The play of colors in the new HRSC image is indeed worth a look: bright surface deposits on the left side merge in the middle of the image with dark surface deposits from the right (see color image). The left side is composed of typical Martian regolith, while the dark areas could represent volcanic ash deposits made up of mafic minerals such as olivine and pyroxene. Interestingly, when the Viking Orbiter captured Mars in 1976, the dark material was not as widespread in Utopia Planitia as it is today. Aeolian Processes must have deposited it over the last 50 years (see right image). The lower left side shows brighter colors than the surroundings (see color image). Conversely, this material appears darker in nighttime thermal imagery, leading to the conclusion that it could be loose, fine-grained sand that loses the heat obtained during the day more quickly at night and therefore appears darker. On the right side, an approximately 15-kilometer-wide impact crater displays its prominent ejecta blanket (see annotated image). The ejecta blanket represents excavated material from the subsurface emplaced during the impact event. In this case, the ejecta shows a layered appearance, which may indicate subsurface ice melted during the impact. The impact crater is also covered by the dark material mentioned above. Besides the large crater there are numerous smaller craters with distinct ejecta blankets (see annotated image). The large crater itself shows a characteristic pattern on its floor, which is interpreted as concentric crater fill (see annotated image). Concentric crater fill is a common feature found in the mid-latitudes of Mars and is mostly composed of ice-rich material showing some “creep” movements. Similar deposits also occur in valleys, where they are referred to as lineated valley fill. Together, these features are considered analogous to terrestrial debris-covered glaciers.