The active broadband (1 kHz-100 MHz) tripole antenna now envisaged to be placed on the European Lunar Lander located at the Lunar South Pole allows for sensitive measurements of the exosphere and ionosphere, and their interaction with the Earths magnetosphere, solar particles, wind and CMEs and studies of radio communication on the moon, that are essential for future lunar human and science exploration. In addition, the lunar South pole provides an excellent opportunity for radio astronomy. Placing a single radio antenna in an eternally dark crater or behind a mountain at the south (or north) pole would potentially provide perfect shielding from man-made radio interference (RFI), absence of ionospheric distortions, and high temperature and antenna gain stability that allows detection of the 21 cm wave emission from pristine hydrogen formed after the big bang and into the period where the first stars formed. A detection of the 21 cm line from the moon at these frequencies would allow for the first time a clue on the distribution and evolution on mass in the early universe between the Epoch of Recombination and Epoch of Reionization (EoR). A single lunar radio antenna would also allow for studies of the effect of solar flares and Coronal Mass Ejections (CMEs) on the solar wind at distances close to earth (space weather) and would open up the study of low frequency radio events from planets such as Jupiter and Saturn, which are known to emit bright (kJy-MJy) radio emission below 30 MHz (Jester & Falcke, 2009). Finally, a single radio antenna on the lunar lander would pave the way for a future large lunar radio interferometer; not only will it demonstrate the possibilities for lunar radio science and open up the last unexplored radio regime, but it will also allow a determination of the limitations of lunar radio science by measuring the local radio background noise.
Chang'e 7 Lunar Lander Optical Camera-Telescope: Optical Astronomy from the Moon
The University of Hong Kong（香港大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；International Lunar Observatory Association（国际月球观测站联盟）
Integrated Lander-Propulsion-GNC Framework for Autonomous Lunar Powered Descent
Turkuzaysan Inc.（Turkuzaysan公司）；Puura Inc.（Puura公司）；Final Proximity Space Systems Inc.（Final Proximity Space Systems公司）；TUBITAK Space Technologies Research Institute（TUBITAK空间技术研究研究所）
Results from NASA's First Radio Telescope on the Moon: Terrestrial Technosignatures and the Low-Frequency Galactic Background Observed by ROLSES-1 Onboard the Odysseus Lander
Electrical coupling of a horizontal dipole antenna to a dielectric half-space: applications to radio astronomy from the lunar surface
Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；University of California, Berkeley（加州大学伯克利分校）；The Blackett Laboratory, Imperial College London（帝国理工学院布莱克特实验室）；Brookhaven National Laboratory（布鲁克海文国家实验室）
The Radio-wave Observations at the Lunar Surface of the photoElectron Sheath (ROLSES) instrument onboard the Intuitive Machines-1 Mission to the Moon
NASA/GSFC（美国国家航空航天局戈达德太空飞行中心）；Space Science Institute（空间科学研究所）；DeepSpace Technologies（深空技术公司）；University of Colorado, Boulder（科罗拉多大学博尔德分校）；University of California, Berkeley（加州大学伯克利分校）
The Lunar Farside Transients and Technology Telescope (LFT3) Mission
University of Oxford（牛津大学）；University of California（加州大学）；Trinity College Dublin（都柏林三一学院）；Stanford University（斯坦福大学）；Heliospace；The University of Edinburgh（爱丁堡大学）；Brookhaven National Laboratory（布鲁克海文国家实验室）；SETI Institute（SETI研究所）；University of New Mexico（新墨西哥大学）
Modelling Radio Frequency Interference on the Lunar Farside
Trinity College Dublin（都柏林三一学院）；The University of Edinburgh（爱丁堡大学）；University of Oxford（牛津大学）；Heliospace（赫利奥空间）；Radio Astronomy Laboratory, University of California, Berkeley（加州大学伯克利分校射电天文实验室）
FARSIDE: A Low Radio Frequency Interferometric Array on the Lunar Farside
FARSIDE（Farside Array for Radio Science Investigations of the Dark ages and Exoplanets）是一个探测器级的概念，用于在月球背面放置低射频干涉阵列。NASA资助的一项设计研究，重点是仪器，部署漫游车，着陆器和基站，提供了一个与探测器任务要求大致一致的架构。这种概念架构由128个双极化天线组成，由一个漫游者部署在10公里的区域内，并连接到一个基站，用于中央处理，电力和数据传输到月球网关。FARSIDE将提供每分钟在1400个频道中对整个天空进行成像的能力，这些频道的频率从100千赫到40兆赫不等，比地面射电天文学可以使用的波段低两个数量级。月球背面可以同时提供对地面射频干扰、极光千米辐射和来自太阳风的等离子体噪声的隔离。这将使得在寻找日冕物质抛射和高能粒子事件的无线电特征时能够对最近的恒星系统进行近乎连续的监测，并且还将探测最近的候选可居住系外行星的磁层。同时，FARSIDE将被用来描述我们太阳系中类似的活动，从太阳到外行星，包括假设的第九行星。通过轨道信标的精确校准和精致的前景表征，FARSIDE还将测量红移z=50-100的黑暗时代全球21厘米信号。FARSIDE提供的独特观测窗口将使更多的科学从探测月球表面到表征太阳系附近的星际介质。
How to Deploy a 10-km Interferometric Radio Telescope on the Moon with Just Four Tethered Robots
Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Blue Origin Enterprises（蓝色起源公司）；California Institute of Technology（加州理工学院）；University of Michigan（密歇根大学）；University of Colorado Boulder（科罗拉多大学博尔德分校）
Gravitational-wave Tomography of the Moon: Constraining Lunar Structure with Calibrated Gravitational Waves
Peking University（北京大学）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学卡尔维天体物理研究所）；Gran Sasso Science Institute（格兰萨索科学研究所）；INFN, Laboratori Nazionali del Gran Sasso（意大利国家核物理研究所格兰萨索国家实验室）
