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Planetary Geologic Mapping and Remote Sensing
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Planetary Geologic Mapping and Remote Sensing

A special issue of Remote Sensing (ISSN 2072-4292). This special issue belongs to the section "Satellite Missions for Earth and Planetary Exploration".

Deadline for manuscript submissions: closed (30 November 2022) | Viewed by 32859

Special Issue Editors

Prof. Dr. Kaichang Di

E-Mail Website
Guest Editor
State Key Laboratory of Remote Sensing Science, Aerospace Information Research Institute, Chinese Academy of Sciences, Beijing 100101, China
Interests: planetary remote sensing; planetary mapping; planetary rover localization and navigation; planetary geomorphology; comparative planetology
Special Issues, Collections and Topics in MDPI journals
Prof. Dr. Long Xiao

E-Mail Website
Guest Editor
School of Earth Sciences, China University of Geosciences, Wuhan 430074, China
Interests: planetary geology; planetary geomorphology; extraterrestrial materials; planetary analogs; comparative planetology
Special Issues, Collections and Topics in MDPI journals
Dr. Jessica Flahaut

E-Mail Website
Guest Editor
Centre de Recherches Pétrographiques et Géochimiques (CRPG), CNRS/Université de Lorraine, 54500 Vandoeuvre-les-Nancy, France
Interests: planetary geology; mars; the moon; landing sites; VNIR spectroscopy; planetary analogs

Special Issue Information

Dear Colleagues,

Planetary geologic maps are spatial and temporal representations of the materials, landforms, structures, and processes of planetary surfaces. Planetary geologic mapping is largely based on analyses of various remote sensing data acquired by space missions, and is fundamental in understanding the formation and evolution of planetary surfaces and shallow subsurfaces. Planetary remote sensing techniques and the ever-increasing data have greatly supported geologic mapping, as well as other scientific studies of the Moon, Mars and other planetary bodies in the solar system.

We would like to invite you to submit articles covering all aspects of planetary geologic mapping and planetary remote sensing, including theory, methods, techniques, algorithms, data validation, mapping products, and applications. Review articles are also welcome. Articles may address, but are not limited to, the following topics:

  • planetary geologic mapping;
  • planetary geomorphologic mapping;
  • photogrammetric remote sensing of planetary surfaces;
  • spectroscopic remote sensing of planetary surfaces;
  • remote sensing methods, data calibration and validation;
  • planetary GIS for geologic mapping;
  • recent and future planetary exploration missions;
  • landing sites studies;
  • analog studies.

Prof. Dr. Kaichang Di
Prof. Dr. Long Xiao
Dr. Jessica Flahaut
Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Remote Sensing is an international peer-reviewed open access semimonthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. The Article Processing Charge (APC) for publication in this open access journal is 2700 CHF (Swiss Francs). Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  • planetary geology
  • planetary topography and geomorphology
  • planetary chronology
  • planetary spectrum
  • planetary remote sensing
  • geologic structures
  • geologic mapping
  • planetary composition
  • planetary GIS
  • planetary exploration missions
  • landing sites

Related Special Issue

Published Papers (15 papers)

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Research

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20 pages, 10536 KiB  
Article
A Cartographic Perspective on the Planetary Geologic Mapping Investigation of Ceres
by Andrea Naß and Stephan van Gasselt
Remote Sens. 2023, 15(17), 4209; https://0-doi-org.brum.beds.ac.uk/10.3390/rs15174209 - 27 Aug 2023
Cited by 1 | Viewed by 1009
Abstract
The NASA Dawn spacecraft visited asteroid 4 Vesta between 2011 and 2012 and dwarf planet 1 Ceres between 2015 and 2018 to investigate their surfaces through optical and hyperspectral imaging and their composition through gamma-ray and neutron spectroscopy. For the global mapping investigation [...] Read more.
The NASA Dawn spacecraft visited asteroid 4 Vesta between 2011 and 2012 and dwarf planet 1 Ceres between 2015 and 2018 to investigate their surfaces through optical and hyperspectral imaging and their composition through gamma-ray and neutron spectroscopy. For the global mapping investigation of both proto-planets, geologic mappers employed Geographic Information System (GIS) software to map 15 quadrangles using optical and hyperspectral data and to produce views of the geologic evolution through individual maps and research papers. While geologic mapping was the core motivation of the mapping investigation, the project never aimed to produce homogeneous and consistent map representations. The chosen mapping approach and its implementation led to a number of inconsistencies regarding cartographic representation, including differential generalization through varying mapping scales, topologic inconsistencies, lack of semantic integrity, and scale consistency, and ultimately, to the management of reusable research data. Ongoing data acquisition during the mapping phase created additional challenges for the homogenization of mapping results and a potential derivation of a global map. This contribution reviews cartographic and data perspectives on the mapping investigation of Ceres and highlights (a) data sources, (b) the cartographic concept, (c) mapping conduct, and (d) dissemination as well as research-data management arrangements. It furthermore discusses decisions and experiences made during mapping and finishes with a set of recommendations from the viewpoint of the cartographic sciences. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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21 pages, 34528 KiB  
Article
Diverse Geological Evolution of Impact Basins on the Moon
by Jiayin Deng, Weiming Cheng and Yimeng Jiao
Remote Sens. 2022, 14(24), 6335; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14246335 - 14 Dec 2022
Viewed by 1371
Abstract
Impact basins are the dominant landforms on the lunar surface, and their geological evolution varies. This research studied the diversity in the geological evolution of three impact basins: the Dirichlet–Jackson Basin, the Nectaris Basin, and the Orientale Basin. First, the regional topography and [...] Read more.
Impact basins are the dominant landforms on the lunar surface, and their geological evolution varies. This research studied the diversity in the geological evolution of three impact basins: the Dirichlet–Jackson Basin, the Nectaris Basin, and the Orientale Basin. First, the regional topography and geomorphology of the three basins were studied using the SLDEM2015 digital elevation model (DEM). Clementine ultraviolet–visible (UVVIS) data and Moon Mineralogy Mapper (M3) data were used to study the chemical composition and mineralogical composition of the three basins. Additionally, the lunar crust thickness data have been used to study the subsurface structure of the three basins. The topographical analogies of the three basins indicate that the shapes of the basins are cavity-like. However, the shape of the Dirichlet–Jackson basin is not an obvious cavity compared with the other basins. The positions with minimum and maximum crustal thickness of the three basins are located at the center and the rim. The uplift of the crust-mantle interface of the Nectaris Basin and Orientale Basin is relatively larger than in the Dirichlet–Jackson Basin. Below the center of the maria of the Nectaris Basin and Orientale Basin, collapses occurred at the crust–mantle interface. The concentrations of FeO and TiO2 in the non-mare formation of the basin and maria show expected bimodal distributions. Moreover, we found exposures of olivine-rich materials in the Nectaris Basin and Orientale Basin which are located in the Rosse and Maunder craters, respectively. These exposures of olivine may be explained by the fact that the formation of the large impact basin, which might penetrate and blast away the upper lunar crust, excavating deep-seated material. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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20 pages, 5463 KiB  
Article
A Generative Adversarial Network for Pixel-Scale Lunar DEM Generation from High-Resolution Monocular Imagery and Low-Resolution DEM
by Yang Liu, Yexin Wang, Kaichang Di, Man Peng, Wenhui Wan and Zhaoqin Liu
Remote Sens. 2022, 14(21), 5420; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14215420 - 28 Oct 2022
Cited by 1 | Viewed by 1561
Abstract
Digital elevation models (DEMs) provide fundamental data for scientific and engineering applications in lunar exploration missions. Lunar DEMs have been mainly generated by laser altimetry and stereophotogrammetry. Complementarity to stereo photogrammetry, reflection-based surface reconstruction methods, such as shape from shading (SFS), have been [...] Read more.
Digital elevation models (DEMs) provide fundamental data for scientific and engineering applications in lunar exploration missions. Lunar DEMs have been mainly generated by laser altimetry and stereophotogrammetry. Complementarity to stereo photogrammetry, reflection-based surface reconstruction methods, such as shape from shading (SFS), have been studied and applied in lunar DEM reconstruction from a single image. However, this method often suffers from solution ambiguity and instability. In this paper, we propose a generative adversarial network (GAN)-based method that is able to generate high-resolution pixel-scale DEMs from a single image aided by a low-resolution DEM. We have evaluated the accuracy of the reconstructed high-resolution DEMs from 25 LROC NAC images of four regions using LROC NAC DEMs (2 m/pixel) as ground truth. The experimental results demonstrate good accuracy and adaptability to changes in illumination conditions. The root mean square error (RMSE) can reach about 2 m in areas where the degree of elevation variation is less than 100 m, and the RMSE value ranges from around 3 m to 10 m without considering the degree of the elevation variation in large-area reconstruction. As high-resolution monocular images and low-resolution DEMs are available for the entire lunar surface, the proposed GAN-based method has great potential in high-resolution lunar DEM reconstruction for lunar mapping applications. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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19 pages, 27855 KiB  
Article
Study of the Buried Basin C-H, Based on the Multi-Source Remote Sensing Data
by Xiaojian Xu, Teng Hu, Zhizhong Kang, Xing Du and Lin Zhao
Remote Sens. 2022, 14(21), 5284; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14215284 - 22 Oct 2022
Viewed by 1276
Abstract
We use multi-source remote sensing data to identify the details of a mascon south-east of the lunar Copernicus crater. Studies of the topography, gravity, geochronology and mineral are combined to prove that the mascon is a buried peak-ring basin with diameters of about [...] Read more.
We use multi-source remote sensing data to identify the details of a mascon south-east of the lunar Copernicus crater. Studies of the topography, gravity, geochronology and mineral are combined to prove that the mascon is a buried peak-ring basin with diameters of about 130 km and 260 km. The underground structure is covered by 890 m thick mare basalts, as determined by analyzing the spectral features of the impact crater, Copernicus H. The determination of the crater size–frequency distribution (CSFD) suggests that the impact that created the C-H basin occurred earlier than 3.9 Ga. Then, a Hawaiian-style eruption in the late Imbrian period formed the Sinus Aestuum-I dark mantling deposit (DMD). Soon, mare basalts covered the basin several times from 3.8 Ga. Finally, the ejecta from the Copernicus impact event at about 800 Ma, and the weathering processes caused the disappearance of the C-H basin rim from the lunar surface. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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26 pages, 12833 KiB  
Article
Quantitative Inversion of Lunar Surface Chemistry Based on Hyperspectral Feature Bands and Extremely Randomized Trees Algorithm
by Shuangshuang Wu, Jianping Chen, Li Li, Cheng Zhang, Rujin Huang and Quanping Zhang
Remote Sens. 2022, 14(20), 5248; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14205248 - 20 Oct 2022
Cited by 1 | Viewed by 1601
Abstract
In situ resource utilization (ISRU) is required for the operation of both medium and long-term exploration missions to provide metallic materials for the construction of lunar base infrastructure and H2O and O2 for life support. The study of the distribution [...] Read more.
In situ resource utilization (ISRU) is required for the operation of both medium and long-term exploration missions to provide metallic materials for the construction of lunar base infrastructure and H2O and O2 for life support. The study of the distribution of the lunar surface elements (Fe, Ti, Al, and Si) is the basis for the in situ utilization of mineral resources. With the arrival of the era of big data, the application of big data concepts and technical methods to lunar surface chemistry inversion has become an inevitable trend. This paper is guided by big data theory, and the Apollo 17 region and the area near the Copernicus crater are selected for analysis. The dimensionality of the first-order differential spectral features of lunar soil samples is reduced based on Pearson correlation analysis and the successive projections algorithm (SPA), and the extremely randomized trees (Extra-Trees) algorithm is applied to Chang’E-1 Interference Imaging Spectrometer (IIM) data to establish a prediction model for the lunar surface chemistry and generate FeO, TiO2, Al2O3, and SiO2 distribution maps. The results show that the optimum number of variables for FeO, TiO2, Al2O3, and SiO2 is 17, 5, 8, and 30, respectively. The accuracy of the Extra-Trees model using the best variables was improved over that of the original band model, with determination coefficients (R2) of 0.962, 0.944, 0.964, and 0.860 for FeO, TiO2, Al2O3, and SiO2, and root mean square errors (RMSEs) of 1.028, 0.672, 0.942, and 0.897, respectively. The modeling feature variables and model preference methods in this study can improve the inversion accuracy of chemical abundance to some extent, demonstrating the potential of IIM data in predicting chemical abundance and providing a good data basis for lunar geological evolution studies and ISRU. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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21 pages, 12456 KiB  
Article
Population of Degrading Small Impact Craters in the Chang’E-4 Landing Area Using Descent and Ground Images
by Teng Hu, Ze Yang, Zhizhong Kang, Hongyu Lin, Jie Zhong, Dongya Zhang, Yameng Cao and Haomin Geng
Remote Sens. 2022, 14(15), 3608; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14153608 - 28 Jul 2022
Cited by 3 | Viewed by 1520
Abstract
The landing camera (LCAM) of Chang’e-4 lander provides a series of low (46 cm/pixel) to high (2.3 cm/pixel) resolution images, which are suitable for centimeter-scale craters. In this paper, we analyze the degradation of those small-sized craters to provide detailed information on the [...] Read more.
The landing camera (LCAM) of Chang’e-4 lander provides a series of low (46 cm/pixel) to high (2.3 cm/pixel) resolution images, which are suitable for centimeter-scale craters. In this paper, we analyze the degradation of those small-sized craters to provide detailed information on the local geological evolution of the lunar surface. From the mosaicked descent image, 6316 craters were extracted and classified into four degradation levels based on their morphology on the image: fresh, slightly degraded, moderately degraded, and severely degraded. The ground terrain camera (TCAM) image and the DEM of the Yutu-2 panoramic camera (PCAM) validate the crater degradation levels from a qualitative and quantitative perspective, respectively. The results show that the smaller the size of the craters, the more easily they are degraded. The crater populations in equilibrium in the four study areas indicate that the cumulative size–frequency distribution (SFD) slope is different from previous research results, and the smaller the craters, the more difficult to reach an equilibrium state (for craters smaller than a given size, the production rate is exactly balanced by the removal rate), which may be due to secondary cratering and surface resurfacing caused by the burial of ejecta from neighboring craters. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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31 pages, 36810 KiB  
Article
High-Resolution Regional Digital Elevation Models and Derived Products from MESSENGER MDIS Images
by Madeleine R. Manheim, Megan R. Henriksen, Mark S. Robinson, Hannah R. Kerner, Bradley A. Karas, Kris J. Becker, Matthew Chojnacki, Sarah S. Sutton and David T. Blewett
Remote Sens. 2022, 14(15), 3564; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14153564 - 25 Jul 2022
Cited by 1 | Viewed by 1812
Abstract
The Mercury Dual Imaging System (MDIS) on the Mercury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft has provided global images of Mercury’s surface. A subset of off-nadir observations acquired at different times resulted in near-global stereo coverage and enabled the creation of [...] Read more.
The Mercury Dual Imaging System (MDIS) on the Mercury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft has provided global images of Mercury’s surface. A subset of off-nadir observations acquired at different times resulted in near-global stereo coverage and enabled the creation of local area digital elevation models (DEMs). We derived fifty-seven DEMs covering nine sites of scientific interest and tied each to a geodetic reference derived from Mercury Laser Altimeter (MLA) profiles. DEMs created as part of this study have pixel scales ranging from 78 m/px to 500 m/px, and have vertical precisions less than the DEM pixel scale. These DEMs allow detailed characterizations of key Mercurian features. We present a preliminary examination of small features called “hollows” in three DEM sites. Depth measurements from the new DEMs are consistent with previous shadow and stereo measurements. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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18 pages, 9908 KiB  
Article
Spectroscopic and Petrographic Investigations of Lunar Mg-Suite Meteorite Northwest Africa 8687
by Lang Qin, Xing Wu, Liying Huang, Yang Liu and Yongliao Zou
Remote Sens. 2022, 14(12), 2952; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14122952 - 20 Jun 2022
Viewed by 2233
Abstract
Magnesian suite (Mg-suite) rocks represent plutonic materials from the lunar crust, and their global distribution can provide critical information for the early magmatic differentiation and crustal asymmetries of the Moon. Visible and near-infrared (VNIR) spectrometers mounted on orbiters and rovers have been proven [...] Read more.
Magnesian suite (Mg-suite) rocks represent plutonic materials from the lunar crust, and their global distribution can provide critical information for the early magmatic differentiation and crustal asymmetries of the Moon. Visible and near-infrared (VNIR) spectrometers mounted on orbiters and rovers have been proven to be powerful approaches for planetary mineral mapping, which are instrumental in diagnosing Mg-suite rocks. However, due to the scarcity and diversity of Mg-suite samples, laboratory measurements with variable proportions of minerals are imperative for spectral characterization. In this study, spectroscopic investigation and petrographic study were conducted on lunar Mg-suite meteorite Northwest Africa 8687. We classify the sample as a pink spinel-bearing anorthositic norite through spectral and petrographic characteristics. The ground-truth information of the Mg-suite rock is provided for future exploration. Meanwhile, the results imply that the VNIR technique has the potential to identify highland rock types by mineral modal abundance and could further be applied in extraterrestrial samples for primary examination due to its advantage of being fast and non-destructive. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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25 pages, 26481 KiB  
Article
Potential Applications of CE-2 Microwave Radiometer Data in Understanding Basaltic Volcanism in Heavily Ejecta-Contaminated Mare Frigoris
by Jietao Lei, Zhiguo Meng, Yongzhi Wang, Shaopeng Huang, Jinsong Ping, Zhanchuan Cai and Yuanzhi Zhang
Remote Sens. 2022, 14(11), 2725; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14112725 - 06 Jun 2022
Cited by 4 | Viewed by 1655
Abstract
Mare Frigoris is the fifth largest and almost northernmost mare located on the near side of the Moon. Mare Frigoris has an elongated shape, with a length of approximately 1500 km and a width of approximately 200 km, which makes it susceptible to [...] Read more.
Mare Frigoris is the fifth largest and almost northernmost mare located on the near side of the Moon. Mare Frigoris has an elongated shape, with a length of approximately 1500 km and a width of approximately 200 km, which makes it susceptible to becoming contaminated by the impact ejecta from the nearby highlands. Comparatively speaking, microwave radiometer (MRM) data have good penetration capabilities. Therefore, the MRM data from Chang’e-2 satellite were employed to study the volumetric thermal emission features of basaltic deposits in Mare Frigoris. Combining the MRM data with the basaltic units with FeO and TiO2 abundances identified using the small crater rim and ejecta probing (SCREP) methodology and with the gravity from Gravity Recovery and Interior Laboratory (GRAIL), the four potential conclusions that were obtained are as follows: (1) The MRM data are strongly related to the (FeO + TiO2) abundance of pristine basalts and are less influenced by ejecta contamination; (2) in every quadrant of Mare Frigoris, the (FeO + TiO2) abundance of the basalt decreases with an increase in age; (3) at least in Mare Frigoris, the main influencing factor regarding the brightness temperature remains the (FeO + TiO2) abundance of surface deposits; (4) a warm microwave anomaly was revealed in the western-central and eastern-central areas of Mare Frigoris which has a strong relationship with the positive Bouguer gravity anomaly derived from GRAIL data in terms of spatial distribution. The results are significant in the context of improving our understanding the basaltic igneous rock and thermal evolution of the Moon using MRM data. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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26 pages, 6142 KiB  
Article
Remote Sensing Survey of Altiplano-Puna Volcanic Complex Rocks and Minerals for Planetary Analog Use
by Gen Ito, Jessica Flahaut, Osvaldo González-Maurel, Benigno Godoy, Vincent Payet and Marie Barthez
Remote Sens. 2022, 14(9), 2081; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14092081 - 26 Apr 2022
Cited by 3 | Viewed by 3482
Abstract
The Altiplano-Puna Volcanic Complex (APVC) of the Central Andes is an arid region with extensive volcanism, possessing various geological features comparable to those of other solar system objects. The unique features of the APVC, e.g., hydrothermal fields and evaporite salars, have been used [...] Read more.
The Altiplano-Puna Volcanic Complex (APVC) of the Central Andes is an arid region with extensive volcanism, possessing various geological features comparable to those of other solar system objects. The unique features of the APVC, e.g., hydrothermal fields and evaporite salars, have been used as planetary analogs before, but the complexity of the APVC presents a wealth of opportunities for more analog studies that have not been exploited previously. Motivated by the potential of using the APVC as an analog of the volcanic terrains of solar system objects, we mapped the mineralogy and silica content of the APVC up to ~100,000 km2 in northern Chile based on a combination of remote sensing data resembling those of the Moon and Mars. The band ratio indices of Landsat 8 Operational Land Imager multispectral images and mineral classifications based on spectral hourglass approach using Earth Observing-1 Hyperion hyperspectral images (both in the visible to shortwave infrared wavelengths) were used to map iron-bearing and alteration minerals. We also used Hyperion imagery to detect feldspar spectral signatures and demonstrated that feldspar minerals can be detected on non-anorthosites, which may influence interpretations of feldspar spectral signatures on Mars. From the Terra Advanced Spaceborne Thermal Emission and Reflection Radiometer Global Emissivity Dataset, we derived the silica percentage of non-evaporite rocks within errors of approximately 2–3 wt.% SiO2 for those in the 60–70 wt.% range (about 8 wt.% errors for the 50–60 wt.% range). Based on an integrated assessment of the three datasets, we highlighted three regions of particular interest worthy of further field investigation. We also evaluated the benefits and limitations of all three remote sensing methods for mapping key minerals and capturing rock diversity, based on available samples and existing geological maps. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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17 pages, 47550 KiB  
Article
High-Precision Registration of Lunar Global Mapping Products Based on Spherical Triangular Mesh
by Zheng Bo, Kaichang Di, Bin Liu, Jia Wang, Zhaoqin Liu, Xin Xin, Ziqing Cheng and Jinkuan Yin
Remote Sens. 2022, 14(6), 1442; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14061442 - 16 Mar 2022
Cited by 2 | Viewed by 2390
Abstract
Lunar global mapping products provide a solid data foundation for lunar scientific research and exploration. As the widespread geometric inconsistencies among multi-source mapping products seriously affect the synergistic use of the products, high-precision registration of multiple lunar global products is critical, and it [...] Read more.
Lunar global mapping products provide a solid data foundation for lunar scientific research and exploration. As the widespread geometric inconsistencies among multi-source mapping products seriously affect the synergistic use of the products, high-precision registration of multiple lunar global products is critical, and it is highly challenging due to large coverage and complex local geometric inconsistencies. In this research, we propose a spherical triangular-mesh-based method for high-precision registration of lunar global mapping products, which involves four steps: data preprocessing, feature point extraction and matching, spherical Delaunay triangulation, and geometric correction with spherical barycentric coordinates. This global registration method avoids map projection distortions by using spherical coordinates directly, and achieves high precision by confining the geometric models to spherical triangular facets. Experiments are conducted using two groups of different types of mapping products to verify the proposed method quantitatively and qualitatively. The results show that the geometric inconsistencies are reduced from hundreds of pixels to sub-pixel level globally after the registration, demonstrating the effectiveness of the proposed method. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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17 pages, 5632 KiB  
Article
Robotic Mapping Approach under Illumination-Variant Environments at Planetary Construction Sites
by Sungchul Hong, Pranjay Shyam, Antyanta Bangunharcana and Hyuseoung Shin
Remote Sens. 2022, 14(4), 1027; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14041027 - 20 Feb 2022
Cited by 7 | Viewed by 2306
Abstract
In planetary construction, the semiautonomous teleoperation of robots is expected to perform complex tasks for site preparation and infrastructure emplacement. A highly detailed 3D map is essential for construction planning and management. However, the planetary surface imposes mapping restrictions due to rugged and [...] Read more.
In planetary construction, the semiautonomous teleoperation of robots is expected to perform complex tasks for site preparation and infrastructure emplacement. A highly detailed 3D map is essential for construction planning and management. However, the planetary surface imposes mapping restrictions due to rugged and homogeneous terrains. Additionally, changes in illumination conditions cause the mapping result (or 3D point-cloud map) to have inconsistent color properties that hamper the understanding of the topographic properties of a worksite. Therefore, this paper proposes a robotic construction mapping approach robust to illumination-variant environments. The proposed approach leverages a deep learning-based low-light image enhancement (LLIE) method to improve the mapping capabilities of the visual simultaneous localization and mapping (SLAM)-based robotic mapping method. In the experiment, the robotic mapping system in the emulated planetary worksite collected terrain images during the daytime from noon to late afternoon. Two sets of point-cloud maps, which were created from original and enhanced terrain images, were examined for comparison purposes. The experiment results showed that the LLIE method in the robotic mapping method significantly enhanced the brightness, preserving the inherent colors of the original terrain images. The visibility and the overall accuracy of the point-cloud map were consequently increased. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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Review

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26 pages, 172805 KiB  
Review
Lunar Mare Fecunditatis: A Science-Rich Region and a Concept Mission for Long-Distance Exploration
by Siyuan Zhao, Yuqi Qian, Long Xiao, Jiannan Zhao, Qi He, Jun Huang, Jiang Wang, Hui Chen and Weiyang Xu
Remote Sens. 2022, 14(5), 1062; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14051062 - 22 Feb 2022
Cited by 4 | Viewed by 4113
Abstract
Mare Fecunditatis is a ~310,000 km2 flat basalt plain located in the low-latitude area of the Moon. Plenty of volcanic features (multiple episodes of mare basalts, sinuous rilles, lava tubes, pyroclastic deposits, domes, irregular mare patches (IMP), ring-moat dome structures (RMDS), floor-fractured [...] Read more.
Mare Fecunditatis is a ~310,000 km2 flat basalt plain located in the low-latitude area of the Moon. Plenty of volcanic features (multiple episodes of mare basalts, sinuous rilles, lava tubes, pyroclastic deposits, domes, irregular mare patches (IMP), ring-moat dome structures (RMDS), floor-fractured craters), tectonic features (grabens and wrinkle ridges), impact-related features, and other features (swirls, pit craters) are identified in Mare Fecunditatis. An in-situ mission to Mare Fecunditatis is scientifically significant to better understand the lunar thermal histories and other questions. All previous in-situ and human missions (Apollo, Luna, Chang’E) were limited to small areas, and no traverse longer than 40 km has been made yet. With the development of technology, long-distance movement will be possible in the future on the lunar surface, providing opportunities to explore multiple sites at one mission with complete documentation of the regional geology. Eight high-value targets (pit crater, IMPs, RMDSs, young basalts, high-Al basalts, pyroclastic deposits, swirls, and fresh craters) were found in Mare Fecunditatis, and a ~1400 km-traverse in 5 years is proposed to explore them to solve the most fundamental lunar questions. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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16 pages, 9047 KiB  
Technical Note
Basalt Chronology of the Orientale Basin Based on CE-2 CCD Imaging and Implications for Lunar Basin Volcanism
by Jingwen Liu, Jianzhong Liu, Juntao Wang, Kai Zhu and Li Zhang
Remote Sens. 2022, 14(6), 1426; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14061426 - 15 Mar 2022
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Abstract
The specific duration between the impact event and subsequent volcanic flows is highly variable based on previous works. The method of crater size-frequency distribution (CSFD) has been previously used to date the basalt in Orientale Basin, which yielded inconsistent resultant Absolute Model Age [...] Read more.
The specific duration between the impact event and subsequent volcanic flows is highly variable based on previous works. The method of crater size-frequency distribution (CSFD) has been previously used to date the basalt in Orientale Basin, which yielded inconsistent resultant Absolute Model Age (AMA) ranges. The inconsistency may be attributed to the choice of counting area and identified superposed craters. In this study, we integrated the Chang’E-2 (CE-2) imaging data (7 m/pix) and the IIM and 20 m CE-2 DTMS data, re-divided Mare Orientale, and re-estimated the age of the basalts there. The ages revealed that (1) the central basalts had multiphase eruptions, beginning at 3.77 Ga (30 My after the impact event) with the longest duration of 1.51 Gy; (2) the edge basalts have a similar features as the central basalts, beginning at 3.75–3.50 Ga (50–300 My after the impact) with the longest duration of 0.67 Gy. Compared with the basalts along the basinal margin, the central basalts have higher Ti but lower Mg# contents, consistent with the basaltic magma fractionation trend. Spatial distribution characteristics indicate that the basalt eruption occurred in the impact direction upstream and in the center, but almost absent in the impact direction downstream. Accordingly, we speculate that the longevity of the lunar mare basaltic volcanism was affected by gravity changes, material balance, and other post-impact processes. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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Technical Note
Chronology of the Basalt Units Surrounding Chang’e-4 Landing Area
by Zongyu Yue, Ke Shi, Gregory Michael, Kaichang Di, Sheng Gou, Jianzhong Liu and Shengli Niu
Remote Sens. 2022, 14(1), 49; https://0-doi-org.brum.beds.ac.uk/10.3390/rs14010049 - 23 Dec 2021
Viewed by 2541
Abstract
The Chang’e-4 (CE-4) lunar probe, the first soft landing spacecraft on the far side of the Moon, successfully landed in the Von Kármán crater on 3 January 2019. Geological studies of the landing area have been conducted and more intensive studies will be [...] Read more.
The Chang’e-4 (CE-4) lunar probe, the first soft landing spacecraft on the far side of the Moon, successfully landed in the Von Kármán crater on 3 January 2019. Geological studies of the landing area have been conducted and more intensive studies will be carried out with the in situ measured data. The chronological study of the maria basalt surrounding the CE-4 landing area is significant to the related studies. Currently, the crater size-frequency distribution (CSFD) technique is the most popular method to derive absolute model ages (AMAs) of geological units where no returned sample is available, and it has been widely used in dating maria basalt on the lunar surface. In this research, we first make a mosaic with multi-orbital Chang’e-2 (CE-2) images as a base map. Coupled with the elevation data and FeO content, nine representative areas of basalt units surrounding the CE-4 landing area are outlined and their AMAs are derived. The dating results of the nine basalt units indicate that the basalts erupted from 3.42 to 2.28 Ga ago in this area, a period much longer than derived by previous studies. The derived chronology of the above basalt units establishes a foundation for geological analysis of the returned CE-4 data. Full article
(This article belongs to the Special Issue Planetary Geologic Mapping and Remote Sensing)
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