Photonic Lanterns (PLs) are tapered waveguides that gradually transition from a multi-mode fiber geometry to a bundle of single-mode fibers (SMFs). They can efficiently couple multi-mode telescope light into a multi-mode fiber entrance at the focal plane and convert it into multiple single-mode beams. Thus, each SMF samples its unique mode (lantern principal mode) of the telescope light in the pupil, analogous to subapertures in aperture masking interferometry (AMI). Coherent imaging with PLs can be enabled by interfering SMF outputs and applying phase modulation, which can be achieved using a photonic chip beam combiner at the backend (e.g., the ABCD beam combiner). In this study, we investigate the potential of coherent imaging by interfering SMF outputs of a PL with a single telescope. We demonstrate that the visibilities that can be measured from a PL are mutual intensities incident on the pupil weighted by the cross-correlation of a pair of lantern modes. From numerically simulated lantern principal modes of a 6-port PL, we find that interferometric observables using a PL behave similarly to separated-aperture visibilities for simple models on small angular scales ($<λ/D$) but with greater sensitivity to symmetries and capability to break phase angle degeneracies. Furthermore, we present simulated observations with wavefront errors and compare them to AMI. Despite the redundancy caused by extended lantern principal modes, spatial filtering offers stability to wavefront errors. Our simulated observations suggest that PLs may offer significant benefits in the photon noise-limited regime and in resolving small angular scales at low contrast regime.
Seidr update: photonic 'black magic' for high-contrast interferometry using kernel-nulling and photonic lanterns
University of Sydney（悉尼大学）；Observatoire de la Cote d’Azur, Université Côte d’Azur（蔚蓝海岸天文台，蔚蓝海岸大学）；Australian National University（澳大利亚国立大学）；University of Exeter（埃克塞特大学）；Leiden University（莱顿大学）
Empirical verification of principal mode orthogonality and relative phase calibration in photonic lanterns
Sydney Institute for Astronomy, School of Physics, The University of Sydney（悉尼大学物理学院天体物理学研究所）；Sydney Astrophotonics Instrumentation Laboratory, School of Physics, The University of Sydney（悉尼大学物理学院天文光子学仪器实验室）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）
Overcoming the low signal-to-noise problem for hybrid mode-selective photonic lantern-based wavefront correction using machine learning
University of Sydney（悉尼大学）；Sydney Institute for Astronomy (SIfA)（悉尼天文研究所）；School of Physics, University of Sydney（悉尼大学物理学院）；Sydney Astrophotonics Instrumentation Laboratories（悉尼天体光子学仪器实验室）；Observatoire de la Cote d’Azur（蔚蓝海岸天文台）；Université Côte d’Azur（蔚蓝海岸大学）；Leiden University（莱顿大学）
Demonstration of a multimode-to-multimode photonic lantern for astronomy
Instituto de Astrofísica de Andalucía, CSIC（安达卢西亚天体物理研究所）；Sydney Astrophotonic Instrumentation Laboratories, School of Physics, The University of Sydney（悉尼大学物理学院悉尼天体光子学仪器实验室）；Centro Astronómico Hispano en Andalucía, Observatorio de Calar Alto（安达卢西亚西班牙天文中心卡拉阿尔托天文台）；Astrophotonics (innoFSPEC), Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦阿基米德天体物理研究所天体光子学部门）；Institut für Physik und Astronomie, Universität Potsdam（波茨坦大学物理与天文学研究所）
Demonstrating the integration of a photonic lantern with an all-fiber-based nulling interferometer
Univ. of California, Santa Cruz（加州大学圣克鲁兹分校）；Univ. of California, Los Angeles（加州大学洛杉矶分校）；NASA Ames Research Center（NASA艾姆斯研究中心）；NASA Glenn Research Center（NASA格伦研究中心）；Univ. of Central Florida（中佛罗里达大学）
Combining spectroscopy and wavefront control at deep contrast with photonic lanterns
University of Texas-San Antonio（德克萨斯大学圣安东尼奥分校）；Subaru Telescope, National Astronomical Observatory of Japan（昴星团望远镜，日本国立天文台）；Astrobiology Center（天体生物学中心）；Sydney Institute for Astronomy, School of Physics, University of Sydney（悉尼大学物理学院悉尼天体物理学研究所）；The University of Sydney, Sydney Astrophotonic Instrumentation Laboratory（悉尼大学悉尼天体光子仪器实验室）；California Institute of Technology（加州理工学院）；Space Science and Engineering Initiative, College of Engineering, Institute for Astronomy, University of Hawai’i（夏威夷大学天体物理学院工程学院太空科学与工程倡议）；University of California Los Angeles（加州大学洛杉矶分校）
Information limits of photonic lantern wavefront sensing: a Fisher- and quantum-Fisher-information framework and its relation to Fourier-filtering sensitivity limits
Institut für Physik und Astronomie, Universität Potsdam（波茨坦大学物理与天文学研究所）
Instrumental artifacts in photonic lantern spectroastrometry and their mitigation with PLred
University of California, Los Angeles（加州大学洛杉矶分校）；University of Hawai’i at Hilo（夏威夷大学希洛分校）；University of Hawai’i（夏威夷大学）；University of Arizona（亚利桑那大学）；Subaru Telescope, National Astronomical Observatory of Japan（日本国立天文台昴星团望远镜）；Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS（巴黎天文台、巴黎文理研究大学、索邦大学、巴黎西岱大学、CY塞吉-蓬图瓦兹大学、法国国家科学研究中心）；California Institute of Technology（加州理工学院）
Analysis of Angular-Differential Post-Processing Algorithms for Exoplanet Direct Detection with a Photonic Lantern Nuller
California Institute of Technology（加州理工学院）；University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Leiden Observatory（莱顿天文台）；University of California, Los Angeles（加州大学洛杉矶分校）
Experimentally-determined performance limits for joint imaging and wavefront sensing with a photonic lantern
University of California, Santa Cruz（加州大学圣克鲁兹分校）；Lawrence Livermore National Laboratory（劳伦斯利弗莫尔国家实验室）；Laboratoire d’Astrophysique de Marseille（马赛天体物理学实验室）；University of California, Los Angeles（加州大学洛杉矶分校）；The College of Optics & Photonics, University of Central Florida（中佛罗里达大学光学与光子学院）
FIRST-PL: Commissioning the first visible photonic lantern spectrograph for sub-diffraction-limit astronomy on Subaru/SCExAO
University of Hawai‘i（夏威夷大学）；University of Hawaii at Manoa（夏威夷大学马诺阿分校）；Subaru Telescope, National Astronomical Observatory of Japan（昴星团望远镜，日本国立天文台）；Observatoire de Paris, Université PSL（巴黎天文台，巴黎文理研究大学）；Steward Observatory, University of Arizona（斯图尔德天文台，亚利桑那大学）；Astrobiology Center（天体生物学中心）；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学，法国国家科学研究中心，IPAG）；University of California, Los Angeles（加州大学洛杉矶分校）；Sydney Institute for Astronomy, School of Physics, The University of Sydney（悉尼天体物理研究所，悉尼大学物理学院）；Optical Sharpeners（光学锐化器）；California Institute of Technology（加州理工学院）；Sydney Astrophotonic Instrumentation Laboratory, School of Physics, The University of Sydney（悉尼天体光子仪器实验室，悉尼大学物理学院）；Astralis, School of Physics, University of Sydney（Astralis，悉尼大学物理学院）；University of Texas, San Antonio（得克萨斯大学圣安东尼奥分校）
The Photonic Lantern Nuller: from concept to laboratory and on-sky demonstrations
Caltech（加州理工学院）；Sterrewacht Leiden（莱顿天文台）；University of California, Los Angeles（加利福尼亚大学洛杉矶分校）；NASA Ames Research Center（NASA艾姆斯研究中心）；Subaru Telescope, National Astronomical Observatory of Japan（日本国立天文台昴星望远镜）；University of Hawai’i（夏威夷大学）；The University of Sydney（悉尼大学）；University of Central Florida（中佛罗里达大学）；University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；University of California, Santa Cruz（加利福尼亚大学圣克鲁兹分校）
Towards High-Throughput Visible Photonic Lanterns for the EMARCOT Project
Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦阿基米德天体物理研究所）；Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas（安达卢西亚天体物理研究所，西班牙高等科学研究委员会）；Centro Astronómico Hispano en Andalucía (CAHA), Observatorio de Calar Alto（安达卢西亚西班牙天文中心，卡萨拉托天文台）；Institute of Photonics and Optical Science, School of Physics, University of Sydney（悉尼大学物理学院光子学与光学科学研究所）
Demonstration of a photonic lantern focal-plane wavefront sensor: measurement of atmospheric wavefront error modes and low wind effect in the non-linear regime
Spectroscopy using a visible photonic lantern at the Subaru telescope: Laboratory characterization and first on-sky demonstration on Ikiiki (α Leo) and `Aua (α Ori)
Astrophotonics: molding the flow of light in astronomical instruments
自二十年前出现以来，天文光子学在世界各地许多机构的科学仪器中得到了广泛的应用。随着望远镜推动AO辅助的衍射限制性能，天文光子学的情况变得更加引人注目，这是下一代超大望远镜（ELT）的核心观测模式。甚至AO系统也开始纳入先进的光子原理，因为社区推动更高的性能和更复杂的导星配置。像甚大望远镜上的引力这样的光子仪器在2000 nm处达到了毫角秒的分辨率，这是传统光学很难实现的。虽然空间光子学在此不作评述，但我们预见，遥感平台将在今后几年成为天体光子学组成部分的主要受益者。随着新技术的发展（例如光子灯笼，大面积多芯光纤）已经在其他领域得到广泛应用，该领域已经有所回报; Google Scholar列出了400多篇参考该技术的研究论文。这篇简短的评论涵盖了自2009年《焦点》杂志以来代表性的主要进展。
