PDS MAP-A-PLANET Help Page - Data Sets

PDS MAP-A-PLANET Help Page
Data Sets

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Mars Data Sets Supported

Tnese are cartographic compilations made by processing "raw" Viking images to reduce radiometric and geometric distortions and to form geodetically controlled Mosaicked Digital Image Models (MDIMs). They were produced by the U. S. Gelological Survey, Flagstaff, Arizona.

  • mars_viking_bw is MDIM 1.0
  • v2mars_viking_bw is MDIM 2.0
  • mars_viking_color is the Viking Color data set
  • mars_viking_merged is a merge of the Viking Color and MDIM 1.0 datasets

    Venus Data Sets Supported

  • venus_magellan_fmap_leftlook is the Magellan left-look radar data
  • venus_magellan_fmap_rightlook is the Magellan right-look radar data
  • venus_magellan_fmap_stereolook is the Magellan stereo-look radar data
  • venus_gtdr is the Magellan topography data
  • venus_gsdr is the Magellan meter scale slope data
  • venus_gedr is the Magellan microwave emissivity data
  • venus_gredr is the Magellan fresnel reflectivity data

    Jupiter Data Sets Supported

  • callisto_galileo_bw is the Galileo Callisto black and white MDIM data
  • europa_galileo_bw is the Galileo Europa black and white MDIM data
  • ganymede_galileo_bw is the Galileo Ganymede black and white MDIM data
  • io_galileo_bw is the Galileo Io black and white MDIM data
  • io_galileo_color is the Galileo Io color MDIM data

    Lunar Data Sets Supported

  • The moon_clementine_bw is the Clementine Lunar 750nm basemap data
    The moon_clementine_bw or Clementine "albedo" is the brightness of the Moon as measured at 750 nm wavelength by the UVVIS camera. It is a black-and-white image. This lunar basemap is a radiometrically and geometrically controlled, photometrically modeled global image mosaic compiled using more than 43,000 images from the 750 nanometer filter observations of the Ultraviolet/Visible camera onboard the Clementine Spacecraft. The basemap mosaic is mapped in the Sinusoidal Equal-Area projection at a resolution of 100 meters per pixel. Reduced resolution datasets at 500m/pxl, 2.5km/pxl, and 12.5km/pxl are also provided. The Map-A-Planet interface utilizes these varying resolutions to deliver specific resolutions per user request. Final PDS archive volumes CL_3001 through CL_3015 were produced in July, 1997 by the Astrogeology Team of the U.S. Geological Survey, in cooperation with University of Arizona (Lunar and Planetary Laboratory) and Northwestern University, Evanston, IL.

    Ref: Nozette, S. and 33 others, The Clementine Mission to the Moon: Scientific Overview, Science, 266, 1835-1839.

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  • Clementine UltraViolet-Visible (UVVIS) 5-band Mosaic This multi-spectral lunar DIM is a radiometrically and geometrically controlled, photometrically modeled global image mosaic compiled using more than 400,000 images from multiple filter observations of the Ultraviolet/Visible (UVVIS) camera onboard the Clementine Spacecraft. The DIM mosaic is mapped in the Sinusoidal Equal-Area projection at a resolution of 100 meters per pixel. Five spectral bands are presented at 415, 750, 900, 950, 1000 nm wavelengths. Final PDS archive volumes CL_4001 through CL_4078 were produced in July, 1999 by the Astrogeology Team of the U.S. Geological Survey, in cooperation with University of Arizona (Lunar and Planetary Laboratory) and Northwestern University, Evanston, IL.

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  • The Clementine Ratio or Clementine false color views of the Moon are created by ratioing 3 of 5 UVVIS wavelengths and combining these into a red-green-blue color image: Red=750 nm/415 nm, Green=750 nm/950 nm, Blue=414 nm/750 nm. The color ratio rendition serves to cancel out the dominant brightness variations of the scene (controlled by albedo variations and topographic shading) and enhances color differences related to soil mineralogy and maturity. The lunar highlands, mostly old (~4.5 b.y.) gabbroic anorthosite rocks, are depicted in shades of red (old) and blue (younger). The lunar maria (~3.9 to ~1 b.y.), mostly iron-rich basaltic materials of variable titanium contents, are portrayed in shades of yellow/orange (iron-rich, low titanium) and blue (iron-rich, higher titanium). Superimposed on and intermingled with these basic units are materials from basins and craters of various ages, ranging from the dark reds and blues of ancient basins to the bright blue crater rays of younger craters.

    Ref: Pieters, C.M., M.I. Staid, E.M. Fischer, S. Tompkins, and G. He, 1994, A sharper view of impact craters from Clementine data, Science, 266, 1844-1848.

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  • The shaded relief or "hill-shade" views of lunar topography were created by the U.S. Geological Survey in the 1970s and 1980s using airbrush techniques to blend and merge photographic images (primarily from Lunar Orbiter) of the Moon. This mosaic was created by combining the airbrush maps digitally, and updating coverage with Clementine topographic data. The shaded relief image shows lunar features without the influence of albedo.

    Refs:
    Greeley, R. and R.M. Batson, eds., Plantary Mapping, Cambridge Planetary Science Series, 1990, 296 pp.

    Inge, J.L. and P.M. Bridges, 1976, Applied photointerpretation for airbrush cartography, Photogrammetric Engineering and Remote Sensing, 42 (6), 749-760.

    Rosiek, M.R. and R. Aeschliman, 2001, Lunar shaded relief map updated with Clementine data, LPS XXXII, #1943.

    Zuber, M.T., D.E. Smith, F.G. Lemoine, and G.A. Neumann, 1994, The shape and internal structure of the Moon from the Clementine mission, Science, 266, 1839-1843.

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  • The LIDAR color-coded Clementine topography data are shown overlaid on USGS shaded relief maps of the Moon. The shaded relief data provide interpretations of lunar morphology based on lunar photographic images and were used as a grayscale image for this global mosaic. Topographic data from the Clementine laser altimeter were combined with topographic data collected photogrammetrically from Clementine stereo images. The resulting topographic product was colored based on elevation value and combined with the shaded relief data to form the final photomosaic. Blues and greens are lower elevations, reds and yellows are higher.

    Refs:
    Rosiek, M.R. and R. Aeschliman, 2001, Lunar shaded relief map updated with Clementine data, LPS XXXII, #1943.

    Rosiek, M.R., R. Kirk, and E. Howington-Kraus, 2002, Color-coded topography and shaded relief maps of the lunar hemispheres, LPS XXXIII, #1792.

    U.S. Geological Survey, 2002, Color-coded topography and shaded relief maps of the lunar hemispheres, Geol. Inv. Series I-2769.


    General Information

    PDS MAP-A-PLANET uses global cartographic digital planetary image maps that have been prepared by the United States Geological Survey for the National Aeronautics and Space Administration (NASA). These databases are the products of exhaustive cartographic projects based on data from the Viking Orbiter, Clementine, Voyager, and Magellan missions.

    Black and White digital image maps


    The individual black and white image maps generated by PDS MAP-A-PLANET are derived from global digital image maps (DIMs). The Mars global maps, for example, have a resolution of 1/256-th degree per pixel (230 meters/pixel, or .16 miles/pixel). If the maps were presented as single images, they would contain 92,106 columns and 46,080 rows (more than 4 billion bytes of data). The Mars global image maps were produced by processing approximately 5,000 black/white (broad-band filter) images acquired by the Viking Orbiter spacecraft. The individual spacecraft images were processed to remove camera distortions and project (geometrically transform) the image to a map-based coordinate system of fixed map scale. The individual spacecraft images were then joined together to form a digital mosaic of the entire planetary surface.

    The original black and white Mars mosaic (MDIM 1.0) was completed in 1991. Since then, the Mars Pathfinder and Mars Global Surveyor missions have greatly increased our knowledge about the coordinates of features on the red planet. In 2000 the USGS therefore reprocessed the entire mosaic with more accurate positional control. The new mosaic (MDIM 2.0) is now available through this website. A third, even more accurate version of the mosaic is planned for completion in the near future. Note that the positions of the features in the new black and white mosaic do not necessarily agree with the older color or black and white mosaics. We hope to reprocess the Viking color mosaics also, and eventually to produce a global color mosaic from Mars Gobal Surveyor images.

    In the case of the lunar image maps, the underlying data set is the Clementine 750-nm Basemap Mosaic, similar to the Mars MDIM and generated from imagery acquired by the Clementine spacecraft.

    The Venus maps are created using the Magellan Mission "FMAP" radar global image mosaics.

    The Callisto Europa and Ganymede maps are created from currently unpublished Digital Image Maps derived from Galileo Mission data.

    Note that black and white images viewed at high and medium zoom levels provide spectacular views while images of the lowest zoom level do not display as well due to the sub-sampling of the high-resolution images.


    Color digital image maps (available for Mars only):



    The color image maps generated by PDS MAP-A-PLANET are derived from the global color map of Mars. The global color map has a resolution of 1/64-th degree per pixel (.92 kilometers/pixel, or .56 miles/pixel) and contains approximately 600 million bytes of data. The global color map was generated in a manner similar to the black and white map but the Viking Orbiter color observations of Mars were used. The red and violet band filter image observations were used to construct the color map.
    Color images viewed at low zoom factors provide interesting regional views of Mars. However, color images using medium zoom factor are not as interesting due to the low resolution nature of the color image maps.


    Color merged with Black/White Images (available for Mars only):



    This data sets represents a "merging" of the high-resolution detail of the black and white (MDIM 1.0) image map with the low resolution color information. This data set works well at medium and low zoom factors but does not work well at the lowest zoom.


    
      
      
      
    
    


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