WMS
WMS Titan Server
Planetary WMS service hosted by Astrogeology, USGS
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Titan_Simple_Cylindrical_Rasters
WMS Titan Server
Planetary WMS service hosted by Astrogeology, USGS
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CASSINI
Titan Global Mosaic
PIA19658: Map of Titan - October 2015 . This global digital map of Saturn's moon Titan was created using images taken by the Cassini spacecraft's imaging science subsystem (ISS). The map was produced in June 2015 using data collected through Cassini's flyby on April 7, 2014, known as T100. The images were taken using a filter centered at 938 nanometers, allowing researchers to examine variations in albedo (or inherent brightness) across the surface of Titan. Because of the scattering of light by Titan's dense atmosphere, no topographic shading is visible in these images. The map is an equidistant projection and has a scale of 2.5 miles (4 kilometers) per pixel. Actual resolution varies greatly across the map, with the best coverage (close to the map scale) along the equator near the center of the map at 180 degrees west longitude. The lowest resolution coverage can be seen in the northern mid-latitudes on the sub-Saturn hemisphere.Credit: NASA/JPL-Caltech/SSI
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Titan_ISS_Controlled_Mosaic
Titan ISS Preliminary Controlled Mosaic
Controlled Mosaic of Titan by the Astrogeology Science Center, USGS, Flagstaff, AZ. Preliminary version completed in Jan. 2013. This near-global (45 to -65 latitude, 360 degrees longitude) digital map of Saturn's moon Titan was created using 702 images (21 flybys) taken by the Cassini spacecraft's imaging science subsystem (ISS). The mean square positional error of 1.6 km (for 7848 points) was calculated during the full least squares bundle adjusment. The map is an equidistant projection and has a scale of 450 meters per pixel. Actual resolution varies greatly across the map, with the best coverage (close to the map scale) along the equator near the center of the map at 180 degrees west longitude and near the left and right edges at 0 and 360 degrees west longitude. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. Credit: USGS/NASA/JPL-Caltech/Space Science Institute. https://www.lpi.usra.edu/meetings/lpsc2013/pdf/2957.pdf
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Titan_HiSAR_Mosaic
Titan HiSAR Global Mosaic
Global map of Titan's surface showing the coverage derived from Synthetic Aperture Radar (SAR) and High Altitude Synthetic Aperture Radar (HiSAR) images. This mosaic merges Cassini SAR/HiSAR swaths through flyby T104 into a single mosaic. This is a preliminary product.
The Cassini Titan Radio Detection and Ranging (RADAR) Mapper plays a significant role in investigating the surface of Titan. This multi-mode radar instrument operates in the 13.8 GHz Ku-band (or 2.2 cm wavelength) and is designed to probe the optically inaccessible surface of Titan. The four different modes of the instrument Synthetic Aperture Radar (SAR) imaging, Altimetry, Scatterometry and Radiometry allow surface imaging as well as topographic mapping at spacecraft altitudes between 100,000 km and about 1,000 km, with resolutions for the modes ranging from 100 s of km to a few hundred meters (Elachi et al. 2005) . The observations, particularly when performed in the active modes of SAR, altimetry and scatterometry, are largely unaffected by atmospheric contributions.
References: Elachi, C., et al. (2005), Cassini radar views the surface of Titan, Science, 308, 970-974.
Stephan, K., et al. (2009), Mapping products of Titan's surface, in Titan From Cassini-Huygens, edited by R. H. Brown, and M. Dougherty, pp. 489-510, Springer, New York.
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