A lunar soil simulant (LSS-ISAC-1) for the lunar exploration programme of the Indian Space Research Organisation

Anbazhagan, S.; Venugopal, I.; Arivazhagan, S.; Chinnamuthu, M.; Paramasivam, C.R.; Nagesh, G.; Kannan, S.; Shamarao,; Babu, V. C.; Annadurai, M.; Muthukkumaran, Kasinathan; Rajesh, V.J.

doi:10.1016/j.icarus.2021.114511

Cited by 8 publications

(3 citation statements)

References 39 publications

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“…(2000) (different from the inner region where FeO is ∼10 wt%). These relatively low iron abundances are chemically comparable to the ejecta areas of the feldspathic highlands terrains (Jolliff et al., 2000), and could then represent the deeper crust of the anorthositic covering which dominates the lunar farside (and almost ∼80% of the entire lunar surface, Anbazhagan et al., 2021; Head, 1976; Pieters, 1986). Anorthositic crust is thought to be accumulated by plagioclase floatation after crystallization of the ancient magma ocean (Jolliff et al., 2000) and, along with Mg‐rich rocks such as gabbros, norites, and troctolites, constitute the lower crust of the Moon (Anbazhagan et al., 2021; Jolliff et al., 2000).…”

Section: Discussionmentioning

confidence: 97%

“…Indeed, the Ingenii basin is located within the outer border of the SPA basin, the deepest and the oldest impact basin in our Solar System, which likely exposed the lower lunar crust. M 3 data suggest a strong contribution of the mafic component in the basin, with dominant pyroxene minerals (and local olivine‐rich exposures; Yamamoto et al., 2012, 2023), likely representing the deeper section of the lunar crust dominated by gabbros, norites, and troctolites (Anbazhagan et al., 2021; Jolliff et al., 2000). Several hypotheses have been proposed to account for this mafic exposures, such as a huge collision that penetrated through the Moon's crust (Pieters et al., 1997; Yamamoto et al., 2012) or excavation of the mantle (Lemelin et al., 2019; Lucey et al., 1998; Melosh et al., 2014; Miljkovic et al., 2013; Nakamura et al., 2012; Petro & Jolliff, 2013; Potter et al., 2012; Yamamoto et al., 2010).…”

Section: Discussionmentioning

confidence: 99%

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Spectral Analysis of Mare Ingenii Basin (Lunar Farside)

Salari,

Tognon,

Zambon

et al. 2023

JGR Planets

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Mare Ingenii is a site of great interest for lunar geology as it is one of the few basaltic plains on the farside of the Moon. It is located within the outer edge of the South Pole‐Aitken basin, the largest and oldest impact basin in our Solar System. Mare Ingenii includes two large craters, Thomson and Thomson M, and a prominent swirl, a high‐albedo sinuous feature whose origin is still debated. We conducted spectral analysis on 28 selected regions of interest within Mare Ingenii, with the aim of inferring its mineralogy. We considered reflectance data acquired in the visible to near‐infrared spectral range by the Moon Mineralogy Mapper (M3) imaging spectrometer onboard the Chandrayaan‐1 mission, to derive a set of spectral parameters. Our results show wide compositional variability, with the dark material of the mare basaltic floor showing the centers of the Fe2+ absorption bands of the pyroxenes shifted toward long wavelengths (0.96–0.99 and 2.03–2.12 μm, respectively), consistent with the spectral characteristics of high‐Ca pyroxenes (as well as swirl material and intermediate albedo regions). In contrast, the bright material of the small surrounding craters shows Fe2+ absorption bands shifted toward short wavelengths (0.91–0.94 and 1.91–2.04 μm, respectively), more consistent with low‐Ca or Ca‐free pyroxenes. The obtained results suggest a mafic signature throughout the surface of Mare Ingenii, probably representative of the composition of the lower lunar crust.

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Section: Discussionmentioning

confidence: 97%

Section: Discussionmentioning

confidence: 99%

Spectral Analysis of Mare Ingenii Basin (Lunar Farside)

Salari,

Tognon,

Zambon

et al. 2023

JGR Planets

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“…3 Imaging spectroscopy has become a vital tool for remote compositional assessment of terrestrial as well as planetary bodies. 4,5 In this context, reflectance spectral studies were carried out to characterise lunar analogue material. 6,7 The high-resolution spectral data obtained through imaging spectrometers allow direct identification of materials based on their reflectance characteristics.…”

Section: Introductionmentioning

confidence: 99%

Reflectance spectra and AVIRIS-NG airborne hyperspectral data analysis for mapping ultramafic rocks in igneous terrain

Tamilarasan

Anbazhagan

Maheswaran

et al. 2022

J. Spectral Imaging

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The layered Sittampundi Anorthosite Complex is covered by mafic and ultramafic rocks including anorthosite, gabbro, pyroxenite and other igneous rocks. The ultramafic terrain has frequently undergone metamorphism. In the present study, laboratory spectral measurements were carried out from mafic, ultramafic and felsic rocks in the 350–2500 nm spectral range to characterise their diagnostic spectral features and for further utilisation for rock-type mapping. In 2016, the Sittampundi complex was covered by an AVIRIS-NG airborne survey jointly conducted by the Space Application Centre (SAC-ISRO) and Jet Propulsion Laboratory (NASA). The level-2 AVIRIS-NG data was obtained from SAC and used to interpret various rock types. ENVI 5.3 software was used for digital image processing of the AVIRIS-NG airborne hyperspectral data. The continuum-removed spectra of major rock types including anorthosite, meta-anorthosite, gabbro, meta-gabbro, pyroxenite, pegmatite, granite, gneiss and migmatite were critically analysed and their diagnostic absorption features correlated with chemistry and mineralogy. The AVIRIS-NG data analyses include bad band removal, minimum noise fraction transformation (MNF) and band combination. Out of various band combinations, the MNF composite images B456, B546 and B561 provided an enhanced output for the delineation of various rock types in the ultramafic terrain.

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