Earth-sized planets around nearby stars are being detected for the first time by ground-based radial velocity and space-based transit surveys. This milestone is opening the path towards the definition of missions able to directly detect the light from these planets, with the identification of bio-signatures as one of the main objectives. In that respect, both ESA and NASA have identified nulling interferometry as one of the most promising techniques. The ability to study distant planets will however depend on exozodiacal dust clouds surrounding the target stars. In this paper, we assess the impact of exozodiacal dust clouds on the performance of an infrared nulling interferometer in the Emma X-array configuration. For the nominal mission architecture with 2-m aperture telescopes, we found that point-symmetric exozodiacal dust discs about 100 times denser than the solar zodiacal cloud can be tolerated in order to survey at least 150 targets during the mission lifetime. Considering modeled resonant structures created by an Earth-like planet orbiting at 1 AU around a Sun-like star, we show that the tolerable dust density for planet detection goes down to about 15 times the solar zodiacal density for face-on systems and decreases with the disc inclination. The upper limits on the tolerable exozodiacal dust density derived in this study must be considered as rather pessimistic, but still give a realistic estimation of the typical sensitivity that we will need to reach on exozodiacal discs in order to prepare the scientific programme of future Earth-like planet characterisation missions.
The Nulling Interferometry Cryogenic Experiment (NICE): Architecture, requirements, and preliminary warm precursor results
ETH Zürich, Institute for Particle Physics & Astrophysics（苏黎世联邦理工学院，粒子物理与天体物理研究所）；ETH Zürich, Department of Earth and Planetary Sciences（苏黎世联邦理工学院，地球与行星科学系）
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）
Asgard/NOTT: L-band nulling interferometry at the VLTI -- III. The mid-infrared integrated optics beam combiner for NOTT
I. Physikalisches Institut der Universität zu Köln（科隆大学第一物理研究所）；Department of Physics & Astronomy, University of California, Los Angeles（加州大学洛杉矶分校物理与天文学系）；Institute of Astronomy, KU Leuven（鲁汶大学天体物理研究所）
Tricouplers for nulling interferometry with photonic integrated circuits
California Institute of Technology（加州理工学院）；Astrophotonics Australia（天文光子学澳大利亚）；University of California, Los Angeles（加利福尼亚大学洛杉矶分校）；NASA Jet Propulsion Laboratory（美国国家航空航天局喷气推进实验室）；University of Maryland（马里兰大学）
在1980-2010年的大约30年期间，对空间仪器的光学干涉测量进行了技术研究，认为这有望提高空间分辨率和天体测量精度。研究了高空间分辨率和高对比度的调零干涉术。这些研究是值得进一步历史关注的伟大梦想。欧空局对干涉测量的兴趣始于1980年代初。全球天体测量任务盖亚的光学干涉测量研究始于1993年，1998年结束，当时干涉测量因不适合这一目的而被放弃，而将于2013年发射的盖亚任务不是基于干涉测量。\c{opyright} Anita Publications. All rights reserved.
Tri-coupler geometries for achromatic nulling interferometry in the near-infrared
Astrophotonics Australia；Department of Astronomy, California Institute of Technology（加州理工学院天文学系）；Physics & Astronomy Department, University of California, Los Angeles（加州大学洛杉矶分校物理与天文系）
Technologies and novel components for broadband splitting and coupling in pairwise and nulling interferometry
Astrophotonics Australia, Monash（蒙纳士大学天体光子学澳大利亚）；Department of Astronomy, California Institute of Technology（加州理工学院天文系）；Physics & Astronomy Department, University of California, Los Angeles（加州大学洛杉矶分校物理与天文系）；LIRA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris（巴黎天文台LIRA实验室，巴黎文理研究大学，法国国家科学研究中心，索邦大学，巴黎大学）；Commissariat à l’Energie Atomique, Leti（法国原子能和替代能源委员会LETI实验室）；Astralis-AITC, Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）；Department of Quantum Science, Research School of Physics, Australian National University（澳大利亚国立大学量子科学系，物理研究学院）
Large Interferometer For Exoplanets (LIFE): VII. Practical implementation of a five-telescope kernel-nulling beam combiner with a discussion on instrumental uncertainties and redundancy benefits
Spectrally dispersed non-redundant aperture-masking interferometry in the thermal infrared with LBTI/ALES
The University of Arizona（亚利桑那大学）；University of Wyoming（怀俄明大学）；KU Leuven（荷语鲁汶大学）；Macquarie University（麦考瑞大学）；Large Binocular Telescope Observatory, The University of Arizona（大型双筒望远镜天文台，亚利桑那大学）
Achieving efficient broadband spatial filtering for LIFE: status and plan
ETH Zürich（苏黎世联邦理工学院）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Sydney Institute for Astronomy, School of Physics, University of Sydney（悉尼大学物理学院天体物理研究所）；Research School of Astronomy & Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）
Continuing to Advance European High Contrast Imaging Research and Development towards HWO and LIFE
Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Laboratoire J.-L. Lagrange, Université Cote d’Azur, CNRS, Observatoire de la Cote d’Azur（拉格朗日实验室，尼斯蔚蓝海岸大学，法国国家科学研究中心，蔚蓝海岸天文台）；LIRA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Cité（光与辐射研究实验室，巴黎天文台，巴黎文理研究大学，法国国家科学研究中心，索邦大学，巴黎西岱大学）；NOVA, Leiden University（NOVA，莱顿大学）；European Southern Observatory（欧洲南方天文台）；Space sciences, Technologies, and Astrophysics Research (STAR) Institute, Université de Liège（空间科学、技术和天体物理研究（STAR）研究所，列日大学）
VLTI/MATISSE observations of the hot dust around $β$ Pictoris: Observing faint objects with MATISSE
Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学）；Univ. Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学，蔚蓝海岸天文台）；Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, HUN-REN（孔科利天文台，地球与天文学研究中心）；CSFK, MTA Centre of Excellence（匈牙利科学院天文学研究所，MTA卓越中心）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）
Large Interferometer For Exoplanets (LIFE): III. Spectral resolution, wavelength range and sensitivity requirements based on atmospheric retrieval analyses of an exo-Earth
