In addition, lobate debris aprons can show surface lineations as do rock glaciers on the Earth.
[5][6][7][8][9] In addition, radar studies in Deuteronilus Mensae show that all lobate debris aprons examined in that region contain ice.
Another major advantage of LDAs over other sources of Martian water is that they can easily be detected and mapped from orbit.
Recent analyses of the Nereidum Montes (~35°- 45°S, ~300° - 330°E), and Phlegra Montes (NNE - SSW, between latitudes 30° - 52°N) mountain ranges of Mars have revealed terrains rich in viscous flow features (VFFs), a cyro-geomorphological group of which lobate debris aprons are a sub-class.
[21][22] These LDAs were more extensive and older VFF features (hundreds of Ma) in the range, with the vast majority located in impact craters and surrounding massifs.
[23][24][25] Late Amazonian glaciation may have occurred in the mid-latitudes due to water-ice emplacement from higher latitudes.
[27] The datasets utilized in these studies included MRO Context Camera (CTX; ~5–6 m/pixel), High-Resolution Imaging Science Experiment (HiRISE) (~25 cm/pixel) images, MRO Shallow Radar (SHARAD), 128 pixel/degree (~463 m/pixel) Mars Global Surveyor (MGS), Mars Orbiter Laser Altimeter (MOLA), Digital Elevation Modelling (DEM), 100 m/pixel THEMIS Day and Night IR mosaics, and the GIS-based (ESRI ArcGIS Desktop) software.