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Small-crater counts on Mars light-toned sedimentary rock are ofteninconsistent with any isochron; these data are usually plotted then ignored. Weshow (using an 18-HiRISE-image, >10^4 crater dataset) that these non-isochroncrater counts are often well-fit by a model where crater production is balancedby crater obliteration via steady exhumation. For these regions, we fit erosionrates. We infer that Mars light-toned sedimentary rocks typically erode at~10^2 nm/yr, when averaged over 10 km^2 scales and 10^7-10^8 yr timescales.Crater-based erosion-rate determination is consistent with independenttechniques, but can be applied to nearly all light-toned sedimentary rocks onMars. Erosion is swift enough that radiolysis cannot destroy complex organicmatter at some locations (e.g. paleolake deposits at SW Melas), but radiolysisis a severe problem at other locations (e.g. Oxia Planum). The data suggestthat the relief of the Valles Marineris mounds is currently being reduced bywind erosion, and that dust production on Mars <3 Gya greatly exceeds themodern reservoir of mobile dust.

Mars sedimentary rock erosion rates constrained using crater counts, with applications to organic matter preservation and to the global dust cycle