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The Mare Tyrrhenum quadrangle is bounded by lat 0° and 30° S. and long 225° W. and 270° W. The central part of the quadrangle is dominated by Tyrrhena Patera, a large shield volcano, and associated low-albedo ridged plains that probably are basaltic lava flows similar to the lunar maria. The western, northern, and eastern margins of the quadrangle are located in cratered terrains of higher elevation. The great Hellas Basin is located to the southwest of the mapped area, and the central part of the quadrangle contains a number of arcuate scarps, faults, and ridges that appear to be concentric to Hellas. The southwestern part of the quadrangle contains patches of old knobby terrain that may by ejecta and structurally...
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 between the layered deposits and subjacent units. The polar layered deposit gradually thin toward their margin in many places, and the smooth surface features that characterize the layered deposits are also found on other sedimentary blankets in the south polar region (Murray and others, 1972; Sharp, 1973).
The map area is in the Mangala-Memnonia region, which contains remarkably diverse geologic features and terrain types. Studies of the Mariner 9 images revealed the wide range of ages of the major rock units in this region; age assignments were based on the density of impact craters preserved on the various surfaces (Mutch and others, 1976, p. 56-60; Scott and Carr, 1978; Mutch and Morris, 1979). The region includes ancient cratered highlands, more sparsely cratered smooth plains, young volcanic plains, and the Mangala Valles channel system. The sinuousity of the streamlined landforms within the Mangala Valles, combined with braided channels evident throughout the lower reaches of the valley system, were recognized...
This map is one of a series of large-scale (1:500,000) geologic maps of Mars initiated by the National Aeronautics and Space Administration to investigate areas of high scientific interest. The Gusev crater–Ma’adim Vallis region includes several potential landing sites for future Mars missions, including those with a focus on exobiology studies and sample return. Channels in the map area span a long age range, cut ancient rocks that may contain important biogenic information, and funneled water into exobiologically important lacustrine basins. The map area is characterized by diverse geologic units representing a variety of endogenic and exogenic processes. The geologic history of this region spans the entire history...
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 surface of rugged topography and a high density of craters subdued by erosion. In general, the oldest geologic units occur in the upland terrains, the youngest in the central lowlands.
This location is part of the Arizona Mineral Industry Location System (AzMILS), an inventory of mineral occurences, prospects and mine locations in Arizona. Coconino246 is located in T13N R10E Sec 6 C in the Long Valley - 7.5 Min quad. This collection consists of various reports, maps, records and related materials acquired by the Arizona Department of Mines and Mineral Resources regarding mining properties in Arizona. Information was obtained by various means, including the property owners, exploration companies, consultants, verbal interviews, field visits, newspapers and publications. Some sections may be redacted for copyright. Please see the access statement.
This data set contains imagery from the National Agriculture Imagery Program (NAIP). The NAIP program is administered by USDA FSA and has been established to support two main FSA strategic goals centered on agricultural production. These are, increase stewardship of America's natural resources while enhancing the environment, and to ensure commodities are procured and distributed effectively and efficiently to increase food security. The NAIP program supports these goals by acquiring and providing ortho imagery that has been collected during the agricultural growing season in the U.S. The NAIP ortho imagery is tailored to meet FSA requirements and is a fundamental tool used to support FSA farm and conservation programs....
The Elysium quadrangle includes part of the vast, relatively low and featureless plains that encircle the subpolar region of Mars immediately north of the more elevated and cratered equatorial belt. The plains are interrupted in the northwest by two large volcanoes, second only in size and youthful appearance to some of the large constructs that form the planet’s most prominent volcanic center in the Tharsis region several thousand kilometres to the east (Carr, 1975). The large irregularity shaped crater Orcus Patera, at the east boundary of the map, closely resembles the lunar crater Schiller but is more than twice as long. A band of knobby, relatively old terrain extends in a broad arc northeastward through the...
The Sinus Sabaeus quadrangle lies in the southern equatorial region of Mars. It is bounded on the north by the equator, on the west by the central meridian, on the south by lat 30° S., and on the east by long 315° W. Three classical regions that have low albedos occur within the quadrangle (Lowell Observatory, 1971): (1) half of Sinus Meridiani occupies part of the northwest corner of the quadrangle; (2) Sinus Sabaeus forms a broad east-west band 180 to 360 km wide across the upper part of the quadrangle along lat 10° S.; and (3) Serpentis Minor occupies the southeast corner. The classical high-albedo regions of Deucalionis Regio and Pandorae Fretum occupy the western and central southern parts of the quadrangle;...
The Memnonia quadrangle lies astride the boundary between heavily cratered and sparsely cratered hemispheres of Mars (Carr and others, 1973). Densely cratered terrain occurs in the southwestern part of the quadrangle. Strips of plains material bound the cratered terrain in both the northern and eastern parts of the quadrangle. There is approximately 3 km of relief across the quadrangle, with the highest elevations in the eastern part. Plains materials of this region are situated along the lower Lacus and Tharsis quadrangles. There is little correlation between terrain type and elevation within the Memnonia quadrangle. In particular, the boundary between cratered terrain and plains for the most part is not marked...
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...
This map is one in a series of 1:500,000-scale geologic maps initiated by NASA to investigate areas of particular scientific interest on Mars. The north Kasei Valles area merits detailed geologic study because it contains part of a large channel system whose age can be determined relative to geologic units that range in age from early intermediate (Early Hesperian) to the very late (Late Amazonian) periods of Martian history. Also, many geomorphic features in the map area suggest changes in water level and multiple erosional events associated with the Kasei Valles system. Later erosional events are indicative of spring sapping; small-scale, ground-water runoff; and water-mobilized debris flow. Therefore, this large-scale...
The Pompeii quadrangle is in northern Maja Valles region between Lunae Palum to the west and Xanthe Terra to the east. Approximately two-thirds of the surface is a relatively smooth plain, and the other one-third is subdued, cratered, upland plateau. The crater Pompeii is the largest fresh crater in the quadrangle. The major interest in the map area is evidence of the relatively brief, catastrophic Maja outflow and its associated topographic modification of much of the area. The effects of erosion and deposition by the Maja flood are pronounced and are a chief part of the story; therefore, flood-modified terrain is divided in considerable detail. The stratigraphic units associated with the outflow are true rock...
The Mars Global Digital Dune Database provides a comprehensive and quantitative view of the geographic distribution of dune fields from 65° N to 65° S latitude. The database encompasses ~ 550 dune fields, covering ~ 70,000 km2, with an estimated total volume between 3,600 km3 and 13,400 km3. Over 2300 selected Thermal Emission Imaging System (THEMIS) infrared (IR), THEMIS visible (VIS) and Mars Orbiter Camera Narrow Angle (MOC NA) images were used to build the database and are included in the ArcMap and ArcReader versions of the database. An initial data set of THEMIS band 9 spectral range images covering orbits 816-9601 (spanning 02/2002 - 02/2004 and Ls = 0.085º-358.531º) and comprising more than 30,000 images...
Categories: Data;
Types: Downloadable,
Map Service,
OGC WFS Layer,
OGC WMS Layer,
Shapefile;
Tags: Database,
Dune,
Dunes,
Feature Catalog,
Mars,
USGS Historical Quadrangle in GeoPDF.
Dataset contains latitude, longitude and additional attribute information for mounds in the lowlands of Mars. This version of the database contains data for mounds in the southwestern Utopia Planitia region of the martian lowlands.
Categories: Data;
Tags: Geomorphology,
Mars,
Planetary Sciences,
USGS Science Data Catalog (SDC),
Utopia Planitia,
The geology of the Thaumasia region (fig. 1, sheet 3) includes a wide array of rock materials, depositional and erosional landforms, and tectonic structures. The region is dominated by the Thaumasia plateau, which includes central high lava plains ringed by highly deformed highlands; the plateau may comprise the ancestral center of Tharsis tectonism (Frey, 1979; Plescia and Saunders, 1982). The extensive structural deformation of the map region, which is without parallel on Mars in both complexity and diversity, occurred largely throughout the Noachian and Hesperian periods (Tanaka and Davis, 1988; Scott and Dohm, 1990a). The deformation produced small and large extensional and contractional structures (fig. 2,...
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...
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...
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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