Other
Scientific paper
Jan 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999nvm..conf....8c&link_type=abstract
Workshop on New Views of the Moon 2: Understanding the Moon Through the Integration of Diverse Datasets, p. 8
Other
Craters, Imagery, Lunar Maria, Lunar Surface, Lunar Topography, Meteorite Craters, Relief Maps, Topography, Lunar Geology, Selenology, Selenography, Lunar Maps, Moon, Clementine Spacecraft, Ejecta, Laser Altimeters, Pixels, Spatial Resolution, Structural Basins, Photogrammetry
Scientific paper
Several digital elevation models (DEMs) have been produced at a scale of 1km/pixel and covering approximately one-fifth of the lunar surface. These were produced mostly by semiautomatically matching the stereo available between Clementine UV/VIS images, although some localized DEMs have been produced by applying this technique to Apollo Metric stereo pairs, or by digitizing an existing Apollo Metric contour map. The DEMS that result from Clementine UV/VIS images, although Of Poorer height accuracy (1300-600 in for a single matched point) than the Clementine laser altimeter point measurements (<+/-100 m), do provide considerably higher spatial resolution (e.g., every kilometer vs. every tens of kilometers) and allow topography in the polar regions to be determined. Nadir-pointing Clementine UV-VIS stereo pairs are automatically stereo matched using a patch-based matcher and fed through A stereo intersection camera model to yield a digital terrain model (DTM) of longitude, latitude, and height points. The DTM for each stereo pair is then replotted and interpolated to form map-projected DEM tiles. The DEM files can then be fitted to absolute height laser altimeter points, or iteratively to each other, to form a DEM mosaic. Uncertainties in UV-VIS camera pointing and the need to accumulate a sufficiently good topographic S/N ratio necessitates the use of 1 km pixels for the UV-VIS derived DEMs. For Apollo Metric stereo, an internal camera geometry correction and a full photogrammetric block adjustment must be performed using ground- control points to derive a DEM. The image scale of Apollo Metric, as well as the stereo angle, allow for a DEM with 100 m pixels and a height accuracy of +/- 25m. Apollo Metric imagery had previously been used to derive contour maps for much of the lunar equatorial regions; however, to recover this information in digital form these maps must be digitized. Most of the mare areas mapped contain noticeable topographic noise. This results from the stereo matcher failing in regions of low texture and contrast. Below is a summary of the regions for which DEMs have been generated, and some of the features visible in each (heights are referenced to a 1738km radius sphere): Apollo 15 landing site (1E-7E,20N-30N). Features include Hadley Rille (just visible) and several mountains. Apollo 17 landing site (30.0E-31.5E, 19.5N-21.0N). This DEM was derived by digitizing contours from a map. Alpine Valley (2W-8E, 47N-51N), The valley and Trouvelot crater are visible. Topography ranges from 1 km to -4 km. The valley walls are <1 km high. Aristarchus (60W-40W,20N-30N). Features visible include Aristarchus craters, Vallis Schroteri, and the craters Herodotus, Schiaparelli, and Prinz. Copernicus Crater (30W-10W, 0N-20N). Features visible include Montes Carpatus and the craters Copernicus, Eratosthenes, Reinhold, and Tobias Mayer. Giordano Bruno Crater (101 E-106E, 33N-38N). This DEM reveals about 60% of the crater interior. Kepler Crater (38W, 8N). Using this DEM a perspective view of this crater has been produced with a USGS color-ratio map overlaid. Korolev Basin (I 75W-160W, 10S-20N). Seventy-five percent of the Korolev basin is present in this DEM together with a pre-Nectarian basin the size of Korololev just to the north. The topography in this DEM ranges from 0 km to 9.6 km. Named craters visible include Mach, McMath, Icarus, and Tsander. Luna 9/13 landing site (70W-60W, 0N-30N). The topographic range is from about 0 km to about 4.5 km, the latter being on the floor of Hevelius A crater. Mare Crisium (50E-70E, 0N-20N). This DEM covers the lower half of the basin and surrounding highlands. The topographic range is from +3 km to -5 km. Several protruding floor crater rims are visible on the basin floor (e.g., Picard, Yerkes, and Lick). Mare Orientate (120W-75W, 40S-0N). This area was covered well in stereo, and a regional north-south slope is detectable across the basin. The topography varies from +6 km on the western rim to -5 km on the bottom of Maunder crater. Three rings of the basin are clearly visible in the topography. Mare Serenitatis (1OE-40E,1ON-40N). Highland areas are well depicted in the DEM, as are craters Bessel, Dawes, Le Monier, Menelaus, Plinius, Posidonius, and Ross. North polar region (60deg -90 deg). An analysis of this DEM revealed the newly discovered Sylvester-Nansen pre-Nectarian impact basin (300-400 km diameter, centered on 45E, 83N). The Schwarzchild and Be'lkovich basins are clearly visible, as is the northern extent of the Imbrium basin. Several secondary ejecta scour marks are present in the topography and spread out radially from Mare Imbrium. The crater Hayn contains a north-south running graben which bisects its central peaks. Saha crater area (90E-105E, 5S-5N). Stereo imagery is missing in the center of this region. Schickard (60W-50W, 50S-40S). The floor interior craterlets and surrounding highlands are clearly visible. Sinus Iridum (40W-30W, 30N-50N). South polar region (90S-60S). An analysis of this DEM has revealed two newly discovered pre-Nectarian impact basins (Schrodinger-Zeeman, 250 km in diameter, centered on 165W, 81S, and 330 km diameter Bailly-Newton, centered on 57W, 73S). Several other prominent basins are visible, including the southern half of the South Pole Aitken (SPA) Basin, Bailly, Schrodinger, part of Clavius, and the Amundsen-Ganswindt Basin. The topographic range in this DEM is considerably greater than the north polar DEM due to the presence of the SPA topgraphy. Tsiolkovsky(124E,19S). In this DEM the western flanks of Tsiolkovsky are shown in great detail. Tycho (20W-0W, 50S-40S). This DEM shows Tycho crater and its surroundings as well as the northern interior of Maginus Crater. Original document contains additional information
Cook Anthony C.
Robinson Mark S.
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