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The Eudoxus quadrangle is in the northeastern part of the Moon's nearside hemisphere. It is bordered on the west by Montes Caucasus, which form part of the main rim of the multi-ringed Imbrium basin (Hartmann and Kuiper, 1962), and on the southside by Mare Serenitatis, which occupies another large multi-ringed basin. South and East of the prominent crater Eudoxus elevations decrease and the rugged highland terrain becomes more subdued and covered by mare materials in the Serenitatis basin, Lucas Somniorum and Lucas Mortis.
The Langrenus quadrangle is on the east limb of the lunar nearside, at the southeast margin of Mare Fecunditatis. The crater Langrenus, about 140 km in diameter, is the most prominent feature. Rugged terra materials, scarred by craters of various sizes and ages, occupy much of the east half of the map area, and smooth mare material in the Frecunditatis basin dominate the west. Mare Spumans and other small irregular maria in the northeast are part of a belt of such maria concentric with Mare Crisium, which is centered approximately 500 km north of the quadrangle.
The application of stratigraphic and structural principles to geologic mapping of the moon from telescopic photographs has been discussed by Shoemaker (1962) and Shoemaker and Hackman (1962). Major geologic units are recognized by regional topographic and albedo differences. Pictures returned by Ranger, Surveyor, and Lunar Orbiter spacecraft show that a fragmental regolith, presumably produced by repeated impact and mass wasting, has formed on all but the very youngest of these units. In the Ptolemaeus quadrangle, ages assigned to the rock units are tentative and correlations with the major lunar time stratigraphic units whose type locatlites are in vicinity of Mare Imbrium are uncertian. Materials of each crater...
The Grimaldi quadrangle lies at the southwest margin of Oceanus Procellarum about 1000 km east of Orientale, the youngest of the lunar multi-ring basins. The distal ends of the ejecta blanket surrounding the Orientale basin partly cover the western third of the quadrangle. The relatively small, two-ring Grimaldi basin is in the northwest corner of the quadrangle, and the Humorum basin lies about 750 km to the southeast. A vestigal multi-ring basin mostly engulfed by mare appears to control the distribution of terra and mare craters Hansteen and Billy are on a northwest-trending topographic high which represents part of the ring system of this basin. Terra materials of distinctive texture, apparently unrelated to...
The Rima Hyginus region lies within the Mare Vaporum quadrangle (LAC 59). 7" from the center of the lunar earthside hemisphere, near several large impact basins. The Rima Hyginus region occupies a broad structural trough concentric with the Imbrium basin, which has especially controlled the geology of the area, Plains-forming materials cover most of the region, except for a belt of hilly terrain with about 600m of relief, to the north, and some isolated hills to the west. Numerous linear grabens and a chain of endogenic craters are the prominent structures; the region includes only three craters larger than 5 km in diameter.
The Tolstoj quadrangle in the equitorial region of Mercury contains the southern part of Caloris Planitia, which is the largest and best preserved basin seen by Mariner 10. This basin, about 1300 km in diameter, is surrounded by a discontinuous annulus of ejecta deposits of the Caloris Group (units cm, cn, co, cvl, and cvs) that are embayed and covered by broad expanses of smooth plains (unit ps). the southeast half of the quadrangle is dominated by ancient crater deposits (units c1, c2, and c3) by nondescript rolling to hummocky plains materials (units pi-ps). The ancient and degraded Tolstoj multiring basin, about 350km in diameter, is in the south-central part of the quadrangle. The large, well-preserved crater...
The Phoenicis Lacus quadrangle (named Lake of the Phoenix by Schiaparelli, 1877) includes some of the largest geologic features recognized on the terrestrial planets. Arsia and Pavonis Montes, (“South Spot” and “Middle Spot” of Marine 9) rise 18 and 17 km, respectively, above the surrounding plateau to an elevation large volcanoes Ascraeus and Olympus Montes, located outside the quadrangle to the north, are also about 27 km in height, about three times as high as any volcano on Earth. The summit caldera of Arsia Mons, more than 100 km in diameter, is the largest known. Syria and Sinai Plana are part of the highest plateau of Mars, the Tharsis plateau; their relative elevation, 10 km, is twice that of the Tibetan...
The Margaritifer Sinus quadrangle lies within a broad north-sloping trough, the Chryse lowland, between the elevated Tharsis plateau to the west and the cratered upland to the east. The rugged, uniquely martian chaotic terrain is best developed in this quadrangle. Sinuous furrows a few kilometers wide and as much as several hundred kilometers long cover most of the quadrangle; in several places are broad regions many tens of kilometers wide that appear to be complex channel systems. None of these features can be correlated with markings seen from Earth. The major part of the quadrangle consists of moderately cratered material containing craters of different morphologic types. This region is typical of the most cratered...
The Ismenius Lacus quadrangle includes the northernmost extension of the crated highlands that occupy a major part of the southern martian hemisphere. It includes three prominent physiographic provinces: cratered highlands in the south, relatively featureless plains in the middle, and mottled plains in the north. The highlands are separated from the plains by a belt of dissected terrain, containing mesas and buttes (“fretted terrain” of Sharp, 1973).
Olympus Mons is the largest known volcanic construct in the Solar System; it is more than 600 km across and more than 27 km above datum. The volcano and the great scarp that bounds it have been the subject of much scientific controversy. Although it has been possible to generate an empirical model that closely resembles Olympus Mons, the dynamics of scarp formation are still unproven. The scarp area is thus a logical selection as a scientific study area. It has also been designated as a a candidate site for a proposed lander/rover/sample-return mission to Mars not only because the site may provide information about the origin of the scarp and the evolution of Olympus Mons, but also because rocks of widely diverse...
The quadrangle is in the northern Maja Valles region on the west edge of the Chryse Planitia. This map is one in a sequence of three that also includes MTM 15057 and 20057. The sequence covers that part of the lower reaches of the Maja Valles that includes the transition from the higher Lunae Planum surface to the lower Chryse Planitia surface. The major interest in this quadrangle is the effects of catastrophic outflow and its associated morphologic modification of Chryse Planitia.
Geologic Map of the Descartes Region of the Moon, Apollo 16 Pre-Mission Map Renovation, 1:250k, 2022
The original geologic maps of the Descartes region (I-748) were published in 1972 as two map sheets (1:250,000 and 1:50,000) in a Transverse Mercator projection to support the Apollo 16 mission, the fifth crewed mission to land on the Moon (April 16 – 27, 1972). These renovated versions of the 1:50K and 1:250k maps represent a best effort to capture and preserve the fidelity of the original mapping effort in an interactive digital format. These maps are not updated versions or reinterpretations of the original geologic maps which were based on Lunar Orbiter images and Apollo 14 photography, but spatial adjustments to a Lunar Reconnaissance Orbiter (LRO) Wide Angle Camera (WAC) basemap to make the maps more compatible...
The Sappho Patera quadrangle (V–20) of Venus is bounded by 0° and 30° East longitude, 0° and 25° North latitude. It is one of 62 quadrangles covering the entire planet at a scale of 1:5,000,000. The quadrangle derives its name from Sappho Patera, a large rimmed depression (diameter about 225 km) lying on top of a shield-shaped mountain named Irnini Mons. Sappho, a noted Greek poet born about 612 B.C., spent most of her life on the island of Lesbos. All of her works were burned in 1073 by order of ecclesiastical authorities in Rome and Constantinople. What little survives was discovered in 1897 as parts of papier mâché coffins in the Fayum (Durant, 1939). The Sappho Patera quadrangle includes the central portion...
The Magellan spacecraft orbited Venus from August 10, 1990, until it plunged into the venusian atmosphere on October 12, 1994. Magellan had the objectives of (1) improving knowledge of the geologic processes, surface properties, and geologic history of Venus by analysis of surface radar characteristics, topography, and morphology and (2) improving knowledge of the geophysics of Venus by analysis of venusian gravity. The Magellan spacecraft carried a 12.6-cm radar system to map the surface of Venus. The transmitter and receiver systems were used to collect three datasets: synthetic aperture radar (SAR) images of the surface, passive microwave thermal emission observations, and measurements of the backscattered power...
The Galindo quadrangle (V-40; centered at lat 12.5° S., long 255°) was geologically mapped at 1:5,000,000 scale under the Venus Data Analysis and Venus Geologic Mapping Programs as part of a project focused on the study of venusian geologic terrains containing assemblages of coronae, arachnoids, and novae; these are enigmatic circular features perhaps related to hot-spot volcanism. Mapping of the quadrangle indicates most coronae are related to extension zones, and some aligned coronae and corona-like features show systematic variations in age. Standard photogeologic techniques were used to map the geology on the synthetic aperture radar (SAR) backscatter mosaic of V-40, which was generated by the radar image data...
The area of MC-28 is centered at the east edge of the Hellas Planitia (Hellas basin and surrounding plains) within densely cratered terrain that covers more than half the surface of Mars (Carr, 1973). The deepest part of the basin lies 4-5 km below the surface of the cratered terrain (Hanel and others, 1972). An irregular band of mountain and knobby material about the eastern margin of the basin and broad bands of mantled rough material on the floor of the basin represent ejecta from this very old impact. The vast, gently sloping, featureless eastern and southern part of Hellas Planitia, shown on the Shaded Relief Map of Mars (U.S.G.S., Atlas of Mars, MM 25M IR, 1972), is probably the result of extensive volcanic...
The original geologic maps of the Taurus-Littrow region (I-800) were published in 1972 as two map sheets (1:250,000 and 1:50,000) in a Transverse Mercator projection to support the Apollo 17 mission, the sixth and final crewed mission to land on the Moon (December 7 – 19, 1972). These renovated versions of the 1:50k and 1:250k maps represent a best effort to capture and preserve the fidelity of the original mapping effort in an interactive digital format. These maps are not updated versions or reinterpretations of the original geologic maps which were based on Apollo 15 metric photographs, but spatial adjustments to a Lunar Reconnaissance Orbiter (LRO) Wide Angle Camera (WAC) basemap to make the maps more compatible...
This 1:5,000 scale geolgic map is one of a series made from photographs transmitted by the Ranger VIII spacecraft. The Sabine EB region, in the southwestern part of Mare Tranquillitatis, is adjacent to the Sabine DM area, which was mapped at a scale of 1:50,000 by Trask (1969). The geology of parts of the map area was evaluated by H.H. Schmitt (in Shoemaker, 1966 p. 326-331) and Kuiper, Stroms and LePoole (1966, p. 91-93, p. 115-117). For this study Lunar Orbiter II photographs were used to fill in details on the South and West sides of the map area where the Ranger data are poor. One of the main objectives of the study was to asses the applicability of lunar geologic mapping at this scale and resolution.
The Arcadia quadrangle of Mars contains three distinct geologic provinces: (1) the 1000-km-diameter shield volcano of Alba Patera, which occupies the southwestern quadrant; (2) the complex Tempe province, which comprises a number of younger volcanic and sedimentary blanket deposits over an ancient, highly cratered crust forming a plateau in the southeastern quadrant; and (3) a plains province, consisting of northern wind-swept, cratered plains and some younger subpolar deposits in the northeast corner of the quadrangle, plus less cratered plains surrounding much of the Tempe and Alba regions. The plateau, informally named the Tempe Plateau and part of the proposed formal term Tempe Terra, is separated from the main...
The Systematic mapping of lava flow units in the Tharsis region has been compiled into a series of 16 maps at 1:2,000,000 scale. This work provides information on the sources and areal extent of the lava flows, on their eruptive sequences and relative ages, and on relations between the flows and geologic structure in the largest, most active tectonic and volcanic province on Mars. Some of the maps were made from controlled Viking photomosaics published as quarter quadrangles in the Atlas of Mars Topographic Series (U.S. Geological Survey, 1979) and tied to the Viking control net. Where these photomosaics were not available, larger scale catalog photomosaics tied to the Mariner 9 control net were used. These maps...
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