of the telescope must be corrected in the real time. In this paper, the real-time alignment method of the telescope optical path was studied, and a concrete implementing scheme was proposed about the core problem.
Through in-depth study of the static alignment technology of telescope optical path, combining the demand of real-time alignment, the basic method of the real-time alignment of telescope optical path was put forward. The basic steps were as follows:quantifying the alignment error, designing the alignment detection optical path, testing information processing, solving the alignment error, the evaluation of the alignment state, and the correction of the alignment error. Among them, alignment state evaluation referred to quantitatively evaluating working condition according to the detection results of telescope working optical path. The correction process of the alignment error should be quick and smooth to ensure the stability of the working optical path. The basic method clarified the basic requirements and the work content of the real-time alignment, and it had a certain guiding significance.
The algorithm for solving the alignment error was the core part of the real-time alignment of telescope optical path. The accurate solution of the alignment error or quantification of the judgment conditions and boundary conditions were mainly studied. The algorithms for solving the alignment error based on image information and based on wave front information were studied respectively.
In terms of using image information to solve the alignment error, dynamic optical model was used to study the discrete array light source, out-of-focus stellar images and the slewing mechanism of the secondary mirror to solve the alignment error. Alignment error algorithm based on discrete array light source was using the discrete array reference light source to produce reference light, and then calculating the primary and secondary mirror alignment error through the change of light spot in the detector from the focal position. The result indicated that this method could obtain the alignment accuracy of37μm and50". The algorithm for solving the alignment error based on out-of-focus stellar images was using the secondary mirror to block the incident light, and calculating the primary and secondary mirror alignment error of the telescope according to the information inside and outside the ring of the out-of-focus stellar images. This algorithm for solving the alignment error was used for the alignment experiment of the primary and secondary mirrors of the RC horizon telescope, the best angular resolution of2.4" had been obtained. The algorithm for solving the alignment error based on the secondary mirror rotation was using a linear light source to generate a reference light. Then, the movement trajectory of the spot during the secondary mirror rotating was used to calculate the alignment error of the primary and secondary mirrors.
In using the wave front information to solve the alignment error, the algorithms for solving the alignment error based on linear fit and astigmatic decomposition were studied. Linear fit algorithm referred as follows:firstly, a linear mapping relationship was established by analyzing the relationship of the Zernike coefficient between the pupil front wave error and the alignment error. Then the alignment error could be obtained according to the linear equations after the pupil wave front error was obtained. The results indicated that this method could achieve the alignment accuracy better than1μm and1". The algorithm for solving the alignment error based on astigmatic decomposition firstly obtained the size of the astigmatism with only two alignment error by astigmatic decomposition, and then solved the alignment error by the coma items. The results indicated that this method could achieve the alignment accuracy better than5μm and0.5"
The alignment problems of the telescope work light and the detector module were mainly reflected in the stability of the relative position. To address the issue of multi-light path detection of quantum communication, small detection field of view, the real-time alignment of the work light and the detector module were achieved by the common optical axis detection method. The results of indoor test and outdoor experiment both achieved the expected goal and this method proved to be effective.
Through the study on the real-time alignment of telescope optical path, a basic method to align the optical path in real time was proposed, and the solution for alignment error was in-depth studied. The research had some reference value on practical applications of engineering.
引文
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