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Ganges Chasma Mound (false color) - Mars Reconnaissance Orbiter
An isolated mound of light-toned sediment located on the largely sand-covered floor of the Ganges Chasma canyon system. This mount is likely an isolated remnant of the Ganges Mensa deposit, a 100 x 50 km wide plateau of layered sulfate-bearing sediments located a short distance to the west. The soft nature of this rock has caused the formation of aerodynamic, wind-sculpted landforms called yardangs.
Minerals are more easily identified in infrared light than with visible light. This false color image uses much of the near infrared spectrum to highlight differences in mineralogy. The brown/red color of sandy regions in this image indicate unaltered volcanic minerals, primarily olivine, which is typical for Martian sand.The whitish/pale pink colors are typical of sulfate minerals, which are bland in the wavelengths of infrared light used to construct this image.
This image combines a 40 m/px false color CRISM hyperspectral image (2.53 micron, 1.51 micron, and 1.08 micron as RGB channels, respectively) with a 5 m/px monochrome CTX image. The CRISM image was collected on November 3, 2011, and the CTX image was collected on January 9, 2014.
Image Credit: NASA / JPL / MSSS / JHU / APL / Justin Cowart
Ganges Chasma Mound (false color) - Mars Reconnaissance Orbiter
An isolated mound of light-toned sediment located on the largely sand-covered floor of the Ganges Chasma canyon system. This mount is likely an isolated remnant of the Ganges Mensa deposit, a 100 x 50 km wide plateau of layered sulfate-bearing sediments located a short distance to the west. The soft nature of this rock has caused the formation of aerodynamic, wind-sculpted landforms called yardangs.
Minerals are more easily identified in infrared light than with visible light. This false color image uses much of the near infrared spectrum to highlight differences in mineralogy. The brown/red color of sandy regions in this image indicate unaltered volcanic minerals, primarily olivine, which is typical for Martian sand.The whitish/pale pink colors are typical of sulfate minerals, which are bland in the wavelengths of infrared light used to construct this image.
This image combines a 40 m/px false color CRISM hyperspectral image (2.53 micron, 1.51 micron, and 1.08 micron as RGB channels, respectively) with a 5 m/px monochrome CTX image. The CRISM image was collected on November 3, 2011, and the CTX image was collected on January 9, 2014.
Image Credit: NASA / JPL / MSSS / JHU / APL / Justin Cowart