Photogrammetric analysis of clementine multi-look angle images obtained near mare orientale

Oberst, J.; Zhang, W.; Cook, A. C.; Jaumann, R.; Duxbury, T. C.; Wewel, F.; Uebbing, Robert; Scholten, F.; Albertz, Jörg

doi:10.1016/s0032-0633(96)00060-8

Cited by 15 publications

(5 citation statements)

References 10 publications

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“…With this study of the Apollo 17 site we have only scratched the surface of what could be done in the investigation of local geologic features and formations combining full‐resolution CSR data along with existing high‐resolution topography from Apollo data and more recent Earth‐based radar observations [ Margot et al , 1999, 2000]. Additional topographic data sets for the Moon are available at resolutions below that of the CSR data (∼500–1000 m/pixel [ Oberst et al , 1996, 1997; Cook et al , 1996, 2000]). We have shown that topographic‐photometric corrections maximize the amount of spectral information obtained from orbital color mapping of the Moon.…”

Section: Discussionmentioning

confidence: 99%

Apollo 17 landing site: Topography, photometric corrections, and heterogeneity of the surrounding highland massifs

Robinson

Jolliff²

2002

J.‐Geophys.‐Res.

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[1] A high-resolution digital elevation model for the Apollo 17 landing site (20°N, 31°E) and surrounding region is used to correct the photometry of Clementine ultraviolet-visible multispectral data to standard viewing and illumination geometry on a pixel-by-pixel basis. FeO and TiO 2 concentrations were derived from these topographicphotometrically corrected data, and steep-sloped highland massifs are used to assess the magnitude of the effects of the correction. The effects are significant, yielding errors as high as 5 wt% FeO and 4 wt% TiO 2 (absolute) on 30°slopes. The magnitude of the correction varies for Sun-facing versus anti-Sun slopes, with greater changes on anti-Sun slopes. Because most of the Apollo 17 sample stations were on surfaces with low slope values (<5°), the topography has only a small effect on the use of the Apollo 17 site for calibration of FeO and TiO 2 parameters. Topographically corrected data and derived compositional information are used to show accurately the variation in composition of the highland units such as the massifs and the Sculptured Hills on a fine scale. Massif compositions are consistent with mixtures of noritic impact melt and feldspathic granulitic material, plus variable amounts of high-Ti basalt on flanks at low elevations and pyroclastic deposits at high elevations, as surmised from previous studies. An unexpected enrichment in FeO at intermediate elevations in some places where massif surfaces have not been covered by mass wasting of impact-melt rich material signals an older volcanic component not previously recognized. This component may be correlative with an old, high-plains volcanic unit exposed northeast of the landing site and north of the Sculptured Hills. Downslope movement of regolith on steep slopes appears to have resulted in compositional or grain size sorting, leading to an apparent enrichment in FeO and TiO 2 from volcanic glass in valleys and draws. The Sculptured Hills have highly variable compositions, ranging from feldspathic patches to exposures of mafic rocks. A strong but localized mafic anomaly within the Sculptured Hills may be a small, postbasin volcanic feature consisting of very low Ti basalt.

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Section: Discussionmentioning

confidence: 99%

Apollo 17 landing site: Topography, photometric corrections, and heterogeneity of the surrounding highland massifs

Robinson

Jolliff²

2002

J.‐Geophys.‐Res.

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“…The DLR group determined that the crater Kopff (17.5°S, 270.6°W) is about 2.2 km deep and crater Kopff E is 3.1 km deep with respect to a lunar reference sphere of 1737.4 km in radius. Height accuracy on the DEMs created by the DLR matcher for this region of the Moon is ±0.100 km [ Cook et al , 1996; Oberst et al , 1996]. The DLR measurements are consistent (within the error) with those from the DEM generated by SMTK, 2 and 2.9 km, respectively (±0.100 km).…”

Section: Application To Planetary Data and Error Assessmentmentioning

confidence: 69%

“…One of the special stereo sequences (with adjacent orbits of nadir‐pointing and off‐nadir images) was obtained along the eastern interior rim of Orientale Basin (20°S, 95°W). A DEM of this area was constructed previously using another stereo matcher [ Oberst et al , 1996], making it particularly useful for comparison with a DEM generated by SMTK.…”

Section: Application To Planetary Data and Error Assessmentmentioning

confidence: 99%

“…SMTK results were also compared to point results of a similar Clementine DEM constructed by the group at the Institute of Planetary Exploration as part of the Deutsches Zentrum für Luft‐ und Raumfahrt (DLR), which developed its own set of stereo image processing techniques [ Oberst et al , 1996, 1997]. The DLR group determined that the crater Kopff (17.5°S, 270.6°W) is about 2.2 km deep and crater Kopff E is 3.1 km deep with respect to a lunar reference sphere of 1737.4 km in radius.…”

Section: Application To Planetary Data and Error Assessmentmentioning

confidence: 99%

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Application of an adaptive least squares correlation algorithm for stereo matching planetary image data

et al. 2008

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[1] An adaptive least squares (ALS) correlation algorithm and a region-growing algorithm were implemented into a stereo-matching computer program. This program (referred to as the Stereo Matching Tool Kit (SMTK)) was designed specifically for the application to planetary image data. The ALS algorithm matches a patch of one image to the corresponding area in a second image. The matching procedure is an iterative process that minimizes the sum of the square differences between the two patches to determine an optimal set of transformation parameters. Successful matches are then used to predict potential match points for surrounding locations. Using potential match points in conjunction with the region-growing algorithm, a population of match points between the two images is determined. The stereo-matching process is initiated by using the ALS algorithm in conjunction with Spacecraft, Planet, Instrument, C-matrix, and Events (SPICE) information to automatically determine a set of seed points. SMTK was tested on two planetary image data sets: Mariner 10 and Clementine. SMTK-derived digital elevation models compare well with topography generated by an area-based stereo matcher requiring manual selection of seed points, analog stereo techniques, and photoclinometry.

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“…Frame-to-frame overlap of the UVVIS global dataset was leveraged (Cook et al 1996(Cook et al , 2000 to produce stereo-based topographic maps at resolutions of 2-5 km/pixel (Oberst et al 1996). Improving upon the lower resolution LIDAR topography, these data have revealed previously unknown ancient degraded basins improving our knowledge of cratering rates in the early solar system.…”

Section: Topography and Gravitymentioning

confidence: 99%

Advances in lunar science from the Clementine mission: A decadal perspective

Robinson

Riner

2005

J Earth Syst Sci

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The Clementine spacecraft orbited the Moon and acquired science data for 10 weeks in the Spring of 1994. During this time it collected global 11-band multispectral images and near global altimetry. Select areas of the Moon were imaged at 25 m/pixel in visible light and 60 m/pixel in thermal wavelengths. From these datasets a new paradigm for the evolution of the lunar crust emerged. The Moon is no longer viewed as a two-terrane planet, the Apollo samples were found not to represent the lunar crust as a whole, and the complexity of lunar crustal stratigraphy was further revealed. More than ten years later the Clementine datasets continue to significantly advance lunar science and will continue to do so as new measurements are returned from planned missions such as Chandrayaan, SELENE, and Lunar Reconnaissance Orbiter. This paper highlights the scientific research conducted over the last decade using Clementine data and summarizes the influence of Clementine on our understanding of the Moon.

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Photogrammetric analysis of clementine multi-look angle images obtained near mare orientale

Cited by 15 publications

References 10 publications

Apollo 17 landing site: Topography, photometric corrections, and heterogeneity of the surrounding highland massifs

Apollo 17 landing site: Topography, photometric corrections, and heterogeneity of the surrounding highland massifs

Application of an adaptive least squares correlation algorithm for stereo matching planetary image data

Advances in lunar science from the Clementine mission: A decadal perspective

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