自适应光学系统的计算机模拟
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摘要
随着天文观测和研究水平的提高,天文学家对于观测仪器的要求也在不断提高。地面光学望远镜作为天文研究的主要仪器发挥着越来越重要的作用。但是靠近地面的大气层给地面望远镜的观测带来了很大的困难。为了克服大气对于地面望远镜观测的制约,将望远镜安装在观测条件比较好的台址,并且使用一些新的仪器和方法来减小大气的影响是国内外天文仪器工作者的普遍的做法。在本文中我主要研究了为了改正大气色散而设计的大气色散改正器和为了减少大气湍流对于观测影响的自适应光学系统。其中有关自适应光学系统的模拟主要是由张思炯老师指导的；苏定强老师除了指导我进行了大气色散改正器光学设计之外,也指导我对自适应光学中的波前探测和系统设计进行了研究,并且和我就自适应光学,主动光学和光学系统优化之间的关系进行了深入的探讨,大大加深了我对于这几个方面的认识。
大气色散改正器是一种通过光学仪器产生色散来改正大气色散的一种光学仪器。对于常规的望远镜,这种改正器一般情况下由一套透棱镜系统组成,在工作时,通过旋转来产生不同的色散以补偿不同天顶距下的大气色散。但是,对于我国的LAMOST望远镜,由于其焦面很大,因此,这样的设计会导致原料获取和加工的困难。我们设计了拼接式的大气色散改正器,这种拼接式的改正器产生的色散与其距离焦面的距离大小有关,通过改变它们之间的距离从而补偿不同天顶距下天体产生的色散。我们讨论了这种拼接式结构对于最后的像质的影响。虽然拼接式的改正器会残留0.4角秒的残余像差,但是却校正了3.35角秒的大气色散,满足我们的设计要求。
自适应光学系统是一种通过使用波前探测器实时探测大气湍流对于光波波前相位的作用并且使用波前校正机构进行波前校正的光学系统。这种系统主要包括波前探测机构,波前校正机构和控制器这三个部分。由于系统的每一个部分结构复杂,参数众多,同时系统的最终性能与每个部分的性能关系复杂。因此,这样的系统的设计需要建立模型进行计算机的模拟以减少设计成本和设计时间。本文对于大气湍流,自适应光学系统中的变形镜,Shack-Hartmann波前探测器和控制器等建立了计算机模型,并且.对于在实验室的系统进行小规模实验中的演示模型的建立方法进行了讨论。利用蒙特卡洛模型,我们分别模拟了我国2.16米望远镜的经典自适应光学系统和南极昆仑暗宇宙巡天望远镜(KDUST)的地面层自适应光学系统。经过模拟,我们给出了这些系统的详细的参数,对于系统工作的基本性能和控制要求有了基本的了解。
As the capacity of the astronomical observation increases, the demand of high-quality observation instruments is growing. The ground-based telescope as the workhorse for the observations plays a more and more important role, but the near-ground atmosphere limits the observation ability severely. I studied the atmospheric dispersion corrector and adaptive optics system in this thesis. Most of my research about the adaptive optics system is directed by professor Sijiong Zhang. Professor Dingqiang Su directs me in the study of the wavefront sensing and the system design of the adaptive optics. He also discusses the relations between the adaptive optics, the active optics and the opti-mization of the optical system with me. These discussions deepen my understanding of these subjects.
The atmospheric dispersion corrector is used to correct the dispersion brought by the atmosphere. For the ordinary telescope, the atmospheric dispersion corrector is made of a pair of lens-prisms. The lens-prism will rotate to generate different dispersion to compensate the atmospheric dispersion. But this classical design is not suitable for the LAMOST which has a big focal plane.We designed a segmented atmospheric dispersion corrector. The segmented atmospheric dispersion corrector will correct the dispersion of3.35arcsec with0.4arcsec residual aberration.
The adaptive optics system uses a wavefront sensor to test the wavefront error and a deformable mirror to compensate the error simultaneously. This system includes three parts:the wavefront sensor, the deformable mirror and the control computer. Because each part is complicated and the system performance has complex relation with each part, the simulation is necessary to evaluate the system's performance. We analyzed the operating principle of the whole system and set the numerical model of it including:the atmospheric turbulence, the deformable mirror, the Shack-Hartmann wavefront sensor and the control computer. We simulate the classical adaptive optics system for the2.16m telescope and the ground layer adaptive optics system for the Antarctic KDUST with Monte Carlo model. From the results of these simulations, we have the detailed pa-rameters of these systems and the performance of them.
大气色散改正器是一种通过光学仪器产生色散来改正大气色散的一种光学仪器。对于常规的望远镜,这种改正器一般情况下由一套透棱镜系统组成,在工作时,通过旋转来产生不同的色散以补偿不同天顶距下的大气色散。但是,对于我国的LAMOST望远镜,由于其焦面很大,因此,这样的设计会导致原料获取和加工的困难。我们设计了拼接式的大气色散改正器,这种拼接式的改正器产生的色散与其距离焦面的距离大小有关,通过改变它们之间的距离从而补偿不同天顶距下天体产生的色散。我们讨论了这种拼接式结构对于最后的像质的影响。虽然拼接式的改正器会残留0.4角秒的残余像差,但是却校正了3.35角秒的大气色散,满足我们的设计要求。
自适应光学系统是一种通过使用波前探测器实时探测大气湍流对于光波波前相位的作用并且使用波前校正机构进行波前校正的光学系统。这种系统主要包括波前探测机构,波前校正机构和控制器这三个部分。由于系统的每一个部分结构复杂,参数众多,同时系统的最终性能与每个部分的性能关系复杂。因此,这样的系统的设计需要建立模型进行计算机的模拟以减少设计成本和设计时间。本文对于大气湍流,自适应光学系统中的变形镜,Shack-Hartmann波前探测器和控制器等建立了计算机模型,并且.对于在实验室的系统进行小规模实验中的演示模型的建立方法进行了讨论。利用蒙特卡洛模型,我们分别模拟了我国2.16米望远镜的经典自适应光学系统和南极昆仑暗宇宙巡天望远镜(KDUST)的地面层自适应光学系统。经过模拟,我们给出了这些系统的详细的参数,对于系统工作的基本性能和控制要求有了基本的了解。
As the capacity of the astronomical observation increases, the demand of high-quality observation instruments is growing. The ground-based telescope as the workhorse for the observations plays a more and more important role, but the near-ground atmosphere limits the observation ability severely. I studied the atmospheric dispersion corrector and adaptive optics system in this thesis. Most of my research about the adaptive optics system is directed by professor Sijiong Zhang. Professor Dingqiang Su directs me in the study of the wavefront sensing and the system design of the adaptive optics. He also discusses the relations between the adaptive optics, the active optics and the opti-mization of the optical system with me. These discussions deepen my understanding of these subjects.
The atmospheric dispersion corrector is used to correct the dispersion brought by the atmosphere. For the ordinary telescope, the atmospheric dispersion corrector is made of a pair of lens-prisms. The lens-prism will rotate to generate different dispersion to compensate the atmospheric dispersion. But this classical design is not suitable for the LAMOST which has a big focal plane.We designed a segmented atmospheric dispersion corrector. The segmented atmospheric dispersion corrector will correct the dispersion of3.35arcsec with0.4arcsec residual aberration.
The adaptive optics system uses a wavefront sensor to test the wavefront error and a deformable mirror to compensate the error simultaneously. This system includes three parts:the wavefront sensor, the deformable mirror and the control computer. Because each part is complicated and the system performance has complex relation with each part, the simulation is necessary to evaluate the system's performance. We analyzed the operating principle of the whole system and set the numerical model of it including:the atmospheric turbulence, the deformable mirror, the Shack-Hartmann wavefront sensor and the control computer. We simulate the classical adaptive optics system for the2.16m telescope and the ground layer adaptive optics system for the Antarctic KDUST with Monte Carlo model. From the results of these simulations, we have the detailed pa-rameters of these systems and the performance of them.
引文
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