Low-frequency radio astronomy is limited by severe ionospheric distortions below 50 MHz and complete reflection of radio waves below 10-30 MHz. Shielding of man-made interference from long-range radio broadcasts, strong natural radio emission from the Earth's aurora, and the need for setting up a large distributed antenna array make the lunar far side a supreme location for a low-frequency radio array. A number of new scientific drivers for such an array, such as the study of the dark ages and epoch of reionization, exoplanets, and ultra-high energy cosmic rays, have emerged and need to be studied in greater detail. Here we review the scientific potential and requirements of these and other new scientific drivers and discuss the constraints for various lunar surface arrays. In particular we describe observability constraints imposed by the interstellar and interplanetary medium, calculate the achievable resolution, sensitivity, and confusion limit of a dipole array using general scaling laws, and apply them to various scientific questions. Whichever science is deemed most important, pathfinder arrays are needed to test the feasibility of these experiments in the not too distant future. Lunar low-frequency arrays are thus a timely option to consider, offering the potential for significant new insights into a wide range of today's crucial scientific topics. This would open up one of the last unexplored frequency domains in the electromagnetic spectrum.
The impact of lunar topography on the 21-cm power spectrum for grid-based arrays : Insights for the Dark-ages EXplorer (DEX)
University of Groningen（格罗宁根大学）；Radboud University（拉德堡德大学）；Delft University of Technology（代尔夫特理工大学）；Netherlands Institute for Radio Astronomy (ASTRON)（荷兰射电天文研究所）；INAF - Istituto di Radioastronomia（意大利国家天体物理研究所射电天文分部）
Quantifying Foreground Contamination in the Dark Ages 21 cm Power Spectrum Using an Electromagnetically Simulated Dipole Antenna Atop a Dielectric Surface
Brown University（布朗大学）；National Radio Astronomy Observatory（国家射电天文台）；University of Colorado Boulder（科罗拉多大学博尔德分校）；Lunar Resources, Inc.（月球资源公司）
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
AMPM II. A Lunar-Mass Primordial Black Hole Microlensing Candidate in the Milky Way Halo
Swinburne University of Technology（斯威本科技大学）；ARC Centre of Excellence for Dark Matter Particle Physics（暗物质粒子物理卓越研究中心）；Australian National University（澳大利亚国立大学）；NSF NOIRLab National Optical-Infrared Astronomy Research Laboratory（美国国家光学红外天文研究实验室）；Cerro Tololo Inter-American Observatory（塞罗托洛美洲际天文台）
The FarView Low Frequency Radio Array on the Moon's Far Side: Science and Array Architecture
University of Colorado Boulder（科罗拉多大学博尔德分校）；Arizona State University（亚利桑那州立大学）；California Institute of Technology（加州理工学院）；Space Science Institute（空间科学研究所）；National Radio Astronomy Observatory（美国国家射电天文台）；Brown University（布朗大学）；Lunar Resources, Inc.（月球资源公司）；CSIRO, Space & Astronomy（澳大利亚联邦科学与工业研究组织，太空与天文部）
