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Europa Galileo and Voyager Image Mosaic Globe (shown on the left): The images used for the base of this globe were chosen from coverage supplied by the Galileo solid-state imaging (SSI) camera and Voyager 1 and 2 spacecraft. The individual images were radiometrically calibrated and photometrically normalized using a Lunar-Lambert function with empirically derived values. A linear correction based on the statistics of all overlapping areas was then applied to minimize image brightness variations. The image data were selected on the basis of overall image quality, reasonable original input resolution (from 20 km/pixel for gap fill to as much as 200 m/pixel), and availability of moderate emission/incidence angles for topography. Although consistency was achieved where possible, different filters were included for global image coverage as necessary: clear/blue for Voyager 1 and 2, and clear, near-IR (757 nm), and green (559 nm) for Galileo SSI. Individual images were projected to a Sinusoidal Equal-Area projection at an image resolution of 500 m/pixel, and a final global mosaic was constructed in this same Sinusoidal projection.
The global mosaic was then reprojected so that the entire surface of Europa is portrayed in a manner suitable for the production of a globe. A specialized program was used to create the "flower petal" appearance of the images; the area of each petal from 0 to 75 degrees latitude is in the Transverse Mercator projection, and the area from 75 to 90 degrees latitude is in the Lambert Azimuthal Equal-Area projection. The projections for adjacent petals overlap by 2 degrees of longitude, so that some features are shown twice.
Names shown on the globe are approved by the International Astronomical Union. The number, size, and placement of text were chosen for a 9-inch globe. A complete list of Europa nomenclature can be found at the Gazetteer of Planetary Nomenclature. The northern hemisphere is shown on the left, and the southern hemisphere is shown on the right.
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Ganymede Galileo and Voyager Image Mosaic Globe (shown on the left): The images used for the base of this globe were chosen from coverage supplied by the Galileo solid-state imaging (SSI) camera and Voyager 1 and 2 spacecraft. The monochrome and color data were both processed using Integrated Software for Imagers and Spectrometers (ISIS). The individual images were radiometrically calibrated and photometrically normalized using a Lunar-Lambert function with empirically derived values. A linear correction based on the statistics of all overlapping areas was then applied to minimize image brightness variations. The image data were selected on the basis of overall image quality, reasonable original input resolution (from 20 km/pixel for gap fill to as much as 180 m/pixel), and availability of moderate emission/incidence angles for topography and albedo.
The black and white monochrome base mosaic was constructed separately from the three-band color mosaic. Although consistency was achieved where possible, different filters were included for monochrome global image coverage as necessary: clear for Voyager 1 and 2; clear, near-IR (757 nm), and green (559 nm) for Galileo SSI. Individual images were projected to a Sinusoidal Equal-Area projection at an image resolution of 1 km/pixel.
The global color mosaic was processed in Sinusoidal projection with an image resolution of 6 km/pixel. The color utilized the SSI filters 1-micron (991 nm) wavelength for red, SSI 559 nm for green, and SSI 413 nm for violet. Where SSI color coverage was lacking in the longitude range of 210°-250°, Voyager 2 wide-angle images were included to complete the global coverage. The chosen filters for the Voyager 2 data were ~530 nm for green, and ~480-500 nm for blue. The red band was synthesized in this area based on statistics calculated from the surrounding SSI 1-micron (991 nm) data and SSI and Voyager data in the blue and green bands. The final global color mosaic was then scaled up to 1 km/pixel and merged with the monochrome mosaic. The north pole and south pole regions that lack digital color coverage have been completed with the monochrome map coverage.
The final global mosaic was then reprojected so that the entire surface of Ganymede is portrayed in a manner suitable for the production of a globe. A specialized program was used to create the "flower petal" appearance of the images; the area of each petal from 0 to 75 degrees latitude is in the Transverse Mercator projection, and the area from 75 to 90 degrees latitude is in the Lambert Azimuthal Equal-Area projection. The projections for adjacent petals overlap by 2 degrees of longitude, so that some features are shown twice.
Names shown on the globe are approved by the International Astronomical Union. The number, size, and placement of text were chosen for a 9-inch globe. A complete list of Ganymede nomenclature can be found at the Gazetteer of Planetary Nomenclature. The northern hemisphere is shown on the left, and the southern hemisphere is shown on the right.
New 7/17/2002
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Callisto Galileo and Voyager Image Mosaic Globe (shown on the left): The images used for the base of this globe were chosen from the best image quality and moderate resolution coverage supplied by Galileo SSI and Voyager 1 and 2 (Batson, 1987; Becker and others, 1998; Becker and others, 1999; Becker and others, 2001). The digital map was produced using Integrated Software for Imagers and Spectrometers (ISIS) (Eliason, 1997; Gaddis and others, 1997; Torson and Becker, 1997). The individual images were radiometrically calibrated and photometrically normalized using a Lunar-Lambert function with empirically derived values (McEwen, 1991; Kirk and others, 2000). A linear correction based on the statistics of all overlapping areas was then applied to minimize image brightness variations. The image data were selected on the basis of overall image quality, reasonable original input resolution (from 20 km/pixel for gap fill to as much as 150 m/pixel), and availability of moderate emission/incidence angles for topography. Although consistency was achieved where possible, different filters were included for global image coverage as necessary: clear for Voyager 1 and 2; clear and green (559 nm) for Galileo SSI. Individual images were projected to a Sinusoidal Equal-Area projection at an image resolution of 1.0 kilometer/pixel, and a final global mosaic was constructed in this same projection. The final mosaic was enhanced using commercial software.
The global mosaic was then reprojected so that the entire surface of Callisto is portrayed in a manner suitable for the production of a globe. A specialized program was used to create the "flower petal" appearance of the images; the area of each petal from 0 to 75 degrees latitude is in the Transverse Mercator projection, and the area from 75 to 90 degrees latitude is in the Lambert Azimuthal Equal-Area projection. The projections for adjacent petals overlap by 2 degrees of longitude, so that some features are shown twice.
Names shown on the globe are approved by the International Astronomical Union. The number, size, and placement of text were chosen for a 9-inch globe. A complete list of Callisto nomenclature can be found at the Gazetteer of Planetary Nomenclature. In the image, the northern hemisphere is shown on the left, and the southern hemisphere is shown on the right.
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Europa Galileo and Voyager Image Mosaic Map (shown on the left): This sheet is one in a series of maps of the Galilean satellites of Jupiter at a nominal scale of 1:15,000,000. This series is based on data from the Galileo Orbiter Solid-State Imaging (SSI) camera and the Voyager 1 and 2 spacecraft.
Mercator and Polar Stereographic projections used for this map of Europa are based on a sphere having a radius of 1,562.09 km. The scale is 1:8,388,000 at ±56° latitude for both projections. Longitude increases to the west in accordance with the International Astronomical Union (1971; Davies and others, 1996). Latitude is planetographic.
The process of creating a geometric control network began with selecting control points on the individual images, making pixel measurements of their locations, using reseau locations to correct for geometric distortions, and converting the measurements to millimeters in the focal plane. These data are combined with the camera focal lengths and navigation solutions as input to a photogrammetric triangulation solution (Davies and others, 1998; Davies and Katayama, 1981). The solution used here was computed at the RAND Corporation in June 2000. Solved parameters include the radius (given above) of the best-fitting sphere, the coordinates of the control points, the three orientation angles of the camera at each exposure (right ascension, declination, and twist), and an angle (W0) that defines the orientation of Europa in space. W0-in this solution 36.022°-is the angle along the equator to the east, between the 0° meridian and the equator's intersection with the celestial equator at the standard epoch J2000.0. This solution places the crater Cilix at its defined longitude of 182° west (Davies and others, 1996).
This global map base uses the best image quality and moderate resolution coverage supplied by Galileo SSI and Voyager 1 and 2 (Batson, 1987; Becker and others, 1998; 1999; 2001). The digital map was produced using Integrated Software for Imagers and Spectrometers (ISIS) (Eliason, 1997; Gaddis and others, 1997; Torson and Becker, 1997). The individual images were radiometrically calibrated and photometrically normalized using a Lunar-Lambert function with empirically derived values (McEwen, 1991; Kirk and others, 2000). A linear correction based on the statistics of all overlapping areas was then applied to minimize image brightness variations. The image data were selected on the basis of overall image quality, reasonable original input resolution (from 20 km/pixel for gap fill to as much as 40 m/pixel), and availability of moderate emission/incidence angles for topography and albedo. Although consistency was achieved where possible, different filters were included for global image coverage as necessary: clear/blue for Voyager 1 and 2; clear, near-IR (757 nm), and green (559 nm) for Galileo SSI. Individual images were projected to a Sinusoidal Equal-Area projection at an image resolution of 500 m/pixel. The final constructed Sinusoidal projection mosaic was then reprojected to the Mercator and Polar Stereographic projections included on this sheet.
Names on this sheet are approved by the International Astronomical Union (IAU, 1980, 1986, 1999, and 2001). Names have been applied for features clearly visible at the scale of this map; for a complete list of nomenclature of Europa, please see Gazetteer of Planetary Nomenclature. Font color was chosen only for readability. Je 15M CMN: Abbreviation for Jupiter, Europa (satellite): 1:15,000,000 series, controlled mosaic (CM), nomenclature (N) (Greeley and Batson, 1990).
Batson, R.M., 1987, Digital cartography of the planets-New methods, its status, and its future: Photogrammetric Engineering and Remote Sensing, v. 53, no. 9, p. 1211-1218.
Becker, T.L., Archinal, B., Colvin, T.R., Davies, M.E., Gitlin, A., Kirk, R.L., and Weller, L., 2001, Final digital global maps of Ganymede, Europa, and Callisto, in Lunar and Planetary Science Conference XXXII: Houston, Lunar and Planetary Institute, abs. no. 2009 [CD-ROM].
Becker, T.L, Rosanova, T., Cook, D., Davies, M.E., Colvin, T.R., Acton, C., Bachman, N., Kirk, R.L., and Gaddis, L.R., 1999, Progress in improvement of geodetic control and production of final image mosaics for Callisto and Ganymede, in Lunar and Planetary Science Conference XXX: Houston, Lunar and Planetary Institute, abs. no. 1692 [CD-ROM].
Becker, T.L., Rosanova, T., Gaddis, L.R., McEwen, A.S., Phillips, C.B., Davies, M.E., and Colvin, T.R., 1998, Cartographic processing of the Galileo SSI data-An update on the production of global mosaics of the Galilean satellites, in Lunar and Planetary Science Conference XXIX: Houston, Lunar and Planetary Institute, abs. no. 1892 [CD-ROM].
Davies, M.E., Abalakin, V.K., Bursa, M., Lieske, J.H., Morando, B., Morrison, D., Seidelmann, P.K., Sinclair, A.T., Yallop, B., and Tjuflin, Y.S., 1996, Report of the IAU/IAG/COSPAR Working Group on Cartographic Coordinates and Rotational Elements of the Planets and Satellites, 1994: Celestial Mechanics and Dynamical Astronomy, v. 63, p. 127-148.
Davies, M.E., Colvin, T.R., Oberst, J., Zeitler, W., Schuster, P., Neukum, G., McEwen, A.S., Phillips, C.B., Thomas, P.C., Veverka, J., Belton, M.J.S., and Schubert, G., 1998, The control networks of the Galilean satellites and implications for global shape: Icarus, v. 135, p. 372-376.
Davies, M.E., and Katayama, F.Y., 1981, Coordinates of features on the Galilean satellites: Journal of Geophysical Research, v. 86, no. A10, p. 8635-8657.
Eliason, E.M., 1997, Production of Digital Image Models using the ISIS system, in Lunar and Planetary Science Conference XXVIII: Houston, Lunar and Planetary Institute, p. 331.
Gaddis, L.R., Anderson, J., Becker, K., Becker, T.L., Cook, D., Edwards, K., Eliason, E.M., Hare, T., Kieffer, H.H., Lee, E.M., Mathews, J., Soderblom, L.A., Sucharski, T., Torson, J., McEwen, A.S., Robinson, M., 1997, An overview of the Integrated Software for Imaging Spectrometers (ISIS), in Lunar and Planetary Science Conference XXVIII: Houston, Lunar and Planetary Institute, p. 387.
Greeley, R., and Batson, R.M., 1990, Planetary Mapping, Cambridge University Press, Cambridge, p. 274-275.
International Astronomical Union, 1971, Commission 16-Physical study of planets and satellites, in Proceedings of the 14th General Assembly, Brighton, 1970: Transactions of the International Astronomical Union, v. 14B, p. 128-137.
---1980, Working Group for Planetary System Nomenclature, in Proceedings of the 17th General Assembly, Montreal, 1979: Transactions of the International Astronomical Union, v.17B, p. 300.
---1986, Working Group for Planetary System Nomenclature, in Proceedings of the 19th General Assembly, New Delhi, 1985: Transactions of the International Astronomical Union, v.19B, p. 351.
---1999, Working Group for Planetary System Nomenclature, in Proceedings of the 23rd General Assembly, Kyoto, 1997: Transactions of the International Astronomical Union, v.23B, p. 234-235.
---2001, Working Group for Planetary System Nomenclature, in Proceedings of the 24th General Assembly, Manchester, 2000: Transactions of the International Astronomical Union, v.24B [in press].
Kirk, R.L., Thompson, K.T., Becker, T.L., and Lee, E.M., 2000, Photometric modeling for planetary cartography, in Lunar and Planetary Science Conference XXXI: Houston, Lunar and Planetary Institute, abs. no. 2025 [CD-ROM].
McEwen, A.S., 1991, Photometric functions for photoclinometry and other applications: Icarus, v. 92, p. 298-311.
Torson, J.M., and Becker, K.J., 1997, ISIS-A software architecture for processing planetary images, in Lunar and Planetary Science Conference XXVIII: Houston, Lunar and Planetary Institute, p. 1443.
New 7/17/2002
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Callisto Galileo and Voyager Image Mosaic Map (shown on the left): This sheet is one in a series of maps of the Galilean satellites of Jupiter at a nominal scale of 1:15,000,000. This series is based on data from the Galileo Orbiter Solid-State Imaging (SSI) camera and the cameras of the Voyager 1 and 2 spacecraft.
Mercator and Polar Stereographic projections used for this map of Callisto are based on a sphere having a radius of 2,409.3 km. The scale is 1:8,388,000 at ±56° latitude for both projections. Longitude increases to the west in accordance with the International Astronomical Union (1971) (Seidelmann and others, 2002).
The geometric control network was computed at the RAND Corporation using RAND's most recent solution as of April 1999 (Davies and Katayama, 1981; Davies and others, 1998). This process involved selecting control points on the individual images, making pixel measurements of their locations, using reseau locations to correct for geometric distortions, and converting the measurements to millimeters in the focal plane. These data are combined with the camera focal lengths and navigation solutions as input to photogrammetric triangulation software that solves for the best-fit sphere, the coordinates of the control points, the three orientation angles of the camera at each exposure (right ascension, declination, and twist), and an angle (W0) which defines the orientation of Callisto in space. W0-in this solution 259.51°-is the angle along the equator to the east, between the 0° meridian and the equator's intersection with the celestial equator at the standard epoch J2000.0. This solution places the crater Saga at its defined longitude of 326° west (Seidelmann and others, 2002).
This global map base uses the best image quality and moderate resolution coverage supplied by Galileo SSI and Voyager 1 and 2 (Batson, 1987; Becker and others, 1998; Becker and others, 1999; Becker and others, 2001). The digital map was produced using Integrated Software for Imagers and Spectrometers (ISIS) (Eliason, 1997; Gaddis and others, 1997; Torson and Becker, 1997). The individual images were radiometrically calibrated and photometrically normalized using a Lunar-Lambert function with empirically derived values (McEwen, 1991; Kirk and others, 2000). A linear correction based on the statistics of all overlapping areas was then applied to minimize image brightness variations. The image data were selected on the basis of overall image quality, reasonable original input resolution (from 20 km/pixel for gap fill to as much as 150 m/pixel), and availability of moderate emission/incidence angles for topography. Although consistency was achieved where possible, different filters were included for global image coverage as necessary: clear for Voyager 1 and 2; clear and green (559 nm) for Galileo SSI. Individual images were projected to a Sinusoidal Equal-Area projection at an image resolution of 1.0 kilometer/pixel. The final constructed Sinusoidal projection mosaic was then reprojected to the Mercator and Polar Stereographic projections included on this sheet. The final mosaic was enhanced using commercial software.
Names on this sheet are approved by the International Astronomical Union. Names have been applied for features clearly visible at the scale of this map; for a complete list of nomenclature for Callisto, please see the Gazeteer of Planetary Nomenclature. Font color was chosen only for readability.
Jc 15M CMN: Abbreviation for Jupiter, Callisto (satellite): 1:15,000,000 series, controlled mosaic (CM), nomenclature (N) (Greeley and Batson, 1990).
Batson, R.M., 1987, Digital cartography of the planets-New methods, its status, and its future: Photogrammetric Engineering and Remote Sensing, v. 53, no. 9, p. 1211-1218.
Becker, T.L., Archinal, B., Colvin, T.R., Davies, M.E., Gitlin, A., Kirk, R.L., and Weller, L., 2001, Final digital global maps of Ganymede, Europa, and Callisto, in Lunar and Planetary Science Conference XXXII: Houston, Lunar and Planetary Institute, abs. no. 2009 [CD-ROM].
Becker, T.L., Rosanova, T., Cook, D., Davies, M.E., Colvin, T.R., Acton, C., Bachman, N., Kirk, R.L., and Gaddis, L.R., 1999, Progress in improvement of geodetic control and production of final image mosaics for Callisto and Ganymede, in Lunar and Planetary Science Conference XXX: Houston, Lunar and Planetary Institute, abs. no. 1692 [CD-ROM].
Becker, T.L., Rosanova, T., Gaddis, L.R., McEwen, A.S., Phillips, C.B., Davies, M.E., and Colvin, T.R., 1998, Cartographic processing of the Galileo SSI data-An update on the production of global mosaics of the Galilean satellites, in Lunar and Planetary Science Conference XXIX: Houston, Lunar and Planetary Institute, abs. no. 1892 [CD-ROM].
Davies, M.E., and Katayama, F.Y., 1981, Coordinates of features on the Galilean satellites: Journal of Geophysical Research, v. 86, no. A10, p. 8635-8657.
Eliason, E.M., 1997, Production of Digital Image Models using the ISIS system, in Lunar and Planetary Science Conference XXVIII: Houston, Lunar and Planetary Institute, p. 331.
Gaddis, L.R., Anderson, J., Becker, K.J., Becker, T.L., Cook, D., Edwards, K., Eliason, E.M., Hare, T., Kieffer, H.H., Lee, E.M., Mathews, J., Soderblom, L.A., Sucharski, T., Torson, J., McEwen, A.S., Robinson, M.S., 1997, An overview of the Integrated Software for Imaging Spectrometers (ISIS), in Lunar and Planetary Science Conference XXVIII: Houston, Lunar and Planetary Institute, p. 387.
Greeley, R., and Batson, R.M., 1990, Planetary Mapping: Cambridge University Press, Cambridge, p. 274-275.
International Astronomical Union, 1971, Commission 16-Physical study of planets and satellites, in Proceedings of the 14th General Assembly, Brighton, 1970: Transactions of the International Astronomical Union, v. 14B, p. 128-137.
Kirk, R.L., Thompson, K.T., Becker, T.L., and Lee, E.M., 2000, Photometric modeling for planetary cartography, in Lunar and Planetary Science Conference XXXI: Houston, Lunar and Planetary Institute, abs. no. 2025 [CD-ROM].
McEwen, A.S., 1991, Photometric functions for photoclinometry and other applications: Icarus, v. 92, p. 298-311.
Seidelmann, P.K., Abalakin, V.K., Bursa, M., Davies, M.E., de Bergh, C., Lieske, J.H., Oberst, J., Simon, J.L., Standish, E.M., Stooke, P., and Thomas, P.C., 2002, Report of the IAU/IAG Working Group on Cartographic and Rotational Elements of the Planets and Satellites-2000: Celestial Mechanics and Dynamical Astronomy, v. 82, p. 83-110.
Torson, J.M., and Becker, K.J., 1997, ISIS-A software architecture for processing planetary images, in Lunar and Planetary Science Conference XXVIII: Houston, Lunar and Planetary Institute, p. 1443.
New 7/17/2002
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Download: |
Ganymede Galileo and Voyager Image Mosaic Map (shown on the left): This sheet is one in a series of maps of the Galilean satellites of Jupiter at a nominal scale of 1:15,000,000. This series is based on data from the Galileo Orbiter Solid-State Imaging (SSI) camera and the Voyager 1 and 2 spacecraft.
Mercator and Polar Stereographic projections used for this map of Ganymede are based on a sphere having a radius of 2632.345 km. The scale is 1:8,388,000 at ±56° latitude for both projections. Longitude increases to the west in accordance with the International Astronomical Union (1971) (Davies and others, 1996). Latitude is planetographic.
The geometric control network was computed at the RAND Corporation (Davies and others, 1998; Davies and Katayama, 1981). (This map of Ganymede utilized RAND's most recent solution as of November 1999). This process involved selecting control points on the individual images, making pixel measurements of their locations, using reseau locations to correct for geometric distortions, and converting the measurements to millimeters in the focal plane. These data are combined with the camera focal lengths and navigation solutions as input to photogrammetric triangulation software that solves for the best-fit sphere, the coordinates of the control points, the three orientation angles of the camera at each exposure (right ascension, declination, and twist), and an angle (W0) which defines the orientation of Ganymede in space. W0-in this solution 44.064°-is the angle along the equator to the east, between the 0° meridian and the equator's intersection with the celestial equator at the standard epoch J2000.0. This solution places the crater Anat at its defined longitude of 128° (Davies and others, 1996).
This global map base uses the best image quality and moderate resolution coverage supplied by Galileo SSI and Voyager 1 and 2 (Batson, 1987; Becker and others, 1998; Becker and others, 1999; Becker and others, 2001). The monochrome and color data were both processed using Integrated Software for Imagers and Spectrometers (ISIS) (Eliason, 1997; Gaddis and others, 1997; Torson and Becker, 1997). The individual images were radiometrically calibrated and photometrically normalized using a Lunar-Lambert function with empirically derived values (McEwen, 1991; Kirk and others, 2000). A linear correction based on the statistics of all overlapping areas was then applied to minimize image brightness variations. The image data were selected on the basis of overall image quality, reasonable original input resolution (from 20 km/pixel for gap fill to as much as 180 m/pixel), and availability of moderate emission/incidence angles for topography and albedo. The black and white monochrome base mosaic was constructed separately from the three-band color mosaic. Although consistency was achieved where possible, different filters were included for the monochrome global image coverage as necessary: clear for Voyager 1 and 2; clear, near-IR (757 nm), and green (559 nm) for Galileo SSI. Individual images were projected to a Sinusoidal Equal-Area projection at an image resolution of 1.0 km/pixel. The global color map was processed in Sinusoidal projection with an image resolution of 6.0 km/pixel. The color utilized the SSI filters 1-micron (991 nm) wavelength for red, SSI 559 nm for green, and SSI 413 nm for violet. Where SSI color coverage was lacking in the longitude range of 210°-250°, Voyager 2 wide-angle images were included to complete the global coverage . The chosen filters for the Voyager 2 data were ~530 nm for green, and ~480-500 nm for blue. The red band was synthesized in this area based on statistics calculated from the surrounding SSI 1-micron (991 nm) data and SSI and Voyager data in the green and blue bands. The final global color map was then scaled up to 1.0 km/pixel and merged with the monochrome base mosaic. The north pole and south pole regions that lack digital color coverage have been completed with the monochrome map coverage. The final constructed Sinusoidal projection mosaic was then reprojected to the Mercator and Polar Stereographic projections included on this sheet. The color of the final mosaic was enhanced using commercial software.
Names on this sheet are approved by the International Astronomical Union (IAU, 1980, 1986, 1999, and 2001). Names have been applied for features clearly visible at the scale of this map; for a complete list of nomenclature for Ganymede, please see the Gazeteer of Planetary Nomenclature.
Jg 15M CMNK: Abbreviation for Jupiter, Ganymede (satellite): 1:15,000,000 series, controlled mosaic (CM), nomenclature (N), color (K) (Greeley and Batson, 1990).
Batson, R.M., 1987, Digital cartography of the planets-New methods, its status, and its future: Photogrammetric Engineering and Remote Sensing, v. 53, no. 9, p. 1211-1218.
Becker, T.L., Archinal, B., Colvin, T.R., Davies, M.E., Gitlin, A., Kirk, R.L., and Weller, L., 2001, Final digital global maps of Ganymede, Europa, and Callisto, in Lunar and Planetary Science Conference XXXII: Houston, Lunar and Planetary Institute, abs. no. 2009 [CD-ROM].
Becker, T.L, Rosanova, T., Cook, D., Davies, M.E., Colvin, T.R., Acton, C., Bachman, N., Kirk, R.L., and Gaddis, L.R., 1999, Progress in improvement of geodetic control and production of final image mosaics for Callisto and Ganymede, in Lunar and Planetary Science Conference XXX: Houston, Lunar and Planetary Institute, abs. no. 1692 [CD-ROM].
Becker, T.L., Rosanova, T., Gaddis, L.R., McEwen, A.S., Phillips, C.B., Davies, M.E., and Colvin, T.R., 1998, Cartographic processing of the Galileo SSI data-An update on the production of global mosaics of the Galilean satellites, in Lunar and Planetary Science Conference XXIX: Houston, Lunar and Planetary Institute, abs. no. 1892 [CD-ROM].
Davies, M.E., Abalakin, V.K., Bursa, M., Lieske, J.H., Morando, B., Morrison, D., Seidelmann, P.K., Sinclair, A.T., Yallop, B., and Tjuflin, Y.S., 1996, Report of the IAU/IAG/COSPAR Working Group on Cartographic Coordinates and Rotational Elements of the Planets and Satellites, 1994: Celestial Mechanics and Dynamical Astronomy, v. 63, p. 127-148.
Davies, M.E., Colvin, T.R., Oberst, J., Zeitler, W., Schuster, P., Neukum, G., McEwen, A.S., Phillips, C.B., Thomas, P.C., Veverka, J., Belton, M.J.S., and Schubert, G., 1998, The control networks of the Galilean satellites and implications for global shape: Icarus, v. 135, p. 372-376.
Davies, M.E., and Katayama, F.Y., 1981, Coordinates of features on the Galilean satellites: Journal of Geophysical Research, v. 86, no. A10, p. 8635-8657.
Eliason, E.M., 1997, Production of Digital Image Models using the ISIS system, in Lunar and Planetary Science Conference XXVIII: Houston, Lunar and Planetary Institute, p. 331.
Gaddis, L.R., Anderson, J., Becker, K., Becker, T.L., Cook, D., Edwards, K., Eliason, E.M., Hare, T., Kieffer, H.H., Lee, E.M., Mathews, J., Soderblom, L.A., Sucharski, T., Torson, J., McEwen, A.S., Robinson, M., 1997, An overview of the Integrated Software for Imaging Spectrometers (ISIS), in Lunar and Planetary Science Conference XXVIII: Houston, Lunar and Planetary Institute, p. 387.
Greeley, R., and Batson, R.M., 1990, Planetary mapping; Cambridge University Press, Cambridge, p. 274-275.
International Astronomical Union, 1971, Commission 16-Physical study of planets and satellites, in Proceedings of the 14th General Assembly, Brighton, 1970: Transactions of the International Astronomical Union, v. 14B, p. 128-137.
---1980, Working Group for Planetary System Nomenclature, in Proceedings of the 17th General Assembly, Montreal, 1979: Transactions of the International Astronomical Union, v. 17B, p. 300.
---1986, Working Group for Planetary System Nomenclature, in Proceedings of the 19th General Assembly, New Delhi, 1985: Transactions of the International Astronomical Union, v. 19B, p. 351.
---1999, Working Group for Planetary System Nomenclature, in Proceedings of the 23rd General Assembly, Kyoto, 1997: Transactions of the International Astronomical Union, v. 23B, p. 234-235.
---2001, Working Group for Planetary System Nomenclature, in Proceedings of the 24th General Assembly, Manchester, 2000: Transactions of the International Astronomical Union, v. 24B [in press].
Kirk, R.L., Thompson, K.T., Becker, T.L., and Lee, E.M., 2000, Photometric modeling for planetary cartography, in Lunar and Planetary Science Conference XXXI: Houston, Lunar and Planetary Institute, abs. no. 2025 [CD-ROM].
McEwen, A.S., 1991, Photometric functions for photoclinometry and other applications: Icarus, v. 92, p. 298-311.
Torson, J.M., and Becker, K.J., 1997, ISIS-A software architecture for processing planetary images, in Lunar and Planetary Science Conference XXVIII: Houston, Lunar and Planetary Institute, p. 1443.
For information on how to order USGS planetary maps, please refer to the our Planetary Mapping Program page Map Prices and Information.
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