After decades of fast-paced technical advances, optical/infrared (O/IR) interferometry has seen a revolution in recent years: ▪The GRAVITY instrument at the Very Large Telescope Interferometer (VLTI) with four 8-m telescopes reaches thousand-times-fainter objects than possible with earlier interferometers, and the Center for High Angular Resolution Astronomy array (CHARA) routinely offers up to 330-m baselines and aperture synthesis with six 1-m telescopes.▪The observed objects are fainter than 19 mag, the images have submilliarcsecond resolution, and the astrometry reaches microarcsecond precision.▪This led to breakthrough results on the Galactic Center, exoplanets, active galactic nuclei, young stellar objects, and stellar physics. Following a primer in interferometry, we summarize the advances that led to the performance boost of modern interferometers: ▪Single-mode beam combiners now combine up to six telescopes, and image reconstruction software has advanced over earlier developments for radio interferometry.▪With a combination of large telescopes, adaptive optics (AO), fringe tracking, and especially dual-beam interferometry, GRAVITY has boosted the sensitivity by many orders of magnitude. Another order-of-magnitude improvement will come from laser guide star AO. In combination with large separation fringe tracking, O/IR interferometry will then provide complete sky coverage for observations in the Galactic plane and substantial coverage for extragalactic targets.

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光学/红外干涉测量技术的进展


经过几十年的快速技术进步，光学/红外 （O/IR） 干涉测量法近年来发生了一场革命：▪配备四台 8 米望远镜的甚大望远镜干涉仪 （VLTI） 的重力仪器可以探测到比早期干涉仪暗一千倍的物体，而高角分辨率天文阵列中心 （CHARA） 通常使用六台 1 米望远镜提供高达 330 米的基线和孔径合成。 ▪19等，图像具有亚毫角秒分辨率，天体测量达到微角秒精度，▪这导致了银河系中心、系外行星、活跃的星系核、年轻的恒星天体和恒星物理学的突破性结果。在干涉测量学入门之后，我们总结了导致现代干涉仪性能提升的进步：▪单模光束组合器现在最多可组合六个望远镜，图像重建软件比射电干涉测量的早期发展更先进。 ▪另一个数量级的改进将来自激光导星 AO。结合大间隔条纹跟踪，O/IR 干涉测量将为银河系平面的观测提供完整的天空覆盖，并为银河系外目标提供大量覆盖。