空间引力波探测任务采用的是外差法激光干涉测量技术, 其对系统的噪声和精度要求极为苛刻。望远镜是引力波探测天文台的重要组成部分, 起到激光信号收发的作用, 其光学系统应具备大倍率、高像质、杂光抑制能力强, 波前误差一致性好的特点。针对上述要求, 对大倍率离轴四反无焦光学系统进行了设计和优化。基于初级像差理论阐述了初始结构的求解方法。系统具有中间像面和可用的实出瞳, 便于杂光抑制和与后端科学干涉仪的承接。优化过程中, 建立了波前一致性优化函数, 通过优化设计, 系统入瞳直径为200 mm, 放大倍率为40倍, 科学视场为±8 μrad, 波前误差RMS值优于0.005λ, PV值优于0.023λ(λ=1 064 nm), 波前一致性残差RMS值优于0.000 8λ(λ=1 064 nm), 在捕获视场±200 μrad内的成像质量均接近衍射极限, 并对系统公差进行了分析, 满足引力波探测的应用需求。

The space gravitational wave detection is realized by adopting the technology of heterodyne laser interferometry. The accuracy and noise level of the measurement are extremely rigorous. As an important part of space-based gravitational wave observatory, telescope plays the role of laser signal transceiver, and is characterized by high magnification, high image quality, high similarity of wave-front error over the field of view and extraordinary ability to suppress stray light. Aiming at above requirements, methods of design and analysis of the off-axis four-mirror afocal optical system with high magnification are investigated. Based on the theory of primary aberration, the design method of initial structure is explored. The system has an intermediate image plane and an available exit pupil, which facilitates stray light suppression and integration with the scientific interferometer. The wave-front similarity merit function is established. After optimization, the entrance pupil diameter is 200 mm, the magnification is 40. The Root-Mean-Square (RMS) wave-front error is better than 0.005λ and the Peak-to-Valley (PV) value is less than 0.023λ, moreover, the RMS of wave-front similarity residuals are better than 0.000 8λ(λ=1 064 nm) within the ±8 μrad scientific field of view. Over the field of regard for acquisition, the imaging quality is close to the diffraction limit. The tolerance of the system is analyzed and meets the requirements of space-based gravitational wave detection.