Read the full article: Water in a martian desert
In the ancient cratered southern highlands of Mars, the faint traces of a wet past are seen in the form of channels (lower centre), fluidised debris around craters (bottom right) and blocks of eroded sediments (top left). Volcanic activity may have deposited the fine dusting of dark material visible in the top left.
The image was taken by the High Resolution Stereo Camera on ESA’s Mars Express on 15 January 2013 (orbit 11504), with a ground resolution of approximately 22 m per pixel. The image centre lies at about 4°S / 114°E, close to Tagus Valles in an unnamed region north of Hesperia Planum.
This close-up perspective view focuses on the craters in the centre of the main colour image . Here, a smaller crater clearly overlies the older, larger crater. To the right in this orientation lies a heavily deformed crater. Nearby, a channel appears to flow from the crater – perhaps this once transported water and sediments from a crater lake.
One of the deepest craters in the region of the main colour image lies in the foreground of this perspective view. Numerous landslides have occurred within this crater, leaving grooves in the crater wall as material slumped to the floor below.
This colour-coded overhead view is based on an ESA Mars Express High-Resolution Stereo Camera digital terrain model of the region to the north of Hesperia Planum, including part of the Tagus Valles. Centred at approximately 4°S / 114°E, the image has a ground resolution of 22 m per pixel. It was taken on 15 January 2013, during orbit 11504.
The region north of Hesperia Planum and close to Tagus Valles was imaged during orbit 11504 on 15 January 2013 by ESA’s Mars Express using the High Resolution Stereo Camera (HRSC). Data from HRSC’s nadir channel and one stereo channel have been combined to produce this anaglyph 3D image that can be viewed using stereoscopic glasses with red–green or red–blue filters. Centred at approximately 4°S / 114°E, the image has a ground resolution of 22 m per pixel.