This research introduces the Blind Super-Resolution Generative Adversarial Network (BSRGAN), an advanced model for super-resolution, designed to enhance the perceptual quality of lunar brightness temperature (TB) scatter plot images. By incorporating a more comprehensive high resolution (HR) dataset and adopting larger low resolution (LR) patch sizes, BSRGAN improves training efficiency and restores finer details. The model utilizes a custom loss function combining L1 loss, the Visual Geometry Group (VGG) perceptual loss, and PatchGAN loss, leading to superior performance in generating lunar scatter plots, especially at 3.0 GHz, compared to other traditional methods. This progress demonstrates the potential of BSRGAN for remote sensing tasks, especially in high-resolution lunar microwave data extraction, and paves the way for future advancements in satellite imaging.

Tsiolkovskiy crater presents one of the few mare deposits on the lunar farside, which are significant to understanding the basaltic magmatism of the Moon. In this paper, for the first time, the thermophysical properties of surface deposits in the Tsiolkovskiy crater were assessed with the brightness temperature (TB), normalized TB (nTB), and TB difference (dTB) maps derived from the Chang'E-2 microwave radiometer data combined with the topography, composition, and rock abundance maps. The main results are presented as follows. (1) The nTB is highly influenced by surface topography, particularly at daytime, as observed in high-frequency maps. However, the influence is limited in the nTB maps at low-frequency channels and dTB maps. (2) We postulate that the substrate temperature in the SW portion of the crater floor might be considerably higher than previously understood. (3) Our observations reveal the presence of mare deposits occurring in two distinct episodes within the mare unit. Notably, the younger mare unit is situated in the NE portion of the crater. (4) The centimeter-scale rocks should be widely distributed in the NE portion beyond the Tsiolkovskiy crater. These findings hold significant implications for advancing our comprehension of the Moon's thermal and basaltic evolutionary processes.

Lacus Mortis has been clarified as the landing site of the Astrobotic Mission One lander mission. In this work, the Chang’E-2 microwave radiometer data was first introduced to evaluate thermophysical features of surface deposits in Lacus Mortis. Several findings are noted as follows. (1) Microwave radiometer data shows abnormal thermophysical parameters existing in shallow layer of mare surface. (2) In crater unit, a strong relationship between microwave performances and other parameters including rock abundance and elevation is shown.

Mare Smythii is a special basin, which is one of the oldest mare basins with the considerably young mare basalts and the high density of floor-fractured craters. In this paper, the Chang’E-2 (CE) lunar microwave radiometer (MRM) data was used to evaluate the thermophysical features of the floor deposits in mare Smythii. Based on the theoretical simulation and the previous geological results, several special findings are noted as follows. (1) The substrate temperature in mare Smythii is likely fairly high. (2) The regolith thermophysical parameters change greatly with depth in the northeast unit, and there probably exists a special material in the shallow layer of the lunar regolith with strong thermal absorption ability. These special findings will be of fundamental significance to improve understanding the thermal evolution of the Moon.

Sinus Medii has various geological features, and its location in the central part of the lunar nearside is ideal for calibrating ground-based lunar observation instruments. In this work, the Chang’E-2 (CE-2) microwave radiometer (MRM) data were used to evaluate the microwave thermal properties of the surface deposits in Sinus Medii combined with the previous geological results based on optical data. The findings are as follows: (1) a lunar calibration site (4.98°W, 3.02°N) is found where the TB performances show a good agreement with the compositions of the surface deposits, (2) a TB anomaly (0.24°W, 0.76°N) was found which may be related to high rock abundance in a crater, and (3) a possible cryptomare is revealed in the light plain southeast of Sinus Medii. This study of the microwave thermal properties in Sinus Medii helps search for calibration sites for ground-based observation instruments.

The in situ lunar regolith explorations of Chang'E 3, 4, and 5 landing sites provide an essential reference for lunar research based on microwave radiometer (MRM) data from Chang'E 1 and 2 satellites. To eliminate the influence of the brightness temperature with latitude and highlight the relationship between the brightness temperature and the lunar regolith composition, the normalized brightness temperature and the brightness temperature difference maps were defined and produced. Based on Kaguya MI data, FeO, TiO2, clinopyroxene, and olivine abundances of Chang'E 3, 4, and 5 landing sites were calculated. Combined with the in situ exploration results, the microwave thermal emission properties of the regolith in Chang'E 3, 4, and 5 landing regions were systematically analyzed. The main findings are as follows: (1) the Chang'E 5 landing region has a stable brightness temperature performance, indicating that the variation of the lunar regolith composition with depth is insignificant in this area, which can be used as an essential reference for microwave thermal radiation anomaly research. (2) A stratified structure exists within the lunar regolith detection range of the Chang'E 3 landing region. With the lower, middle, and upper layers represented by the low-frequency data, high-frequency data, and optical results, respectively, the composition significantly changes. (3) Cold microwave anomalies were found and proposed in the Chang'E 4 landing region, and its nature and formation were preliminarily analyzed. The results show that microwave radiometer data can be used for identifying mare basalt, which can provide an important scientific reference for deepening future studies on the evolution of lunar mare magma.

A new kind of surface material is found and defined in the Balmer–Kapteyn (B-K) cryptomare region, Mare-like cryptomare deposits (MCD), representing highland debris mixed by mare deposits with a certain fraction. This postulates the presence of surface materials in the cryptomare regions. In this study, to objectively verify the existence of the MCD in the cryptomare regions, based on the Chang’E-2 microwave radiometer (MRM) data, the support vector machine (SVM) method was adopted, where the K-means algorithm was used to optimize the training samples and the random forest algorithm was used to select the proper band features. Finally, the extracted MCD is identified with the datasets including Lunar Reconnaissance Orbiter Wide Angle Camera, Diviner, and Clementine UV–VIS. The main findings are as follows: (1) Compared to the range outlined via the TB counter, the range of the MCD is objectively extracted using the SVM method in the B-K cryptomare region, which is reasonably indicated by the FeO abundance, TiO2 abundance, and rock abundance distributions. (2) The MCDs were extracted in the Dewar, Lomonosov–Fleming (L-F), and Schiller–Schickard (S-S) regions, indicating that the MCDs are widely distributed in the cryptomaria. (3) The presence of MCDs is concentrated in a limited region, accounting for 64.9%, 52.3%, 76.4%, and 64%, respectively, in the range of Dewar, L-F, S-S, and B-K regions identified using the optical data. The occurrence of the MCD gives a new understanding of the surface evolution in the cryptomare regions.

In this study, two special thermal behaviors are discovered and identified with the brightness temperature (TB) derived from Chang'e-2 MRM data. First, there exists a 37-GHz TB at noon, which is not related to the topography. Second, there exists a low 3.0-GHz TB anomaly. After comparison the distribution pattern and the correlation coefficients between the rock abundance, or FeO and $\text{TiO}_{2}$ abundances, we ascribe the special thermal behaviors to be a composition-related TB anomaly, which likely reflects the heterogeneity of the lunar crust in vertical direction.

Mare Smythii is a special basin, which is one of the oldest mare basins with the considerably young mare basalts and the high density of floor-fractured craters. In this article, the microwave sounder, named CELMS, onboard Chang'E-2 lunar orbiter was first invested to assess the thermophysical characteristics of the floor materials in mare Smythii. Based on the numerical simulation with the radiative transfer model and the previous geological results, several special findings are noted as follows. First, the substrate temperature in mare Smythii is likely fairly high, and a special temperature structure is provided. Second, there likely exists an unrevealed deposit in the upper layer of the regolith with strong thermal absorption ability. Third, the CELMS results show a strong correlation with the subsurface features obtained by lunar radar sounder data and the surface wrinkle ridges. These findings will be of essential importance to strengthen knowing the thermal and magmatic evolutions of the lunar maria.

The volume FeO and TiO2 abundances (FTAs) of lunar regolith can be more important for understanding the geological evolution of the Moon compared to the optical and gamma-ray results. In this paper, the volume FTAs are retrieved with microwave sounder (CELMS) data from the Chang'E-2 satellite using the back propagation neural network (BPNN) method. Firstly, a three-layered BPNN network with five-dimensional input is constructed by taking nonlinearity into account. Then, the brightness temperature (TB) and surface slope are set as the inputs and the volume FTAs are set as the outputs of the BPNN network. Thereafter, the BPNN network is trained with the corresponding parameters collected from Apollo, Luna, and Surveyor missions. Finally, the volume FTAs are retrieved with the trained BPNN network using the four-channel T-B derived from the CELMS data and the surface slope estimated from Lunar Orbiter Laser Altimeter (LOLA) data. The rationality of the retrieved FTAs is verified by comparing with the Clementine UV-VIS results and Lunar Prospector (LP) GRS results. The retrieved volume FTAs enable us to re-evaluate the geological features of the lunar surface. Several important results are as follows. Firstly, very-low-Ti (<1.5 wt.%) basalts are the most spatially abundant, and the surfaces with TiO2 > 5 wt.% constitute less than 10% of the maria. Also, two linear relationships occur between the FeO abundance (FA) and the TiO2 abundance before and after the threshold, 16 wt.% for FA. Secondly, a new perspective on mare volcanismis derived with the volume FTAs in several importantmare basins, although this conclusion should be verified with more sources of data. Thirdly, FTAs in the lunar regolith change with depth to the uppermost surface, and the change is complex over the lunar surface. Finally, the distribution of volume FTAs hints that the highlands crust is probably homogeneous, at least in terms of the microwave thermophysical parameters.

CRATER WITHIN SOUTH POLE-AITKEN BASIN. Z. G. Meng 1,2,3,4* , Y. Z. Zhu 1 , J. S. Ping 4 , Q. Huang 5 , Z. C. Cai 3 , Y. G. Wu 1 , and A. Gusev 6 , 1 College of Geoexploration Science and Technology, Jilin University, China mengzg@jlu.edu.cn, 2 State Key Laboratory of Remote Sensing Science, Institute of Remote Sensing and Digital Earth, CAS, China. 3 Lunar and Planetary Science Laboratory, MUSTPartner Laboratory of Key Laboratory of Lunar and Deep Space Exploration, CAS, China zccai@must.edu.mo, 4 Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatory, CAS, China jsping@bao.ac.cn, 5 Hubei Subsurface Multi-scale Imaging Key Laboratory, Institute of Geophysics and Geomatics, China University of Geosciences, China qianhuang@cug.edu.cn, 6 Geology Institute, Kazan Federal University, Russia agusev33@gmail.com.

Von Kármán crater is located in the northwest of the SPA basin on the far side of the Moon. The crater cuts through the shallow crust and has abnormal distribution in mineral composition. Therefore，the study on the microwave emission features of Von Kármán crater will be of great significance for the thermal evolution and magma evolution of the moon. Based on the microwave sounder（CELMS）data from Chang’e-2，the brightness temperature（TB）maps and TB difference（dTB）maps are generated using the time angle analysis and the bilinear interpolation method. Then the microwave radiation characteristics of Von Kármán crater are studied combined with previous geologic results and the composition map via the ArcGIS software. The discoveries are as followings：（1）a high TB anomaly is found in the north of the crater basin，preliminarily identified as high substrate temperature；（2）the TB shows a good correlation with the（FeO+TiO2）content in the south part of the crater basin；（3）according to the TB behaviors of the Von Kármán crater，new geological units are zoned in the crater floor;（4）according to the TB performances of the Von Kármán crater，high priority of the candidate landing areas should be given to the north part with TB anomaly，followed by the south and west parts.