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Jaumann R, Schmitz N, Ho TM, Schröder SE, Otto KA, Stephan K, Elgner S, Krohn K, Preusker F, Scholten F, Biele J, Ulamec S, Krause C, Sugita S, Matz KD, Roatsch T, Parekh R, Mottola S, Grott M, Michel P, Trauthan F, Koncz A, Michaelis H, Lange C, Grundmann JT, Maibaum M, Sasaki K, Wolff F, Reill J, Moussi-Soffys A, Lorda L, Neumann W, Vincent JB, Wagner R, Bibring JP, Kameda S, Yano H, Watanabe S, Yoshikawa M, Tsuda Y, Okada T, Yoshimitsu T, Mimasu Y, Saiki T, Yabuta H, Rauer H, Honda R, Morota T, Yokota Y, Kouyama T. Images from the surface of asteroid Ryugu show rocks similar to carbonaceous chondrite meteorites. Science 2020; 365:817-820. [PMID: 31439797 DOI: 10.1126/science.aaw8627] [Citation(s) in RCA: 80] [Impact Index Per Article: 20.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/31/2019] [Accepted: 07/23/2019] [Indexed: 11/02/2022]
Abstract
The near-Earth asteroid (162173) Ryugu is a 900-m-diameter dark object expected to contain primordial material from the solar nebula. The Mobile Asteroid Surface Scout (MASCOT) landed on Ryugu's surface on 3 October 2018. We present images from the MASCOT camera (MASCam) taken during the descent and while on the surface. The surface is covered by decimeter- to meter-sized rocks, with no deposits of fine-grained material. Rocks appear either bright, with smooth faces and sharp edges, or dark, with a cauliflower-like, crumbly surface. Close-up images of a rock of the latter type reveal a dark matrix with small, bright, spectrally different inclusions, implying that it did not experience extensive aqueous alteration. The inclusions appear similar to those in carbonaceous chondrite meteorites.
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Affiliation(s)
- R Jaumann
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany. .,Free University of Berlin, Institute of Geosciences, Berlin, Germany
| | - N Schmitz
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - T-M Ho
- DLR, Institute of Space Systems, Bremen, Germany
| | - S E Schröder
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - K A Otto
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - K Stephan
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - S Elgner
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - K Krohn
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - F Preusker
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - F Scholten
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - J Biele
- DLR, Microgravity User Support Center, Linder Höhe, Cologne, Germany
| | - S Ulamec
- DLR, Microgravity User Support Center, Linder Höhe, Cologne, Germany
| | - C Krause
- DLR, Microgravity User Support Center, Linder Höhe, Cologne, Germany
| | - S Sugita
- Department of Earth and Planetary Science, School of Science, University of Tokyo, Tokyo 113-0033, Japan
| | - K-D Matz
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - T Roatsch
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - R Parekh
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany.,Free University of Berlin, Institute of Geosciences, Berlin, Germany
| | - S Mottola
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - M Grott
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - P Michel
- Université Côte d'Azur, Observatoire de la Côte d'Azur, Centre National de la Recherche Scientifique, Laboratoire Lagrange, Nice, France
| | - F Trauthan
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - A Koncz
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - H Michaelis
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - C Lange
- DLR, Institute of Space Systems, Bremen, Germany
| | | | - M Maibaum
- DLR, Microgravity User Support Center, Linder Höhe, Cologne, Germany
| | - K Sasaki
- DLR, Institute of Space Systems, Bremen, Germany
| | - F Wolff
- DLR, Institute of System Dynamics and Control, Oberpfaffenhofen, Germany
| | - J Reill
- DLR, Institute of Robotics and Mechatronics, Oberpfaffenhofen, Germany
| | - A Moussi-Soffys
- Centre National d'Études Spatiales, 18 Avenue E. Belin, Toulouse 31401, France
| | - L Lorda
- Centre National d'Études Spatiales, 18 Avenue E. Belin, Toulouse 31401, France
| | - W Neumann
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - J-B Vincent
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - R Wagner
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany
| | - J-P Bibring
- L'Université de Paris Sud-Orsay, Institut d'Astrophysique Spatiale, Orsay, France
| | - S Kameda
- Department of Physics, Rikkyo University, 3-34-1 Nishi-Ikebukuro, Toshima, Tokyo 171-8501, Japan
| | - H Yano
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - S Watanabe
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan.,Department of Earth and Planetary Sciences, Nagoya University Furo-cho Chikusa-ku, Nagoya, Japan
| | - M Yoshikawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - Y Tsuda
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - T Okada
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - T Yoshimitsu
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - Y Mimasu
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - T Saiki
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - H Yabuta
- Department of Earth and Planetary Systems Science, Hiroshima University, Hiroshima, Japan
| | - H Rauer
- German Aerospace Center (DLR), Institute of Planetary Research, Berlin, Germany.,Free University of Berlin, Institute of Geosciences, Berlin, Germany
| | - R Honda
- Kochi University, Department of Information Science, Akebono, Kochi, Japan
| | - T Morota
- University of Tokyo, Department of Earth and Planetary Science, Hongo, Bunkyo, Tokyo, Japan
| | - Y Yokota
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Japan
| | - T Kouyama
- National Institute of Advanced Industrial Science and Technology, Aomi, Koto, Tokyo, Japan
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Clark RN, Brown RH, Jaumann R, Cruikshank DP, Nelson RM, Buratti BJ, McCord TB, Lunine J, Baines KH, Bellucci G, Bibring JP, Capaccioni F, Cerroni P, Coradini A, Formisano V, Langevin Y, Matson DL, Mennella V, Nicholson PD, Sicardy B, Sotin C, Hoefen TM, Curchin JM, Hansen G, Hibbits K, Matz KD. Compositional maps of Saturn's moon Phoebe from imaging spectroscopy. Nature 2005; 435:66-9. [PMID: 15875014 DOI: 10.1038/nature03558] [Citation(s) in RCA: 127] [Impact Index Per Article: 6.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/21/2004] [Accepted: 03/11/2005] [Indexed: 11/08/2022]
Abstract
The origin of Phoebe, which is the outermost large satellite of Saturn, is of particular interest because its inclined, retrograde orbit suggests that it was gravitationally captured by Saturn, having accreted outside the region of the solar nebula in which Saturn formed. By contrast, Saturn's regular satellites (with prograde, low-inclination, circular orbits) probably accreted within the sub-nebula in which Saturn itself formed. Here we report imaging spectroscopy of Phoebe resulting from the Cassini-Huygens spacecraft encounter on 11 June 2004. We mapped ferrous-iron-bearing minerals, bound water, trapped CO2, probable phyllosilicates, organics, nitriles and cyanide compounds. Detection of these compounds on Phoebe makes it one of the most compositionally diverse objects yet observed in our Solar System. It is likely that Phoebe's surface contains primitive materials from the outer Solar System, indicating a surface of cometary origin.
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Affiliation(s)
- Roger N Clark
- US Geological Survey, MS964, Box 25046, Federal Center, Denver, Colorado 80225, USA.
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