Derivation of elemental abundance maps at intermediate resolution from optical interpolation of lunar prospector gamma-ray spectrometer data

Shkuratov, Yuriy; Kaydash, V. G.; Stankevich, D. G.; Starukhina, L. V.; Pinet, P.; Chevrel, S.; Daydou, Y.

doi:10.1016/j.pss.2005.07.001

Cited by 47 publications

(48 citation statements)

References 29 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Comparison of TiO 2 abundance determinations based on Lunar Prospector neutron spectrometer data and derived with the Lucey method indicate that the latter underestimates abundances by several weight per cent in absolute or several hundred percent in a relative sense for mare regions with "anomalously" low reflectances and flat spectral continua (Gillis et al 2001;Elphic et al 2002;Shkuratov et al 2005). The cause of this discrepancy is not known, but may be related to petrography (Gillis et al 2001;Elphic et al 2002).…”

Section: Discussionmentioning

confidence: 99%

Albedo–color distribution on Mercury

Warell¹,

Valegård²

2006

A&A

View full text Add to dashboard Cite

Aims. The variation of albedo and color of Mercury's surface is studied with disk-resolved image data obtained at six evenly spaced wavelengths in the optical to near infrared wavelength range (447-944 nm) with the 1-m Swedish Solar Telescope on La Palma in April, 2003. Methods. Disk images have been modeled and photometrically normalized with the light scattering theory of Hapke to derive albedocolor properties of a poorly known region (unimaged by Mariner 10) of Mercury's surface between longitudes 210• W and 270• W. Maps of relative abundances of ferrous iron, titanium and optical maturation are derived on the basis of a feldspathic model for the crustal composition and previous results for the Moon, assuming the validity of the general maturation model for mafic silicate regoliths of atmosphereless bodies. Results. The albedo-color scatterplot distributions of Mercury's surface are uniform with respect to wavelength in the near-ultraviolet to near-infrared due to the absence of strong absorption bands in the reflectance spectrum. The extents of the distributions are less than for the global Moon and similar to that of the lunar farside, which is related to the relatively subdued color contrasts of Mercury's primarily feldspathic surface. At the attained 500-km spatial resolution scale, these maps do not indicate the existence of surface regions chemically similar to the lunar maria, which have a high FeO and TiO 2 content. Variations in abundances of ferrous iron and titanium are shown to be less than for the global Moon and similar to the lunar farside at the same spatial scale. Optically bright regions on Mercury are less mature and less opaque than their surroundings consistent with geologically recent immature crater ejecta, while localized dark regions generally have intermediate maturities and iron abundances and higher-than-average titanium abundances. The smaller relative intensity range of spatial variations of spectral parameters in the near infrared compared to the near ultraviolet may imply that relative abundance variations in ferrous iron are smaller than variations in opaque minerals. Conclusions. The results reinforce the similar natures of the Mariner 10-imaged and the poorly known hemispheres of Mercury, as well as their superficial similarity to the lunar farside, and demonstrate that geological interpretation of ground-based observations of albedo features on Mercury is possible.

show abstract

Section: Discussionmentioning

confidence: 99%

Albedo–color distribution on Mercury

Warell¹,

Valegård²

2006

A&A

View full text Add to dashboard Cite

show abstract

“…In combination with elemental abundance maps of low resolution e.g. obtained by the Lunar Prospector Gamma Ray Spectrometer (LP GRS) (Lawrence et al, 1998), the spectral parameter maps allow for the construction of high-resolution maps of the abundances of the main refractory elements Al, Mg, Ca, Fe and Ti Bhatt et al, 2015;Shkuratov et al, 2005). The strength of the absorption around 3 µm related to hydroxyl (OH) can also be mapped (Pieters et al, 2009b).…”

Section: Remote Sensing Methods To Be Appliedmentioning

confidence: 99%

Korean Lunar Lander – Concept Study for Landing-Site Selection for Lunar Resource Exploration

Kim

Wöhler

et al. 2016

Int. Arch. Photogramm. Remote Sens. Spatial Inf. Sci.

View full text Add to dashboard Cite

ABSTRACT:As part of the national space promotion plan and presidential national agendas South Korea's institutes and agencies under the auspices of the Ministry of Science, Information and Communication Technology and Future Planning (MSIP) are currently developing a lunar mission package expected to reach Moon in 2020. While the officially approved Korean Pathfinder Lunar Orbiter (KPLO) is aimed at demonstrating technologies and monitoring the lunar environment from orbit, a lander -currently in pre-phase A -is being designed to explore the local geology with a particular focus on the detection and characterization of mineral resources. In addition to scientific and potential resource potentials, the selection of the landing-site will be partly constrained by engineering constraints imposed by payload and spacecraft layout. Given today's accumulated volume and quality of available data returned from the Moon's surface and from orbital observations, an identification of landing sites of potential interest and assessment of potential hazards can be more readily accomplished by generating synoptic snapshots through data integration. In order to achieve such a view on potential landing sites, higher level processing and derivation of data are required, which integrates their spatial context, with detailed topographic and geologic characterizations. We are currently assessing the possibility of using fuzzy c-means clustering algorithms as a way to perform (semi-) automated terrain characterizations of interest. This paper provides information and background on the national lunar lander program, reviews existing approaches -including methods and tools -for landing site analysis and hazard assessment, and discusses concepts to detect and investigate elemental abundances from orbit and the surface. This is achieved by making use of manual, semi-automated as well as fully-automated remote-sensing methods to demonstrate the applicability of analyses. By considering given boundary conditions, concrete procedures for determining potential landing sites of the Korean lunar lander could be proposed.

show abstract

“…The FeO+TiO 2 content in lunar regolith has been studied based on optical reflectance of lunar surface and laboratory measurement of the Apollo samples. For example, global imaging data were collected by an ultraviolet visible (UVVIS) camera in Clementine mission, and FeO and TiO 2 contents were derived from five-band multispectral optical data [12], and the γ-ray spectrometer of Lunar Prospector [17,18]. The spatial resolution of optical remote sensing is about 100-325 m, and the FeO+TiO 2 content is derived within 1 μm in the lunar surface.…”

Section: Validation and Calibration Of Brightness Temperaturementioning

confidence: 99%

Analysis of microwave brightness temperature of lunar surface and inversion of regolith layer thickness: Primary results of Chang-E 1 multi-channel radiometer observation

Jin

2010

Sci. China Inf. Sci.

View full text Add to dashboard Cite

In China's first lunar exploration project, Chang-E 1 (CE-1), a multi-channel microwave radiometer was aboard the satellite, with the purpose of measuring microwave brightness temperature from lunar surface and surveying the global distribution of lunar regolith layer thickness. In this paper, the primary 621 tracks of swath data measured by Chang-E 1 microwave radiometer from November 2007 to February 2008 are collected and analyzed. Using nearest neighbor interpolation based on the sun incidence angle in observations, global distributions of microwave brightness temperature from lunar surface at lunar daytime and nighttime are constructed. Using the three-layer model (the top dust-soil, regolith and underlying rock media) for microwave thermal emission of lunar surface, the measurements of brightness temperature and dependence upon latitude, frequency and FeO+TiO 2 content, etc. are discussed. On the basis of the ground measurements at Apollo landing sites, the observed brightness temperature at these locations are validated and calibrated by numerical three-layer modeling. Using the empirical dependence of physical temperature upon the latitude verified by the measurements at Apollo landing sites, the global distribution of regolith layer thickness is then inverted from the brightness temperature data of CE-1 at 3 GHz channel. Those inversions at Apollo landing sites are compared with the Apollo in situ measurements. Finally, the statistical property of regolith thickness distribution is analyzed and discussed. KeywordsChang-E 1, multi-channel brightness temperature, Apollo landing site, physical temperature, inversion of regolith layer thickness CitationFa W Z, Jin Y Q. Analysis of microwave brightness temperature of lunar surface and inversion of regolith layer thickness: Primary results of Chang-E 1 multi-channel radiometer observation.

show abstract

Derivation of elemental abundance maps at intermediate resolution from optical interpolation of lunar prospector gamma-ray spectrometer data

Cited by 47 publications

References 29 publications

Albedo–color distribution on Mercury

Albedo–color distribution on Mercury

Korean Lunar Lander – Concept Study for Landing-Site Selection for Lunar Resource Exploration

Analysis of microwave brightness temperature of lunar surface and inversion of regolith layer thickness: Primary results of Chang-E 1 multi-channel radiometer observation

Contact Info

Product

Resources

About