图像脉冲噪声移除是获得高质量图像的关键。本文通过热红外相机成像原理研究，提出了一种基于像素梯度自适应迭代中值滤波器的图像脉冲噪声抑制算法。首先，根据相机的调制传递函数计算获取原始图像的最大像素梯度，继而建立相应的像素梯度集合。然后，计算原始图像与对应像素梯度滤波图像的梯度权重均方根误差集合，并将该集合高斯分布的最大值对应的像素梯度确定为最佳像素梯度。最后，根据图像中脉冲噪声的密度和复杂度，确定所提滤波器的自适应窗口大小和迭代次数。大量实验结果表明，所提滤波器对移除8位、16位的单通道脉冲噪声图像展现出良好的鲁棒性。与其它先进方法相比，该方法可以实时移除真实热红外相机采集图像中低密度的随机值脉冲噪声和SAPN，并实现噪声抑制过程中99.5%以上的原始像素不会遭受破坏。除此之外，针对高密度SAPN抑制，该方法获得了具有竞争力的结果，与运行时间较快的滤波方法相比表现出较好的PSNR和SSIM，与PSNR和SSIM较优秀的去噪方法相比表现出较快的运行时间。对于极限SAPN（99%）破坏的图像，也能够恢复有意义的图像细节。

星载单光子激光雷达以超高灵敏度和超高重频的优势，在海洋探测领域展现了广泛的应用前景。雷达系统中的单光子探测器件具有极高的灵敏度，可以探测光子量级的回波信号，同时也极易受太阳背景光噪声影响。由于背景噪声直接影响激光雷达的工作性能，还会对星上原始的数据量产生影响，在卫星系统设计阶段，对噪声强度的准确估计至关重要。本文综合考虑大气后向散射、水面反射及水体后向散射的贡献，建立了一个星载单光子激光雷达海洋噪声的估计模型。以全球首个对地观测星载激光雷达ATLAS为例，在输入系统参数和环境参数后，模型估计的噪声与ATLAS实测噪声误差在15%以内，证实了该噪声模型的正确性。

低辐射量的高光谱应用对红外焦平面读出电路（ROIC）提出了低噪声的设计要求。相关双采样（CDS）是常用的减少噪声的结构。本文通过调节钳位和采样保持之间的时间间隔来改进CDS，可灵活消除低频噪声。采用180 nm CMOS工艺设计和制造了640×512规模、15 μm 像元中心距的读出电路。输入级集成了低噪声CTIA与本文提出的可调复位时间CDS（AICDS），所设计的时序产生器使CDS复位时间可以延长0~270个时钟周期。通过延长复位时间减少这个时间间隔，噪声电子数可以由39 e^-减少到18.3 e^-。SPECTRE仿真结果和实验测试结果证实了提出的AICDS结构可以提升高光谱应用读出电路的噪声性能，因此可以广泛应用。

文章在超薄势垒AlN/GaN异质结构上采用金属有机化学气相沉积（MOCVD）原位生长SiN_x栅介质，成功制备了高性能的SiN_x/AlN/GaN金属-绝缘体-半导体高电子迁移率晶体管（MIS-HEMTs）。深能级瞬态谱（DLTS）技术测试SiN_x/AlN的界面信息，显示其缺陷能级深度为0.236 eV，俘获截面为3.06×10^-19 cm^-2，提取的界面态密度为10¹⁰~10¹² cm^-2eV^-1，表明MOCVD原位生长的SiN_x可以有效降低界面态。同时器件表现出优越的直流、小信号和噪声性能。栅长为0.15 μm的器件在2 V的栅极电压（V_gs）下具有2.2 A/mm的最大饱和输出电流，峰值跨导为506 mS/mm，最大电流截止频率（f_T）和最大功率截止频率（f_MAX）分别达到了65 GHz和123 GHz，40 GHz下的最小噪声系数（NF_min）为1.07 dB，增益为 9.93 dB。V_ds = 6 V时对器件进行双音测试，器件的三阶交调输出功率（OIP3）为32.6 dBm，OIP3/P_dc达到11.2 dB。得益于高质量的SiN_x/AlN界面，SiN_x/AlN/GaN MIS-HEMT显示出了卓越的低噪声及高线性度，在毫米波领域具有一定的应用潜力。

为了解决硅光电倍增器（Silicon Photomultiplier，SiPM）受环境噪声影响大的问题，设计了一款SiPM耦合塑料闪烁体探测器的信号放大电路。以AD8014放大芯片和CR电路构成负反馈选通放大电路，并且与OPA657跨阻式放大电路进行对比。该款电路以RC滤波输入部分和集成运算放大器构成信号放大电路，具有快上升时间及低输入噪声；以CR高通滤波电路作为比较器信号输入能够有效防止信号反射。实验结果表明：该信号放大电路能够有效滤除环境噪声，并且具备快上升时间。将该电路与塑料闪烁体探测器耦合，在室温下对¹³⁷Cs源进行暗噪声水平和输出信号一致性测量，其输出脉冲上升时间小于12 ns，暗噪声水平低于30 mV，优于跨阻式放大电路。

本文基于0.1-μm砷化镓赝配高电子迁移率晶体管（GaAs pHEMT）工艺，研制了一款覆盖整个W波段的宽带低噪声放大器。提出了一种由双并联电容组成的旁路电路，能够提供宽带射频接地，减小了级间串扰，利于实现宽带匹配。采用双谐振匹配网络实现了宽带的输入匹配和最佳噪声匹配。实测结果显示，最大增益在108 GHz处达到20.4 dB，在66~112.5 GHz范围内，小信号增益为16.9~20.4 dB。在90 GHz处，实测噪声系数为3.9 dB。实测的输入1-dB压缩点在整个W波段内约为-12 dBm。

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.

Taking the LISA system as a reference, the phase noise of the inter-satellite transmission needs to be less than 1 pm. Research has shown that the defocus and the astigmatism are the main aberrations affecting jitter noise at a distance of 2.5×10⁹ m. There is a deviation between the phase stationary point and the origin position. To minimize the phase noise, the telescope angle needs to be adjusted. The gravitational wave detection at the phase stationary point can effectively reduce the phase noise and the requirements of the telescope exit pupil wavefront RMS. The large defocus and small coma can make the phase stationary point close to the optical axis and increase the received laser power.

Overview: In order to achieve the measurement of gravitational wave signals in the millihertz frequency band, the space-based gravitational wave detection projects such as LISA, TianQin, and Taiji projects, which are based on laser interference systems, require the hardware noise floor of the interferometers to be lower than the interstellar weak light shot noise limit. This imposes stringent engineering specifications on the optical-mechanical design and the corresponding interferometer payload. This paper approaches the issue from the perspective of detection mode selection and derives the expressions of readout noise and stray light noise in the interference signal under the single detector mode and the balanced mode. Furthermore, a detailed discussion is provided on the weak-light interference process of the scientific interferometer. The results demonstrate that the balanced mode is capable of suppressing the interference phase noise caused by laser power fluctuations and backscattered stray light across multiple orders of magnitude. However, the suppression capability is constrained by the unequal splitting property of the beam combiner. To address this, a relative gain factor is introduced to compensate for the unequal splitting property of the beam combiner. Further analysis reveals that electronic gain compensation can only eliminate the impact of unequal splitting on one of the two noises rather than both simultaneously. Therefore, a balance must be struck in selecting gain compensation between the suppression of laser power fluctuation noise and stray light noise. Even with this consideration, the balanced mode still offers significant noise suppression capabilities at a magnitude difference, thus potentially reducing the engineering requirements for laser power fluctuations and telescope backscattered stray light.