Data

The brightly rayed crater Coperincus, one of the most familiar features of the Moon served as the type example of an impact crater in Shoemaker's (1962) classic analysis. This map shows the geology of the crater as interpreted in photographs taken by Lunar Orbiter V. A geologic map at 1:1,000,000 scale showing the regional setting of Copernicus and the extent of the rim deposits and...

The Geminus quadrangle, centrally located in the northeast quadrant of the lunar near side, is dominated geologically by several multiringed circular basins outside the quadrangle and five relatively young, large craters mapped here. The terra and the older craters apparently are mantled by a nearly continuous blanket of ejecta from the Serenitatis, Crisium, Humboldtianum, and Imbrium...

The Cassini quadrangle is in the north-central part of the nearside lunar disk and includes most of the northeast quadrant of Mare Imbrium. Lunar geologic units in the area have been distinguished according to topographic expression, albedo, and infrared stratigraphic relations, and the distribution of each unit is portrayed on the accompanying map. the nature and disposition of geologic...

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...

The Bach region encompasses the south polar part of Mercury poleward of lat 65 degrees S. About half of the region was beyond the terminator during the three Mariner 10 encounters and hence not visible. The entire mapped area was covered by near-vertical photography from the second encounter, and the eastern part, from long 15 degrees to about 110 degrees, was covered by oblique...

The Lavinia Planitia quadrangle (V-55) is in the southern hemisphere of Venus and extends from 25 degrees to 50 degrees south latitude and from 330 degrees to 360 degrees longitude. It covers the central and northern part of Lavinia Planitia and parts of its margins. Lavinia Planitia consists of a centralized, deformed lowland flooded by volcanic deposits and surrounded by Dione Regio to...

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...

The Coprates quadrangle lies to the east of the Tharsis volcanic complex and the Noctis Labyrinthus tectonic complex. To the north are the plains of Lunae Planum, to the east the vast patches of chaotic terrain and the large sinuous channels that trend northward into Chryse Planitia. On the southwest is the Thaumasia Fossae region of tectonically deformed cratered terrain, to the...

The geology for this map was compiled using Viking Orbiter images on 1:500,000- scale photomosaics of the Mars Transverse Mercator quadrangles -40262, -40267, and -40272. This map represents a detailed extension of regional geologic mapping of the east Hellas rim (Crown and others 1990, 1992) and is published at 1:1,000,000 scale. The map area is on the east rim of one of the largest...

The Diacria quadrangle lies within the north circumpolar lowlands of Mars (Carr and others, 1973; Scott and Carr, 1978). The dominant structural and physiographic features are low, relatively smooth plains (Arcadia Planitia, Vastitas Borealis) that form the northern two-thirds of the quadrangle. The plains rise to the south to form the north edge of the Amazonis Planitia and to the...

The east Mangala Valles area merits detailed geologic study because it contains several small channels whose ages can be determined relative to geologic units that range in age from early (Noachian) to late (Amazonian) periods of Martian history. Because small channels are of three ages and geomorphic types, their study increases our understanding of the continuity of fluvial processes...

The Valles Marineris region lies east of Tharsis Montes (which extend from lat 12 degrees to 16 degrees., long 101 degrees to 125 degrees). Part of the region is in the midst of a vast plateau bounded on the west and east by Claritas and Nectaris Fossae, respectively; the remainder extends farther east into southern Xanthe Terr and western Margaritifer Terra. Channel trends...