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Planetary Exploration Using Remote Sensing

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A special issue of Remote Sensing (ISSN 2072-4292). This special issue belongs to the section "Engineering Remote Sensing".

Deadline for manuscript submissions: closed (31 August 2022) | Viewed by 17210

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Special Issue Editors

Dr. Jungrack Kim

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Guest Editor

Department of Geo-Informatics, University of Seoul, Seoul 02504, Republic of Korea
Interests: reconstruction and monitoring of topography; InSAR/SAR; detection of geomorphological feature; planetary topography
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Dr. Sungkoo Bae

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Guest Editor

Applied Research Laboratories at The University of Texas, Austin, TX 78705, USA
Interests: active remote sensing; small footprint LIDAR; precise attitude determination of spaceborne sensor; extraterrestrial LIDAR application

Prof. Dr. Shih-Yuan Lin

E-Mail Website
Guest Editor

Department of Land Economics, National Chengchi University, Taipei 11605, Taiwan
Interests: InSAR; planetary mapping; error regulation of planetary topography
Special Issues, Collections and Topics in MDPI journals

Special Issue Information

Dear Colleagues,

The 21st century will be recorded as a turning point for the development of humankind’s knowledge about extraterrestrial objects. The capability of high-resolution sensor is now being applied to the farthest frontiers of the solar system. Moreover, data sets accumulated through planetary remote sensing missions are being investigated by cutting edge processing algorithms such as machine vision and learning. At this moment, we need to evaluate our progress on planetary remote sensing and initiate the design for the next strategy that will allow us to transfer our knowledge to incoming peers in the essential enterprise of solar system exploration.

Hence, this issue was proposed as a platform for exchanging vision, skill, and experience in planetary remote-sensing. The major topics will focus on remote-sensing technologies, background algorithm, and scientific achievements of solid planetary and satellite surfaces.

However, it is not limited only to the surface of terrestrial planets. The sub-surfaces of planets and satellites and the atmosphere of giant planets are within the scope of this issue. In particular, contributions to algorithms, sensor design, and mapping results in the following topics will be encouraged:

Ground perpetration radar applications for planetary subsurface studies;
Other quantitative and qualitative planetary optical sensing tools such as multi-hyper spectral sensors;
Active sensing of planet surfaces using technologies such as SAR and LIDAR;
Propositions to innovative planetary remote sensing mission and sensor;
Bridging works between scientific model/interpretation and remote-sensing technology.

Dr. Jungrack Kim
Dr. Sungkoo Bae
Prof. Dr. Shih-Yuan Lin
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

Solid planet/satellite
Topographic survey
Subsurface mapping
Extraterrestrial SAR and LIDAR
Giant planet
Hyper/multi spectral sensing of planetary mineral
Planetary geodesy

Related Special Issue

Planetary Exploration Using Remote Sensing II in Remote Sensing

Published Papers (7 papers)

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Research

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23 pages, 5960 KiB

Open AccessArticle

Investigation of Absorption Bands around 3.3 μm in CRISM Data

by Paola Manzari, Cosimo Marzo and Eleonora Ammannito

Remote Sens. 2022, 14(19), 5028; https://doi.org/10.3390/rs14195028 - 09 Oct 2022

Viewed by 1069

Abstract

Absorptions in the range 3.1 μm to 3.6 μm are under the spotlight in the context of planetary research, because hydrocarbon molecules show absorption bands in this range. Consequently, even knowing that the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) was designed for the detection of mineralogical features on Mars’s surface, we exploited CRISM data in the range 3.2 μm to 3.4 μm to search for potential hydrocarbon compounds. To date, methane has been the only hydrocarbon detected on Mars. Therefore, we began our investigation into CRISM data in locations in which methane had been detected and where it could form due to the mineralogy of the specific site. The datasets chosen for this study included observation sites in the Oxia Planum, the Gale Crater, and Nili Fossae areas. We mapped the modified Gaussian model (MGM) to fit the CRISM data in order to extract the band parameters of the absorptions in the 3.3 μm spectral region. As a result, we found clusters of pixels with spectra that exhibited band centers between approximately 3.28 and 3.35 μm. The hydrocarbons showing absorptions in this range included polycyclic aromatic compounds as well as methane, ethane, and aliphatic compounds. We speculated that some absorptions of approximately 3.3 μm could be related to methane, so we calculated a theoretical lower limit of detection for each observation in the selected CRISM datasets. This was performed by simulating the CRISM spectra for the different sites, with diverse concentrations of CH₄, using NASA’s Planetary Spectrum Generator online tool. These simulations established the relationship between the concentration and methane band depths, as detected by the CRISM. Methane band depths exceeding the thresholds varied from one observation to another, in the range of 0.0136 to 0.0237, which corresponded to a range of theoretically lower limits of concentration between 180 and 600 ppbv. Although we could not confirm or deny the occurrences of methane seepages or hydrocarbons in the investigated datasets, we demonstrated a possible method for searching for hydrocarbons in other CRISM data and for assessing a confidence limit in the detection of the methane band in CRISM data. Full article

(This article belongs to the Special Issue Planetary Exploration Using Remote Sensing)

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16 pages, 6905 KiB

Open AccessArticle

Plausible Detection of Feasible Cave Networks Beneath Impact Melt Pits on the Moon Using the Grail Mission

by Ik-Seon Hong and Yu Yi

Remote Sens. 2022, 14(16), 3926; https://doi.org/10.3390/rs14163926 - 12 Aug 2022

Viewed by 1728

Abstract

In the future, when humans build their bases on terrestrial planets and their moons, caves will be the safest place for inhabitation. Large holes, believed to be cave entrances, have been discovered on the Moon, along with small features called “impact melt pits.” In the Gravity Recovery and Interior Laboratory (GRAIL) gravity model, which is expressed in spherical harmonics (SH), it is difficult to express the gravity anomaly created by a small empty space below the surface. Nevertheless, we propose that a cave network, akin to an anthill, exists under the impact melt pits discovered on the Moon. This is because we think it is natural to apply a network created by Earth’s small caves to the Moon. We obtained accurate Bouguer gravity measurements by calculating regional crustal density using localized admittance of the study area and detected weak gravity (mass deficit) information. By increasing the degrees and order of SH at regular intervals, we estimated the change in gravity at a specific position at high degrees and order, thereby extracting shallow depth information. To validate our method, we compared our results with those of existing studies that analyzed the previously known Marius Hills Hole (MHH) area. The analysis of seven regions in our study area revealed a mass deficit in some impact melt pits in four lunar regions (Copernicus, King, Stevinus, and Tycho). We propose that there is a cave network in this region, indicated by the gravitation reduction in the impact melt pits region. Our results can be useful for the selection of landing sites for future in situ explorations of lunar caves. Full article

(This article belongs to the Special Issue Planetary Exploration Using Remote Sensing)

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17 pages, 10864 KiB

Open AccessArticle

Generation and Optimization of Spectral Cluster Maps to Enable Data Fusion of CaSSIS and CRISM Datasets

by Michael Fernandes, Alexander Pletl, Nicolas Thomas, Angelo Pio Rossi and Benedikt Elser

Remote Sens. 2022, 14(11), 2524; https://doi.org/10.3390/rs14112524 - 25 May 2022

Cited by 2 | Viewed by 1743

Abstract

Four-band color imaging of the Martian surface using the Color and Stereo Surface Imaging System (CaSSIS) onboard the European Space Agency’s ExoMars Trace Gas Orbiter exhibits a high color diversity in specific regions. Not only is the correlation of color diversity maps with local morphological properties desirable, but mineralogical interpretation of the observations is also of great interest. The relatively high spatial resolution of CaSSIS data mitigates its low spectral resolution. In this paper, we combine the broad-band imaging of the surface of Mars, acquired by CaSSIS with hyperspectral data from the Compact Reconnaissance Imaging Spectrometer (CRISM) onboard NASA’s Mars Reconnaissance Orbiter to achieve a fusion of both datasets. We achieve this using dimensionality reduction and data clustering of the high dimensional datasets from CRISM. In the presented research, CRISM data from the Coprates Chasma region of Mars are tested with different machine learning methods and compared for robustness. With the help of a suitable metric, the best method is selected and, in a further step, an optimal cluster number is determined. To validate the methods, the so-called “summary products” derived from the hyperspectral data are used to correlate each cluster with its mineralogical properties. We restrict the analysis to the visible range in order to match the generated clusters to the CaSSIS band information in the range of 436–1100 nm. In the machine learning community, the so-called UMAP method for dimensionality reduction has recently gained attention because of its speed compared to the already established t-SNE. The results of this analysis also show that this method in combination with the simple K-Means outperforms comparable methods in its efficiency and speed. The cluster size obtained is between three and six clusters. Correlating the spectral cluster maps with the given summary products from CRISM shows that four bands, and especially the NIR bands and VIS albedo, are sufficient to discriminate most of these clusters. This demonstrates that features in the four-band CaSSIS images can provide robust mineralogical information, despite the limited spectral information using semi-automatic processing. Full article

(This article belongs to the Special Issue Planetary Exploration Using Remote Sensing)

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20 pages, 14090 KiB

Open AccessArticle

Recomputation and Updating of MOLA Geolocation

by Haifeng Xiao, Alexander Stark, Hao Chen and Jürgen Oberst

Remote Sens. 2022, 14(9), 2201; https://doi.org/10.3390/rs14092201 - 05 May 2022

Cited by 3 | Viewed by 1689

Abstract

The Mars Orbiter Laser Altimeter (MOLA) Precision Experiment Data Records (PEDR) serve as the geodetic reference of Mars. However, these MOLA footprints were geolocated using outdated auxiliary information that dates back to 2003. In this study, we recompute the MOLA PEDR footprint locations and investigate the impact of the updated spacecraft orbit model and Mars rotational model on MOLA’s geolocation. We observe quasi-exponential increases near the poles of up to 30 m in the recomputation residuals for the nadir profiles. Meanwhile, we demonstrate that limitations exist in the stored MOLA PEDR attitude records, which can shift the footprint up to hundreds of meters laterally and several meters radially. The usage of the Navigation and Ancillary Information Facility (NAIF)-archived attitude information instead can circumvent this issue and avoid the approximation errors due to discrete samplings of the attitude information used in geolocation by the PEDR dataset. These approximation errors can be up to 60 m laterally and 1 m radially amid controlled spacecraft maneuvers. Furthermore, the incorporation of the updated spacecraft orbit and Mars rotational model can shift the MOLA profiles up to 200 m laterally and 0.5 m radially, which are much larger in magnitude than the aforementioned dramatic increases near the poles. However, the shifted locations of the reprocessed profiles are significantly inconsistent with the PEDR profiles after the global cross-over analysis. Full article

(This article belongs to the Special Issue Planetary Exploration Using Remote Sensing)

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18 pages, 43012 KiB

Open AccessArticle

An Investigation on the Morphological and Mineralogical Characteristics of Posidonius Floor Fractured Lunar Impact Crater Using Lunar Remote Sensing Data

by Imen Ben Salem, Manish Sharma, P. R. Kumaresan, A. Karthi, Fares M. Howari, Yousef Nazzal and Cijo M. Xavier

Remote Sens. 2022, 14(4), 814; https://doi.org/10.3390/rs14040814 - 09 Feb 2022

Cited by 2 | Viewed by 2993

Abstract

Lunar floor-fractured craters (FFCs) are a distinguished type of crater found on the surface of the Moon with radial, concentric, and/or polygonal fractures. In the present study, we selected the Posidonius FCC to explore the mineralogy, morphology and tectonic characteristics using remote sensing datasets. The Posidonius crater is vested with a wide moat of lava separating the crater rim inner wall terraces from the fractured central floor. Lunar Reconnaissance Orbiter’s (LRO) images and Digital Elevation Model (DEM) data were used to map the tectonics and morphology of the present study. The Moon Mineralogy Mapper (M³) data of Chandrayaan-1 were used to investigate the mineralogy of the region through specified techniques such as integrated band depth, band composite and spectral characterization. The detailed mineralogical analysis indicates the noritic-rich materials in one massif among four central peak rings and confirm intrusion (mafic pluton). Spectral analysis from the fresh crater of the Posidonius moat mare unit indicates clinopyroxene pigeonite in nature. Integrated studies of the mineralogy, morphology and tectonics revealed that the study region belongs to the Class-III category of FFCs. The lithospheric loading by adjacent volcanic load (Serenitatis basin) generates a stress state and distribution of the fracture system. Full article

(This article belongs to the Special Issue Planetary Exploration Using Remote Sensing)

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Review

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58 pages, 16729 KiB

Open AccessReview

Remote Sensing and Data Analyses on Planetary Topography

by Jungrack Kim, Shih-Yuan Lin and Haifeng Xiao

Remote Sens. 2023, 15(12), 2954; https://doi.org/10.3390/rs15122954 - 06 Jun 2023

Cited by 1 | Viewed by 3403

Abstract

Planetary mapping product established by topographic remote sensing is one of the most significant achievements of contemporary technology. Modern planetary remote sensing technology now measures the topography of familiar solid planets/satellites such as Mars and the Moon with sub-meter precision, and its applications extend to the Kuiper Belt of the Solar System. However, due to a lack of fundamental knowledge of planetary remote sensing technology, the general public and even the scientific community often misunderstand these astounding accomplishments. Because of this technical gap, the information that reaches the public is sometimes misleading and makes it difficult for the scientific community to effectively respond to and address this misinformation. Furthermore, the potential for incorrect interpretation of the scientific analysis might increase as planetary research itself increasingly relies on publicly accessible tools and data without a sufficient understanding of the underlying technology. This review intends to provide the research community and personnel involved in planetary geologic and geomorphic studies with the technical foundation of planetary topographic remote sensing. To achieve this, we reviewed the scientific results established over centuries for the topography of each planet/satellite in the Solar System and concisely presented their technical bases. To bridge the interdisciplinary gap in planetary science research, a special emphasis was placed on providing photogrammetric techniques, a key component of remote sensing of planetary topographic remote sensing. Full article

(This article belongs to the Special Issue Planetary Exploration Using Remote Sensing)

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Other

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15 pages, 36345 KiB

Open AccessTechnical Note

A Remote Sensing Perspective on Mass Wasting in Contrasting Planetary Environments: Cases of the Moon and Ceres

by Lydia Sam and Anshuman Bhardwaj

Remote Sens. 2022, 14(4), 1049; https://doi.org/10.3390/rs14041049 - 21 Feb 2022

Cited by 1 | Viewed by 2273

Abstract

Mass wasting, as one of the most significant geomorphological processes, contributes immensely to planetary landscape evolution. The frequency and diversity of mass wasting features on any planetary body also put engineering constraints on its robotic exploration. Mass wasting on other Solar System bodies shares similar, although not identical, morphological characteristics with its terrestrial counterpart, indicating a possible common nature for their formation. Thus, planetary bodies with contrasting environmental conditions might help reveal the effects of the atmosphere, subsurface fluids, mass accumulation/precipitation, and seismicity on mass wasting, and vice versa. Their relative positions within our Solar System and the environmental and geophysical conditions on the Moon and the dwarf planet Ceres are not only extremely different from Earth’s but from each other too. Their smaller sizes coupled with the availability of global-scale remote sensing datasets make them ideal candidates to understand mass wasting processes in widely contrasting planetary environments. Through this concept article, we highlight several recent advances in and prospects of using remote sensing datasets to reveal unprecedented details on lunar and Cerean mass wasting processes. We start with briefly discussing several recent studies on mass wasting using Lunar Reconnaissance Orbiter Camera (LROC) data for the Moon and Dawn spacecraft data for Ceres. We further identify the prospects of available remote sensing data in advancing our understanding of mass wasting processes under reduced gravity and in a scant (or absent) atmosphere, and we conclude the article by suggesting future research directions. Full article

(This article belongs to the Special Issue Planetary Exploration Using Remote Sensing)

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