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This page describes the data sets available on Map-a-Planet. Use the following links to jump down the page to that section.
Venus Data Sets
Magellan was launched in 1989 to collect radar imagery, topography, and gravity field data of Venus. Magellan orbited Venus for four years during its extended mission. At the conclusion of the mission, Magellan was intentionally crashed into the planet's surface, allowing the spacecraft to collect data on Venus' atmosphere before it was destroyed. It was the first time a working planetary spacecraft was ever intentionally crashed. For more about the Magellan mission, visit the NASA/JPL Magellan Mission web page.
Map-a-Planet offers a comprehensive collection of global Magellan products, listed below. The following table lists the highest available resolution for each data set. Click the data set name to jump down to a description of the data set.
| Data Set |
Resolution px/deg |
Scale km/px |
|---|---|---|
| Venus Magellan SAR (left-, right-, and stereo-look) | 1408 | 0.075 |
| Venus Magellan Topography (GTDR) | 22.75 | |
| Venus Magellan Meter Scale Slope (GSDR) | 22.75 | |
| Venus Magellan Microwave Emissivity (GEDR) | 22.75 | |
| Venus Magellan Fresnel Reflectivity (GREDR) | 22.75 |
Magellan Synthetic Aperture Radar (SAR)
Because Venus is shrouded by a dense, opaque atmosphere, conventional optical cameras cannot be used to image its surface. Instead, Magellan's imaging radar uses bursts of microwave energy somewhat like a camera flash to illuminate the planet's surface. The radar pulses are not sent directly downward but rather at a slight angle to the side of the spacecraft--the radar is thus called "side-looking radar." In addition, special processing techniques are used on the radar data to result in higher resolution as if the radar had a larger antenna, or "aperture"; the technique is thus often called "synthetic aperture radar," or SAR. (Reference: NASA/JPL Magellan Mission)
Example images created from the three Venus SAR FMAP data sets available on Map-a-Planet
Magellan Synthetic Aperture Radar (SAR) FMAP Left-Look
As mentioned above, the Magellan SAR is a side-looking radar system. Radar pulses are not sent directly downward but rather at a slight angle to the side of the spacecraft. In the case of Left-Look Magellan SAR data, the radar system was sending signals to the left of the spacecraft. The SAR operated in this left-looking mode during cycles 1 and 3 of the mission. The global left-looking SAR data set created by the USGS Astrogeology Research Program, served here on the Map-a-Planet website, is referred to as the Magellan FMAP Left-Look (full-resolution left-looking radar map).
Start mapping Venus with the Magellan SAR FMAP Left-Look image data set
Magellan Synthetic Aperture Radar (SAR) FMAP Right-Look
As mentioned above, the Magellan SAR is a side-looking radar system. In the case of Right-Look Magellan SAR data, the radar system was sending signals to the right of the spacecraft. The SAR operated in this right-looking mode during cycle 2 of the mission. The global left-looking SAR data set created by the USGS Astrogeology Research Program, served here on the Map-a-Planet website, is referred to as the Magellan FMAP Left-Look (full-resolution left-looking radar map).
Start mapping Venus with the Magellan SAR FMAP Right-Look image data set
Magellan Synthetic Aperture Radar (SAR) FMAP Stereo-Look
The Magellan SAR operated in this left-looking mode during cycles 1 and 3 of the mission. The overlapping left-look data collected by the mission was used to create stereo views of portions of the surface.
Start mapping Venus with the Magellan SAR FMAP Stereo-Look image data set
Topography: Magellan Global Topography Data Record (GTDR)
During the collection of the SAR (radar) data, Magellan also collected altimetry (surface height data), which was used to create the Global Topography Data Record (GTDR) topography data set.
Start mapping Venus with the Magellan GTDR (topography) data set
Meter Scale Slope: Magellan Global Slope Data Record (GSDR)
During the collection of the SAR (radar) data, Magellan also collected altimetry (surface height data), which was used to create the Global Slope Data Record (GSDR) (meter scale slope) data set.
Start mapping Venus with the Magellan GSDR (meter scale slope) image data set
Microwave Emissivity: Magellan Global Emissivity Data Record (GEDR)
During the collection of the SAR (radar) data, Magellan's radiometer also passively collected radiated thermal microwave energy data, used to create the Global Emissivity Data Record (GEDR) data set.
Start mapping Venus with the Magellan GEDR (microwave emissivity) image data set
Fresnel Reflectivity: Magellan Global Reflectivity Data Record (GREDR)
Global Reflectivity Data Record (GREDR) (reflectivity) data set.
Lunar Cartographic Data Sets
The table below lists the highest available resolution for each data set. Click the data set name to jump down to a description of the data set.
| Data Set |
Resolution px/deg |
Scale km/px |
|---|---|---|
| Lunar Shaded Relief "Hillshade" Topographic Map | 64 | 0.4738 |
| Lunar Clementine Color-coded Elevation | 32 | 0.9476 |
| Lunar Clementine Greyscale (750 nm 'Albedo' Base Map) | 303 | 0.1 |
| Lunar Clementine UVVIS 'Natural' Color Composite | 303 | 0.1 |
| Lunar Clementine UVVIS Color-Ratio | 303 | 0.1 |
| Lunar Clementine NIR 'Enhanced' Color | 303 | 0.1 |
| Lunar Photography: Lunar Orbiter Photo-Mosaic | 512 | 0.0592 |
| Lunar Prospector: Elemental Abundance | 2 | 15.16 |
Shaded Relief or "Hillshade" Topographic Map
Shaded relief or "hill-shade" lunar topographic maps of the Moon 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 in 2002 (see Rosiek et all., 2002) at 1:10 million scale by combining the airbrush maps digitally, and updating coverage with Clementine topographic data. The shaded relief image shows lunar topographic features without the influence of albedo.
Start mapping the Moon with the Shaded Relief image data set
References
Greeley, R. and R.M. Batson, eds., Planetary 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.
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 Map of the Lunar Near Side and Far Side Hemispheres, U.S. Geological Survey Geologic Investigation Series I-2769.
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.
Clementine Elevation Map
|
Color-coded elevation data from the Clementine laser altimeter (Smith et al., 1997) are shown overlaid on the updated 1:10 M-scale USGS shaded relief map of the Moon. The shaded relief data provide interpretations of lunar morphology based on lunar photographs and were used as a grayscale image for this global mosaic (USGS, 2002, I-Map 2769). Elevation data from the Clementine laser altimeter were updated with topographic data collected photogrammetrically from Clementine stereo images (Cook et al., 2000; Margot et al., 2000). The resulting topographic map was color-coded based on elevation value (USGS, 2002) and coregistered to the shaded relief data to form the final photomosaic. Blues and greens are lower elevations, reds and yellows are higher (see key at right). |
|
Start mapping the Moon with the Clementine elevation data
References
Cook, A., Watters, T.R., Robinson, M.S., Spudis, P.D., and Bussey, D.B.J., 2000, Lunar polar topography derived from Clementine stereoimages: Journal of Geophysical Research, v. 105, no. E5, p. 12,023-12,033.
Margot, J.L., Campbell, D.B., Jurgens, R.F., Slade, M.A., 2000, Digital elevation models of the Moon from Earth-based radar interferometry: IEEE Transactions on Geoscience and Remote Sensing, v. 38, no. 2, p. 1122-1133.
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.
Smith, David E., Zuber, Maria T., Neumann, Gregory A. and Lemoine, Frank G., 1997, Topography Of The Moon From The Clementine Lidar, JGR, Vol. 102, No. E1, Pages 1591-1611.
U.S. Geological Survey, 2002, Color-coded Topography and Shaded Relief Map of the Lunar Near Side and Far Side Hemispheres, U.S. Geological Survey Geologic Investigation Series I-2769.
Clementine Multispectral Mosaic: Ultraviolet/Visible and Near Infrared (NIR)
UVVIS 750nm Basemap | UVVIS 'Natural' Color | UVVIS Ratio 'False' Color | NIR 'Enhanced' Color |
The Clementine experiment carried four scientific imaging cameras: the Ultraviolet/Visible (UVVIS), Near-Infrared (NIR), High-Resolution (HiRES), and Long-wave Infrared (LWIR) cameras. The Ultraviolet/Visible (UVVIS) camera imaged the surface of the Moon at five wavelengths spanning the ultraviolet to near-infrared spectrum and the Near-Infrared (NIR) camera collected data at six wavelengths extending into the short-wave infrared (see tables below). This experiment yielded information on the color and inferred compositional properties of lunar soils and surface units, and also provided images useful for morphologic studies and cratering statistics. Most images were taken at low Sun angles, which is useful for compositional studies but not for observing morphology. Global mosaics at the five UVVIS and six NIR coregistered wavelengths were created using nearly 1 million images and are displayed here at a resolution of ~100 m/pixel.
| UVVIS Center Wavelength (nm) |
Band- Width (nm) |
Description |
|---|---|---|
| 415 | 40 | Ultraviolet |
| 750 | 10 | Red-Near Infrared |
| 900 | 20 | Near Infrared |
| 950 | 30 | Near Infrared |
| 1000 | 30 | Near Infrared |
| NIR Center Wavelength (nm) |
Band- Width (nm) |
Description |
|---|---|---|
| 1100 | 30 | Near Infrared |
| 1250 | 30 | Near Infrared |
| 1500 | 30 | Short-wave Infrared |
| 2000 | 30 | Short-wave Infrared |
| 2600 | 30 | Short-wave Infrared |
| 2780 | 60 | Short-wave Infrared |
See this reference for these wavelength ranges: http://en.wikipedia.org/wiki/Infrared
References
Eliason, E., C. Isbell, E. Lee, T. Becker, L. Gaddis, A. McEwen, M. Robinson, Mission to the Moon: The Clementine UVVIS Global Lunar Mosaic, PDS Volumes USA_NASA_PDS_CL_4001 through 4078, produced by the U.S. Geological Survey and distributed on CD media by the Planetary Data System, 1999.
Eliason, E.M., A.S. McEwen, M.S. Robinson, E.M. Lee, T.L. Becker, L. Gaddis, L.A. Weller, C.E. Isbell, J.R. Shinaman, T. Duxbury, E. Malaret, Clementine: A Global Multi-Spectral Map of the Moon from the Clementine UVVIS Imaging Instrument: Lunar and Planetary Science Conference 30th, pp. 1933-1934, 1999.
Eliason, E.M., E.M. Lee, T.L. Becker, L.A. Weller, C.E. Isbell, M.I. Staid, L.R. Gaddis, A.S. McEwen, M.S. Robinson, T. Duxbury, D. Steutel, D.T. Blewett, and P.G. Lucey, A Near-Infrared (NIR) global multispectral map of the Moon from Clementine, Lunar and Planetary Science Conference XXXIV, abstract #2093, 2003.
Gaddis, Lisa, Chris Isbell, Matt Staid, Eric Eliason, Ella Mae Lee, Lynn Weller, Tracie Sucharski, Paul Lucey, Dave Blewett, John Hinrichs, and Donovan Steutel, 2007 (in review), The Clementine NIR Global Lunar Mosaic, PDS Volumes USA_NASA_PDS_CL_5001 through 5078, produced by the U.S. Geological Survey and distributed online and on DVD media by the Planetary Data System.
Lucey, P.G., D.T. Blewett, E. Eliason, L.A. Weller, R. Sucharski, E. Malaret, J.L. Hinrichs, and P.D. Owensby, Optimized calibration constants for the Clementine NIR camera, Lunar and Planetary Science Conference XXIX, #1273, 2000.
McEwen, A.S., M. Robinson, Mapping of the Moon by Clementine: Adv. Space Research, Vol. 19, No. 10, pp. 1523-1533, 1997.
Nozette, S., P. Rustan, L.P. Pleasance, D.M. Horan, P. Regeon, E.M. Shoemaker, P.D. Spudis, C.H. Acton, D.N. Baker, J.E. Blamont, B.J. Buratti, M.P. Corson, M.E. Davies, T.C. Duxbury, E.M. Eliason, B.M. Jakosky, J.F. Kordas, I.T. Lewis, C.L. Lichtenberg, P.G. Lucey, E. Malaret, M.A. Massie, J.H. Resnick, C.J. Rollins, H.S. Park, A.S. McEwen, R.E. Priest, C.M. Pieters, R.A. Reisse, M.S. Robinson, D.E. Smith, T.C. Sorenson, R.W. Vorder Breugge, and M.T. Zuber, The Clementine Mission to the Moon: Scientific Overview: Science, Vol. 266, pp. 1835-1839, 1994.
UVVIS/NIR Overview | UVVIS 750nm Basemap | UVVIS 'Natural' Color | UVVIS Ratio 'False' Color | NIR 'Enhanced' Color | Moon | Top
Clementine UVVIS Greyscale Image (750 nm 'Albedo' Basemap)
The Clementine 750 nm mosaic is a greyscale data set representing the albedo (brightness of the lunar surface) as measured at the 750 nm wavelength by the UVVIS camera. This lunar base map 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 UVVIS (Eliason et al., 1997; Eliason et al., 1999; Isbell et al., 1999)
Start mapping the Moon with the Clementine Grayscale Albedo (750 nm Base Map) image data set
References
Eliason, E., C. Isbell, E. Lee, T. Becker, L. Gaddis, A. McEwen, M. Robinson, Mission to the Moon: The Clementine UVVIS Global Lunar Mosaic, PDS Volumes USA_NASA_PDS_CL_4001 through 4078, produced by the U.S. Geological Survey and distributed on CD media by the Planetary Data System, 1999.
Eliason, E., C. Isbell, E. Lee, T. Becker, L. Gaddis, A. McEwen, M. Robinson, Clementine Basemap Mosaic, PDS Volumes USA_NASA_PDS_CL_3001 through 3015, produced by the U.S. Geological Survey and distributed on CD media by the Planetary Data System, 1997.
Isbell, C. E., E.M. Eliason, K.C. Adams, T.L. Becker, A.L. Bennett, E.M. Lee, A. McEwen, M. Robinson, J. Shinaman, L.A. Weller, 1999, Clementine: A Multi-Spectral Digital Image Model Archive of the Moon, LPS XXX: Lunar and Planetary Institute, Houston, Abs. #1812.
UVVIS/NIR Overview | UVVIS 750nm Basemap | UVVIS 'Natural' Color | UVVIS Ratio 'False' Color | NIR 'Enhanced' Color | Moon | Top
Clementine UVVIS 'Natural' Color Composite Mosaic
The Clementine 'natural' color composite mosaic (5 UVVIS bands available) is presented here for browsing by utilizing three of the five UVVIS multispectral bands, combined in red, green and blue channels of a color image (see table below). (Note: The composite image is not truly "natural color," but mimics natural color to the human eye.) This multispectral lunar mosaic 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 (Eliason et al., 1999).
| Channel | Band | Description |
|---|---|---|
| Red | 1000 nm | Near Infrared |
| Green | 900 nm | Near Infrared |
| Blue | 415 nm | Ultraviolet |
This '3-band' view is presented for browsing purposes. All five bands of the Clementine global mosaic are available when ordering data downloads of the UVVIS 'Natural Color' product.
Start mapping the Moon with the Clementine UVVIS 'Natural Color' data set
References
Eliason, E., C. Isbell, E. Lee, T. Becker, L. Gaddis, A. McEwen, M. Robinson, Mission to the Moon: The Clementine UVVIS Global Lunar Mosaic, PDS Volumes USA_NASA_PDS_CL_4001 through 4078, produced by the U.S. Geological Survey and distributed on CD media by the Planetary Data System, 1999.
UVVIS/NIR Overview | UVVIS 750nm Basemap | UVVIS 'Natural' Color | UVVIS Ratio 'False' Color | NIR 'Enhanced' Color | Moon | Top
Clementine UVVIS 'False Color' or Color-Ratio Image
The Clementine UVVIS Ratio ("false color") views of the Moon are created by creating ratio images using 3 of the 5 Clementine UVVIS camera bands and combining these into the red, green, and blue channels of a color image:
| Channel | Ratio (band/band) |
|---|---|
| Red | 750 nm/415 nm |
| Green | 750 nm/950 nm |
| Blue | 414 nm/750 nm |
The color ratio image product 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 billion years) gabbroic anorthosite rocks, are depicted in shades of red (old) and blue (younger). The lunar maria (~3.9 to ~1 billion years), mostly iron-rich basaltic materials of variable titanium contents, are portrayed in shades of yellow/orange (iron-rich, lower 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 (e.g., Mcewen et al., 1999; Pieters et al., 1999).
Start mapping the Moon with the Clementine Ratio image data set
References
Eliason, E., C. Isbell, E. Lee, T. Becker, L. Gaddis, A. McEwen, M. Robinson, Mission to the Moon: The Clementine UVVIS Global Lunar Mosaic, PDS Volumes USA_NASA_PDS_CL_4001 through 4078, produced by the U.S. Geological Survey and distributed on CD media by the Planetary Data System, 1999.
McEwen, A.S., M.S. Robinson, E.M. Eliason, P.G. Lucey, T.C. Duxbury, and P.D. Spudis, 1999, Clementine Observations of the Aristarchus Region of the Moon, Science, 266, pp. 1858-1861.
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
UVVIS/NIR Overview | UVVIS 750nm Basemap | UVVIS 'Natural' Color | UVVIS Ratio 'False' Color | NIR 'Enhanced' Color | Moon | Top
Clementine NIR 'Enhanced' Color Composite Mosaic
The Clementine NIR 'enhanced' color composite mosaic available for browsing on the site is comprised of three of the five Clementine UVVIS multispectral bands, combined in the red, green, and blue channels of a color image (see table below). (Note: The composite image is 'false color' but mimics natural color to the human eye.) This multispectral lunar mosaic is a radiometrically and geometrically controlled, photometrically modeled global image mosaic compiled using more than 400,000 images from multiple filteri observations of the Near Infrared (NIR) camera onboard the Clementine spacecraft (Gaddis et al., 2007).
| Channel | Band | Description |
|---|---|---|
| Red | 2000 nm | Short-wave Infrared |
| Green | 1500 nm | Short-wave Infrared |
| Blue | 1100 nm | Near Infrared |
This '3-band' color view is presented for browsing purposes. All six bands of this Clementine global mosaic are available when ordering data downloads of the NIR 'Enhanced' Color product.
Start mapping the Moon with the Clementine NIR 'Enhanced' Color data set
References
Gaddis, Lisa, Chris Isbell, Matt Staid, Eric Eliason, Ella Mae Lee, Lynn Weller, Tracie Sucharski, Paul Lucey, Dave Blewett, John Hinrichs, and Donovan Steutel, 2007 (in review), The Clementine NIR Global Lunar Mosaic, PDS Volumes USA_NASA_PDS_CL_5001 through 5078, produced by the U.S. Geological Survey and distributed online and on DVD media by the Planetary Data System.
Lucey, P.G., J.L. Hinrichs, and E. Malaret, Progress Toward Calibration of the Clementine Near Infrared Camera Data Set, Lunar and Planetary Science Conference XXXVIII, Abstract #1401, 1997.
Lucey, P.G., J. Hinrichs, C. Budney, G. Smith, C. Frost, B.R. Hawke, E. Malaret, M.S. Robinson, B. Bussey, T. Duxbury, D. Cook, P. Coffin, E. Eliason, T. Sucharski, A. McEwen, C.M. Pieters, Calibration of the Clementine Near Infrared Camera: Ready for Prime Time, Lunar and Planetary Science Conference XXXI, Abstract #1576, 1998.
Lucey, P.G., D.T. Blewett, E. Eliason, L.A. Weller, R. Sucharski, E. Malaret, J.L. Hinrichs, and P.D. Owensby, Optimized calibration constants for the Clementine NIR camera, Lunar and Planetary Science Conference XXIX, #1273, 2000.
UVVIS/NIR Overview | UVVIS 750nm Basemap | UVVIS 'Natural' Color | UVVIS Ratio 'False' Color | NIR 'Enhanced' Color | Moon | Top
Lunar Orbiter Digital Photographic Mosaic
Five Lunar Orbiter missions were launched by the U.S. in 1966 and 1967 to study the Moon. Lunar Orbiter images were photographic products acquired on the spacecraft during those five missions (LO-I through -V; Hansen, 1970; Bowker and Hughes, 1971). The first three missions mapped potential Apollo lunar landing sites. Lunar Orbiter IV photographed most of the near and far sides of the Moon medium- and high- resolutions. Lunar Orbiter V completed the photography of the far side and collected additional images of 36 sites of scientific interest. The global mosaic presented here is comprised largely of LO-IV and -V digital photographic images and high-resolution that were scanned and mosaicked at USGS (Gaddis et al., 2001, 2003; Becker et al., 2004, 2005; Weller et al., 2006, 2007). The nominal resolution of the mosaic is ~60 m/pixel.
Start mapping the Moon with the Lunar Orbiter Mosaic data set
References
Becker, T., L. Weller, L. Gaddis, D. Soltesz, D. Cook, A. Bennett, D. Galuszka, B. Redding, and J. Richie, 2004, Progress on Reviving Lunar Orbiter: Scanning, Archiving, and Cartographic Processing at USGS, LPS XXXV, abs. #1791.
Becker, T., L. Weller, L. Gaddis, D. Soltesz, D. Cook, B. Archinal, A. Bennett, T. McDaniel, B. Redding, and J. Richie, 2005, Lunar Orbiter Revived: Update on Final Stages of Scanning, Archiving, and Cartographic Processing at USGS, LPS XXXVI, abs. #1836.
Bowker, D.E. and J.K. Hughes, 1971, Lunar Orbiter Photographic Atlas of the Moon, NASA SP-206.
Gaddis, L.R., T. Sucharski, T. Becker, and A. Gitlin, 2001, Cartographic Processing of Digital Lunar Orbiter data, LPS XXXII, abs. #1892.
Gaddis, L., T. Becker, L. Weller, D. Cook, J. Richie, A. Bennett, B. Redding, and J. Shinaman, 2003, Reviving Lunar Orbiter: Scanning, Archiving, and Cartographic Processing at USGS, LPS XXXIV, abs. #1459.
Hansen, Thomas P., 1970, Guide to Lunar Orbiter Photographs, NASA SP-242.
Weller, L., B. Redding, T. Becker, L. Gaddis, R. Sucharski, D. Soltesz, D. Cook, B. Archinal, A. Bennett and T. McDaniel, 2006, Lunar Orbiter Revived: Very High Resolution Views of the Moon, LPS XXXVII, abs. #2143.
Weller, L., T. Becker, B. Archinal, A. Bennett, D. Cook, L. Gaddis, D. Galuska, R. Kirk, B. Redding, D. Soltesz, 2007, USGS Lunar Orbiter Digitization Project: Updates and Status, LPS XXXVIII, abstract #2092.
Lunar Prospector Datasets
Lunar Prospector data presented here are derived from Lunar Prospector Reduced Spectrometer source data provided by the PDS Geosciences Node. See the former site for introductory and detailed descriptive information pertaining to the original data source. Note especially units information and varying scale factors applied when ASCII table values were converted to raw/binary images. All products (5° and ½° cell size) are provided at 2pxl/°
In addition to the original ASCII table, newly derived products (this site) include a reformatted raw/binary image (.raw), an ISIS2 image cube (.cub), and an 8-bit JPEG browse image (*.jpg);
| Original ASCII table | .asc | Identical to original ASCII file.
See ASCII file header for more information |
| Raw/Binary Image | .raw | Raw/binary image. 720 samples x 360 lines
16-bit LSB Signed Integer Reprocessed with north at top of image |
| ISIS2 Image Cube | .cub | ISIS2 Image map. Simple Cylindrical Projection
2pxl/deg, -180,180 East Longitude -90,90 Latitude Range (north at top) |
| JPEG Browse Image | .jpg | Not a science product.
Intended for browse/viewing purposes only |
View table of Lunar Prospector data sets
References
Feldman W. C., B. L. Barraclough, K. R. Fuller, D. J. Lawrence, S. Maurice, M. C. Miller, T. H. Prettyman, and A. B. Binder, the Lunar Prospector Gamma-Ray and Neutron Spectrometers, Nuclear Instruments and Methods in Physics Research A, 422, 562-566, 1999.
Feldman, W. C., S. Maurice, D. J. Lawrence, R. C. Little, S. L. Lawson, O. Gasnault, R. C. Wiens, B. L. Barraclough, R. C. Elphic, T. H. Prettyman, J. T. Steinberg, and A. B. Binder, Evidence for water ice near lunar poles, J. Geophys. Res., in press, 2001c.
Lawrence, D. J., W. C. Feldman, R. C. Elphic, S. Maurice, T. H. Prettyman, and A. B. Binder, Iron abundances on the lunar surface as measured by the Lunar Prospector Gamma-Ray Spectrometer, 32nd Lunar and Planetary Science Conference, Abstract #1830, 2001a.
Lawrence D. J., et al., Data reduction procedures for the Lunar Prospector Gamma-ray Spectrometer, in preparation, 2001b.
Lawson, S. L., W. C. Feldman, D. J. Lawrence, K. R. Moore, S. Maurice, R. D. Belian, and A. B. Binder, Maps of lunar radon-222 and polonium-210, 33rd Lunar and Planetary Science Conference, Abstract #1835, 2002.
Maurice, S., et al., Data reduction procedures for the Lunar Prospector Neutron Spectrometer, in preparation, 2001a.
Prettyman, T. H., W. C. Feldman, D. J. Lawrence, G. W. McKinney, A. B. Binder, R. C. Elphic, O. M. Gasnault, S. Maurice, and K. R. Moore, Library least squares analysis of Lunar Prospector gamma-ray spectra, 33rd Lunar and Planetary Science Conference, Abstract #2012, 2002.
Mars Data Sets
The following table lists the highest available resolution for each data set. Click the data set name to jump down to a description of the data set.
| Data Set |
Resolution px/deg |
Scale km/px |
|---|---|---|
| Mars Viking Color | 64 | 0.9254 |
| Mars Viking Color-MDIM Merge | 64 | 0.9254 |
| Mars Viking MDIM (version 2) | 256 | 0.2314 |
| Mars Viking MDIM (version 1) | 256 | 0.2314 |
| Mars MGS MOLA Topography | 32 |
Viking Orbiter Visual Imaging Subsystem (VIS)
The Viking Visual Imaging Subsystem (VIS) on the Viking orbiters consisted of twin high-resolution, slow-scan television framing cameras. A filter wheel between the lens and shutter held six color filter positions, listed in the following table.
| Band Wavelength Range (µm) | Filter Description |
|---|---|
| 0.35 - 0.47 | Violet |
| 0.35 to 0.53 | Blue |
| 0.50 - 0.60 | Green |
| 0.48 - 0.70 | Minus-blue (visible spectrum above the blue wavelengths) |
| 0.55 - 0.70 | Red |
| Panchromatic | Clear (no filter) |
There are several Viking products available on Map-a-Planet. These products are described below.
Viking Color
The Viking Color data set is a natural color mosaic, combining the red, green, and blue Viking VIS bands into the respective channels of a color image.
Start mapping Mars with the Viking Color image data set
Viking Mars Digital Image Model Version 2 (MDIM2)
Viking MDIM2 is a specialized cartographic product generated from Viking VIS data (primarily the red, minus blue, and clear bands) described above, where albedo (surface brightness) was removed from the VIS mosaics, emphasizing topographic features. Each version of MDIM released by the USGS Astrogeology Research Program has accuracy, photometric, and cosmetic improvements. For more information about MDIM work, see the MDIM 2.1: Mars Global Digital Image Mosaic web page.
Start mapping Mars with the MDIM2 image data set
Viking Mars Digital Image Model Version 1 (MDIM1)
Viking MDIM1 is the first released version of a specialized cartographic product generated from Viking VIS data (primarily the red, minus blue, and clear bands) described above, where albedo (surface brightness) was removed from the VIS mosaics, emphasizing topographic features. Each version of MDIM released by the USGS Astrogeology Research Program has accuracy, photometric, and cosmetic improvements. For more information about MDIM work, see the MDIM 2.1: Mars Global Digital Image Mosaic web page.
Start mapping Mars with the MDIM1 image data set
Viking Color-MDIM Merge
The Viking Color-MDIM Merged data set is a product created by merging the Viking Color and MDIM1 data sets described above. This combination provides spectral and albedo with enhanced topography not apparent in the Viking Color data set.
Start mapping Mars with the Viking Color-MDIM Merge image data set
Mars Global Surveyor Mars Orbiter Laser Altimeter (MGS MOLA) Topography
The Mars Global Surveyor mission carries the Mars Orbiter Laser Altimeter (MOLA) instrument, which measures the height of surfaces on Mars. The data from MOLA have been used to create the most accurate topographic map of Mars to date. On Map-a-Planet, this data set is a grayscale image where the level brightness is equivalent to surface elevation (brighter areas are higher elevation than darker areas).
Start mapping Mars with the MGS MOLA Topography image data set
Satellites of Jupiter Data Sets
The following table lists the highest available resolution for each data set. Click the data set name to jump down to a description of the data set.
| Data Set |
Resolution px/deg |
Scale km/px |
|---|---|---|
| Callisto Galileo (grayscale) | 42 | 0.9974 |
| Io Galileo (grayscale) | 32 | |
| Io Galileo (Color) | 6 | |
| Ganymede Galileo (Color) | 45 | 0.9974 |
| Ganymede Galileo (grayscale) | 45 | |
| Europa Galileo (grayscale) | 54 |
Callisto: Galileo Solid State Imaging (SSI) and Voyagers 1 & 2 (Color)
This global map of Callisto utilizes the best image quality and moderate resolution coverage supplied by Galileo SSI (Solid State Imaging instrument) and Voyager 1 and 2. This mosaic was prepared by the USGS Astrogeology Research Program using the ISIS 2 image processing and cartographic system. The image data was selected on the basis of overall image quality, reasonable input resolution, and availability of moderate viewing and sun angles for topography. The average input resolution was 1.0 kilometers/pixel. The resolution ranged from 60 km/pixel for gap fill up to 400 meters/pixel. For more information, see the USGS Astrogeology Jupiter Satellites - Voyager and Galileo Global Mosaics project page.
Start mapping Callisto with the Galileo/Voyager grayscale image data set
Europa: Galileo Solid State Imaging (SSI) and Voyagers 1 & 2 (grayscale)
This global map base of Europa utilizes the best image quality and moderate resolution coverage supplied by Galileo SSI (Solid State Imaging instrument) and Voyager 1 and 2. This mosaic was prepared by the USGS Astrogeology Research Program using the ISIS 2 image processing and cartographic system. The image data was selected on the basis of overall image quality, reasonable input resolution, and availability of moderate viewing and sun angles for topography. For more information, see the USGS Astrogeology Jupiter Satellites - Voyager and Galileo Global Mosaics project page.
Start mapping Europa with the Galileo/Voyager grayscale image data set
Ganymede: Galileo Solid State Imaging (SSI) and Voyagers 1 & 2 (Color)
This global map base of Ganymede utilizes the best image quality and moderate resolution coverage supplied by Galileo Solid State Imaging (SSI) and Voyager 1 and 2. This mosaic was prepared by the USGS Astrogeology Research Program using the ISIS 2 image processing and cartographic system. The image data was selected on the basis of overall image quality, reasonable input resolution (from 20 km/pixel for gap fill to approximately 400 meters/pixel), and availability of moderate viewing and sun angles for topography. For more information, see the USGS Astrogeology Jupiter Satellites - Voyager and Galileo Global Mosaics project page.
Start mapping Ganymede with the Galileo/Voyager Color image data set
Ganymede: Galileo Solid State Imaging (SSI) and Voyagers 1 & 2 (grayscale)
This global map base of Ganymede utilizes the best image quality and moderate resolution coverage supplied by Galileo Solid State Imaging (SSI) and Voyager 1 and 2. This mosaic was prepared by the USGS Astrogeology Research Program using the ISIS 2 image processing and cartographic system. The image data was selected on the basis of overall image quality, reasonable input resolution (from 20 km/pixel for gap fill to approximately 400 meters/pixel), and availability of moderate viewing and sun angles for topography. For more information, see the USGS Astrogeology Jupiter Satellites - Voyager and Galileo Global Mosaics project page.
Start mapping Ganymede with the Galileo/Voyager grayscale image data set
Io: Galileo Solid State Imaging (SSI) (grayscale)
The best quality global monitoring images taken by the Galileo imaging system at spatial resolutions up to 1 km/pixel have been assembled here to depict the global and regional morphology of Io. This mosaic is made up of 32 monochrome images taken at various phase angles and local times of day, so care must be taken to note the solar illumination direction when deciding whether topographic features display positive or negative relief. In general, the illumination is from the west over longitudes 0 to 270 W, and from the east over longitudes 270 W to 360 W. The images were empirically adjusted in brightness and contrast to match one another in areas of overlap. Most of the images were taken in the clear filter, but green and 756 nm filter images were substituted when they were more detailed than other available images. Image resolutions range from 1.3 to 10 km/pixel along the equator, with the poorest coverage on the Jupiter-facing side of Io.
Start mapping Io with the Galileo (Color) image data set
References
David A. Williams, Laszlo P. Keszthelyi, David A. Crown, Windy L. Jaeger, Paul E. Geissler, Paul M. Schenk, Tammy L. Becker, "Techniques for the Global Geologic Mapping of Io using Voyager and Galileo datasets", submitted to Icarus, 2006.
Satellites of Saturn Data Sets
The following table lists the highest available resolution for each data set. Click the data set name to jump down to a description of the data set.
| Data Set |
Resolution px/deg |
Scale km/px |
|---|---|---|
| Rhea Voyager (grayscale) | 16 | |
| Dione Voyager (grayscale) | 16 | |
| Tethys Voyager (grayscale) | 16 | |
| Iapetus Voyager (grayscale) | 16 | |
| Enceladus Voyager (grayscale) | 16 |
Rhea: Voyager 1 & 2 (grayscale)
This image mosaic is one of several products created as the first step of cartography planning in support of the Cassini-Huygens Mission to Saturn & Titan. The data included in these mosaics were collected by both Voyager I and Voyager II missions. The Cassini spacecraft is targeting these moons and others during the mission. For more information about these mosaics, see the USGS Astrogeology Saturn Satellites - Voyager Global Image Maps project.
Start mapping Rhea with the Voyager (grayscale) image data set
Dione: Voyager 1 & 2 (grayscale)
This image mosaic is one of several products created as the first step of cartography planning in support of the Cassini-Huygens Mission to Saturn & Titan. The data included in these mosaics were collected by both Voyager I and Voyager II missions. The Cassini spacecraft is targeting these moons and others during the mission. For more information about these mosaics, see the USGS Astrogeology Saturn Satellites - Voyager Global Image Maps project.
Start mapping Dione with the Dione grayscale image data set
Tethys: Voyager 1 & 2 (grayscale)
This image mosaic is one of several products created as the first step of cartography planning in support of the Cassini-Huygens Mission to Saturn & Titan. The data included in these mosaics were collected by both Voyager I and Voyager II missions. The Cassini spacecraft is targeting these moons and others during the mission. For more information about these mosaics, see the USGS Astrogeology Saturn Satellites - Voyager Global Image Maps project.
Start mapping Tethys with the Voyager (grayscale) image data set
Iapetus: Voyager 1 & 2 (grayscale)
This image mosaic is one of several products created as the first step of cartography planning in support of the Cassini-Huygens Mission to Saturn & Titan. The data included in these mosaics were collected by both Voyager I and Voyager II missions. The Cassini spacecraft is targeting these moons and others during the mission. For more information about these mosaics, see the USGS Astrogeology Saturn Satellites - Voyager Global Image Maps project.
Start mapping Iapetus with the Voyager (grayscale) image data set
Enceladus: grayscale:
This image mosaic is one of several products created as the first step of cartography planning in support of the Cassini-Huygens Mission to Saturn & Titan. The data included in these mosaics were collected by both Voyager I and Voyager II missions. The Cassini spacecraft is targeting these moons and others during the mission. For more information about these mosaics, see the USGS Astrogeology Saturn Satellites - Voyager Global Image Maps project.
Start mapping Enceladus with the Voyager grayscale image data set
General Information About the Data Sets
Map-a-Planet uses global cartographic digital planetary image maps that have been prepared by the USGS Astrogeology Research Program for NASA. These image maps are the products of exhaustive cartographic projects based on data from the Viking Orbiter, Clementine, Voyager, Magellan, and other missions.