Chang’E-4 (CE-4) was the first mission to accomplish the goal of a successful soft landing on the lunar farside. The landing trajectory and the location of the landing site can be effectively reconstructed and determined using series of images obtained during descent when there were no Earth-based radio tracking and the telemetry data. Here we reconstructed the powered descent trajectory of CE-4 using photogrammetrically processed images of the CE-4 landing camera, navigation camera, and terrain data of Chang’E-2. We confirmed that the precise location of the landing site is 177.5991°E, 45.4446°S with an elevation of −5935 m. The landing location was accurately identified with lunar imagery and terrain data with spatial resolutions of 7 m/p, 5 m/p, 1 m/p, 10 cm/p and 5 cm/p. These results will provide geodetic data for the study of lunar control points, high-precision lunar mapping, and subsequent lunar exploration, such as by the Yutu-2 rover.

The distribution range, time-varying characteristics, and sources of lunar water are still controversial. Here we show the Chang’E-5 in-situ spectral observations of lunar water under Earth’s magnetosphere shielding and relatively high temperatures. Our results show the hydroxyl contents of lunar soils in Chang’E-5 landing site are with a mean value of 28.5 ppm, which is on the weak end of lunar hydration features. This is consistent with the predictions from remote sensing and ground-based telescopic data. Laboratory analysis of the Chang’E-5 returned samples also provide critical clues to the possible sources of these hydroxyl contents. Much less agglutinate glass contents suggest a weak contribution of solar wind implantation. Besides, the apatite present in the samples can provide hydroxyl contents in the range of 0 to 179 ± 13 ppm, which shows compelling evidence that, the hydroxyl-containing apatite may be an important source for the excess hydroxyl observed at this young mare region.

On 15 May 2021, the Zhurong rover of China’s first Mars mission, Tianwen-1 (TW-1), successfully landed in southern Utopia Planitia on Mars. Various landforms were present in the landing area, and this area recorded a complex geological history. Cones are one of the typical landforms in the landing area and Utopia Planitia, and they have a great significance to the local geological processes due to the diversity of their origins. Using High-Resolution Imaging Camera (HiRIC) images collected by the TW-1 orbiter, we identified a total of 272 well-preserved circular cones in the landing area. Detailed surveys of their spatial distribution, morphological characteristics, and morphometric parameters were conducted. A preliminary analysis of the surface characteristics of these cones also provides additional information to strengthen our understanding of them. The results of the high-resolution topographic analysis show that the cone heights are in the range of 10.5–90.8 m and their basal diameters range from 178.9–1206.6 m. We compared the morphometric parameters of the cones in the landing area with terrestrial and Martian analogous features and found that our measured cones are consistent with the ranges of mud volcanoes and also a small subset of igneous origin cones. However, the result of spatial analysis is more favorable to mud volcanoes, and the lower thermal inertia of the cones in the landing area compared to their surrounding materials is also a typical characteristic of mud volcanoes. Based on current evidence and analysis, we favor interpreting the cones in the TW-1 landing area as mud volcanoes.

Chang’E-6 mission successfully achieved humanity’s first sample return from the farside of the Moon. Here, we report a high-precision terrain dataset with millimeter-to-decimeter spatial resolution around the CE-6 landing site. Based on this dataset, the accurate location of the landing site is determined to be (153.9776° W, 41.6251° S, -5273 m), and a micro-scale geological analysis of the landing area is conducted. Comparative analysis suggests that the surface exposure time of Chang’ E-6 landing area is likely between that of Chang’E-4 and Chang’E-5 landing areas. Studies of the ejecta thickness from possible craters in mare and non-mare areas indicate that Chang’E-6 samples may contain materials from diverse provenances. Detailed topographic analysis reveals that the Chang’E-6 landing area is primarily covered by local mare materials, which were excavated from a nearby unnamed crater with a diameter of ~ 51 m and account for 30%–35% in volume.

The processes driving the formation and distribution of lunar water (OH/H ₂ O), particularly in the subsurface, remain poorly understood. An opportunity to study subsurface water comes from lander plumes, which can displace and expose millimetre- to centimetre-sized regolith during the descent of the lander. Here we analyse data from the Chang’e-6 landing site and find that plume-disturbed areas exhibit distinct temperature and water-content patterns, which are driven by the redistribution of fine regolith. The average water content of the exposed fine regolith of the shallow subsurface is ~76 ppm, which is lower than the surface abundance of ~105 ppm measured at the surface. The Chang’e-6 landing site also contains on average approximately twice the water content than the Chang’e-5 one. Temporal variations of water content are observed at identical locations but different local times, exhibiting a minimum at local noon. We suggest that the differences in water content are correlated with the regolith glass abundance, particle sizes, depths and local times, reinforcing the hypothesis that solar wind implantation and impact gardening govern lunar water formation and distribution.