Figure 3
Mastcam images show characteristics of the Rugged Terrain Unit (RTU) at the Cooperstown (A), the Dingo Gap (B), the South Wall of the Dingo Gap (C), the Kylie (D), and the Kimberley (E) locations. The RTU overlies the Hummocky Plains Unit (HPU) and/or the Striated Unit (SU) with sharp contacts at all locations. The Dillinger member (DM) consists of thin-bedded siltstone to fine-grained sandstone. It is about 2 m thick at the Kimberley location but thins northward to about 0.5 m at the Cooperstown area (see Fig. 4). The Mt. Remarkable member (MRM) is about 3 m thick at the Kimberley area but thins northward to less than 1 m at the Cooperstown location (Fig. 4). The lithology and the geometry of the MRM changes from north to south. At the Cooperstown, the Dingo Gap, and the Kylie locations, the MRM forms a near horizontal layer and is composed of a massively-bedded sandstone that grades upward to a massively-bedded, matrix supported conglomerate. At the Kimberley location, however, the MRM occurs as a north–south oriented ridge and consists of a basal conglomerate that grades upward to a sandstone and shows fining upward grain size distribution (see Fig. 4). The contact between the MRM and the DM is sharp and erosional at all localities. The BM consists of about 1 m sandstone and siltstones. It is cross bedded at the base but becoms of laminated toward the top. It overlies the massive conglomerate of the MRM with a sharp contact. It is best preserved at the Dingo Gap (Mastcam mosaic C). Unprocessed images used to generate mosaics of this figure are publically available at the Planetary Data System web site at https://pds-imaging.jpl.nasa.gov/. The credit for the Mastcam mosaic images of this figure goes to Malin Space Science Systems and NASA/JPL. Please see the Supplemental Document 1 for additional information on these images.
