Automated identification of basalt spectra in Clementine lunar data

Antonenko, I.; Osinski, G. R.

doi:10.1016/j.pss.2011.02.007

Cited by 3 publications

(4 citation statements)

References 14 publications

(21 reference statements)

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“…3). Previous studies proposed that the solar incidence angles can affect small craters' detection and measurement (Ostrach et al 2011;Antonenko et al 2013). To examine this, we compared numerous NAC images of the same area taken with different incidence angles.…”

Section: The Identification Of Dark-haloed Cratersmentioning

confidence: 99%

The subsurface structure and stratigraphy of the Chang’E-4 landing site: orbital evidence from small craters on the Von Kármán crater floor

Qiao

Zhang

et al. 2020

Res. Astron. Astrophys.

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Chang’E-4 (CE-4) successfully landed on the floor of the Von Kármán crater within the South Pole-Aitken basin (SPA). One of its scientific objectives is to determine the subsurface structure and the thickness of lunar regolith at the landing site and along the traverse route of the Yutu-2 rover. Using orbital data, we employed small craters (diameters <1 km) on the floor of the Von Kármán crater as probes to investigate the subsurface structure and stratigraphy of the CE-4 landing site. In this study, 40 dark-haloed craters that penetrate through the surface Finsen ejecta and excavate underlying mare deposits were identified, and 77 bright ray craters that expose only the underlying fresh materials but do not penetrate through the surface Finsen ejecta were found. The excavation depths of these craters and their distances from the Finsen crater center were calculated, and the thickness distribution of Finsen ejecta on the Von Kármán floor was systematically investigated. The boundary between Finsen ejecta and underlying mare basalt at the CE-4 landing site is constrained to a depth of 18m.We have proposed the stratigraphy for the CE-4 site and interpreted the origins of different layers and the geological history of the Von Kármán crater. These results provide valuable geological background for interpreting data from the Lunar Penetrating Radar (LPR) and Visible and Near-infrared Imaging Spectrometer (VNIS) on the Yutu-2 rover. The CE-4 landing site could provide a reference point for crater ejecta distribution and mixing with local materials, to test and improve ejecta thickness models according to the in situ measurements of the CE-4 LPR.

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Section: The Identification Of Dark-haloed Cratersmentioning

confidence: 99%

The subsurface structure and stratigraphy of the Chang’E-4 landing site: orbital evidence from small craters on the Von Kármán crater floor

Qiao

Zhang

et al. 2020

Res. Astron. Astrophys.

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“…A. Giguere et al, , 2006Hawke et al, 2005). From these criteria, a higher iron content ejecta has been proposed as the most robust identifier of DHCs (Antonenko, 2013).…”

Section: Previously Proposed Cryptomaria Distributionmentioning

confidence: 99%

“…DHCs are traditionally identified by having a darker ejecta pattern than the surrounding terrain, however, previous work has also used the maturity of the soils, the iron content of the ejecta, the symmetry of their halo, and the presence of melts as identifiers (Bell & Hawke, 1984; T. A. Giguere et al., 2003, 2006; Hawke et al., 2005). From these criteria, a higher iron content ejecta has been proposed as the most robust identifier of DHCs (Antonenko, 2013). Because of the different and somewhat incompatible criteria used to identify DHCs, different data sets of DHCs exist and the compilation of these data sets into a global one is challenging.…”

Section: Introductionmentioning

confidence: 99%

“…Values of albedo, rock abundance, and roughness of the lunar surface are indistinguishable between cryptomare deposits and non‐volcanic light plains, limiting the use of these surface properties to quantify cryptomaria (Whitten & Head, 2015). Robust geologic evidence of cryptomaria relies on the presence of dark halo craters (DHC) (Antonenko, 2013; Whitten & Head, 2015). These craters excavate the underlying cryptomare layer and expose volcanic material as part of their ejecta.…”

Section: Introductionmentioning

confidence: 99%

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Global Distribution and Volume of Cryptomare and Visible Mare on the Moon From Gravity and Dark Halo Craters

Izquierdo,

Sori,

Checketts

et al. 2024

JGR Planets

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The present‐day distribution of mare basalts on the Moon is an important constraint on the timing, duration, and flux of volcanism on the Moon. In this work, we find the global distribution of visible mares and cryptomares using the effective density (ρeff) of the Moon, which is sensitive to the vertical density distribution of the crust. We compute ρeff using the Gravity Recovery and Interior Laboratory (GRAIL) data and the Lunar Orbiter Laser Altimeter (LOLA) topography data. We apply this ρeff approach to the search of cryptomare for the first time, and we use a higher resolution grid and larger search area to constrain visible mare thicknesses compared to previous work. We use a Bayesian approach to find the distribution of mare thicknesses and density gradients of the underlying crust that is consistent with the localized ρeff. Assuming a bulk density of the mare basalts of 3,460 kg/m3, we find a mean visible mare thickness of km which is consistent with previous work. We find a candidate cryptomare volume of km3 representing more than half of the total mare volume on Moon. This volume is consistent with the higher end of the previously proposed values. Finally, we search for dark halo craters (DHC) globally to obtain geologic evidence of cryptomares and find 258 craters. Our results are consistent with extensive ancient volcanism, which explains the previously identified discrepancy between the early high volcanic flux predicted by thermal models of the Moon and the dearth of ancient volcanic deposits currently exposed.

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A multispectral geological study of the Schrödinger impact basin

et al. 2013

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Schrödinger basin is a well-preserved peak-ring basin located on the lunar farside, along the rim of the much larger South Pole – Aitken (SPA) basin. The relatively young age (Lower Imbrian series, or 3.8 Ga) of this basin makes it an ideal site to study the geology of peak-ring basins in general, and the geological history of SPA specifically. Impact materials still recognizable include a well-defined crater rim, wall terraces, quasi-circular peak ring, and interior and exterior melt units. A small pyroclastic deposit fills a portion of the basin floor, along with several mare patches. This study uses Clementine multispectral ultraviolet–visible (UV–VIS) data, and a limited set of higher spectral resolution Chandrayaan-1 Moon Mineralogy Mapper (M3) data, as well as radar, camera, and topography data from the Lunar Reconnaissance Orbiter to better understand Schrödinger’s geology. Sampled spectral profiles and linear unmixing models applied to the Clementine data indicate there is a heterogeneous distribution of both anorthositic and basaltic materials in the crater floor. M3 data further validates this observation, and the high spectral resolution shows that most of the mafic content is dominated by pyroxene. These results challenge the traditional assumption that Schrödinger was formed in mostly highland terrain. Our assessment brings forth a new understanding regarding the placement of Schrödinger within SPA and the role SPA impact materials played in shaping the composition of Schrödinger.

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Automated identification of basalt spectra in Clementine lunar data

Cited by 3 publications

References 14 publications

The subsurface structure and stratigraphy of the Chang’E-4 landing site: orbital evidence from small craters on the Von Kármán crater floor

The subsurface structure and stratigraphy of the Chang’E-4 landing site: orbital evidence from small craters on the Von Kármán crater floor

Global Distribution and Volume of Cryptomare and Visible Mare on the Moon From Gravity and Dark Halo Craters

A multispectral geological study of the Schrödinger impact basin

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