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1. Space weathering record and pristine state of Ryugu samples from MicrOmega spectral analysis

Author

Le Pivert-Jolivet, T., Brunetto, R., Pilorget, C., Bibring, J.-P., Nakato, A., Hamm, V., Hatakeda, K., Lantz, C., Loizeau, D., Riu, L., Yogata, K., Baklouti, D., Poulet, F., Aléon-Toppani, A., Carter, J., Langevin, Y., Okada, T., Yada, T., Hitomi, Y., Kumagai, K., Miyazaki, A., Nagashima, K., Nishimura, M., Usui, T., Abe, M., Saiki, T., Tanaka, S., Nakazawa, S., Tsuda, Y., and Watanabe, S.

Published
2023
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2. Three-dimensional textures of Ryugu samples and their implications for the evolution of aqueous alteration in the Ryugu parent body

Author

Tsuchiyama, Akira, Matsumoto, Megumi, Matsuno, Junya, Yasutake, Masahiro, Nakamura, Tomoki, Noguchi, Takaaki, Miyake, Akira, Uesugi, Kentaro, Takeuchi, Akihisa, Okumura, Shota, Fujioka, Yuri, Sun, Mingqi, Takigawa, Aki, Matsumoto, Toru, Enju, Satomi, Mitsukawa, Itaru, Enokido, Yuma, Kawamoto, Tatsuhiko, Mikouchi, Takeshi, Michikami, Tatsuhiro, Morita, Tomoyo, Kikuiri, Mizuha, Amano, Kana, Kagawa, Eiichi, Rubino, Stefano, Dionnet, Zelia, Aléon-Toppani, Alice, Brunetto, Rosario, Zolensky, Michael E., Nakano, Tsukasa, Nakano, Naoto, Yurimoto, Hisayoshi, Okazaki, Ryuji, Yabuta, Hikaru, Naraoka, Hiroshi, Sakamoto, Kanako, Yada, Toru, Nishimura, Masahiro, Nakato, Aiko, Miyazaki, Akiko, Yogata, Kasumi, Abe, Masanao, Okada, Tatsuaki, Usui, Tomohiro, Yoshikawa, Makoto, Saiki, Takanao, Tanaka, Satoshi, Nakazawa, Satoru, Terui, Fuyuto, Tachibana, Shogo, Watanabe, Sei-ichiro, and Tsuda, Yuichi

Published
2024
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4. Small grains from Ryugu: handling and analysis pipeline for infrared synchrotron microspectroscopy

Author

Rubino, Stefano, Dionnet, Zélia, Aléon-Toppani, Alice, Brunetto, Rosario, Nakamura, Tomoki, Baklouti, Donia, Djouadi, Zahia, Lantz, Cateline, Mivumbi, Obadias, Borondics, Ferenc, Lefrançois, Stephane, Sandt, Christophe, Capitani, Francesco, Héripré, Eva, Troadec, David, Matsumoto, Megumi, Amano, Kana, Morita, Tomoyo, Yurimoto, Hisayoshi, Noguchi, Takaaki, Okazaki, Ryuji, Yabuta, Hikaru, Naraoka, Hiroshi, Sakamoto, Kanako, Tachibana, Shogo, Watanabe, Seiichiro, and Tsuda, Yuichi

Published
2023
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5. Correlated IR-SEM-TEM studies of three different grains from Ryugu: From the initial material to post-accretional processes

Author

Aléon-Toppani, Alice, Brunetto, Rosario, Dionnet, Zélia, Rubino, Stefano, Baklouti, Donia, Brisset, François, Vallet, Maxime, Heripre, Eva, Nakamura, Tomoki, Lantz, Cateline, Djouadi, Zahia, Borondics, Ferenc, Sandt, Christophe, Troadec, David, Mivumbi, Obadias, Matsumoto, Megumi, Amano, Kana, Morita, Tomoyo, Yurimoto, Hisayoshi, Noguchi, Takaaki, Okazaki, Ryuji, Yabuta, Hikaru, Naraoka, Hiroshi, Sakamoto, Kanako, Tachibana, Shogo, Yada, Toru, Nishimura, Masahiro, Nakato, Aiko, Miyazaki, Akiko, Yogata, Kasumi, Abe, Masanao, Okada, Tatsuaki, Usui, Tomohira, Yoshikawa, Makoto, Saiki, Takanao, Tanaka, Satoshi, Terui, Fuyuto, Nakazawa, Satoru, Watanabe, Sei-ichiro, and Tsuda, Yuichi

Published
2024
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6. Constraints on Solar System early evolution by MicrOmega analysis of Ryugu carbonates

Author

Loizeau, D., Pilorget, C., Riu, L., Brunetto, R., Bibring, J.-P., Nakato, A., Aléon-Toppani, A., Hatakeda, K., Yogata, K., Carter, J., Le Pivert-Jolivet, T., Yada, T., Okada, T., Usui, T., Langevin, Y., Lantz, C., Baklouti, D., Miyazaki, A., Nishimura, M., Nagashima, K., Kumagai, K., Hitomi, Y., Abe, M., Saiki, T., Tanaka, S., Nakazawa, S., Tsuda, Y., and Watanabe, S.

Published
2023
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7. Small grains from Ryugu: handling and analysis pipeline for infrared synchrotron microspectroscopy

Author

Stefano Rubino, Zélia Dionnet, Alice Aléon-Toppani, Rosario Brunetto, Tomoki Nakamura, Donia Baklouti, Zahia Djouadi, Cateline Lantz, Obadias Mivumbi, Ferenc Borondics, Stephane Lefrançois, Christophe Sandt, Francesco Capitani, Eva Héripré, David Troadec, Megumi Matsumoto, Kana Amano, Tomoyo Morita, Hisayoshi Yurimoto, Takaaki Noguchi, Ryuji Okazaki, Hikaru Yabuta, Hiroshi Naraoka, Kanako Sakamoto, Shogo Tachibana, Seiichiro Watanabe, Yuichi Tsuda, and the Hayabusa2-initial-analysis team

Subjects
Sample-return mission, Hayabusa2, IR spectroscopy, Precious samples, Non-destructive analysis, Analytical pipeline, Geography. Anthropology. Recreation, Geodesy, QB275-343, Geology, QE1-996.5
Abstract

Abstract Sample-return missions allow the study of materials collected directly from celestial bodies, unbiased by atmospheric entry effects and/or terrestrial alteration and contamination phenomena, using state-of-the-art techniques which are available only in a laboratory environment—but only if the collected material stays pristine. The scarcity of outer-space unaltered material recovered until now makes this material extremely precious for the potential scientific insight it can bring. To maximize the scientific output of current and future sample-return missions, the scientific community needs to plan for ways of storing, handling, and measuring this precious material while preserving their pristine state for as long as the ‘invasiveness’ of measurements allows. In July 2021, as part of the Hayabusa2 (JAXA) “Stone” preliminary examination team, we received several microscopic particles from the asteroid Ryugu, with the goal of performing IR hyper-spectral imaging and IR micro-tomography studies. Here, we describe the sample transfer, handling methods and analytical pipeline we implemented to study this very precious material while minimizing and surveilling their alteration history on Earth. Graphical Abstract

Published
2023
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9. First compositional analysis of Ryugu samples by the MicrOmega hyperspectral microscope

Author

Pilorget, C., Okada, T., Hamm, V., Brunetto, R., Yada, T., Loizeau, D., Riu, L., Usui, T., Moussi-Soffys, A., Hatakeda, K., Nakato, A., Yogata, K., Abe, M., Aléon-Toppani, A., Carter, J., Chaigneau, M., Crane, B., Gondet, B., Kumagai, K., Langevin, Y., Lantz, C., Le Pivert-Jolivet, T., Lequertier, G., Lourit, L., Miyazaki, A., Nishimura, M., Poulet, F., Arakawa, M., Hirata, N., Kitazato, K., Nakazawa, S., Namiki, N., Saiki, T., Sugita, S., Tachibana, S., Tanaka, S., Yoshikawa, M., Tsuda, Y., Watanabe, S., and Bibring, J.-P.

Published
2022
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10. Three‐dimensional multiscale assembly of phyllosilicates, organics, and carbonates in small Ryugu fragments.

Author

Dionnet, Zelia, Rubino, Stefano, Aléon‐Toppani, Alice, Brunetto, Rosario, Tsuchiyama, Akira, Lantz, Cateline, Djouadi, Zahia, Baklouti, Donia, Nakamura, Tomoki, Borondics, Ferenc, Sandt, Christophe, Heripre, Eva, Troadec, David, Mivumbi, Obadias, Aléon, Jérome, Ternier, Theo, Matsumoto, Megumi, Amano, Kana, Morita, Tomoyo, and Yurimoto, Hisayoshi

Subjects
ORGANIC compounds, PHYLLOSILICATES, TOMOGRAPHY, CARBONATES, SILICATES
Abstract

We report μm‐scale nondestructive infrared (IR) hyperspectral results (IR computed tomography, IR‐CT) in 3‐D and IR surface imaging, IR‐S) in 2‐D, at SOLEIL) combined with X‐ray nano‐computed tomography analyses (at SPring‐8) performed on eight small Ryugu fragments extracted from mm‐sized grains coming both from touchdown first and second sites. We describe the multiscale assembly of phyllosilicates, carbonates, sulfides, oxides, and organics. Two types of silicates, as well as diverse kinds of organic matter, were detected inside Ryugu material. Their spatial correlations are described to discuss the role of the mineralogical microenvironments in the formation/evolution of organic matter. In particular, we have shown that there is a redistribution of the organic matter diffuse component during aqueous alteration on the parent body, with a preferential circulation among fine‐grained phyllosilicates. [ABSTRACT FROM AUTHOR]

Published
2024
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11. Ryugu’s Anhydrous Ingredients and Their Spectral Link to Primitive Dust from the Outer Solar System

Author

R. Brunetto, C. Lantz, Y. Fukuda, A. Aléon-Toppani, T. Nakamura, Z. Dionnet, D. Baklouti, F. Borondics, Z. Djouadi, S. Rubino, K. Amano, M. Matsumoto, Y. Fujioka, T. Morita, M. Kukuiri, E. Kagawa, M. Matsuoka, R. Milliken, H. Yurimoto, T. Noguchi, R. Okazaki, H. Yabuta, H. Naraoka, K. Sakamoto, S. Tachibana, T. Yada, M. Nishimura, A. Nakato, A. Miyazaki, K. Yogata, M. Abe, T. Okada, T. Usui, M. Yoshikawa, T. Saiki, S. Tanaka, F. Terui, S. Nakazawa, S. Watanabe, and Y. Tsuda

Subjects
Asteroids, Dust composition, Meteorites, Laboratory astrophysics, Infrared spectroscopy, Astrophysics, QB460-466
Abstract

Ryugu is a second-generation C-type asteroid formed by the reassembly of fragments of a previous larger body in the main asteroid belt. While the majority of Ryugu samples returned by Hayabusa2 are composed of a lithology dominated by aqueously altered minerals, clasts of pristine olivine and pyroxene remain in the least-altered lithologies. These clasts are objects of great interest for revealing the composition of the dust from which the original building blocks of Ryugu's parent asteroid formed. Here we show that some grains rich in olivine, pyroxene, and amorphous silicates discovered in one millimeter-sized stone of Ryugu have infrared spectra similar to the D-type asteroid Hektor (a Jupiter Trojan), to comet Hale–Bopp, and to some anhydrous interplanetary dust particles of probable cometary origin. This result indicates that Ryugu's primary parent body incorporated anhydrous ingredients similar to the building blocks of asteroids (and possibly some comets) formed in the outer solar system, and that Ryugu retained valuable information on the formation and evolution of planetesimals at different epochs of our solar system's history.

Published
2023
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15. Contributors

Author

Abe, Masanao, primary, Aléon, Jérôme, additional, Aléon-Toppani, Alice, additional, Bennett, Allan, additional, Berthoud, Lucy, additional, Borg, Janet, additional, Bridges, John C., additional, Brownlee, Donald E., additional, Brunetto, Rosario, additional, Burnett, Don, additional, Brucato, John Robert, additional, Corte, Vincenzo Della, additional, Debaille, Vinciane, additional, Dirri, Fabrizio, additional, Djouadi, Zahia, additional, Enos, Heather L., additional, Ferrière, Ludovic, additional, Folco, Luigi, additional, Foucher, Frédéric, additional, Franchi, Ian A., additional, Fujiwara, Akira, additional, Gounelle, Matthieu, additional, Grady, Monica M., additional, Holt, John, additional, Hutzler, Aurore, additional, Jerde, Eric A., additional, Jurewicz, Amy, additional, Kawaguchi, Junichiro, additional, Lauretta, Dante S., additional, Leuko, Stefano, additional, Longobardo, Andrea, additional, Lunine, Jonathan I., additional, Marrocchi, Yves, additional, Meneghin, Andrea, additional, Palomba, Ernesto, additional, Polit, Anjani T., additional, Pottage, Thomas, additional, Qian, Yuqi, additional, Reisenfeld, Dan, additional, Rettberg, Petra, additional, Roper, Heather L., additional, Rotundi, Alessandra, additional, Russell, Sara S., additional, Sandford, Scott A., additional, Smith, Caroline L., additional, Slyuta, Evgeny, additional, Tachibana, Shogo, additional, Tasker, Elizabeth J., additional, Tsuchiyama, Akira, additional, Vrublevskis, John, additional, Wang, Qian, additional, Wang, Qiong, additional, Westall, Frances, additional, Wiens, Roger C., additional, Wolner, Catherine W.V., additional, Xiao, Long, additional, Yoshikawa, Makoto, additional, Zipfel, Jutta, additional, and Zolensky, Michael E., additional

Published
2021
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18. Combining Visible/Infrared Spectroscopy and Transmission-Electron-Microscopy To Investigate Space-Weathering Induced Changes In Hydrated Silicates

Author

Stefano Rubino, Cateline Lantz, Alice Aléon-Toppani, Donia Baklouti, Zahia Djouadi, David Troadec, Ernesto Palomba, Ferenc Borondics, Hugues Leroux, and Rosario Brunetto

Abstract

The study of small bodies in our solar system is fundamental for understanding its youth and evolution. These "primitive" bodies are "undifferentiated" (their components did not separate according to their density, irreversibly altering their mineralogy). They have evolved very little since their birth, spurring a composition relatively close to that of the primordial proto-planetary disk (Scott et al. 2018). However, other processes such as thermal alteration, aqueous alteration, shocks, or space weathering can affect these bodies’ surfaces. This may introduce certain compositional biases in remote-sensed data focusing on the surface of these bodies. Therefore, it is paramount to understand the processes affecting the surface of primitive asteroids to correctly assess their composition.There are several ways to study the surface of primitive asteroids, such as remotely, by acquiring spectroscopic data (gaining access to surface chemical and mineralogical composition). It is also possible to study these bodies in a laboratory environment, by working on analogous materials such as certain classes of "primitive" meteorites (Greenwood et al. 2020) (carbonaceous chondrites), on terrestrial analogues such as hydrated silicates - which dominates the mineral composition of “primitive” bodies (Usui et al. 2018), or directly on extra-terrestrial materials brought back by sample return missions (Yokoyama et al. 2022, Nakalura et al. 2022, Noguchi et al. 2022).In this work, we replicate in a laboratory environment the effects of space weathering (SpWe) on the surface of primitive asteroids. We focus on the effects of solar wind, the dominant SpWe process on "young" surfaces (Brunetto et al. 2015, Clark et al. 2002). We have chosen three terrestrial minerals analogous to a "primitive" surface - three hydrated minerals (two serpentines and one saponite) - of which we have produced several pellets which have been bombarded using He and Ar ions. In doing so, we made analogous materials of weathered primitive surface matter. These analogues were then characterized by infrared spectroscopy, from the visible to the far-infrared range, to study chemical changes prompted by ion bombardment. This was done by investigating how certain spectroscopic features – characteristic of hydrated silicates – changed upon ion-bombardment. We detected several effects, such as darkening in the visible range, visible slope reddening and bluing as well as a systematic shift towards longer wavelength affecting the position of several spectroscopic features.This was followed by a study at a smaller scale, using electron microscopy. We first characterized the surface of our weathered analogues using scanning electron microscopy, and then investigated the morphological and physicochemical changes taking place in the bombarded layer, at a nanometre scale, using transmission electron microscopy. Strong vesiculation effects of various kinds were identified in the ion bombarded amorphized layers, as well as textural changes and some elemental concentration evolution (such as the loss of oxygen in the utmost top surfaces, preferential amorphization of magnesium, etc.).The coupling between these two techniques, Vis/IR spectroscopy and electron microscopy, has allowed us to start probing the relations between SpWe induced effects seen at different scales.

Published
2023

19. Formation and evolution of carbonaceous asteroid Ryugu: Direct evidence from returned samples

Author

Nakamura, T., primary, Matsumoto, M., additional, Amano, K., additional, Enokido, Y., additional, Zolensky, M. E., additional, Mikouchi, T., additional, Genda, H., additional, Tanaka, S., additional, Zolotov, M. Y., additional, Kurosawa, K., additional, Wakita, S., additional, Hyodo, R., additional, Nagano, H., additional, Nakashima, D., additional, Takahashi, Y., additional, Fujioka, Y., additional, Kikuiri, M., additional, Kagawa, E., additional, Matsuoka, M., additional, Brearley, A. J., additional, Tsuchiyama, A., additional, Uesugi, M., additional, Matsuno, J., additional, Kimura, Y., additional, Sato, M., additional, Milliken, R. E., additional, Tatsumi, E., additional, Sugita, S., additional, Hiroi, T., additional, Kitazato, K., additional, Brownlee, D., additional, Joswiak, D. J., additional, Takahashi, M., additional, Ninomiya, K., additional, Takahashi, T., additional, Osawa, T., additional, Terada, K., additional, Brenker, F. E., additional, Tkalcec, B. J., additional, Vincze, L., additional, Brunetto, R., additional, Aléon-Toppani, A., additional, Chan, Q. H. S., additional, Roskosz, M., additional, Viennet, J.-C., additional, Beck, P., additional, Alp, E. E., additional, Michikami, T., additional, Nagaashi, Y., additional, Tsuji, T., additional, Ino, Y., additional, Martinez, J., additional, Han, J., additional, Dolocan, A., additional, Bodnar, R. J., additional, Tanaka, M., additional, Yoshida, H., additional, Sugiyama, K., additional, King, A. J., additional, Fukushi, K., additional, Suga, H., additional, Yamashita, S., additional, Kawai, T., additional, Inoue, K., additional, Nakato, A., additional, Noguchi, T., additional, Vilas, F., additional, Hendrix, A. R., additional, Jaramillo-Correa, C., additional, Domingue, D. L., additional, Dominguez, G., additional, Gainsforth, Z., additional, Engrand, C., additional, Duprat, J., additional, Russell, S. S., additional, Bonato, E., additional, Ma, C., additional, Kawamoto, T., additional, Wada, T., additional, Watanabe, S., additional, Endo, R., additional, Enju, S., additional, Riu, L., additional, Rubino, S., additional, Tack, P., additional, Takeshita, S., additional, Takeichi, Y., additional, Takeuchi, A., additional, Takigawa, A., additional, Takir, D., additional, Tanigaki, T., additional, Taniguchi, A., additional, Tsukamoto, K., additional, Yagi, T., additional, Yamada, S., additional, Yamamoto, K., additional, Yamashita, Y., additional, Yasutake, M., additional, Uesugi, K., additional, Umegaki, I., additional, Chiu, I., additional, Ishizaki, T., additional, Okumura, S., additional, Palomba, E., additional, Pilorget, C., additional, Potin, S. M., additional, Alasli, A., additional, Anada, S., additional, Araki, Y., additional, Sakatani, N., additional, Schultz, C., additional, Sekizawa, O., additional, Sitzman, S. D., additional, Sugiura, K., additional, Sun, M., additional, Dartois, E., additional, De Pauw, E., additional, Dionnet, Z., additional, Djouadi, Z., additional, Falkenberg, G., additional, Fujita, R., additional, Fukuma, T., additional, Gearba, I. R., additional, Hagiya, K., additional, Hu, M. Y., additional, Kato, T., additional, Kawamura, T., additional, Kimura, M., additional, Kubo, M. K., additional, Langenhorst, F., additional, Lantz, C., additional, Lavina, B., additional, Lindner, M., additional, Zhao, J., additional, Vekemans, B., additional, Baklouti, D., additional, Bazi, B., additional, Borondics, F., additional, Nagasawa, S., additional, Nishiyama, G., additional, Nitta, K., additional, Mathurin, J., additional, Matsumoto, T., additional, Mitsukawa, I., additional, Miura, H., additional, Miyake, A., additional, Miyake, Y., additional, Yurimoto, H., additional, Okazaki, R., additional, Yabuta, H., additional, Naraoka, H., additional, Sakamoto, K., additional, Tachibana, S., additional, Connolly, H. C., additional, Lauretta, D. S., additional, Yoshitake, M., additional, Yoshikawa, M., additional, Yoshikawa, K., additional, Yoshihara, K., additional, Yokota, Y., additional, Yogata, K., additional, Yano, H., additional, Yamamoto, Y., additional, Yamamoto, D., additional, Yamada, M., additional, Yamada, T., additional, Yada, T., additional, Wada, K., additional, Usui, T., additional, Tsukizaki, R., additional, Terui, F., additional, Takeuchi, H., additional, Takei, Y., additional, Iwamae, A., additional, Soejima, H., additional, Shirai, K., additional, Shimaki, Y., additional, Senshu, H., additional, Sawada, H., additional, Saiki, T., additional, Ozaki, M., additional, Ono, G., additional, Okada, T., additional, Ogawa, N., additional, Ogawa, K., additional, Noguchi, R., additional, Noda, H., additional, Nishimura, M., additional, Namiki, N., additional, Nakazawa, S., additional, Morota, T., additional, Miyazaki, A., additional, Miura, A., additional, Mimasu, Y., additional, Matsumoto, K., additional, Kumagai, K., additional, Kouyama, T., additional, Kikuchi, S., additional, Kawahara, K., additional, Kameda, S., additional, Iwata, T., additional, Ishihara, Y., additional, Ishiguro, M., additional, Ikeda, H., additional, Hosoda, S., additional, Honda, R., additional, Honda, C., additional, Hitomi, Y., additional, Hirata, N., additional, Hayashi, T., additional, Hayakawa, M., additional, Hatakeda, K., additional, Furuya, S., additional, Fukai, R., additional, Fujii, A., additional, Cho, Y., additional, Arakawa, M., additional, Abe, M., additional, and Tsuda, Y., additional

Published
2023
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21. Determination of the initial hydrogen isotopic composition of the solar system

Author

J. Aléon, D. Lévy, A. Aléon-Toppani, H. Bureau, H. Khodja, F. Brisset, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'Etudes des Eléments Légers (LEEL - UMR 3685), Nanosciences et Innovation pour les Matériaux, la Biomédecine et l'Energie (ex SIS2M) (NIMBE UMR 3685), Institut Rayonnement Matière de Saclay (IRAMIS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut Rayonnement Matière de Saclay (IRAMIS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de Chimie Moléculaire et des Matériaux d'Orsay (ICMMO), Institut de Chimie du CNRS (INC)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and This work was supported by ATM grants from the Museum National d’Histoire Naturelle and by the French National Program of Planetology PNP INSU/CNRS

Subjects
Meteoritics, Astronomy and Astrophysics, [CHIM.MATE]Chemical Sciences/Material chemistry, Early solar system, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; The initial isotopic composition of water in the Solar System is of paramount importance to understanding the origin of water on planetary bodies but remains unknown, despite numerous studies. Here we use the isotopic composition of hydrogen in calcium–aluminium-rich inclusions (CAIs) from primitive meteorites, the oldest Solar System rocks, to establish the hydrogen isotopic composition of water at the onset of Solar System formation. We report the hydrogen isotopic composition of nominally anhydrous minerals from CAI fragments trapped in a once-melted host CAI. Primary minerals have extremely low D/H ratios, with δD values down to −850‰, recording the trapping of nebular hydrogen. Minerals rich in oxidised iron formed before the capture of the fragments record the existence of a nebular gas reservoir with an oxygen fugacity substantially above the solar value and a D/H ratio within 20% of that of the Earth’s oceans. Hydrogen isotopes also correlate with oxygen and nitrogen isotopes, indicating that planetary reservoirs of volatile elements formed within the first 2 × 10$^5$ years of the Solar System, during the main CAI formation epoch. We propose that the isotopic composition of inner Solar System water was established during the collapse of the protosolar cloud core owing to a massive admixture of interstellar water.

Published
2022

22. First compositional analysis of Ryugu samples by the MicrOmega hyperspectral microscope

Author

C. Pilorget, T. Okada, V. Hamm, R. Brunetto, T. Yada, D. Loizeau, L. Riu, T. Usui, A. Moussi-Soffys, K. Hatakeda, A. Nakato, K. Yogata, M. Abe, A. Aléon-Toppani, J. Carter, M. Chaigneau, B. Crane, B. Gondet, K. Kumagai, Y. Langevin, C. Lantz, T. Le Pivert-Jolivet, G. Lequertier, L. Lourit, A. Miyazaki, M. Nishimura, F. Poulet, M. Arakawa, N. Hirata, K. Kitazato, S. Nakazawa, N. Namiki, T. Saiki, S. Sugita, S. Tachibana, S. Tanaka, M. Yoshikawa, Y. Tsuda, S. Watanabe, and J.-P. Bibring

Subjects
Astronomy and Astrophysics
Published
2021

23. Formation and evolution of carbonaceous asteroid Ryugu: Direct evidence from returned samples

Author

T. Nakamura, M. Matsumoto, K. Amano, Y. Enokido, M. E. Zolensky, T. Mikouchi, H. Genda, S. Tanaka, M. Y. Zolotov, K. Kurosawa, S. Wakita, R. Hyodo, H. Nagano, D. Nakashima, Y. Takahashi, Y. Fujioka, M. Kikuiri, E. Kagawa, M. Matsuoka, A. J. Brearley, A. Tsuchiyama, M. Uesugi, J. Matsuno, Y. Kimura, M. Sato, R. E. Milliken, E. Tatsumi, S. Sugita, T. Hiroi, K. Kitazato, D. Brownlee, D. J. Joswiak, M. Takahashi, K. Ninomiya, T. Takahashi, T. Osawa, K. Terada, F. E. Brenker, B. J. Tkalcec, L. Vincze, R. Brunetto, A. Aléon-Toppani, Q. H. S. Chan, M. Roskosz, J.-C. Viennet, P. Beck, E. E. Alp, T. Michikami, Y. Nagaashi, T. Tsuji, Y. Ino, J. Martinez, J. Han, A. Dolocan, R. J. Bodnar, M. Tanaka, H. Yoshida, K. Sugiyama, A. J. King, K. Fukushi, H. Suga, S. Yamashita, T. Kawai, K. Inoue, A. Nakato, T. Noguchi, F. Vilas, A. R. Hendrix, C. Jaramillo-Correa, D. L. Domingue, G. Dominguez, Z. Gainsforth, C. Engrand, J. Duprat, S. S. Russell, E. Bonato, C. Ma, T. Kawamoto, T. Wada, S. Watanabe, R. Endo, S. Enju, L. Riu, S. Rubino, P. Tack, S. Takeshita, Y. Takeichi, A. Takeuchi, A. Takigawa, D. Takir, T. Tanigaki, A. Taniguchi, K. Tsukamoto, T. Yagi, S. Yamada, K. Yamamoto, Y. Yamashita, M. Yasutake, K. Uesugi, I. Umegaki, I. Chiu, T. Ishizaki, S. Okumura, E. Palomba, C. Pilorget, S. M. Potin, A. Alasli, S. Anada, Y. Araki, N. Sakatani, C. Schultz, O. Sekizawa, S. D. Sitzman, K. Sugiura, M. Sun, E. Dartois, E. De Pauw, Z. Dionnet, Z. Djouadi, G. Falkenberg, R. Fujita, T. Fukuma, I. R. Gearba, K. Hagiya, M. Y. Hu, T. Kato, T. Kawamura, M. Kimura, M. K. Kubo, F. Langenhorst, C. Lantz, B. Lavina, M. Lindner, J. Zhao, B. Vekemans, D. Baklouti, B. Bazi, F. Borondics, S. Nagasawa, G. Nishiyama, K. Nitta, J. Mathurin, T. Matsumoto, I. Mitsukawa, H. Miura, A. Miyake, Y. Miyake, H. Yurimoto, R. Okazaki, H. Yabuta, H. Naraoka, K. Sakamoto, S. Tachibana, H. C. Connolly, D. S. Lauretta, M. Yoshitake, M. Yoshikawa, K. Yoshikawa, K. Yoshihara, Y. Yokota, K. Yogata, H. Yano, Y. Yamamoto, D. Yamamoto, M. Yamada, T. Yamada, T. Yada, K. Wada, T. Usui, R. Tsukizaki, F. Terui, H. Takeuchi, Y. Takei, A. Iwamae, H. Soejima, K. Shirai, Y. Shimaki, H. Senshu, H. Sawada, T. Saiki, M. Ozaki, G. Ono, T. Okada, N. Ogawa, K. Ogawa, R. Noguchi, H. Noda, M. Nishimura, N. Namiki, S. Nakazawa, T. Morota, A. Miyazaki, A. Miura, Y. Mimasu, K. Matsumoto, K. Kumagai, T. Kouyama, S. Kikuchi, K. Kawahara, S. Kameda, T. Iwata, Y. Ishihara, M. Ishiguro, H. Ikeda, S. Hosoda, R. Honda, C. Honda, Y. Hitomi, N. Hirata, T. Hayashi, M. Hayakawa, K. Hatakeda, S. Furuya, R. Fukai, A. Fujii, Y. Cho, M. Arakawa, M. Abe, Y. Tsuda, Tohoku University [Sendai], NASA Johnson Space Center (JSC), NASA, The University of Tokyo (UTokyo), Tokyo Institute of Technology [Tokyo] (TITECH), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Planetary Exploration Research Center [Chiba] (PERC), Chiba Institute of Technology (CIT), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Nagoya University, Department of Earth and Planetary Science [Tokyo], Graduate School of Science [Tokyo], The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Guangzhou Institute of Geochemistry, Ritsumeikan University, Japan Synchrotron Radiation Research Institute [Hyogo] (JASRI), Institute of Low Temperature Science [Sapporo], Hokkaido University [Sapporo, Japan], Department of Earth, Environmental and Planetary Sciences [Providence], Brown University, The University of Aizu, University of Washington [Seattle], Osaka University, Kavli Institute for the Physics and Mathematics of the Universe [Tokyo] (Kavli IPMU), The University of Tokyo Institutes for Advanced Study (UTIAS), Japan Atomic Energy Agency, Goethe-University Frankfurt am Main, Department of Inorganic and Physical Chemistry, Ghent University, Universiteit Gent = Ghent University (UGENT), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Department of Earth Sciences, Royal Holloway, University of London, Egham, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Advanced Photon Source [ANL] (APS), Argonne National Laboratory [Lemont] (ANL)-University of Chicago-US Department of Energy, Kindai University, Kyushu University, Department of Earth and Atmospheric Sciences [Houston], University of Houston, Texas Materials Institute (TMI), University of Texas at Austin [Austin], Department of Geoscience, Virginia Tech, Blacksburg, VA, United States, National Institute for Materials Science (NIMS), Department of Earth Sciences [NHM London] (DES-NHM), The Natural History Museum [London] (NHM), Kanazawa University (KU), Graduate University for Advanced Studies [Hayama] (SOKENDAI), Division of Earth and Planetary Sciences [Kyoto], Kyoto University, Planetary Science Institute [Tucson] (PSI), Pennsylvania State University (Penn State), Penn State System, California State University [San Marcos] (CSUSM), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), University of Shizuoka, Ehime University [Matsuyama, Japon], European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), KEK (High energy accelerator research organization), Hitachi, Ltd, Institute for integrated Radiation and Nuclear Science (KURNS), National Metrology Institute of Japan, National Institute of Advanced Industrial Science and Technology (AIST), Department of Physics, Rikkyo University, Tokyo, Japan Fine Ceramics Center (JFCC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), The Aerospace Corporation, Earth-Life Science Institute [Tokyo] (ELSI), University of Chinese Academy of Sciences [Beijing] (UCAS), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Photone Sciences, Deutsches Elektronen-Synchrotron (DESY), Graduate School of Life Science, University of Hyogo, International Christian University, Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany], Center for Advanced Radiation Sources [University of Chicago] (CARS), University of Chicago, Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), Institut de Chimie Physique (ICP), Institut de Chimie du CNRS (INC)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Graduate School of Information Science [Nagoya], Department of Natural History Sciences, Department of Earth and Planetary Sciences [Fukuoka], Graduate School of Advanced Science and Engineering [Higashi-Hiroshima], Hiroshima University, Rowan University, Lunar and Planetary Laboratory [University of Arizona] (LPL), University of Arizona, Kanagawa Institute of Technology, Marine Works Japan Ltd., Faculty of Science, Niigata University, National Astronomical Observatory of Japan (NAOJ), Department of Physics and Astronomy [Seoul], Seoul National University [Seoul] (SNU), Kochi University, Department of Planetology, Graduate School of Science, Graduate School of Science [Kobe], Kobe University-Kobe University, Kobe University, Supported by KAKENHI from the Japanese Society for Promotion of Science (JSPS), grants JP20H00188 and 19H05183 to T.N., JP19K14776 to M.M., 21K18645 to T.M. and K.S., JP20H00205 to A.Ts., M.M., A.M. and J.M., 17H06458 to K.F., Y.T., S.Y. and M.K., JP17H06459 to T.N., T.U., S.W., M.M., N.N., T.M., T.O., Y.S., N.S., and R.N., JP15H05695 to A.Ts. and K.U., 20H05846 to S.T., JP17H06457 to H.G., JP17H06458 to Y. T. and K. F., JP19H00726 to K.K., H. G., and T.M., JP21J13337 to K.A., and JP18H05456,JP20H00189 to K.S., 18H05463 to T.T., S.N., and S.W., 18H05460 to K.N. and T.O., 18H05464 to Y.M., 18H05457 to K.N., T.T., S.W., and Y.M., and JP18H05479 to M.U. Also supported by the JSPS Core-to-Core program ' International Network of Planetary Sciences', and from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) (grants JPMXS0450200421 and JPMXS0450200521) to SS. A.K. acknowledges funding support from UK Research and Innovation (UKRI) grant MR/T020261/1. A.B. acknowledges funding support from NASA Emerging Worlds grant - 80NSSC18K0731. P.B. acknowledges funding from the European Research Council (ERC) under grant agreement no. 771691 (Solarys) and the CNES., and European Project: 771691,SOLARYS

Subjects
Multidisciplinary, [SDU]Sciences of the Universe [physics], Ryugu Hayabusa2 Carbonaceous asteroid Sample return
Abstract

Samples of the carbonaceous asteroid Ryugu were brought to Earth by the Hayabusa2 spacecraft. We analyzed 17 Ryugu samples measuring 1 to 8 millimeters. Carbon dioxide–bearing water inclusions are present within a pyrrhotite crystal, indicating that Ryugu’s parent asteroid formed in the outer Solar System. The samples contain low abundances of materials that formed at high temperatures, such as chondrules and calcium- and aluminum-rich inclusions. The samples are rich in phyllosilicates and carbonates, which formed through aqueous alteration reactions at low temperature, high pH, and water/rock ratios of

Published
2022

24. Small grains from Ryugu: handling and analysis pipeline for Infrared Synchrotron Microspectroscopy

Author

Rubino, Stefano, primary, Dionnet, Zélia, additional, Aléon-Toppani, Alice, additional, Brunetto, Rosario, additional, Nakamura, Tomoki, additional, Baklouti, Donia, additional, Djouadi, Zahia, additional, Lantz, Cateline, additional, Mivumbi, Obadias, additional, Borondics, Ferenc, additional, Lefrançois, Stephane, additional, Sandt, Christophe, additional, Capitani, Francesco, additional, Héripré, Eva, additional, Troadec, David, additional, Matsumoto, Megumi, additional, Amano, Kana, additional, Morita, Tomoyo, additional, Yurimoto, Hisayoshi, additional, Noguchi, Takaaki, additional, Okazaki, Ryuji, additional, Yabuta, Hikaru, additional, Naraoka, Hiroshi, additional, Sakamoto, Kanako, additional, Tachibana, Shogo, additional, Watanabe, Seiichiro, additional, and Tsuda, Yuichi, additional

Published
2022
Full Text
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25. Multiscale correlated analysis of the Aguas Zarcas CM chondrite

Author

Dionnet, Zélia, primary, Aléon‐Toppani, Alice, additional, Brunetto, Rosario, additional, Rubino, Stefano, additional, Suttle, Martin D., additional, Lantz, Cateline, additional, Avdellidou, Chrysa, additional, Baklouti, Donia, additional, Borondics, Ferenc, additional, Djouadi, Zahia, additional, Greco, Francesco, additional, Héripré, Eva, additional, Nakamura, Tomoki, additional, Rotundi, Alessandra, additional, and Scheel, Mario, additional

Published
2022
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26. Combining IR and X‐ray microtomography data sets: Application to Itokawa particles and to Paris meteorite

Author

Akira Tsuchiyama, David Troadec, Tomoki Nakamura, Rosario Brunetto, Zahia Djouadi, Christophe Sandt, Anne Cécile Buellet, Alessandra Rotundi, Donia Baklouti, Ferenc Borondics, Alice Aléon-Toppani, Andrew King, Stefano Rubino, Z. Dionnet, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Physiogénomique / NeuroTranscriptomes et Paléogénétique (LPG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), Tohoku University [Sendai], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), SMIS Beamline, Synchrotron SOLEIL, Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Centrale de Micro Nano Fabrication - IEMN (CMNF - IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Division of Earth and Planetary Sciences [Kyoto], Kyoto University, Centre National d’Etudes Spatiales, Agence Nationale de la Recherche, This work is supported by the 'IDI 2015' project funded by the IDEX Paris-Saclay (Grant ANR-11-IDEX- 0003-02). The FT-IR microspectroscopy activities are supported by grants from Région Ile-de-France (DIM-ACAV) and SOLEIL. This work has been funded by the Centre National d’Etudes Spatiales (CNES-France, Hayabusa2 mission) and by the ANR project CLASSY (Grant ANR-17-CE31-0004-02) of the French Agence Nationale de la Recherche. This work was partly supported by the French RENATECH network. We wish to thank the Italian Space Agency (ASI, Italy) contract no. I/024/12/2 and MIUR, contracts PNRA16-00029 and PRIN2015-20158W4JZ7. We are grateful to the JAXA Curator for allocating the Hayabusa particles. We thank T. Yada and L. Bonal for useful discussion, B. Zanda for providing the Paris meteorite sample, and the ANATOMIX team (SOLEIL) for their help with Avizo., Renatech Network, ANR-11-IDEX-0003,IPS,Idex Paris-Saclay(2011), ANR-17-CE31-0004,CLASSY,Composition des surfaces du Système Solaire de bas albédo(2017), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centrale de Micro Nano Fabrication - IEMN (CMNF-IEMN), and Kyoto University [Kyoto]

Subjects
[SPI]Engineering Sciences [physics], Geophysics, X-ray microtomography, Materials science, Meteorite, Space and Planetary Science, 0103 physical sciences, Mineralogy, 010502 geochemistry & geophysics, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences
Abstract

International audience; In the near future, a new generation of sample return missions (Hayabusa2, OSIRIS-REx, MMX, etc.) will collect samples from small solar system bodies. To maximize the scientific outcome of laboratory studies and minimize the loss of precious extraterrestrial samples, an analytical sequence from less destructive to more destructive techniques needs to be established. In this work, we present a combined X-ray and IR microtomography applied to five Itokawa particles and one fragment of the primitive carbonaceous chondrite Paris. We show that this analytical approach is able to provide a 3-D physical and chemical characterization of individual extraterrestrial particles, using the measurement of their 3-D structure and porosity, and the detection of mineral and organic phases, and their spatial co-localization in 3-D. We propose these techniques as an efficient first step in a multitechnique analytical sequence on microscopic samples collected by space missions.

Published
2020

27. Multiscale correlated analysis of the Aguas Zarcas CM chondrite

Author

Zélia Dionnet, Alice Aléon‐Toppani, Rosario Brunetto, Stefano Rubino, Martin D. Suttle, Cateline Lantz, Chrysa Avdellidou, Donia Baklouti, Ferenc Borondics, Zahia Djouadi, Francesco Grieco, Eva Héripré, Tomoki Nakamura, Alessandra Rotundi, and Mario Scheel

Subjects
Geophysics, Space and Planetary Science
Abstract

In this paper, we report the results of a campaign of measurements on four fragments of the CM Aguas Zarcas (AZ) meteorite, combining X‐ray computed tomography analysis and Fourier‐transform infrared (FT‐IR) spectroscopy. We estimated a petrologic type for our sampled CM lithology using the two independent techniques, and obtained a type CM2.5, in agreement with previous estimations. By comparing the Si‐O 10‐µm signature of the AZ average FT‐IR spectra with other well‐studied CMs, we place AZ in the context of aqueous alteration of CM parent bodies. Morphological characterization reveals that AZ has heterogeneous distribution of pores and a global porosity of 4.5 ± 0.5 vol%. We show that chondrules have a porosity of 6.3 ± 1 vol%. This larger porosity could be inherited due to various processes such as temperature variation during the chondrule formation and shocks or dissolution during aqueous alteration. Finally, we observed a correlation between 3D distributions of organic matter and mineral at micrometric scales, revealing a link between the abundance of organic matter and the presence of hydrated minerals. This supports the idea that aqueous alteration in AZ’s parent body played a major role in the evolution of the organic matter.

Published
2022

28. First compositional analysis of Ryugu samples by the MicrOmega hyperspectral microscope

Author

Pilorget, C., primary, Okada, T., additional, Hamm, V., additional, Brunetto, R., additional, Yada, T., additional, Loizeau, D., additional, Riu, L., additional, Usui, T., additional, Moussi-Soffys, A., additional, Hatakeda, K., additional, Nakato, A., additional, Yogata, K., additional, Abe, M., additional, Aléon-Toppani, A., additional, Carter, J., additional, Chaigneau, M., additional, Crane, B., additional, Gondet, B., additional, Kumagai, K., additional, Langevin, Y., additional, Lantz, C., additional, Le Pivert-Jolivet, T., additional, Lequertier, G., additional, Lourit, L., additional, Miyazaki, A., additional, Nishimura, M., additional, Poulet, F., additional, Arakawa, M., additional, Hirata, N., additional, Kitazato, K., additional, Nakazawa, S., additional, Namiki, N., additional, Saiki, T., additional, Sugita, S., additional, Tachibana, S., additional, Tanaka, S., additional, Yoshikawa, M., additional, Tsuda, Y., additional, Watanabe, S., additional, and Bibring, J.-P., additional

Published
2021
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29. NORTHWEST AFRICA (NWA) 12563 and ungrouped C2 chondrites: Alteration styles and relationships to asteroids

Author

R. Maupin, R. H. Hewins, Zahia Djouadi, J. Gattacceca, Alice Aléon-Toppani, V. Malarewicz, Ashley J. King, Hugues Leroux, Sylvain Courrech du Pont, C. Le Guillou, Pierre-Marie Zanetta, Damien Deldicque, Z. Dionnet, Thomas Rigaudier, Sylvain Bernard, Rosario Brunetto, Laurette Piani, C. Sognzoni, Ferenc Borondics, Brigitte Zanda, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Unité Matériaux et Transformations - UMR 8207 (UMET), Centrale Lille-Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de géologie de l'ENS (LGENS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), ANR-19-CE31-0027,HYDRaTE,Distribution of HYdrogen in the protoplanetary Disk and deliveRy to the Terrestrial planEts(2019), ANR-10-LABX-0038,P2IO,Physics of the 2 infinities and the origins(2010), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Centrale Lille Institut (CLIL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris)

Subjects
Chondrite parent bodies, Olivine, Chemistry, Geochemistry, Chondrule, Hyperspectral cartography, Pyroxene, engineering.material, 010502 geochemistry & geophysics, 01 natural sciences, Parent body, Silicate, Porphyritic, Chondrite-asteroid connection, chemistry.chemical_compound, Geochemistry and Petrology, Chondrite, [SDU]Sciences of the Universe [physics], 0103 physical sciences, engineering, Phenocryst, C2-ungrouped chondrites, Amorphous silicate, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

International audience; Many asteroids in the main belt have spectra like those of Mighei-type CM chondrites, but some Near Earth Objects (NEO) resemble less well known types of C2 chondrite. Northwest Africa (NWA) 12563, a new find with affinities to C2 chondrites, could help us understand the differences between observations of CM2 chondrites and bodies that are currently being studied by the Hayabusa2 and OSIRIS-REx space missions. NWA 12563 contains 14% chondrules supported by 86% fine grained matrix consistent with CM2 chondrites, but differs from them in other respects. In both matrix and chondrules, olivine is unaltered and pyroxene shows incipient alteration. Metal in chondrules is pseudomorphed by serpentine, and mesostasis is replaced by serpentine-saponite and chlorite. Many Type I chondrules have highly irregular shapes resulting from fracturing and selective metal replacement. Type II porphyritic chondrules are clusters of phenocrysts set in matrix-like material. Type II chondrules may be kinked and partially disbarred. The matrix of NWA 12563 differs from CM2 chondrites in the absence of tochilinite-cronstedtite intergrowths. It contains hydrated and oxidized amorphous silicate (Fe3+/∑Fe ~75%) richer in magnesium than in other chondrites (with embedded sulfides). Serpentine-saponite is also present, as well as abundant framboidal magnetite.NWA 12563 has similarities to a number of ungrouped magnetite-rich and 18O-rich chondrites (Bells, Essebi, Niger I, WIS 91600, Tagish Lake, and MET 00432) that we call C2-ung1, as opposed to C2-ung2 chondrites (poorer in 18O and magnetite). The oxygen isotopic composition coupled with a magnetic susceptibility of log χ = 4.67 places NWA 12563 with these ungrouped chondrites in a cluster distinct from CM2 chondrites. NWA 12563 is closest to WIS 91600 among the C2-ung1 chondrites in alteration style and light element compositions. WIS 91600, however, has suffered light thermal metamorphism, suggesting that NWA 12563 might represent its altered but unheated precursor material within the same parent body if it were zoned. The average Vis-NIR spectrum of NWA 12563 matches the asteroid taxonomic class K and resembles that of CO3 Frontier Mountain (FRO) 95002, but its spectra range from very “red” in dark matrix areas and very “blue” in magnetite-rich areas. The average MIR spectrum shows features indicating phyllosilicates, aliphatic CH compounds, hydrated silicates, and olivine. It is significantly different from those of other chondrites including FRO 95002, and closest to Bells (from which it differs in carbon isotopic composition) and WIS91600. The variety of mineralogical, chemical and isotopic properties among C2-ung1 chondrites requires several different parent bodies. However, the high abundance of magnetite common to this cluster of ungrouped chondrites, and to a lesser extent CI chondrites, indicates that they should be considered as possible material from Bennu, which has an 18 µm magnetite signal in its spectrum not seen in the CM2 chondrites (Hamilton et al., 2019).

Published
2021

30. A preparation sequence for multi‐analysis of µm‐sized extraterrestrial and geological samples

Author

Alice Aléon-Toppani, François Brisset, Jérôme Aléon, David Troadec, Michael E. Zolensky, Ferenc Borondics, Rosario Brunetto, Daniel Lévy, Andrew King, Stefano Rubino, Z. Dionnet, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Physics of Complex Systems, Weizmann Institute of Science [Rehovot, Israël], Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-JUNIA (JUNIA), Université catholique de Lille (UCL)-Université catholique de Lille (UCL), Centrale de Micro Nano Fabrication - IEMN (CMNF - IEMN), Université catholique de Lille (UCL)-Université catholique de Lille (UCL)-Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-JUNIA (JUNIA), Institut de Chimie Moléculaire et des Matériaux d'Orsay (ICMMO), Institut de Chimie du CNRS (INC)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), PSICHÉ beamline, Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), his work was partly supported by the French RENATECH network, grants from Ile de France (DIM-ACAV) and SOLEIL (IR microscopic analyses), and grants from LabeX CHARMMMAT, LaSIPS, and Region Ile de France (TEM). It was also supported by the CNRS INSU PNP National Planetary Programme and by the CentreNational d’Etudes Spatiales (CNES-France, Hayabusa2 mission), Renatech Network, ANR-11-LABX-0039,CHARMMMAT,CHimie des ARchitectures MoléculairesMultifonctionnelles et des MATériaux(2011), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-JUNIA (JUNIA)-Centrale Lille-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-JUNIA (JUNIA)

Subjects
[SPI]Engineering Sciences [physics], Geophysics, Materials science, Space and Planetary Science, Extraterrestrial life, 0103 physical sciences, Mineralogy, 010502 geochemistry & geophysics, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences, Sequence (medicine)
Abstract

International audience; With the recent and ongoing sample return missions and/or the developments of nano-to microscale 3-D and 2-D analytical techniques, it is necessary to develop sample preparation and analysis protocols that allow combination of different nanometer-to micrometer-scale resolution techniques and both maximize scientific outcome and minimize sample loss and contamination. Here, we present novel sample preparation and analytical procedures to extract a maximum of submicrometer structural, mineralogical, chemical, molecular, and isotopic information from micrometric heterogeneous samples. The sample protocol goes from a nondestructive infrared (IR) tomography of~10 to~70 µm-sized single grains, which provides the distribution and qualitative abundances of both mineral and organic phases, followed by its cutting in several slices at selected sites of interest for 2-D mineralogical analysis (e.g., transmission electron microscopy), molecular organic and mineral analysis (e.g., Raman and/or IR microspectroscopy), and isotopic/chemical analysis (e.g., NanoSIMS). We also discuss here the importance of the focused ion beam microscopy in the protocol, the problems of sample loss and contamination, and at last the possibility of combining successive different analyses in various orders on the same micrometric sample. Special care was notably taken to establish a protocol allowing correlated NanoSIMS/TEM/IR analyses with NanoSIMS performed first. Finally, we emphasize the interest of 3-D and 2-D IR analyses in studying the organics-minerals relationship in combination with more classical isotopic and mineralogical grain characterizations.

Published
2021

33. Techniques and instruments to analyze, characterize and study returned samples

Author

Alice Aléon-Toppani, Jérôme Aléon, Zahia Djouadi, Janet Borg, and Rosario Brunetto

Subjects
Computer science, Extraterrestrial life, Systems engineering, Sample (statistics), Space exploration
Abstract

Since the pioneer lunar sample return missions, the development of advanced techniques for the laboratory analysis of retrieved samples has run in parallel with the advances in space studies. All along the last decades, a common goal of these developments has been to maximize the scientific outcomes of laboratory studies while minimizing the loss of precious extraterrestrial samples. We provide an overview of the techniques and instruments used so far to analyze, characterize and study returned extraterrestrial samples. Considering the limited amount of material that is retrieved by the space missions, a multi-analytical sequence from less destructive techniques to more destructive techniques needs to be established. The return of Hayabusa2 and OSIRIS-REx samples will probably trigger a wave of laboratory studies, which, in turn, will support new developments of space instruments for observations of Solar System bodies.

Published
2021

34. Contributors

Author

Masanao Abe, Jérôme Aléon, Alice Aléon-Toppani, Allan Bennett, Lucy Berthoud, Janet Borg, John C. Bridges, Donald E. Brownlee, Rosario Brunetto, Don Burnett, John Robert Brucato, Vincenzo Della Corte, Vinciane Debaille, Fabrizio Dirri, Zahia Djouadi, Heather L. Enos, Ludovic Ferrière, Luigi Folco, Frédéric Foucher, Ian A. Franchi, Akira Fujiwara, Matthieu Gounelle, Monica M. Grady, John Holt, Aurore Hutzler, Eric A. Jerde, Amy Jurewicz, Junichiro Kawaguchi, Dante S. Lauretta, Stefano Leuko, Andrea Longobardo, Jonathan I. Lunine, Yves Marrocchi, Andrea Meneghin, Ernesto Palomba, Anjani T. Polit, Thomas Pottage, Yuqi Qian, Dan Reisenfeld, Petra Rettberg, Heather L. Roper, Alessandra Rotundi, Sara S. Russell, Scott A. Sandford, Caroline L. Smith, Evgeny Slyuta, Shogo Tachibana, Elizabeth J. Tasker, Akira Tsuchiyama, John Vrublevskis, Qian Wang, Qiong Wang, Frances Westall, Roger C. Wiens, Catherine W.V. Wolner, Long Xiao, Makoto Yoshikawa, Jutta Zipfel, and Michael E. Zolensky

Published
2021

36. Vis–NIR Reflectance Microspectroscopy of IDPs

Author

Rosario Brunetto, Alice Aléon-Toppani, Romain Maupin, Pierre Vernazza, Zahia Djouadi, Cateline Lantz, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and ANR-16-CE29-0015,RAHIIA_SSOM,Analyses de résidus provenant d'analogues de glace interstellaire pour la compréhension de la formation de la matière organique du Système Solaire(2016)

Subjects
Astronomy and Astrophysics, 010502 geochemistry & geophysics, 01 natural sciences, Reflectivity, Astrobiology, Geophysics, Interplanetary dust cloud, Meteorite, 13. Climate action, Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Spectroscopy, 010303 astronomy & astrophysics, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

Visible near-infrared (Vis–NIR) reflectance spectroscopy is a powerful nondestructive technique allowing the parent bodies identification of cosmomaterials such as meteorites, micrometeorites, and interplanetary dust particles (IDPs) studied in the laboratory. Previous studies showed that meteorites do not represent the full diversity of the solar system small bodies. We present here an experimental setup we developed for measuring Vis–NIR microspectroscopy of individual IDPs. We acquired diffuse Vis–NIR reflectance spectra of 15 particles ranging 7–31 μm in size. We discuss the requirements, the abilities, as well as the limitations of the technique. For sizes smaller than 17 μm, the slopes increase with decreasing particles sizes, while for sizes larger than 17 μm, the slopes are randomly distributed. The visible reflectance levels do not appear to be affected by the size of the IDPs, and show a bimodal distribution. Among the studied particles, we identified an IDP (L2079C18) exhibiting a feature at 0.66 μm, which is similar to the one observed by remote sensing on the surface of hydrated asteroids. This is the first detection of a hydration band in the reflectance spectrum of an IDP that could indicate a possible link between hydrated IDPs with hydrated asteroid surfaces.

Published
2020

37. VIS-NIR DIFFUSE REFLECTANCE MICRO-SPECTROSCOPIC ANALYSIS OF IDPs

Author

Pierre Vernazza, Alice Aléon-Toppani, Cateline Lantz, Romain Maupin, Zahia Djouadi, and Rosario Brunetto

Abstract

Introduction: Meteorites seem to come from a small number of primary parent bodies [1]. B-, C-, Cb-, Cg-, P- and D-types, representing not less than 66% of the mass of the main belt have no analogues clearly identified in the meteorite collections [2]. However, meteorites are not the only cosmomaterials found on Earth since no less than 30 000 tons of interplanetary dust particles (IDPs) enter the Earth’s atmosphere each year [3]. IDPs originate from different parent bodies throughout the solar system [4, 5, 6]. The link between IDPs and asteroids can be investigated thanks to Vis-NIR spectroscopy commonly used for the classification of asteroids (0.4 - 2.5 µm). The reflectance measurements in the visible range (0.4 - 0.8 μm) performed on IDPs in the 90s [7] and the simulated visible near infrared (Vis-NIR) spectra of IDPs with comparison of mid infrared (Mid-IR) spectra [2] have shown that IDPs may be good analogues to some asteroids and in particular to the classes not sampled by meteorites. But Vis-NIR reflectance measurements of IDPs is challenging and we must understand how the measurement on an isolated micro-metric particle can be affected by physical parameters of the sample such as size, composition, and roughness. We report here the requirements, the abilities as well as the limitations of the technique and the results obtained on 15 IDPs particles ranging 7-31 µm in size in the Vis-NIR range (0.45 - 1.0 µm). Experiments: Our setup, installed in a clean room, consists of a Vis-NIR spectrometer (Maya2000 Pro from Ocean Optics) coupled to a macroscope (Leica Z16 APO). A Vis-NIR optical fiber (100 or 50 μm in diameter) is used to collect the light diffused by the sample which is unilaterally illuminated by a halogen source through a 1000 μm diameter fiber (phase angle of ~ 45°). By changing the magnification and/or the diameter of the collection fiber it is possible to adapt the collection spot to the grain size down to 7 μm size. Results and discussion: To obtain a reliable reflectance spectrum of a micro-metric grain with this setup, we show that it is necessary to average spectra taken at different azimuth angles, by rotating the particle several times in the observation plane with respect to the incident light. Based on the study of spectral slopes we found that for particles with sizes below ~ 17 µm the spectral slope increases linearly with decreasing particle sizes. This behavior is due to a bias encountered in the reflectance measurement in this size range, inducing thus a loss of the chemical information. For particle sizes larger than ∼ 17 µm the spectral slopes seem randomly distributed between ∼ -0.3 and 0.4 µm−1, and the spectra must therefore carry chemical information of the particles. We found that the visible reflectance levels of the IDPs show a multimodal distribution. There is a lack of IDPs with reflectance level ~ 5 and ~ 8%. In addition, the majority of IDPs have rather low reflectance levels (< 10%). Some particles have reflectance levels that may be influenced by the presence of magnetite, which is sometimes found in extraterrestrial materials and could form upon atmospheric entry. Among the studied particles we identified an IDP (L2079C18) exhibiting a feature at 0.66 µm which is similar to the one observed by remote sensing at the surface of hydrated asteroids. This is the first detection of a hydration band in the reflectance spectrum of an IDP which could indicate a possible link between hydrated IDPs with hydrated asteroid surfaces. Acknowledgments: We are grateful to the CAPTEM NASA for providing the IDPs. This work is supported by the Programme National de Planétologie (PNP) of CNRS/INSU, co-funded by CNES. The authors also thank the ANR RAHIIA SSOM and the P2IO LabEx (ANR-10-LABX0038) in the framework Investissements d’Avenir (ANR11-IDEX-0003-01) for their supports. We thank O. Mivumbi and Y. Longval for their help and technical support for the development of the device. References: [1] R. Greenwood et al. (2020) Geochimica et Cosmochimica Acta 277, 377-406. [2] P. Vernazza et al. (2015) The Astrophysical Journal 806 :204. [3] Love and Brownlee. (1993) Science, 262, 550-553. [4] Dermott et al. (1994) Nature, 369, 719-723. [5] Liou et al. (1996) Icarus, 124, 429-440. [6] Brunetto et al. (2011) Icarus, 212, 896-910. [6] Bradley, J. P. (2003) Treatise on Geochemistry, 1, 689. [7] Bradley, et al. (1996) Meteoritics & Planetary Science, 31, 394-402.

Published
2020

38. Hyperspectral imaging of carbonaceous chondrites in view of the Hayabusa2 sample return

Author

Tomoki Nakamura, K. Amano, Moe Matsuoka, David Troadec, Zahia Djouadi, Akira Tsuchiyama, Cateline Lantz, Miki Takahashi, Ferenc Borondics, Alice Aléon-Toppani, Yann Arribard, Stefano Rubino, Donia Baklouti, Megumi Matsumoto, Rosario Brunetto, and Z. Dionnet

Subjects
Chondrite, Hyperspectral imaging, Mineralogy, Sample (graphics), Geology
Abstract

1. Introduction The Hayabusa2/JAXA spacecraft has orbited and studied near-Earth object Ryugu [1]. Two sample collections have been performed and the spacecraft is currently on its way back to the Earth for an expected return in late 2020. A preliminary examination phase will follow [2], expected to elucidate the formation and evolution of Ryugu. Considering the limited amount of material that will be retrieved, a multi-analytical sequence is needed to maximize the scientific outcome and minimize sample loss. Among the possible laboratory techniques, IR spectroscopy is important in being totally non-destructive and comparable to remote sensing observations of small bodies [3]. Thanks to IR imaging micro-spectroscopy, it is possible to detect and study the spatial distribution of molecular bonds associated to minerals, water and organic compounds, and their co-localization [4]. We consider IR three dimensional (3D) micro-tomography (IR-CT) an excellent starting point in a multi-analytical sequence to be applied on returned samples [5]. Here we report IR hyperspectral measurements of carbonaceous chondrites as a rehearsal of IR-CT and IR hyperspectral imaging that will be part of the multi-analytical sequence of the “MIN-PET CG” Hayabusa2 team (mineralogy and petrology of coarse grains) led by T. Nakamura. 2. Methods We performed IR measurements in reflectance on bulk fragments of selected meteorites, and both in reflectance and transmittance on several isolated grains (sizing 20-50 µm) extracted from carbonaceous chondrites. We also analyzed individual grains of the Murchison CM meteorite prepared at Tohoku University (Japan) from three bulk samples: (1) unheated, (2) heated at 400°C, and (3) heated at 600°C [6]. The laboratory-controlled heating was applied to simulate potential heating undergone by Ryugu surface materials, as suggested by some Hayabusa2 observations [7]. Some of these Murchison grains were mounted on tungsten needles by means of a platinum welding performed in IEMN-Lille (France) with a focused ion beam microscope. Other grains were prepared at Tohoku University, mounted on carbon fibers using epoxy (Fig. 1). We analyzed the samples using an IR hyperspectral imaging and micro-tomography setup installed at the SMIS beamline of the SOLEIL synchrotron (France). This setup has already been used for analyzing Hayabusa samples from asteroid Itokawa [8]. FTIR data were collected using an Agilent Cary 670/620 microspectrometer. In transmission mode we used a X25 objective coupled with high magnification optics (providing an additional X2.5 magnification) placed in front of a 128x128 pixels FPA detector, to obtain a projected pixel size of ~0.66 µm on the focal plane, and a field of view of ~84 µm. IR-CT is performed in transmission mode using the method described by Dionnet et al. [8]. In reflection mode we used a X15 objective, with a projected pixel size of ~5.5 µm on the focal plane, and a field of view of ~700 µm (Fig. 1). In both cases we collected hyperspectral data: for each pixel we obtained an IR spectrum in the 850-3950 cm-1 spectral range. The spatial resolution was diffractionlimited for the whole investigated spectral range. 3. Results Infrared spectra show the presence of bending and stretching absorption bands of chemical bonds (C-H, OH, Si-O, C=O, etc.) of different functional groups, as expected from literature IR spectra of Murchison and other chondrites [9,10]. The relative intensities of these bands are found to vary among different grains, and their 3D spatial distribution is heterogeneous within individual grains (see Fig. 1). Noticeable differences are found between the IR spectra of unheated and heated Murchison samples, with a general trend of increasing the anhydrous to hydrated silicate content with increasing temperature, and reducing the organic content. Fig. 1. A typical IR reflectance hyperspectral map of an unheated Murchison sample mounted on a carbon needle (top left, microscope images in bright and dark field), with the detection of hydrated (bottom left) and anhydrous (bottom right) areas. The epoxy contribution can be clearly separated (top right). 4. Summary and Conclusions IR data provide a first quick look at the composition, abundance and 3D distribution of mineral phases and carbonaceous materials at the scale of a few micrometers. Once regions of interest are identified by IR measurements, thin sliced sections of the samples can be analyzed by more destructive techniques to retrieve the structure and the elemental and isotopic composition of the carbonaceous component and its mineral host, down to the nanometer scale [11]. In addition, the IR data are useful in the comparison with remote sensing observations of asteroid surfaces [7,12]. This top-down sequence will help us building a bridge between the remote sensing and in situ observations of Ryugu at macroscopic scale and the chemical and physical processes operating at the nanoscale. Acknowledgments The micro-spectroscopy measurements were supported by grants from Region Ile-de-France (DIM-ACAV) and SOLEIL. This work has been funded by the CNES (France) and by the ANR project CLASSY (Grant ANR-17-CE31-0004-02) of the French Agence Nationale de la Recherche. This work was partly supported by the French RENATECH network. References [1] Watanabe S. et al. (2019) Science 364, 268-272. [2] Tachibana S. et al. (2018) AGU Fall Meeting, abstract #P33C-3846. [3] Brunetto R. et al. (2011) Icarus 212, 896–910. [4] Dionnet Z. et al. (2018) Meteoritics & Planet. Sci. 53, 2608-2623. [5] Dionnet Z. et al. (2018) Microscopy and Microanalysis 24, 2100-2101. [6] Mogi K. et al. (2017) 80th Annual Meeting of the Meteoritical Society, Abstract #6225. [7] Kitazato K. et al. (2019) Science 364, 272-275. [8] Dionnet Z. et al. (2020) Meteoritics & Planet. Sci., in press. [9] Lantz C. et al. (2015) A&A 577, A41. [10] Beck P. et al. (2014) Icarus 229, 263-277. [11] Aléon-Toppani A. et al. (2020) Lunar and Planetary Science Conference 2682. [12] Hamilton V. et al. (2019) Nat. Astron. 3, 332–340.

Published
2020

39. Alkali magmatism on a carbonaceous chondrite planetesimal

Author

Alice Aléon-Toppani, François Brisset, Kevin D. McKeegan, Jacques-Marie Bardintzeff, Jérôme Aléon, Bernard Platevoet, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Géosciences Paris Saclay (GEOPS), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California-University of California, Institut de Chimie Moléculaire et des Matériaux d'Orsay (ICMMO), Institut de Chimie du CNRS (INC)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and University of California (UC)-University of California (UC)

Subjects
Planetesimal, Multidisciplinary, 010504 meteorology & atmospheric sciences, Partial melting, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, 010502 geochemistry & geophysics, 01 natural sciences, Mantle (geology), Astrobiology, Meteorite, 13. Climate action, Chondrite, [SDU]Sciences of the Universe [physics], Carbonaceous chondrite, Physical Sciences, Formation and evolution of the Solar System, Planetary differentiation, Geology, 0105 earth and related environmental sciences
Abstract

International audience; Recent isotopic and paleomagnetic data point to a possible connection between carbonaceous chondrites and differentiated planetary materials, suggesting the existence, perhaps ephemeral, of transitional objects with a layered structure whereby a metal-rich core is enclosed by a silicate mantle, which is itself overlain by a crust containing an outermost layer of primitive solar nebula materials. This idea has not received broad support, mostly because of a lack of samples in the meteoritic record that document incipient melting at the onset of planetary differentiation. Here, we report the discovery and the petrologic–isotopic characterization of UH154-11, a ferroan trachybasalt fragment enclosed in a Renazzo-type carbonaceous chondrite (CR). Its chemical and oxygen isotopic compositions are consistent with very-low-degree partial melting of a Vigarano-type carbonaceous chondrite (CV) from the oxidized subgroup at a depth where fluid-assisted metamorphism enhanced the Na content. Its microdoleritic texture indicates crystallization at an increasing cooling rate, such as would occur during magma ascent through a chondritic crust. This represents direct evidence of magmatic activity in a carbonaceous asteroid on the verge of differentiating and demonstrates that some primitive outer Solar System objects related to icy asteroids and comets underwent a phase of magmatic activity early in the Solar System. With its peculiar petrology, UH154-11 can be considered the long-sought first melt produced during partial differentiation of a carbonaceous chondritic planetary body, bridging a previously persistent gap in differentiation processes from icy cometary bodies to fully melted iron meteorites with isotopic affinities to carbonaceous chondrites.

Published
2020

40. IR micro-spectroscopy and micro-tomography of isolated murchison grains in preparation of the Hayabusa2 sample return

Author

Brunetto, R., Aléon-Toppani, A., Rubino, S., Baklouti, D., Borondics, F., Dionnet, Z., Djouadi, Z., Lantz, C., Nakamura, T., Takahashi, M., Troadec, David, Tsuchiyama, A., Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Centrale de Micro Nano Fabrication - IEMN (CMNF-IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Renatech Network, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and Centrale de Micro Nano Fabrication - IEMN (CMNF - IEMN)

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

International audience; We report the incorporation of IR-CT and IR hyperspectral imaging in the multi-analytical sequence of the MIN-PET CG Hayabusa2 preliminary examination team.

Published
2020

41. A Preparation Sequence for Multi-Analysis of Micrometer-Sized Extraterrestrial Samples

Author

Aléon-Toppani, A., Brunetto, R., Aléon, J., Dionnet, Z., Rubino, S., Levy, D., Troadec, D., Borondics, F., Brisset, F., Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Centrale de Micro Nano Fabrication - IEMN (CMNF-IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Renatech Network, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and Centrale de Micro Nano Fabrication - IEMN (CMNF - IEMN)

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology
Abstract

POSTER; International audience; We developed a new sample preparation and characterization sequence combining IR tomography, TEM, IR mapping, and NanoSIMS analyses on individual 20 µm grains.

Published
2020

42. Determination of optical constants from Martian analog materials using a spectro-polarimetric technique

Author

Rosario Brunetto, O. Mivumbi, V. Godard, Alice Aléon-Toppani, E. Garcia-Caurel, C. Boukari, R. G. Urso, François Poulet, Ferenc Borondics, John Carter, G. Alemanno, FRA, Institut d'astrophysique spatiale (IAS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)

Subjects
Complex data type, Materials science, 010504 meteorology & atmospheric sciences, Infrared, business.industry, Optical constants Mars surface Spectroscopy Ellipsometry Laboratory, Polarimetry, Physics::Optics, Astronomy and Astrophysics, 01 natural sciences, Characterization (materials science), Optics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Ellipsometry, 0103 physical sciences, Light beam, Bidirectional reflectance distribution function, business, Spectroscopy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

The technique of spectroscopic ellipsometry is a powerful tool for the characterization of the optical properties of materials. This technique represents a significant refinement over the semi-empirical approach to optical constants determination using BRDF (Bidirectional Reflectance Distribution Function) measurements of a finite set of grain sizes for each mineral. It also allows obtaining, not only the optical constants, but also information about the dependence of optical response on sample orientation respect to the illuminating light beam. In this work, we present our experimental approach to derive optical constants of Martian analogue materials based on an infrared ellipsometry technique. We derived the optical constants of gypsum between 750 and 5000 ​cm−1 (2–13 ​μm) using data obtained with an infrared spectroscopic Mueller ellipsometer. Thanks to the high sensitivity of the ellipsometric measurements, and despite of a rather complex data analysis protocol, the results obtained for the gypsum samples show that it is possible to successfully use this technique for direct determination of optical constants of natural minerals. The method discussed here can provide the planetary science community with laboratory derived optical constants of a large number of minerals and materials (either natural or synthetic).

Published
2020

45. Hyperspectral imaging of carbonaceous chondrites in view of the Hayabusa2 sample return

Author

Brunetto, Rosario, primary, Aléon-Toppani, Alice, additional, Dionnet, Zélia, additional, Rubino, Stefano, additional, Arribard, Yann, additional, Baklouti, Donia, additional, Borondics, Ferenc, additional, Djouadi, Zahia, additional, Lantz, Cateline, additional, Matsumoto, Megumi, additional, Matsuoka, Moe, additional, Nakamura, Tomoki, additional, Amano, Kana, additional, Takahashi, Miki, additional, Troadec, David, additional, and Tsuchiyama, Akira, additional

Published
2020
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47. Combining IR and X‐ray microtomography data sets: Application to Itokawa particles and to Paris meteorite

Author

Dionnet, Zelia, primary, Brunetto, Rosario, additional, Aléon‐Toppani, Alice, additional, Rubino, Stefano, additional, Baklouti, Donia, additional, Borondics, Ferenc, additional, Buellet, Anne‐Cécile, additional, Djouadi, Zahia, additional, King, Andrew, additional, Nakamura, Tomoki, additional, Rotundi, Alessandra, additional, Sandt, Christophe, additional, Troadec, David, additional, and Tsuchiyama, Akira, additional

Published
2020
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48. NanoSIMS imaging of D/H ratios on FIB sections

Author

Hélène Bureau, Hicham Khodja, Alice Aléon-Toppani, Adriana Gonzalez-Cano, Daniel Lévy, Rémi Duhamel, David Troadec, Jérôme Aléon, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Centrale de Micro Nano Fabrication - IEMN (CMNF-IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Laboratoire d'Etudes des Eléments Légers (LEEL - UMR 3685), Nanosciences et Innovation pour les Matériaux, la Biomédecine et l'Energie (ex SIS2M) (NIMBE UMR 3685), Institut Rayonnement Matière de Saclay (IRAMIS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Institut Rayonnement Matière de Saclay (IRAMIS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Museum National d'Histoire Naturelle, CNRS-INSU PNP national planetology program, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centrale de Micro Nano Fabrication - IEMN (CMNF - IEMN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut Rayonnement Matière de Saclay (IRAMIS), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Mineral hydration, 010504 meteorology & atmospheric sciences, Chemistry, [SDU]Sciences of the Universe [physics], Analytical chemistry, [CHIM.MATE]Chemical Sciences/Material chemistry, 010502 geochemistry & geophysics, Nanoscale secondary ion mass spectrometry, 01 natural sciences, Focused ion beam, 0105 earth and related environmental sciences, Analytical Chemistry
Abstract

International audience; The D/H ratio imaging of weakly hydrated minerals prepared as Focused Ion Beam (FIB) sections is developed in order to combine isotopic imaging by Nanoscale Secondary Ion Mass Spectrometry (NanoSIMS) of micrometer-sized grains with other nanoscale imaging techniques, such as Transmission Electron Microscopy. In order to maximize the accuracy, sensitivity, precision and reproducibility of D/H ratios at the micrometer-size, while minimizing the surface contamination at the same time, we explored all instrumental parameters known to influence the measurement of D/H ratios in situ. Optimal conditions were found to be obtained with the use of (i) a Cs$^+$ ion source and detection of H$^-$ and D$^-$at low mass resolving power, (ii) a primary beam intensity of 100 pA, and (iii) raster sizes in the range 8-15 $\mu$m. Nominally anhydrous minerals were used to evaluate the detection limits and indicate a surface contamination level of about 200 ppm equivalent H$_2$O in these conditions. With the high primary intensity used here, the dwell time is not a parameter as critical as found in previous studies and a dwell time of 1 ms/px is used to minimize dynamic contamination during analysis. Analysis of FIB sections was found to reduce significantly static contamination due to sample preparation and improved accuracy compared to using polished sections embedded not only in epoxy but in indium as well. On amphiboles, the typical overall uncertainty including reproducibility is about 20 ‰ on bulk FIB sections and about 50 ‰ at the 1.5 $\mu$m scale using image processing (1$\sigma$).

Published
2019

49. FTIR and X-ray micro-tomography on Itokawa particles and carbonaceous chondrites

Author

Brunetto, Rosario, Dionnet, Zélia, Aléon-Toppani, Alice, Baklouti, Donia, Borondics, Ferenc, Djouadi, Zahia, King, Andrew, Nakamura, Tomoki, Rubino, Stefano, Sandt, Christophe, Troadec, David, Tsuchiyama, Akira, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut d’Électronique, de Microélectronique et de Nanotechnologie - UMR 8520 (IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Centrale de Micro Nano Fabrication - IEMN (CMNF-IEMN), Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)-Centrale Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), Renatech Network, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and Centrale de Micro Nano Fabrication - IEMN (CMNF - IEMN)

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

International audience; We report a combined IR and X micro-tomography analysis of five particles from asteroid Itokawa and a few selected fragments of several carbonaceous chondrites. These techniques are an efficient first-step in a multi-technique analytical sequence to be applied on small Solar System bodies samples, collected by space missions such as Hayabusa2 and OSIRIS-REx.

Published
2019

50. Organic and mineralogic heterogeneity of the Paris meteorite followed by FTIR hyperspectral imaging

Author

Donia Baklouti, Ferenc Borondics, Alice Aléon-Toppani, François Brisset, Zahia Djouadi, Christophe Sandt, Rosario Brunetto, Z. Dionnet, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), Institut de Chimie Moléculaire et des Matériaux d'Orsay (ICMMO), Université Paris-Sud - Paris 11 (UP11)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)

Subjects
Materials science, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mineralogy, Hyperspectral imaging, 010502 geochemistry & geophysics, 01 natural sciences, Geophysics, Meteorite, Space and Planetary Science, 0103 physical sciences, Fourier transform infrared spectroscopy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

International audience

Published
2018

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