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1. Fe-Phosphates in the Jezero Crater Fan: Implications for Habitability and Sample Return

Author

T V Kizovski, M E Schmidt, L O'Neil, D Klevang, N Tosca, M Tice, M Cable, E Hausrath, C T Adcock, J Hurowitz, A Treiman, M Jones, F M McCubbin, A Allwood, Y Liu, S Sharma, B Clark, S VanBommel, J Christian, A Knight, J Labrie, P Lawson, D Catling, E Cloutis, L Wade, C Heirwegh, T. Elam, N Randazzo, and C D K Herd

Subjects
Lunar and Planetary Science and Exploration
Abstract

In the ~1000 sols since the Mars 2020 Perseverance rover landed on the floor of Jezero crater, it has traversed >23 km, carrying out analyses of the crater floor and western fan. The fan is comprised of sediments transported and deposited by streams that once flowed into Jezero crater in the late Noachian to early Hesperian[1]. Detailed investigation of the sediments and rocks of the western fan can thus provide insights into ancient fluvial to lacustrine environments on Mars, whether they were habitable, and/or if biosignatures maybe preserved.

Published
2024

2. Sampling of Jezero Crater Máaz Formation By Mars 2020 Perseverance Rover

Author

J.I. Simon, H.E.F. Amundsen, L.W. Beegle, J. Bell, K.C. Benison, E.L. Berger, T. Bosak, T.M. Casademont, A.D. Czaja, B.A. Cohen, V. Debaille, A. G. Fairen, K. A. Farley, A. C. Fox, Y. Goreva, K. Hand, S.-E. Hamran, E. M. Hausrath, C. D. K. Herd, B. Horgan, J. Hurowitz, C. H. Lee, L. Mandon, S. Maurice, J.M. Madariaga, L.E. Mayhew, S. McLennan, R.C. Moeller, E.L. Scheller, S. Sharma, S. Siljeström, V.Z. Sun, D.L. Shuster, K.M. Stack, A. Udry, S. VanBommel, M. Wadhwa, B.P. Weiss, R. Wiens, Amy Williams, P.A. Willis, and M.-P. Zorzano

Subjects
Lunar And Planetary Science And Exploration
Abstract

Collection of samples that could be returned to Earth from the floor of Jezero crater is a major goal of the Mars 2020 mission. Laboratory analyses of these will expand exploration of Jezero, a Noachian crater on Mars characterized by a delta–lake system with high potential for habitability. The samples will also be used to test current ideas about the early planetary evolution of Mars. The Perseverance rover has collected samples from two members of the Máaz formation, mapped in orbital images as the Crater floor fractured rough unit by [1]. Type localities of the Roubion and Rochette members have been targeted and abraded prior to sample collection. Here we summarize these sampling activities and the potential of sampling the Chal member of Máaz. A similar summary for samples collected from the Séítah formation is described in Hickman-Lewis et al. (this meeting).

Published
2022

3. An Examination of Soil Crusts on the Floor of Jezero Crater, Mars

Author

E.M. Hausrath, C.T. Adcock, A. Bechtold, P. Beck, K. Benison, A. Brown, E.L. Cardarelli, N.A. Carman, B. Chide, J. Christian, B.C. Clark, E. Cloutis, A. Cousin, O. Forni, T.S.J. Gabriel, O. Gasnault, M. Golombek, F. Gómez, M.H. Hecht, T.L.J. Henley, J. Huidobro, J. Johnson, M. W. M. Jones, P. Kelemen, A. Knight, J.A. Lasue, S. Le Mouélic, J.M. Madariaga, J. Maki, L. Mandon, G. Martinez, J. Martínez‐Frías, T.H. McConnochie, P‐Y. Meslin, M‐P. Zorzano, H. Newsom, G. Paar, N. Randazzo, C. Royer, S. Siljeström, M.E. Schmidt, S. Schröder, Mark A Sephton, R. Sullivan, N. Turenne, A. Udry, S. VanBommel, A. Vaughan, R.C. Wiens, N. Williams, null the SuperCam team, and null the Regolith working group

Subjects
Geophysics, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous)
Published
2023
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4. Samples Collected from the Floor of Jezero Crater with the Mars 2020 Perseverance Rover

Author

J. I. Simon, K. Hickman‐Lewis, B. A. Cohen, L.E. Mayhew, D.L. Shuster, V. Debaille, E. M. Hausrath, B.P. Weiss, T. Bosak, M.‐P. Zorzano, H. E. F. Amundsen, L.W. Beegle, J.F. Bell, K. C. Benison, E. L. Berger, O. Beyssac, A.J. Brown, F. Calef, T. M. Casademont, B. Clark, E. Clavé, L. Crumpler, A. D. Czaja, A. G. Fairén, K. A. Farley, D. T. Flannery, T. Fornaro, O. Forni, F. Gómez, Y. Goreva, A. Gorin, K. P. Hand, S.‐E. Hamran, J. Henneke, C. D. K. Herd, B. H. N. Horgan, J. R. Johnson, J. Joseph, R. E. Kronyak, J. M. Madariaga, J. N. Maki, L. Mandon, F. M. McCubbin, S. M. McLennan, R. C. Moeller, C. E. Newman, J. I. Núñez, A. C. Pascuzzo, D. A. Pedersen, G. Poggiali, P. Pinet, C. Quantin‐Nataf, M. Rice, J. W. Rice, C. Royer, M. Schmidt, M. Sephton, S. Sharma, S. Siljeström, K. M. Stack, A. Steele, V. Z. Sun, A. Udry, S. VanBommel, M. Wadhwa, R. C. Wiens, A. J. Williams, and K. H. Williford

Subjects
Mars Sample Return, rock core, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Jezero Crater, Mars 2020, Earth and Planetary Sciences (miscellaneous)
Abstract

The first samples collected by the Mars 2020 mission represent units exposed on the Jezero Crater floor, from the potentially oldest Séítah formation outcrops to the potentially youngest rocks of the heavily cratered Máaz formation. Surface investigations reveal landscape-to-microscopic textural, mineralogical, and geochemical evidence for igneous lithologies, some possibly emplaced as lava flows. The samples contain major rock-forming minerals such as pyroxene, olivine, and feldspar, accessory minerals including oxides and phosphates, and evidence for various degrees of aqueous activity in the form of water-soluble salt, carbonate, sulfate, iron oxide, and iron silicate minerals. Following sample return, the compositions and ages of these variably altered igneous rocks are expected to reveal the geophysical and geochemical nature of the planet’s interior at the time of emplacement, characterize martian magmatism, and place timing constraints on geologic processes, both in Jezero Crater and more widely on Mars. Petrographic observations and geochemical analyses, coupled with geochronology of secondary minerals, can also reveal the timing of aqueous activity as well as constrain the chemical and physical conditions of the environments in which these minerals precipitated, and the nature and composition of organic compounds preserved in association with these phases. Returned samples from these units will help constrain the crater chronology of Mars and the global evolution of the planet’s interior, for understanding the processes that formed Jezero Crater floor units, and for constraining the style and duration of aqueous activity in Jezero Crater, past habitability, and cycling of organic elements in Jezero Crater.

Published
2023
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5. Elemental geochemistry of sedimentary rocks at Yellowknife Bay, Gale crater, Mars.

Author

McLennan SM, Anderson RB, Bell JF 3rd, Bridges JC, Calef F 3rd, Campbell JL, Clark BC, Clegg S, Conrad P, Cousin A, Des Marais DJ, Dromart G, Dyar MD, Edgar LA, Ehlmann BL, Fabre C, Forni O, Gasnault O, Gellert R, Gordon S, Grant JA, Grotzinger JP, Gupta S, Herkenhoff KE, Hurowitz JA, King PL, Le Mouélic S, Leshin LA, Léveillé R, Lewis KW, Mangold N, Maurice S, Ming DW, Morris RV, Nachon M, Newsom HE, Ollila AM, Perrett GM, Rice MS, Schmidt ME, Schwenzer SP, Stack K, Stolper EM, Sumner DY, Treiman AH, VanBommel S, Vaniman DT, Vasavada A, Wiens RC, and Yingst RA

Subjects
Bays, Calcium Sulfate analysis, Calcium Sulfate chemistry, Chlorine analysis, Chlorine chemistry, Ferrosoferric Oxide analysis, Ferrosoferric Oxide chemistry, Halogens analysis, Halogens chemistry, Hydrogen-Ion Concentration, Iron analysis, Iron chemistry, Magnesium analysis, Magnesium chemistry, Silicates analysis, Silicates chemistry, Water chemistry, Exobiology, Extraterrestrial Environment chemistry, Geologic Sediments chemistry, Mars
Abstract

Sedimentary rocks examined by the Curiosity rover at Yellowknife Bay, Mars, were derived from sources that evolved from an approximately average martian crustal composition to one influenced by alkaline basalts. No evidence of chemical weathering is preserved, indicating arid, possibly cold, paleoclimates and rapid erosion and deposition. The absence of predicted geochemical variations indicates that magnetite and phyllosilicates formed by diagenesis under low-temperature, circumneutral pH, rock-dominated aqueous conditions. Analyses of diagenetic features (including concretions, raised ridges, and fractures) at high spatial resolution indicate that they are composed of iron- and halogen-rich components, magnesium-iron-chlorine-rich components, and hydrated calcium sulfates, respectively. Composition of a cross-cutting dike-like feature is consistent with sedimentary intrusion. The geochemistry of these sedimentary rocks provides further evidence for diverse depositional and diagenetic sedimentary environments during the early history of Mars.

Published
2014
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6. Isotope ratios of H, C, and O in CO2 and H2O of the martian atmosphere.

Author

Webster CR, Mahaffy PR, Flesch GJ, Niles PB, Jones JH, Leshin LA, Atreya SK, Stern JC, Christensen LE, Owen T, Franz H, Pepin RO, Steele A, Achilles C, Agard C, Alves Verdasca JA, Anderson R, Anderson R, Archer D, Armiens-Aparicio C, Arvidson R, Atlaskin E, Aubrey A, Baker B, Baker M, Balic-Zunic T, Baratoux D, Baroukh J, Barraclough B, Bean K, Beegle L, Behar A, Bell J, Bender S, Benna M, Bentz J, Berger G, Berger J, Berman D, Bish D, Blake DF, Blanco Avalos JJ, Blaney D, Blank J, Blau H, Bleacher L, Boehm E, Botta O, Böttcher S, Boucher T, Bower H, Boyd N, Boynton B, Breves E, Bridges J, Bridges N, Brinckerhoff W, Brinza D, Bristow T, Brunet C, Brunner A, Brunner W, Buch A, Bullock M, Burmeister S, Cabane M, Calef F, Cameron J, Campbell J, Cantor B, Caplinger M, Caride Rodríguez J, Carmosino M, Carrasco Blázquez I, Charpentier A, Chipera S, Choi D, Clark B, Clegg S, Cleghorn T, Cloutis E, Cody G, Coll P, Conrad P, Coscia D, Cousin A, Cremers D, Crisp J, Cros A, Cucinotta F, d'Uston C, Davis S, Day M, de la Torre Juarez M, DeFlores L, DeLapp D, DeMarines J, DesMarais D, Dietrich W, Dingler R, Donny C, Downs B, Drake D, Dromart G, Dupont A, Duston B, Dworkin J, Dyar MD, Edgar L, Edgett K, Edwards C, Edwards L, Ehlmann B, Ehresmann B, Eigenbrode J, Elliott B, Elliott H, Ewing R, Fabre C, Fairén A, Farley K, Farmer J, Fassett C, Favot L, Fay D, Fedosov F, Feldman J, Feldman S, Fisk M, Fitzgibbon M, Floyd M, Flückiger L, Forni O, Fraeman A, Francis R, François P, Freissinet C, French KL, Frydenvang J, Gaboriaud A, Gailhanou M, Garvin J, Gasnault O, Geffroy C, Gellert R, Genzer M, Glavin D, Godber A, Goesmann F, Goetz W, Golovin D, Gómez Gómez F, Gómez-Elvira J, Gondet B, Gordon S, Gorevan S, Grant J, Griffes J, Grinspoon D, Grotzinger J, Guillemot P, Guo J, Gupta S, Guzewich S, Haberle R, Halleaux D, Hallet B, Hamilton V, Hardgrove C, Harker D, Harpold D, Harri AM, Harshman K, Hassler D, Haukka H, Hayes A, Herkenhoff K, Herrera P, Hettrich S, Heydari E, Hipkin V, Hoehler T, Hollingsworth J, Hudgins J, Huntress W, Hurowitz J, Hviid S, Iagnemma K, Indyk S, Israël G, Jackson R, Jacob S, Jakosky B, Jensen E, Jensen JK, Johnson J, Johnson M, Johnstone S, Jones A, Joseph J, Jun I, Kah L, Kahanpää H, Kahre M, Karpushkina N, Kasprzak W, Kauhanen J, Keely L, Kemppinen O, Keymeulen D, Kim MH, Kinch K, King P, Kirkland L, Kocurek G, Koefoed A, Köhler J, Kortmann O, Kozyrev A, Krezoski J, Krysak D, Kuzmin R, Lacour JL, Lafaille V, Langevin Y, Lanza N, Lasue J, Le Mouélic S, Lee EM, Lee QM, Lees D, Lefavor M, Lemmon M, Lepinette Malvitte A, Léveillé R, Lewin-Carpintier É, Lewis K, Li S, Lipkaman L, Little C, Litvak M, Lorigny E, Lugmair G, Lundberg A, Lyness E, Madsen M, Maki J, Malakhov A, Malespin C, Malin M, Mangold N, Manhes G, Manning H, Marchand G, Marín Jiménez M, Martín García C, Martin D, Martin M, Martínez-Frías J, Martín-Soler J, Martín-Torres FJ, Mauchien P, Maurice S, McAdam A, McCartney E, McConnochie T, McCullough E, McEwan I, McKay C, McLennan S, McNair S, Melikechi N, Meslin PY, Meyer M, Mezzacappa A, Miller H, Miller K, Milliken R, Ming D, Minitti M, Mischna M, Mitrofanov I, Moersch J, Mokrousov M, Molina Jurado A, Moores J, Mora-Sotomayor L, Morookian JM, Morris R, Morrison S, Mueller-Mellin R, Muller JP, Muñoz Caro G, Nachon M, Navarro López S, Navarro-González R, Nealson K, Nefian A, Nelson T, Newcombe M, Newman C, Newsom H, Nikiforov S, Nixon B, Noe Dobrea E, Nolan T, Oehler D, Ollila A, Olson T, de Pablo Hernández MÁ, Paillet A, Pallier E, Palucis M, Parker T, Parot Y, Patel K, Paton M, Paulsen G, Pavlov A, Pavri B, Peinado-González V, Peret L, Perez R, Perrett G, Peterson J, Pilorget C, Pinet P, Pla-García J, Plante I, Poitrasson F, Polkko J, Popa R, Posiolova L, Posner A, Pradler I, Prats B, Prokhorov V, Purdy SW, Raaen E, Radziemski L, Rafkin S, Ramos M, Rampe E, Raulin F, Ravine M, Reitz G, Rennó N, Rice M, Richardson M, Robert F, Robertson K, Rodriguez Manfredi JA, Romeral-Planelló JJ, Rowland S, Rubin D, Saccoccio M, Salamon A, Sandoval J, Sanin A, Sans Fuentes SA, Saper L, Sarrazin P, Sautter V, Savijärvi H, Schieber J, Schmidt M, Schmidt W, Scholes D, Schoppers M, Schröder S, Schwenzer S, Sebastian Martinez E, Sengstacken A, Shterts R, Siebach K, Siili T, Simmonds J, Sirven JB, Slavney S, Sletten R, Smith M, Sobrón Sánchez P, Spanovich N, Spray J, Squyres S, Stack K, Stalport F, Stein T, Stewart N, Stipp SL, Stoiber K, Stolper E, Sucharski B, Sullivan R, Summons R, Sumner D, Sun V, Supulver K, Sutter B, Szopa C, Tan F, Tate C, Teinturier S, ten Kate I, Thomas P, Thompson L, Tokar R, Toplis M, Torres Redondo J, Trainer M, Treiman A, Tretyakov V, Urqui-O'Callaghan R, Van Beek J, Van Beek T, VanBommel S, Vaniman D, Varenikov A, Vasavada A, Vasconcelos P, Vicenzi E, Vostrukhin A, Voytek M, Wadhwa M, Ward J, Weigle E, Wellington D, Westall F, Wiens RC, Wilhelm MB, Williams A, Williams J, Williams R, Williams RB, Wilson M, Wimmer-Schweingruber R, Wolff M, Wong M, Wray J, Wu M, Yana C, Yen A, Yingst A, Zeitlin C, Zimdar R, and Zorzano Mier MP

Abstract

Stable isotope ratios of H, C, and O are powerful indicators of a wide variety of planetary geophysical processes, and for Mars they reveal the record of loss of its atmosphere and subsequent interactions with its surface such as carbonate formation. We report in situ measurements of the isotopic ratios of D/H and (18)O/(16)O in water and (13)C/(12)C, (18)O/(16)O, (17)O/(16)O, and (13)C(18)O/(12)C(16)O in carbon dioxide, made in the martian atmosphere at Gale Crater from the Curiosity rover using the Sample Analysis at Mars (SAM)'s tunable laser spectrometer (TLS). Comparison between our measurements in the modern atmosphere and those of martian meteorites such as ALH 84001 implies that the martian reservoirs of CO2 and H2O were largely established ~4 billion years ago, but that atmospheric loss or surface interaction may be still ongoing.

Published
2013
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