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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 outoing close-encounter images. At the time the pictures were obtained, the terminator was at about long 7° to 8°, within the eastern part of the quadrangle. A large gap in coverage between in the incoming and outgoing images appears as a northeast-trending diagonal blank strip on the base map. A small part of this gap was filled in the southwestern part of the quadrangle by very poor second-encounter images.
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The U.S. Geological Survey provides a wide range of scientific information to an even wider group of stakeholders. Understanding what capacities are needed and if and or where these capacities exist across the USGS landscape is critical in moving science to the next level of use, implementation, and visualization. The concept behind the groups organized to conduct and interpret the survey that collected these data took advantage of the USGS’s position as a science organization with expertise spanning a wide range of science disciplines, stakeholders, and responsibilities. A survey was conducted of USGS employees (Sep 20-Nov 20) to get a current sample of the capacities that exist across the USGS.
A point layer of sites known to be useful analogs for planetary science, such as impact craters, dunes, volcanoes, and other processes observed on bodies across the solar system.
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A polygon layer of regions of multiple planetary bodies beyond Earth that are covered by proposed or published planetary geologic maps published by the USGS.
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Mariner 10 photographic coverage was available for only the eastern two-thirds of the Tolstoj quadrangle. Image data from three Mariner 10 encounters with Mercury were used in mapping the quadrangle.
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These data represents laboratory reflectance and emissivity spectral measurements of dune sand samples collected from a variety of dune types and mineralogical compositions from eight dune field locations in Alaska, Arizona, California, Colorado, Idaho, Nevada and New Mexico (labeled and designated as samples DS-1 through DS-8). Each sample was sieved into various size classes and measured both prior to and after sieving. Visible through Near Infrared through Shortwave Infrared (~0.4 - 2.5 microns) reflectance were measured using an artificial light source attached to an Analytical Spectral Devices (ASD) spectrometer. Hemispherical reflectance measurements spanning Mid-IR wavelengths, including the Thermal Infrared...
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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 Beethvoen and adjacent quadrangles. Mismatches are especially common along the borders withthe Kuiper and Discovery quadrangles to the east and southeast.
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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 discrepancies in feature positions on this sheet and those on the Kuiper (H-6) quadrangle to the north and the Bach (H-15) quadrangle to the south. The latter sheets were controlled by an earlier, more preliminary net.
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Most images used in mapping the geology of the Shakespeare quadrangle were taken during the near-equatorial first pass, with close encounter on teh 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-encounter north-polar trajectory. Because the spacecraft viewed the same areas from different positions during the first and second passes, stereoscopic pictures are available for certain areas of the southern hemisphere; however, such pictures are not available for the Shakespeare quadrangle. This map includes a strip...
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These geotiffs represent the raster GIS outputs of Linear Deconvolution (Linear Spectral Unmixing) analysis of ASTER image pixels covering various sand dune and sand sheet fields throughout the Western United States and Alaska. The accompanying sets of zip files contain linear deconvolution-derived mineral fractional abundance maps for various 2-, 3-, 4-, and 5-component mixture models of various dune-forming minerals, as well as RMS and residual errors for each model. Each geotiff layer has an associated metadata file with further details on each dune field and linearly deconvolved mineral distribution.
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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 for the Borealis region.
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The Terrestrial Analogs Data Portal (TADP; https://tadp.astrogeology.usgs.gov/) has been established as a repository and data discovery portal which leverages USGS ScienceBase, a trusted long-term digital repository that provides access to all USGS data services. Creation of the TADP service is in response to a number of NASA-generated reports identifying the need for a permanent planetary analog repository which adheres to standards-based archives. Presented here is the first version of the Planetary Aeolian Analog Database (PAAD) that will be incorporated into the TADP. This dataset is focused on dune field analogs, currently comprising 45 sites from all over the world and includes a set of "core" attributes (that...
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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° of longitude of the H-13 quadrangle (Solitudo Persephones Province) adjacent to the west is included in the map area because not enough Mariner 10 data were acquired of this quadrangle to justify the production of another map.
    map background search result map search result map Visible, Near Infrared, Shortwave Infrared and Thermal Infrared Laboratory Spectra of Samples of Compositionally Variable Dune Fields in the Western United States and Alaska Linear Deconvolution Mineral Maps of Compositionally Variable Dune Fields in the Western United States and Alaska Geologic Map fo the Beethoven Quadrangle of Mercury Geologic Map of the Discovery Quadrangle of Mercury Geologic Map of the Victoria Quadrangle of Mercury Known Terrestrial Analog Sites for Planetary Science USGS Earthmap Capacity Assessment Dataset PAAD: The Planetary Aeolian Analog Database Visible, Near Infrared, Shortwave Infrared and Thermal Infrared Laboratory Spectra of Samples of Compositionally Variable Dune Fields in the Western United States and Alaska Linear Deconvolution Mineral Maps of Compositionally Variable Dune Fields in the Western United States and Alaska Geologic Map of the Discovery Quadrangle of Mercury Geologic Map of the Victoria Quadrangle of Mercury Geologic Map fo the Beethoven Quadrangle of Mercury USGS Earthmap Capacity Assessment Dataset Known Terrestrial Analog Sites for Planetary Science PAAD: The Planetary Aeolian Analog Database