The impact of the off-axis for the spatial light to multimode fiber coupling system

The electric field distribution of Gaussian beam and properties of Cassegrain optical antenna are discussed and their images have been simulated. By analysis of Cassegrain optical antenna with collimation and off-axis circumstance, laser power distribution and the curve of coupling efficiency are obtained. The question of spatial light to multimode fiber coupling efficiency with alignment and off-axis are researched. At last, taking into account off-axis situation of Cassegrain and laser beam to multimode fiber, the coupling efficiency of the whole system is discussed. These researches are necessary and useful for increasing spatial light to multimode fiber coupling efficiency.     

卡塞格伦光学天线偏轴及性能分析

设计了具有抛物面结构的卡塞格伦光学天线.通过对偏轴下的卡塞格伦光学天线系统的分析,得到了不同偏转角所对应的接收光斑面积表达式和功率衰减曲线.讨论了偏轴下的接收天线增益与波长及偏转角的关系,仿真出在偏轴与轴对准两种情形下的增益曲线.仿真结果表明,〖JP2〗最大偏轴比轴对准情形增益降低了6.564dB.最后分别针对轴对准与某种偏轴情形下的系统做了光斑测试实验与天线耦合效率测试实验.结果为：偏轴下天线耦合效率降低了26.966%.这些研究为星间光通信中控制系统实现光轴的精确对准提供了理论依据,具有重要的实用价值 关键词： 偏轴 卡塞格伦光学天线 偏转角 增益     

Theoretical analysis and test for off-axis Cassegrain optical antenna

By detailed analysis of Cassegrain optical antenna with inclined optical axis, the receiving antenna power and the curve of power attenuation are obtained for different deflection angles. Three-dimensional images which describe the power distribution of the receive laser beam have been obtained. The coupling efficiency of antenna system is obtained from specific experiment. If the deflection angle is less than 0.1519 rad, the coupling efficiency is beyond 80%. In this case, the optical antenna system can be viewed as in alignment approximately. This research will provide a theoretical base and broad application for achieving precise alignment of optical axis in the field of optical communications and three-dimensional laser radar images.     

主三镜一体化离轴三反光学天线设计

为提高空间激光通信离轴三反光学天线的装调效率,需要对反射镜总的装调自由度进行优化设计。基于共轴三反无焦系统的设计原理,提出一种主三镜一体化的设计方法,并推导了光学系统结构参数之间的关系,利用Zemax光学软件设计了一种结构紧凑、主三镜一体化的离轴三反光学天线。设计结果表明:全视场光学像质优于衍射极限,主镜和三镜空间位置相接近,可共母板加工和面形共基准检测,为主三镜的一体化加工提供了方法。光学天线的装调自由度减少了6个,降低了装调难度,提高了装调效率。     

Quasi-optical assessment of the ALMA band 9 front-end

The ALMA band 9 (600–720 GHz) receiver is a dual channel heterodyne system which is capable of detecting orthogonally polarised signals utilising a wire grid beam splitter. Two Superconductor–Insulator–Superconductor (SIS) mixers mounted behind hybrid mode corrugated horns are coupled to the 12 m Cassegrain antenna via a wavelength independent configuration of two off-axis elliptical mirrors.We outline an approach involving accurate physical optics simulations in conjunction with precise experimental measurements of the complete optical front-end which guarantees the highest performances. This practical verification approach can be generalised to all quasi-optical receivers to validate system performance. In this paper, we verify the optical design and estimate antenna system efficiency. Comparison between measurement and simulation indicates precise information is achievable in estimating system performance allowing potential improvements in ALMA instrument calibration accuracy.     

Analysis of athermalizing performance of thermal infrared optical system with Cassegrain antenna

The thermal infrared imaging system is of greatest importance in modern optics and the image quality closely relies on the accuracy of the optical system. Heat-induced mirror deformation influences the transmission performance of the optical antenna system significantly, which further degrades the accuracy of the whole system. In this work, the simulation on lens deformation circumstances under the thermal environment is carried out using the finite-element analysis software ANSYS. The focus shift property caused by the thermal effect is studied in the cases of reflective and refractive Cassegrain optical antennas, and the athermalizing performance of Cassegrain optical antenna system is also concluded. This work presents a direction to accurate designing of the thermal infrared optical system.     

星间激光通信终端光学天线的隔离度

为满足星间激光通信对高隔离水平光学天线的要求,实现对光学天线隔离度的仿真分析和优化,提出了一种将红外系统冷反射的特征控制量YNI值作为衡量光学元件表面后向反射能量强度,并控制光学天线优化以提高隔离度水平的方法。在Light Tools软件中为某激光通信终端的卡塞格林天线创建了实体模型,通过仿真分析得出了各元件表面的后向反射率。在ZEMAX软件中以增大各元件表面的YNI值为目标优化天线结构。对比优化前后的结果,系统的后向反射率从3.068 8×10~(-4)减小到1.075 5×10~(-5),隔离度从-35.13 d B减小到-49.68 d B。优化后的卡塞格林天线具备较高的隔离度水平,可用于星间激光通信。     

外场紫外与可见光双波段可调焦装置校准设计

设计了一种用来校准紫外与可见光光轴平行性的可调焦光学系统,调焦范围为70 m~。针对目前大多数校准系统无法进行调焦的问题,提出一种既能校准紫外与可见光光轴平行性又能对紫外部分进行调焦的方法。采用离轴卡塞格林系统作为初始结构进行设计,通过在传统的卡塞格林系统中加入调焦组和补偿组来实现调焦以及像差补偿,所设计的系统可以有效地解决紫外与可见光双光轴平行性失调的校准问题,提高紫外与可见光双光轴平行性校准效率,并且在不同视距下光学传递函数值及点列斑均接近衍射极限,能量集中度达到90%,整个视场的像质均匀,像面清晰,有利于后续的图像处理工作。     

计算机辅助装调方法在离轴卡塞格林系统中的应用

针对高成像质量的离轴光学系统的计算机辅助装调问题,许多研究者提出了利用泽尼克系数建立灵敏度矩阵来求解失调量,但这种方法只有在泽尼克系数和失调量存在线性关系的前提下才能准确求解。提出了一种新的能求解较大失调量的计算机辅助装调方法,用此方法对一个口径为250mm的离轴卡塞格林系统进行了装调,得到了中心视场波像差RMS为0.0405λ(λ=632.8nm)。由这种方法计算出的失调量不仅准确,而且能够用于系统装调初期存在大失调量的情况。因此用这种方法能够显著提高离轴光学系统的装调效率。     

非视线散射大气光通信的光学天线

由于大气衰减的影响,非视线散射大气光通信需要使用光学天线以提高对光信号的采集能力,进而增加通信距离。针对非视线大气光通信的需求,利用ZEMAX软件对半球透镜、复合抛物面聚光器（CPC）和卡塞格伦望远镜等光学天线进行了性能分析。分析表明：半球透镜和CPC视场较大,增益值高。利用蒙特卡罗法模拟计算了一定条件下,非视线散射光通信在有无半球透镜或CPC作光学天线时到达探测元件的能量随通信距离的变化。结果表明：CPC聚光能力更强,适合作为非视线散射光通信的光学天线。     

利用调整技术补偿离轴抛物面反射镜面形误差

为了提高光学系统的成像质量,对离轴抛物面反射镜的面形准确度要求越来越高,这大大增加了反射镜的加工难度.本文基于波像差理论,分析了在离轴抛物面反射镜中调整量引入的波像差,提出通过适当调整离轴抛物面反射镜的位置补偿反射镜的面形误差,可以降低离轴反射镜的加工难度、缩短其加工周期、减少加工成本.并借助于ZEMAX软件对一块面形准确度低于λ/40 RMS (λ=632.8 nm)离轴抛物面反射镜进行仿真实验,根据理论计算的调整量调整反射镜的位置,得到了补偿后的离轴抛物面反射镜的面形误差小于λ/60 RMS,仿真结果表明在离轴抛物面反射镜中引入适当的调整量可以有效地补偿反射镜的面形误差.     

Cavity-enhanced absorption spectroscopy for shocktubes: Design and optimization

Cavity-enhanced absorption spectroscopy (CEAS) has generated much interest in shocktube kinetics studies because of its recent success in achieving improved sensitivity and high time resolution with robust optical alignment. While recent progress demonstrated experimental schemes including off-axis scanned-wavelength approach and on-axis ps-pulsed laser approach, that both successfully suppressed the laser-cavity coupling noise, this paper develops a theoretical model to predict the CEAS sensor performance that can be used as a design tool applicable to more generalized cases. The method models the optical field in the cavity based on the decentered Gaussian beam model, from which the cavity transmission spectrum and the laser-cavity coupling noise can be numerically calculated. The simulation results predict sensor performance for different cavity configurations and laser characteristics, including various degrees of laser-cavity mode-matching, laser linewidths, scanning rates, and cavity filling conditions. Simulation with example wavelengths in the ultraviolet, near-infrared, and mid-infrared showed increasing mode-matched beam waist size for increasing wavelengths. An off-axis alignment scheme was found to be capable of suppressing the coupling noise by two orders-of-magnitude at a moderate laser linewidth of 1?GHz. Coupling noise level on the order of 1e-5 for scanned-wavelength off-axis alignment case with a narrowband mid-infrared laser was obtained by model calculation and agreed with experimental results within acceptable uncertainty range. The developed method can serve to guide future design and optimization of CEAS system in shocktube studies.     

卡塞格林系统光学装调技术研究

介绍卡塞格林系统非球面主镜使用三坐标测量仪进行定心装调的方案。系统的主镜口径为300 mm,需要使用结构胶进行胶结固定,选用微应力粘接方法,将胶层粘接应力与热应力变形控制在极小的范围内。利用ZYGO干涉仪获得光学系统的波前信息,将测得的波相差转化为初级像差,根据光学系统失调量与像差的关系对卡塞格林系统进行计算机辅助装调。调试后,系统的RMS值达到0.10,分辨率达到1以内,检测结果表明:该系统的成像质量接近理论衍射分辨率,该方案可以实现快速定心,并且能够满足计算机辅助装调对定心精度的要求。     

New type optical Cassegrain antenna with lenses telescope system

The loss, which caused by the secondary mirror of Cassegrain antenna, is analyzed with Gaussian theory. Under the diameter of secondary mirror being one-fifth of the primary diameter, the loss goes beyond 15%. Optimum structure of optical antenna, which is made up of Cassegrain antenna and lenses system, is devised to solve the waste effectively. The optimal diameter of the mirror is analyzed with Matlab. The relation, the transmitting distance with the ratio of P_{r min}/P_out1 is attained by Gaussian theory, where P_{r min} is the minimum power of receiver signals required by optimum antenna; P_out1 is the power emitted by the optimum antenna.     

ALMA Band 10 tertiary optics

The ALMA Band 10 (787–950 GHz) receiver is a dual-polarization heterodyne system based on NbTiN superconducting technology. The coupling of energy from the secondary mirror of the ALMA Cassegrain antenna to the Superconductor–Insulator–Superconductor (SIS) mixers used for down-conversion is achieved by a frequency-independent optical system composed of two elliptical mirrors to focus and redirect the incoming radiation, a wire-grid to separate orthogonal linear polarizations and two corrugated horns, one for each polarization and SIS mixer. In this paper, we present the ALMA Band 10 tertiary optics design and evaluate its performance by quasi-optical techniques, Physical Optics simulations and measurements. Detailed results of secondary aperture efficiency and beam-squint are provided. The characterization procedure described in this paper can be used for any optical system at around 1 THz.     

Fully automatic system for the coupling alignment of optical fibres

To realize the low-loss connection of two optical fibres intended as a transmission medium for optical signals, very tight tolerances have to be observed on account of the small geometrical dimensions involved. The present work describes a fully automatic system for the alignment of optical fibres in thex-y planes relative to a light source, which has only a single intensity peak, so that maximum optical power is launched into the fibre. The light source can be, for instance, the radiating end of a fibre, a semi-conductor laser or a light-emitting diode. The optical power coupled into the fibre serves as the control signal. Three precision displacement stages driven by stepping motors serve to align the fibres. Various sequential control algorithms for optimal coupling are investigated with reference to theory. Two algorithms are tested with the aid of a computer with reference to the alignment accuracy and speed requirements which have to be met and the one shown by theoretical simulation to be the more favourable is selected for technical realization. The resulting system was used for numerous alignment operations for the coupling of two graded-index fibres. The alignment time is below 1 s and the coupling efficiency compared with manual coupling alignment efficiency (= 100%) is above 99%, corresponding to an additional loss of <0.05 dB.     

离轴八程放大器自动准直技术研究

展示了基于离轴八程激光放大器的闭环自动准直技术研究,该项技术旨在用自动准直系统取代手动光路准直的方式,明显提高了该构型复杂的多程激光放大器的运行效率、准直精度与其输出光束质量。该技术利用主激光照明和像传递系统实现离轴八程激光放大器中滤波器小孔空间位置的精确标定,通过边缘检测处理远场光斑得到其指向中心。基于光斑中心与基准间的差值,对特定反射镜架进行二维控制进行光束指向补正,从而实现离轴八程放大器系统的闭环自动准直。研究结果表明,实验结果契合离轴八程放大器系统对光束准直准确率与效率的要求,验证了该准直技术在离轴八程激光放大光路中应用的可行性。     

天文光学望远镜的调校与检测

本文扼要叙述了天文光学望远镜的通用调校步骤与方法，适用于诸如卡氏（Ｃａｓｓｅｇｒａｉｎ）、葛氏（Ｇｒｅｇｏｒｙ）、奈氏（Ｎａｓｍｙｔｈ）、折轴（Ｃｏｕｄé）、施密特（Ｓｃｈｍｉｄｔ）、牛顿（Ｎｅｗｔｏｎ）望远镜、…等的光学元件及系统的调校。对极轴的高度与方位的调整，也给以简要介绍。本文还概述了对成像质量的检测。文中以通光口径２．１６ｍ天文望远镜为例，给出了光路调整图。     

多光轴校轴仪调校关键技术研究

针对多传感器光电系统存在的光轴平行性调校需求,介绍了一种光轴跨距较大的高精度校轴仪及其工作原理。该装置核心为卡赛格林系统,其主镜采用了一种新型粘接与光学定中心方案用于解决受力变形,实际变形结果验证了该方案的可行性。通过精确调校卡赛格林系统以及检测光路的光轴平行性,文中的校轴仪理论检测精度可达10以内,因此其配合大口径离轴反射式平行光管使用时,能实现对多传感器光电系统光轴平行性的高精度调校。     

弹载卡式红外光学系统消热差设计

为了消除环境温度变化对弹载红外光学系统成像质量的影响,设计了一种在3.7 m~4.8 m波段工作的弹载卡塞格林式红外消热差光学系统。利用ANSYS软件分析了整流罩在大气中的受热变形对光学系统成像质量的影响,采用光学被动式消热差法对光学系统在-40℃~+65℃范围内进行了温度补偿。设计结果表明,系统MTF在20 lp/mm时轴外可达0.41以上,不同视场下的弥散斑直径小于一个像元尺寸且系统结构简单。该设计可保证光学系统的像面稳定性,有效提高火控系统对目标探测与识别能力。