Data

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 particular correlated with differences in topography. Discontinuities in the areal variation permit the surface material to be divided into map units, each

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 partially correlated with differences in topography. Discontinuities in the areal variation permit the surface material to be divided into map units, each

Material exposed on the surface of the moon is heterogenous. 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 from another, and the variations are partially correlated with differences in topography. Discontinuities in the areal variation permit the surface material to be divided up into map units, e

The surface of the moon is heterogenous. Similar surface materials are grouped into map units by means of telescope observations, study of lunar photographs, and photometric measurements. Each map unit has lateral continuity and limited range of physiographic characteristics and optical properties (mainly albedo, the reflectivity under full moon illumination). Such units are equivalent to the rock

The surface of the Moon is heterogeneous. Surface materials are classed on the basis of telescopic observations into map units, each having lateral continuity and a limited range of physiographic characteristics and optical properties (mainly polarization and albedo, the reflectivity under full moon illumination). Such units are analogous to the rock-stratigraphic formations of terrestrial geology

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 Eridania quadrangle is located within the densely cratered terrain of the southern hemisphere of Mars, east of the large circular Hellas Basin. The area contains three distinct physiographic provinces that divide the quadrangle into latitudinal belts. The northern part of the quadrangle is dominated by cratered upland plateau, the central part by plains, the southern part by a mottled surfac

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, 70 quart

Most images used in mapping the geology of the Shakespeare quadrangle were taken during the near-equatorial first pass, with close encounter on the dark side of the planet. The second, south-polar pass did not image the Shakespeare quadrangle at high resolution. High-resolution images of small areas within the quadrangle were also obtained during the third pass, when the spacecraft was on the near

Almost all the pictures acquired by Mariner 10 that were used for mapping were obtained during the first encounter: those covering the southeast half of the quadrangle are incoming close-encounter images, and those covering the north-west corner are outgoing close-encounter images. At the time the pictures were obtained, the terminator was at about long 7 degrees to 8 degrees, within the eastern p

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 resolve dis

Mariner 10 data include complete photographic coverage of the quadrangle at a resolution of about 2 km. In addition, twelve stereopairs cover scattered areas in the quadrangle (Davies and others, 1978, p. 114-115); these photographs were used to supplement the geologic interpretation. About 10 degrees of longitude of the H-13 quadrangle (Solitudo Persephones Province) adjacent to the west is inclu