Data produced in Putnam and Palucis (2021)

Three types of datasets are maintained in this repository. This information is also contained in a ReadMe textfile as well.<br>1. Crater_count_data.xlsx: We performed crater counts on portions of the ejecta of Garu crater to determine its approximate impact age. We limited the count to the southern half of the ejecta blanket because Garu lies directly on the Martian crustal dichotomy, and the northern portion of Garu’s ejecta is located over the dichotomy scarp. This partial portion of the ejecta covers a fairly large area (&gt; 1400 km²) and contains 43 craters &gt;500 m in diameter to ensure statistically robust surface ages (Palucis et al., 2020; Warner et al., 2015). We mapped craters on the CTX basemap in ArcGIS using the CraterTools software (Kneissl et al., 2011). Craters were included only if their centers were within the mapped ejecta. We extracted crater areas and converted them into crater diameters in ArcGIS. We input crater size-frequency data into CraterStats II (Michael &amp; Neukum, 2010) and determined a surface age from crater diameter bins &gt;500 m using the Hartmann (2005) chronology and production functions with root-2 binning. When comparing ages between Garu and Gale crater, we report both the observed crater population (e.g., N(1 km)) and the model absolute age, as different approaches can make the latter difficult to compare between studies.<br>2. Shapefiles_Garu_JGR: We produced a geomorphic map using a blended CTX mosaic (5 m/pixel, Dickson et al., 2018), with georeferenced High-Resolution Imaging Science Experiment (HiRISE, ~25 cm/pixel) imagery overlain where available (McEwen et al., 2007). We also used the global Thermal Emission Imaging System (THEMIS, ~100 m/pixel) map (Christensen et al., 2004) to identify the thermal inertia and induration of various mapped geomorphic units within Garu crater and its surroundings.<br>3. DEMS.zip: We produced Context Camera (CTX) (Malin et al., 2007) DEMs for the entirety of the Garu sedimentary deposit and its upslope canyon using the open-source NASA Ames Stereo Pipeline software (Moratto et al., 2010). CTX stereopairs were processed to produce initial point clouds that were then tied to Mars Orbital Laser Altimeter (MOLA) point shot data (Beyer et al., 2018; Smith et al., 2001). The MOLA-tied point clouds were then used to make DEMs registered to the Mars aeroid (3,396,190 m) with ~5 m/pixel spatial resolution and an elevation uncertainty of ~24 m.