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/红外干涉测量的进展

经过数十年的快节奏技术进步，光学/红外 (O/IR) 干涉测量近年来发生了一场革命： ▪ 甚大望远镜干涉仪 (VLTI) 中的重力仪器配有四个 8 米望远镜，可达到千倍-与早期干涉仪相比，可以观测到更暗的天体，高角分辨率天文学中心阵列 (CHARA) 通常通过六台 1 米望远镜提供长达 330 米的基线和孔径合成。 ▪ 观测物体亮度小于19 星等，图像分辨率达到亚毫角秒，天体测量精度达到微角秒。 ▪ 这导致在银河系中心、系外行星、活动星系核、年轻恒星物体和恒星物理学方面取得突破性成果。在介绍干涉测量学基础知识之后，我们总结了导致现代干涉仪性能提升的进展： ▪ 单模光束组合器现在组合了多达六台望远镜，图像重建软件比射电干涉测量的早期开发更先进。 ▪ 通过结合大型望远镜、自适应光学（AO）、条纹跟踪，特别是双光束干涉测量，GRAVITY 已将灵敏度提高了多个数量级。另一个数量级的改进将来自激光导星 AO。与大间隔条纹跟踪相结合，O/IR 干涉测量将为银河平面内的观测提供完整的天空覆盖，并为河外目标提供大量覆盖。