Overview: The space gravitational wave detection telescope is one of the core payloads of the gravitational wave detection satellite, simultaneously expanding and contracting the transmitted beam. Optical path stability is one of the core indices for the telescope, closely related to its structural stability. To meet the ultra-high path stability and structural stability requirements posed by the gravitational wave detection mission, it is essential to study the structural deformation measurement of the telescope. Currently, there are still several shortcomings in the research of multi-degree-of-freedom deformation measurement methods for gravitational wave detection telescopes, such as inaccurate selection of measurement points, inability to decouple multi-degree-of-freedom coupling, and unclear identification of error sources in multi-degree-of-freedom measurement. This paper deeply investigates the high-precision measurement of structural deformation of space-borne telescopes designed for space gravitational wave detection. It preliminarily establishes a framework and method system for measuring the structural deformation of space-borne telescopes, theoretically describing the measurement principle of the method. The feasibility of this method applied to space gravitational wave detection is verified through simulation analysis and error decomposition. The paper focuses on resolving the issue of decoupling multiple degrees of freedom, establishing a mathematical model using analytical methods, and conducting preliminary validation using Zemax. Finally, noise analysis of the measurement system is carried out, with experimental testing of the main noise components in the measurement system, validating the correctness of the theoretical noise model proposed in this paper. The experimental results show that near 1 Hz, the displacement noise background of the single-link interferometer is 100 pm/Hz^1/2. At 1 mHz in the low-frequency range, the displacement noise background reaches 10 nm/Hz^1/2. The noise level of the measurement system below 1 mHz is mainly limited by environmental temperature noise, while above 10 mHz, it is primarily constrained by laser frequency noise, phase acquisition background noise, and vibration noise. During the development phase of the space gravitational wave detection telescope, the research on this measurement method is expected to fulfill the telescope's multi-degree-of-freedom deformation measurement needs. It also provides data feedback for telescope design and offers guidance for the study of the telescope's optical path stability.

海水折射率测量在海洋学中发挥了重要作用，但对于海洋气候和海水流场监测领域，现有的折射率传感器无法满足应用场景的高精度与高采样率要求。有鉴于此，文中基于光外差干涉原理设计了海水折射率传感器，分析了该原理下的散粒噪声、相位解调噪声对传感器折射率测量的影响，研制了高精度海水折射率传感器样机，其采样频率为24 kHz，折射率变化量测量值的标准偏差为 $1.584\;8\times $$ {10}^{-8}\;\mathrm{R}\mathrm{I}\mathrm{U}$，该技术促进了海水折射率测量在海洋气候及海洋洋流等领域的应用。

采用灵敏度函数分析法对冷原子重力仪的噪声进行了分析，并基于各噪声对应的传递函数建立噪声传递模型，定量分析评估了振动噪声、拉曼光相位噪声和磁场噪声对重力测量灵敏度的影响。基于科里奥利力和稳定平台倾斜角等系统效应的修正公式，建立系统效应分析模型，定量分析评估了航向角偏差、速度偏差和纬度偏差对科里奥利力修正量的影响，以及倾斜角偏差对稳定平台倾角修正量的影响。仿真和部分实测数据表明，一方面，各噪声被限制到特定水平时，其对原子干涉灵敏度的影响仍可达μGal级；另一方面，1°的航向角偏差或0.1 m/s的速度偏差对科里奥利力修正量的影响可达1 mGal以上，1′的倾斜角偏差对稳定平台修正量的影响也可达0.42 mGal，说明噪声和系统效应的影响都是不容忽视的。因此，在动态条件下，冷原子重力仪必须进行噪声抑制和系统效应修正，才能获得预期的高灵敏度、高精度重力测量结果。

在调频连续波激光雷达中，用于中频信号采集的模拟-数字采集模块是其关键组件，信噪比、信纳比、无杂散动态范围等参数是衡量该数据采集信号链交流特性的重要指标，直接决定着调频连续波激光雷达的探测范围和测距精度等性能。设计了用于调频连续波激光雷达的中频信号采集模块，获得49.13 dB的信噪比和48.90 dB的信纳比；然后研究了其噪声特性，获得系统的主要噪声来源为采样时钟的相位噪声，并且通过引入数字滤波器将信噪比和信纳比分别提升11.38 dB和11.32 dB，理论上激光雷达的探测范围提高3.7倍。可通过采用专业时钟芯片降低噪声，经计算可将信噪比提高8.65 dB；最后，搭建了光学相控阵调频连续波激光雷达系统，验证了数据采样模块的有效性，完成了40 m距离的探测，最大测量误差为7.7 cm，最大探测范围为133.67 m。

借助于称重测量原理的噪声抑制效果，提出了一种基于S矩阵狭缝阵列的短波红外光谱成像方法，通过构建S矩阵狭缝阵列替换光谱成像系统的单狭缝，实现空、谱信息的混叠测量。对该系统的探测器噪声和光子噪声进行了分析，计算了系统噪声抑制效果。仿真结果表明，该方法在弱光条件下可有效地降低噪声水平，提高成像质量。搭建了原理样机进行成像实验，对一均匀面目标成像，通过对比单狭缝成像数据，使用S矩阵狭缝阵列的光谱成像方法在23%和10%探测器势阱光强下信噪比分别提升了9%和21%。