A Mars 2020 <i>Perseverance</i> SuperCam Perspective on the Igneous Nature of the Máaz Formation at Jezero Crater and Link With Séítah, Mars
Arya Udry, Amanda Ostwald, V. Sautter, A. Cousin, O. Beyssac, O. Forni, Gilles Dromart, Karim Benzerara, M. Nachon, B. Horgan, Lucia Mandon, Elise Clavé, E. Dehouck, E. Gibbons, S. Alwmark, Eleni Ravanis, R. C. Wiens, Carey Legett, R. B. Anderson, P. Pilleri, N. Mangold, M. E. Schmidt, Yisi Liu, Jorge I. Núñez, Kepa Castro, Juan Manuel Madariaga, T. V. Kizovski, Pierre Beck, Sylvain Bernard, Tanja Bosak, A. J. Brown, S. M. Clegg, E. A. Cloutis, B. A. Cohen, Samuel Connell, L. S. Crumpler, Vinciane Debaille, David Flannery, Thierry Fouchet, T. S. J. Gabriel, O. Gasnault, C. D. K. Herd, J. R. Johnson, J. A. Manrique, S. Maurice, F. M. McCubbin, S. M. McLennan, A. Ollila, P. Pinet, Cathy Quantin‐Nataf, Clément Royer, Sangita Sharma, Justin I. Simon, A. Steele, Nicholas J. Tosca, A. H. Treiman, the SuperCam team
Abstract
Abstract The Máaz formation consists of the first lithologies in Jezero crater analyzed by the Mars 2020 Perseverance rover. This formation, investigated from Sols (Martian days) 1 to 201 and from Sols 343 to 382, overlies the Séítah formation (previously described as an olivine‐rich cumulate) and was initially suggested to represent an igneous crater floor unit based on orbital analyses. Using SuperCam data, we conducted a detailed textural, chemical, and mineralogical analyses of the Máaz formation and the Content member of the Séítah formation. We conclude that the Máaz formation and the Content member are igneous and consist of different lava flows and/or possibly pyroclastic flows with complex textures, including vesicular and non‐vesicular rocks with different grain sizes. The Máaz formation rocks exhibit some of the lowest Mg# (=molar 100 × MgO/MgO + FeO) of all Martian igneous rocks analyzed so far (including meteorites and surface rocks) and show similar basaltic to basaltic‐andesitic compositions. Their mineralogy is dominated by Fe‐rich augite to possibly ferrosilite and plagioclase, and minor phases such as Fe‐Ti oxides and Si‐rich phases. They show a broad diversity of both compositions and textures when compared to Martian meteorites and other surface rocks. The different Máaz and Content lava or pyroclastic flows all originate from the same parental magma and/or the same magmatic system, but are not petrogenetically linked to the Séítah formation. The study of returned Máaz samples in Earth‐based laboratories will help constrain the formation of these rocks, calibrate Martian crater counting, and overall, improve our understanding of magmatism on Mars.