Reflectance spectra of analog basalts; implications for remote sensing of lunar geology

Anbazhagan, S.; Arivazhagan, S.

doi:10.1016/j.pss.2009.06.020

Cited by 26 publications

(9 citation statements)

References 21 publications

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“…Moreover, masking of the Fe 2+ plagioclase bands in rock spectra occurs when there are strong absorptions from ferrous iron in other minerals such as pyroxenes or olivine (Adams & Goullaud, 1978). Plagioclase occurrence then seems only to increase the albedo of a plagioclase‐bearing lithology (Anbazhagan & Arivazhagan, 2009), even though space weathering is able to affect the spectral features of plagioclase, reducing significantly the absorption bands (Lucey et al., 2000; Yamamoto et al., 2015). Similarly, the spectral characteristics of ilmenite is rather complex and variable and its reflectance spectra result generally very dark.…”

Section: Discussionmentioning

confidence: 99%

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: 99%

Spectral Analysis of Mare Ingenii Basin (Lunar Farside)

Salari,

Tognon,

Zambon

et al. 2023

JGR Planets

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“…The rock samples were A powdered sample provides increased albedo and depth of absorption bands. 7,[57][58][59][60] A powder sample provides a better contrasted spectral signature between albedo and absorption bands than a hand specimen. It is easier to use for the extraction of absorption bands from the spectra.…”

Section: Reflectance Spectral Studiesmentioning

confidence: 99%

“…The presence of pyroxene minerals in anorthosites provides diagnostic absorption features between 900 nm and 1000 nm in the IR region. 7 The absorption band centre systematically changes with the composition of iron, magnesium and calcium exchange in pyroxene minerals. 57,63,64 In the present case, the pyroxene mineral (diopside) in the anorthosite influences the absorption band centre.…”

Section: Samplementioning

confidence: 99%

“…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. 1,2,[8][9][10][11][12][13][14][15][16] Several workers have evaluated the high-resolution airborne imaging spectrometer for mapping mineralogical variations and correlated absorption features with various mineral compositions.…”

Section: Introductionmentioning

confidence: 99%

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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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“…The specific characteristic absorption Features at various wavelengths across the electromagnetic spectrum is mainly because of electronic transitions and vibrational processes (Burns, 1993). Because of the compositional structure of the mineral, the shape and strength of the characteristic absorption and the wavelength position varies across the spectrum (Kramer, 2010, Anbazhagan, 2009. Mineral mixing analysis of the lunar surface offers a platform to better understand the origin, crustal and overall evolution and geological history of the moon (Jin et al, 2013).…”

Section: Introductionmentioning

confidence: 99%

Mineral Mapping Using Chandrayaan-1 Hyperspectral (Hysi) Data From Mare Vaporum

Sayyad¹,

Mohammed²,

Deshmukh

2018

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

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<p><strong>Abstract.</strong> The imaging spectroscopy offers an opportunity to map and discriminate different minerals on the lunar surface which further helps to understand the origin, evolution process, and the crustal composition on the surface of the moon. Compositional mapping of the lunar surface is considered as a standard approach for mineral mapping. This paper reports surface mineralogy of the lunar surface from Mare Vaporum using Chandrayaan-1 Hyperspectral remotely sensed data from HySi sensor. False color composite is created using different band shaping algorithms like band strength; band curve and band tilt parameters at crucial wavelength for spatial analysis. The Spectral analysis has been done by deriving reflectance spectra at varying locations from the area under study. The Study shows the mineral map with different categories of minerals which are high-Ca pyroxene and/or olivine and low Ca-pyroxene. However because of the limited spectral coverage of HySi, data at the longer wavelengths required to discriminate among different group of minerals.</p>

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Reflectance spectra of analog basalts; implications for remote sensing of lunar geology

Cited by 26 publications

References 21 publications

Spectral Analysis of Mare Ingenii Basin (Lunar Farside)

Spectral Analysis of Mare Ingenii Basin (Lunar Farside)

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

Mineral Mapping Using Chandrayaan-1 Hyperspectral (Hysi) Data From Mare Vaporum

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