The highland regions of the southern hemisphere of Mars are covered with impact craters. The craters are much more numerous than in the northern hemisphere, which proves that these regions are among the oldest on the planet. One of these regions is called Noachis Terra and gave its name to the Noachian Period, an epoch that lasted from approximately 4.1 to 3.7 billion years ago and was marked by a strong bombardment by meteorites and asteroids. In this early phase of the planet, large regions were topographically shaped, hence the name Noah, after the ark builder in the Old Testament. The images show three superimposed impact craters. The largest of them measures 45 kilometres across, the middle one approximately 34 and the smallest 28. One scenario for the formation of the craters could be that a meteoroid broke into at least three pieces before all three bodies hit the surface of Mars in succession.

However, it could also be a coincidence that three impactors hit Mars independently at almost the same location over a somewhat longer time interval. Due to the fact that there are still residues of its ejecta blanket around the smallest crater, it is obvious that this smaller crater was formed after the two larger ones. Their ejecta blankets have long since been eroded and blurred. At the northern rim of the crater triplet (top right in the color image, color-coded terrain model, anaglyph) another small, circular structure is visible, possibly representing a fourth, now filled impact crater.

Like many other impact craters in the southern highlands, these three craters show typical rims that have already been smoothed out by erosion, as well as shallow and fairly flat crater floors, indicating that they are filled with sediment. Parts of the crater walls seem to have 'melted' and sunk into the centre of the crater depression, and numerous wide gullies cut through the slopes. Particularly striking are the linear structures in the northernmost crater (lower right in the color image, color-coded terrain model, anaglyph). Its surface morphology resembles that of terrestrial block or debris glaciers, which are common in alpine and polar regions.

This typical flow structure was formed when a mixture of debris and ice from a glacier in the crater flowed downhill to the centre of the crater triplet at a breakthrough in the inner crater rim. The debris traces the movements of the plastic ice flow in the subsurface. This is particularly visible on the colour-coded terrain model. The dark patch in the largest crater represents a small accumulation of dark sands, which form numerous and quite impressive dune fields elsewhere on Mars.

The plain around the impact craters, which also has a smooth, flat surface, shows interesting landscape features. It is not covered by countless small and medium-sized impact craters, as one would expect for a surface of this age on Mars. Secondary craters, which are formed when ejected material hits the area around a newly formed crater, are not visible either. Only a handful of bowl-shaped, lightly eroded and therefore young craters can be found there. It appears that craters older than a certain age have been subject to 'melting' and that many of the smaller and medium-sized impact craters that were even older have disappeared as a result. Ice in the Marian subsurface seems to have played the key role in this levelling process.

Given enough time, smaller surface structures formed on an ice-rich surface may also 'melt' again due to the flow of the ice, breaking down to a certain extent and smoothing the surface again. The process, which is typical of glacial activity on Mars, is referred to as 'terrain softening'. This observation shows that there were once large quantities of water on Mars. They created glacier-like flow structures with very large ice masses, especially during the Noachian Period. Today, most of the glacier ice has long since sublimed and left the debris masses it carried with it as witnesses of its flow processes, similar to glacial moraines on Earth. However, ground ice is still abundant on Mars today. It was first detected in 2008 by NASA’s Phoenix lander in the high latitudes of the northern lowlands.