Mare Deposits Identification and Feature Analysis in Mare Australe Based on CE‐2 CELMS Data

Meng, Zhiguo; Chen, S.B.; Zheng, Yongchun; Cheng, Weiming; Zhu, Yuqing; Cai, Zhanchuan; Zhang, Y. Z.; Cao, Wei; Hou, Lele

doi:10.1029/2019je006330

Cited by 9 publications

(19 citation statements)

References 47 publications

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“…Finally, the linear interpolation method is used to generate the TB maps at 3.0, 7.8, 19.35, and 37.0 GHz with a spatial resolution of 0.25 • × 0.25 • . This data pre-processing algorithm has been tested and works well in previously published papers [30,32,33,44,51].…”

Section: Tb Maps Generationmentioning

confidence: 86%

“…The CELMS data processing has been described in detail by Chan et al [50], Zheng et al [35,49], and Meng et al [30,33,51]. The same processing method is adopted in this study.…”

Section: Tb Maps Generationmentioning

confidence: 99%

“…In this study, the normalized TB (nTB), TB difference (dTB), and emissivity maps are applied to solve latitude-dependent TB variation issues [30,32,33,44,51]. Moreover, to better understand the TB performances, the geological units identified by Qian et al [2] are vectorized and overlain on the following generated maps.…”

Section: Proper Tb Maps Generationmentioning

confidence: 99%

“…In order to obtain the nTB maps, the standard TB values of every latitude are calculated [32,33,51]. Firstly, one TB is selected for every latitude on the conditions that the FTA, surface slope, and rock abundance are similar in all selected positions (from the JMARS, https://jmars.asu.edu/).…”

Section: Ntb Mapsmentioning

confidence: 99%

“…Then, a fitting curve is made according to the selected TB, and the fitted value is defined as the standard TB for the corresponding frequency and latitude. Finally, the nTB maps are generated using the TB divided by the standard TB of the latitude (Figure 4, noon; Figure 5, night) [33,51].…”

Section: Ntb Mapsmentioning

confidence: 99%

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Thermophysical Features of the Rümker Region in Northern Oceanus Procellarum: Insights from CE-2 CELMS Data

et al. 2020

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The Rümker region is located in the northern Oceanus Procellarum, which has been selected as the landing and sampling region for China’s Chang’e-5 (CE-5) mission. The thermophysical features of the mare units are studied in detail using the brightness temperature (TB) maps (TB, normalized TB, TB difference) derived from the CE-2 microwave radiometer data. The previously interpreted geological boundaries of the Rümker region are revisited in this study according to their TB behaviors: IR1, IR2, and IR3 Rümker plateau units are combined into one single unit (IR); and a hidden unit is found on the Mons Rümker; Mare basaltic units Im1 and Em1 are combined into Em1; and Em2 is more likely the extending of Im2. Each of the previous proposed landing sites and their scientific value are summarized and reevaluated. Based on this, four landing sites are recommended in order to maximize the scientific outcome of the CE-5 mission. We suggest that the Eratosthenian-aged Em4 and Em1 units as the top priority landing site for the CE-5 mission; the age-dating results will provide important clues concerning the thermal evolution of the Moon.

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Section: Tb Maps Generationmentioning

confidence: 86%

“…The CELMS data processing has been described in detail by Chan et al [50], Zheng et al [35,49], and Meng et al [30,33,51]. The same processing method is adopted in this study.…”

Section: Tb Maps Generationmentioning

confidence: 99%

Section: Proper Tb Maps Generationmentioning

confidence: 99%

Section: Ntb Mapsmentioning

confidence: 99%

Section: Ntb Mapsmentioning

confidence: 99%

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Thermophysical Features of the Rümker Region in Northern Oceanus Procellarum: Insights from CE-2 CELMS Data

et al. 2020

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A New Method for the Identification of Lunar Cryptomaria and Their Analysis in the Schiller‐Schickard Region

Jingran

Chen

et al. 2023

JGR Planets

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Cryptomaria play critical roles in elucidating the early thermal history of the Moon. In contrast with traditional dark halo impact crater (DHC) identification methods, this study focused on exposed rock (0.5%–29.54% rock abundance) surfaces as windows for cryptomare identification. We classified the lithology of these rock surfaces to find those that match mare basalt using major element oxide products based on data from the Diviner instrument aboard the Lunar Reconnaissance Orbiter (LRO) and by Lunar Prospector thorium products, in accordance with laboratory lithological classification criteria. Then, by combining the locations of 0.5%–29.54% rock abundance values with the lithologies, we created a map of exposed basaltic rock surfaces and 14 cryptomare candidate regions with dozens of closely spaced basaltic rock pixels were identified across the Moon. Among 14 candidate regions, 11 cryptomaria were consistent with results in literature (Whitten & Head, 2015a; https://doi.org/10.1016/J.ICARUS.2014.09.031) based on DHCs, and 3 cryptomaria were newly identified. In the Schiller‐Schickard region, we refined the boundaries of 18 individual cryptomare units using our rock analysis combined with LRO color shaded relief maps. A detailed analysis of the distribution, composition, area, depth, thickness, and volume and the morphological features of these 18 identified cryptomare units indicates that the basalt materials covered by the Orientale basin or other impact crater ejecta display variable thicknesses and discontinuous layers. These identified cryptomare units and their morphological features provide information on regional stratigraphy as well as on the thermal evolution of the Moon.

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Mineralogical Characterization of the Lunar South Polar Region: 1. The Artemis Exploration Zone

Moriarty,

Petro

2024

JGR Planets

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The lunar south pole is a region of focused scientific and exploration interest, with several crewed and robotic missions to this region planned within the next decade. Understanding the mineralogy of the region is essential to inform landing site characterization and selection and provides the key context for interpreting samples and in situ observations. At high latitudes, extreme illumination conditions (high phase angles) can negatively impact the data quality of orbital instruments. This is especially true for passive near‐infrared spectrometers such as the Moon Mineralogy Mapper (M3) and the Kaguya Spectral Profiler, which measure the spectral properties of the surface using reflected sunlight. Using Moon Mineralogy Mapper data, we observed that the south polar region is associated with a detectable mafic signature consistent with the presence of pyroxenes. The strongest mafic signatures are associated with the South Pole—Aitken Basin, suggesting that impact melt and basin ejecta from the lower crust and upper mantle are present within this region. This observation is validated in several ways: (a) comparisons between M3 data acquired during different mission phases, (b) comparisons between multiple spectral parameters sensitive to the presence of mafic minerals, (c) comparisons between the north and south lunar polar regions, and (d) comparisons with publicly available Kaguya polar mineralogy maps and Lunar Prospector elemental abundances. We also investigate the nature of an anomalous high‐albedo region within 2–3° of the south pole observed in Lunar Orbiter Laser Altimeter reflectance data exhibiting a spatially conflicting apparent FeO abundance pattern between several data sets.

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Mare Deposits Identification and Feature Analysis in Mare Australe Based on CE‐2 CELMS Data

Cited by 9 publications

References 47 publications

Thermophysical Features of the Rümker Region in Northern Oceanus Procellarum: Insights from CE-2 CELMS Data

Thermophysical Features of the Rümker Region in Northern Oceanus Procellarum: Insights from CE-2 CELMS Data

A New Method for the Identification of Lunar Cryptomaria and Their Analysis in the Schiller‐Schickard Region

Mineralogical Characterization of the Lunar South Polar Region: 1. The Artemis Exploration Zone

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