Origin of Martian Interior Layered Deposits (ILDs) by atmospherically driven processes

Since the first photogeologic exploration of Mars, vast mounds of layered sediments found within the Valles Marineris canyon system (Interior Layered Deposits or ILDs) have remained unexplained. Recent spectroscopic results showing that these materials contain coarse-grained hematite [1] and sulfate [2-8] suggest that they are fundamentally similar to layered sulfate deposits seen elsewhere on Mars [3], and are therefore a key piece of Mars' global aqueous history. Layered sulfate deposits (including ILDs) are often considered to have formed in association with transient, wet surface environments caused by groundwater upwelling [9] in the Hesperian. Here, we use spectroscopic mapping along with geomorphic observations and mass balance calculations to demonstrate that the sulfate-bearing ILDs likely did not form due to groundwater upwelling or any similar playa-lacustrine scenario. Instead, the ILDs likely formed from atmospherically driven processes in a configuration similar to that observed today. We suggest that Hesperian layered sulfate deposits formed in response to massive amounts of pyroclastic volcanism and SO2-outgassing that peaked near 3.5-3.7 Ga in a Martian climate that was largely cold and dry. This origin for the ILDs is also applicable to other layered terrain of similar age and characteristics, including sulphate-bearing crater fill, chaos terrains, and the Meridiani Planum sediments. [1] Weitz, C. M., Lane, M. D., Staid, M. & Dobrea, E. N. Gray hematite distribution and formation in Ophir and Candor chasmata. Journal of Geophysical Research-Planets 113, doi:E02016 10.1029/2007je002930 (2008). [2] Wendt, L. et al. Sulfates and iron oxides in Ophir Chasma, Mars, based on OMEGA and CRISM observations. Icarus 213, 86-103, doi:10.1016/j.icarus.2011.02.013 (2011). [3] Murchie, S. et al. Evidence for the origin of layered deposits in Candor Chasma, Mars, from mineral composition and hydrologic modeling. Journal of Geophysical Research-Planets 114, doi:E00d05 10.1029/2009je003343 (2009). [4] Mangold, N. et al. Spectral and geological study of the sulfate-rich region of West Candor Chasma, Mars. Icarus 194, 519-543, doi:10.1016/j.icarus.2007.10.021 (2008). [5] Le Deit, L. et al. Morphology, stratigraphy, and mineralogical composition of a layered formation covering the plateaus around Valles Marineris, Mars: Implications for its geological history. Icarus 208, 684-703, doi:10.1016/j.icarus.2010.03.012 (2010). [6] Gendrin, A. et al. Suffates in martian layered terrains: the OMEGA/Mars Express view. Science 307, 1587-1591, doi:10.1126/science.1109087 (2005). [7] Bibring, J.-P. et al. Coupled Ferric Oxides and Sulfates on the Martian Surface. Science 317, 1206-1210, doi:10.1126/science.1144174 (2007). [8] Roach, L. H., Mustard, J. F., Lane, M. D., Bishop, J. L. & Murchie, S. L. Diagenetic haematite and sulfate assemblages in Valles Marineris. Icarus 207, 659-674, doi:10.1016/j.icarus.2009.11.029 (2010). [9] Andrews-Hanna, J. C. & Lewis, K. W. Early Mars hydrology: 2. Hydrological evolution in the Noachian and Hesperian epochs. Journal of Geophysical Research-Planets 116, doi:E02007 10.1029/2010je003709 (2011).