Figure 1. (A) Topographic map of Aeolis Dorsa, Mars. Red box highlights the study site channel AD1; yellow shaded regions demarcate fan-like remnants interpreted as deltas from the literature ( Di Achille and Hynek, 2010 ) and from primary observations. Three illustrative basins (a, b, c

Figure 1. Sinuous ridges in Aeolis Dorsa, Mars, shown in Mars Reconnaissance Orbiter Context Camera (CTX) images ( Malin et al., 2007 ). (A) Sinuous ridge (black arrows; Mars ridge 3 in Section S5 of the Supplemental Material [see footnote 1 ]) classified as “thin” and interpreted as an inverted

TABLE 1. CLASSIFICATIONS OF DEPOSITS IN AEOLIS DORSA, MARS

Figure 5. Examples of thin features in Aeolis Dorsa. See Figure 1 for locations. Scale bars in lower left corners are 100 m wide, chevrons in lower right corners point north, and illumination is from the northwest. (A) Relatively straight thin features may have sharp crests and/or flat-topped

Figure 11. Units in southeast Aeolis Dorsa. See Figure 9 for area locations. (A) Network of fluvial channel fills (blue arrows) has a thin fluvial channel fill (green arrow) stratigraphically stacked on top. (B) Fluvial channel fills form a subparallel network (network 1) and dendritic network

Figure 3. Examples of flat features in Aeolis Dorsa. See Figure 1 for location. Scale bars in the lower left corners are 100 m wide, chevrons in lower right corners point north, and illumination is from the northwest. (A) HiRISE image mosaic shows type 1 and type 2 flat features forming

Figure 7. Examples of fan features in Aeolis Dorsa. See Figure 1 for locations. (A) An example of a fan with radiating ridges (pink arrows), which have been interpreted as alluvial fan deposits (e.g., Burr et al., 2009 ; Kite et al., 2015a ). Black arrow points downslope from the fan head

Figure 9. Delineations of over 1600 individual features in the Aeolis Dorsa region displayed over topographic shaded relief and colors, derived from Mars Orbiter Laser Altimeter data ( Smith et al., 2001 ). Flat features, thin features, fan features, and Aeolis Serpens have different geospatial

TABLE 2. SUMMARY OF LOCAL AREA MAPS, AEOLIS DORSA, MARS

Figure 12. Units in northwest Aeolis Dorsa. See Figure 9 for area locations. (A) Subparallel fluvial channel fills (blue arrows) form in area 45N. The lower channel fill has a thin channel fill (green arrow) on its upper surface. (B) Network of fluvial channel fills (blue arrows) with flat

Figure 2. Diagram showing the formation model of the Aeolis Dorsa deposits (adapted from Williams et al., 2007 ; Burr et al., 2009 ). (A,B) Hydrologic activity and concomitant sedimentation act together to form deposits. (C) Preservation processes, such as burial and geochemical cementation

Figure 8. Terrestrial analogs of fan units in Aeolis Dorsa. (A) Dolomite fan is located in eastern California, USA (near 36.60°N, 117.97°W) and includes deposits of debris flows ( Blair and McPherson, 1998 ). (B) Map showing interpreted units in A, adapted from mapping by Blair and McPherson

Figure 10. Stratigraphic columns of the four local areas in the Aeolis Dorsa region. See Figure 9 for locations. See the Supplemental File [ footnote 1 ] for maps and detailed descriptions of mapped units. Broken contacts between units represent an uncertain stratigraphic relationship

Figure 1. (A) Mars Orbiting Laser Altimeter (MOLA) digital elevation model (DEM) showing the location of Aeolis Dorsa. The sharp increase in elevation (black line) marks the boundary between the southern highlands and northern lowlands, known as the crustal dichotomy of Mars ( Tanaka et al., 2014

Figure 8. (A) Image shows the location of an example profile A-A′ used to take a measurement of deposit thickness in the red valley at Aeolis Dorsa (location shown in Fig. 1B ) from a Context Camera (CTX)–derived digital elevation model (DEM). A portion of the valley wall appears to have been

and their mineralogical identifications indicated (Supplemental Dataset 1 [see text footnote 1 ]). Black box with solid lines shows location of Aeolis Dorsa study area in panel C. Areas indicated by fuzzy black lines encompass Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) data (Fig. S2 [see text footnote