The floors of the depressions not only show fewer impact craters, but a closer look also reveals intriguing materials and surface features that provide valuable insights into Martian history – particularly its climatic evolution. In many locations, a specific streamlined pattern is visible, characteristic of what is known as lineated valley fill (see annotated image). The same pattern was recently observed in the August Press Release on Acheron Fossae West , a region located at similar latitudes on the opposite side of the planet. Lineated valley fill typically forms through the viscous flow of ice-rich debris and is interpreted as a glacial feature, resembling terrestrial rock glaciers – glaciers covered by a layer of debris or rock. These deposits are believed to consist of more than 80% ice, buried beneath a thick cover of rocky material. When such glacial features fill a valley, they are referred to as lineated valley fill. However, when similar features occur inside impact craters, they are known as concentric crater fill. In the HRSC image, this is not the most prominent feature, but upon a closer look, concentric crater fill can be observed in a few craters (see annotated image). But how did these glacial features accumulate so far from the Martian poles?