High resolution imaging is achieved using increasingly larger apertures and successively shorter wavelengths. Optical aperture synthesis is an important high-resolution imaging technology used in astronomy. Conventional long baseline amplitude interferometry is susceptible to uncontrollable phase fluctuations, and the technical difficulty increases rapidly as the wavelength decreases. The intensity interferometry inspired by HBT experiment is essentially insensitive to phase fluctuations, but suffers from a narrow spectral bandwidth which results in a lack of effective photons. In this study, we propose optical synthetic aperture imaging based on spatial intensity interferometry. This not only realizes diffraction-limited optical aperture synthesis in a single shot, but also enables imaging with a wide spectral bandwidth, which greatly improves the optical energy efficiency of intensity interferometry. And this method is insensitive to the optical path difference between the sub-apertures. Simulations and experiments present optical aperture synthesis diffraction-limited imaging through spatial intensity interferometry in a 100 nm spectral width of visible light, whose maximum optical path difference between the sub-apertures reaches 69λ. This technique is expected to provide a solution for optical aperture synthesis over kilometer-long baselines at optical wavelengths.

基于宏观反射式傅里叶叠层成像理论，提出一种主动相干光学合成孔径超分辨成像空间目标探测系统。采用主动相干光源配合单个小孔径相机，采集目标低分辨图像序列，通过傅里叶叠层拼接算法重构接近等效合成孔径倍率的超分辨图像。给出了系统的总体方案和详细设计，并通过搭建的宏观反射式近红外主动相干光学合成孔径超分辨成像地面实验装置验证了系统的超分辨成像能力。该系统有望通过小孔径实现等效合成孔径全天时高分辨成像效果，大幅缩减载荷口径需求。弥补传统空间目标探测系统夜间成像能力的不足，提升空间目标夜间探测能力。

针对天文观测和深空探测需求，提出了星载10 m合成孔径相干成像望远镜概念和形式。给出了波长可调谐激光本振相干探测器形式，分析了大口径衍射薄膜镜的双波段实现方式和系统主要参数。提出了基于子镜结构的光学合成孔径相干成像算法，给出了基于相位恢复的阵列形变误差波前估计仿真结果，由于多个子镜所接收复信号的成像处理在计算机软件中完成，相比传统望远镜，可降低对微调机构等硬件的精度要求。该望远镜在短波红外1.45~1.65 μm光谱范围内的中心波长角分辨率为0.15 μrad；在中波红外4.55~4.75 μm光谱范围内的中心波长角分辨率为0.46 μrad，其探测灵敏度在原理上是传统10 m口径望远镜的约2.8倍。