基于主动相位稳定的长基线光学干涉成像
Long baseline optical interferometric imaging with active phase stabilization
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中文总结 AI 辅助
研究旨在通过长基线光学干涉测量提高天文成像分辨率，采用量子通信相位稳定技术及量子最优测量技术，稳定了170km伪基线光学干涉仪，在1.5%误差内分辨出更小源范围，让全尺寸天空长基线干涉仪更具潜力。
中文摘要 AI 辅助
天文观测有助于增进我们对宇宙的理解。随着观测更小、更远的天体特征，会遇到观测系统的衍射极限。通过干涉测量可合成更大的主孔径，长基线光学干涉测量能显著提高天文成像分辨率。构建自由空间基线的光学干涉仪随基线增加难度增大，基于光纤连接望远镜的干涉仪因光纤介质不均匀更易受相位噪声影响，导致天文测量干涉信号严重退化。我们采用量子通信中的相位稳定技术稳定了具有170km伪基线的光学干涉仪，用量子最优测量技术在1.5%误差内分辨出比系统衍射极限小四分之一的源范围。这些结果使全尺寸天空长基线干涉仪的潜力更接近现实，350km基线的1550nm光学干涉仪将能分辨宇宙中的亚微角秒特征。
英文摘要
Astronomical observations allow us to better our understanding of the universe. As we observe smaller and more distance features, we run into the diffraction limit of our observation system. This limit is a function of the wavelength observed and the size of the primary aperture used. We can synthesize a larger primary aperture by implementing interferometry. Long baseline optical interferometry would lead to significant improvements in astronomical imaging resolution. Building optical interferometers with free space baselines becomes significantly more difficult as the baseline increases. A promising alternative is to use optical fiber to connect telescopes. Fiber-based interferometers are much more susceptible to phase noise than their free-space counterparts due to inhomogeneities in the fiber medium. This leads to significant degradation of interferometric signals used for astronomical measurements. We implement phase stabilization techniques used in quantum communications to stabilize an optical interferometer with a 170km pseudo-baseline. We use a quantum optimal measurement technique with this interferometer to resolve the extent of a source four times smaller than the diffraction limit of the system within 1.5% error. These results bring the potential for a full-scale on-sky long baseline interferometer significantly closer. A 350km baseline optical interferometer at 1550nm would allow us to resolve sub microarcsecond features in the universe.
