Data

Basic information about the planetary surface of the Kuiper quadrangle is provided by three sequences of high-quality photographs designated Mercury I, II, and II, obtained during the incoming phases of three encounters of the Mariner 10 spacecraft with Mercury. Mercury I includes 75 whole-frame photographs of the Kuiper quadrangle; Mercury II, 13 whole-frame photographs; and Mercury III...

This map sheet is one of a series covering that part of the surface of Mercury that was illuminated during the Mariner 10 encounters. Planimetric control is provided by photogrammetric triangulation using Mariner 10 pictures (Davies and Batson, 1975). Discrepancies between images in the base mosaic and computed control-point positions appear to be less than 5 km. No attempt was made to...

Most of the photographs used for geologic mapping were acquired by the departing spacecraft during the first pass (Mercury I). The Mercury II encounter provided no usable images of the map area; two low-oblique photographs suitable for geologic mapping were acquired during the third flyby on March 17, 1975 (Davies and others, 1978, p. 31). No stereoscopic phtographic pairs are available...

The Beethoven quadrangle is located in the equatorial region of Mercury, in the center of the imaged area. Most pictures of the quadrangle were obtained at high sun angles as the Mariner 10 spacecraft receded from the planet. Images in the northeastern part of the quadrangle are very poor to unusable. Another difficulty in mapping is the poor match in topographic bases between Beethoven...

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...

Since the 1970's, when the Mariner 9 spacecraft revealed the geologic diversity of Mars, the Chryse Planitia region has been noted for its immense outflow channels and chaotic terrain (McCauley and others, 1972; Sharp and Malin, 1975; Baker, 1982, chap. 3; Mars Channel Working Group, 1983). Various proposals for the origin of these features have been offered; most workers have favored a...

The surface of the moon is heterogeneous. The differences from area to area of characteristic topographic forms and of physical properties such as albedo (reflectivity under full-Moon illumination) indicate that the materials underlying the surface vary from one area to another and that different processes have operated in the development of the surface. In lunar geologic mapping, areas...

Published geologic maps of south polar region of Mars have been based on either Mariner 9 (Condit Soderblom, 1978; Scott and Carr, 1978) or Viking Orbiter (Tanaka and Scott, 1987) images. The mapped extent of the southern layered deposits differs in many places on these maps and on our maps. These differences reflect the difficulty in accurately determining the location of the contact...

This map is one of a series prepared from photographs transmitted by Ranger IX (Jet Propulsion Lab, 1966, pls A56-58, B70-82). It depicts the geology of some 724 sq km in the northeast part of the floor of Alphonsus (Diameter about 115 km), a typical flat-floored old terra crater or basin with a subdued rim. Similar basins abound in the south central terrae of the visable hemisphere and...

This 1:50,000 scale geolgic map is one of a series constructed at various scales from photographs trasmitted by the Ranger VII, VIII and IX spacecraft. The center of the map area is about 23 km southwest of the Ranger VIII (US Air Force Aeronautical Chart and Information Center Chart AIC 60C, Arago). In general, geologic maps of the moon portray similarities and differences in the...

The Sabin EB region is a rolling plain which consists entirely of crater and mare materials. The areal density of craters, though variable within the region, is sufficiently high so that the craters are the dominant morphological feature. Crater morphology ranges from bright, sharp-rimmed craters to pan-shaped depressions. Superposition relations indicate that the bright-rimmed craters...

Material exposed on the surface of the moon is heterogeneous. The albedo and other physical characteristics that have been determined with the use of optical and radio telescopes vary from one part of the moon to another, and the variations are patially correlated with differences in topography . Discontinuities in the areal variation permit the surfaces material to be divided into map...