This mosaic of Hebes Chasma is composed of eight single images taken with the High Resolution Stereo Camera on Mars Express, corresponding to orbits 360 (2 May 2004), 2149 (16 September 2005), 3217 (12 July 2006), 5142 (3 January 2008), 5160 (8 January 2008), 5178 (13 January 2008), 6241 (11 November 2008), and 7237 (24 August 2009). The image centre lies at about 1°S / 284°E.
Hebes Chasma is an enclosed, almost 8 km-deep trough stretching 315 km in an east–west direction and 125 km from north to south at its widest point. It sits about 300 km north of the vast Valles Marineris canyon. A flat-topped mesa is located in the centre of Hebes Chasma, which was likely shaped by the action of wind and water.
This colour-coded topography map shows the relative heights and depths of features in and around Hebes Chasma. White and red show the highest terrains, while blue and purple show the deepest.
This region of Mars was imaged by the High Resolution Stereo Camera on ESA’s Mars Express on eight occasions between 2004 and 2009 to create this new mosaic.
The details of the central mesa inside Hebes Chasma are seen in close-up detail in this perspective view. A horseshoe-shaped chunk has been taken out of one side of the mound (left in this image); the material has slumped down onto the floor of the valley below. A dark patch appears to pool like spilt ink across the debris. It is most likely loose material that has slid down the walls from an intermediate layer. Melted ice could have played a role by weakening the rocks to create its flow-like appearance.
Along the side of the mound fine horizontal layering is seen. The layers likely comprise a mix of wind-blown dust and ancient lake sediments, along with remnants of the older plateau.
A flat-topped mesa is located in the centre of Hebes Chasma and rises to a similar height as the surrounding plains. Exposed within the walls of the mesa are layers of sediments deposited by wind and water.
Numerous grooves are etched into the mountain, suggesting the material is weak and easily eroded. The walls of Hebes Chasma are also weak – a large landslide dominates the right side of this image.
Data from the nadir channel and one stereo channel of the High Resolution Stereo Camera on ESA’s Mars Express have been combined to produce this anaglyph 3D image of Hebes Chasma, which can be viewed using stereoscopic glasses with red–green or red–blue filters.