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1. Spectro-photometry of Phobos simulants: II. Effects of porosity

Author

Wargnier, Antonin, Poch, Olivier, Poggiali, Giovanni, Gautier, Thomas, Doressoundiram, Alain, Beck, Pierre, Nakamura, Tomoki, Miyamoto, Hideaki, Kameda, Shingo, Ruscassier, Nathalie, Buch, Arnaud, Hasselmann, Pedro H., Sultana, Robin, Quirico, Eric, Fornasier, Sonia, and Barucci, Antonella

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Surface porosity has been found to be an important property for small bodies. Some asteroids and comets can exhibit an extremely high surface porosity in the first millimeter layer. This layer may be produced by various processes and maintained by the lack of an atmosphere. However, the influence of porosity on the spectro-photometric properties of small body surfaces is not yet fully understood. In this study, we looked into the effect of porosity on the spectro-photometric properties of Phobos regolith spectroscopic simulants; created by mixing the simulants with ultra-pure water, producing ice-dust particles, and then sublimating the water. The reflectance spectroscopic properties in the visible and near-infrared (0.5-4.2 $\mu$m) show no strong variations between the porous and compact samples. However, one simulant exhibits a bluing of the slope after increasing porosity, providing possible insights into the differences between the blue and red units observed on Phobos. In the mid-infrared range, a contrast increase of the 10-$\mu$m emissivity plateau due to silicates is observed. Photometry reveals a modification in the phase reddening behavior between the compact powder and the sublimation residue for both simulants. However, the observed behavior is different between the simulants, suggesting that the phase reddening may be dependent on the composition of the simulants. The phase curve also appears to be modified by the addition of porosity, with a higher contribution of forward scattering observed for the sublimation residue. The derivation of the Hapke parameters indicates an increase in roughness for the porous sample, but no significant modification of the opposition effect. This study aims to provide new insights into the understanding of porosity by using two Phobos simulants in the context of the upcoming JAXA/Martian Moons eXploration mission., Comment: Submitted to Icarus

Published
2024

2. GAUSS -- A Sample Return Mission to Ceres

Author

Shi, Xian, Castillo-Rogez, Julie, Hsieh, Henry, Hui, Hejiu, Ip, Wing-Huen, Lei, Hanlun, Li, Jian-Yang, Tosi, Federico, Zhou, Liyong, Agarwal, Jessica, Barucci, Antonella, Beck, Pierre, Bagatin, Adriano Campo, Capaccioni, Fabrizio, Coates, Andrew, Cremonese, Gabriele, Duffard, Rene, Jaumann, Ralf, Jones, Geraint, Grande, Manuel, Kallio, Esa, Lin, Yangting, Mousis, Olivier, Nathues, Andreas, Oberst, Jürgen, Showman, Adam, Sierks, Holger, Ulamec, Stephan, and Wang, Mingyuan

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The goal of Project GAUSS is to return samples from the dwarf planet Ceres. Ceres is the most accessible ocean world candidate and the largest reservoir of water in the inner solar system. It shows active cryovolcanism and hydrothermal activities in recent history that resulted in minerals not found in any other planets to date except for Earth's upper crust. The possible occurrence of recent subsurface ocean on Ceres and the complex geochemistry suggest possible past habitability and even the potential for ongoing habitability. Aiming to answer a broad spectrum of questions about the origin and evolution of Ceres and its potential habitability, GAUSS will return samples from this possible ocean world for the first time. The project will address the following top-level scientific questions: 1) What is the origin of Ceres and the origin and transfer of water and other volatiles in the inner solar system? 2) What are the physical properties and internal structure of Ceres? What do they tell us about the evolutionary and aqueous alteration history of icy dwarf planets? 3) What are the astrobiological implications of Ceres? Was it habitable in the past and is it still today? 4) What are the mineralogical connections between Ceres and our current collections of primitive meteorites? GAUSS will first perform a high-resolution global remote sensing investigation, characterizing the geophysical and geochemical properties of Ceres. Candidate sampling sites will then be identified, and observation campaigns will be run for an in-depth assessment of the candidate sites. Once the sampling site is selected, a lander will be deployed on the surface to collect samples and return them to Earth in cryogenic conditions that preserves the volatile and organic composition as well as the original physical status as much as possible., Comment: Section 3.4 revised; List of team members updated; Typos corrected

Published
2019

3. ASIME 2018 White Paper. In-Space Utilisation of Asteroids: Asteroid Composition -- Answers to Questions from the Asteroid Miners

Author

Graps, Amara L., Abbud-Madrid, Angel, Abell, Paul, Barucci, Antonella, Beck, Pierre, Bonal, Lydie, Bonin, Grant, Borgersen, Øystein Risan, Britt, Daniel, Campins, Humberto, Cannon, Kevin, Carnelli, Ian, Carry, Benoît, Crawford, Ian, de Leon, Julia, Drube, Line, Donaldson-Hanna, Kerri, Elvis, Martin, Fitzsimmons, Alan, Galache, JL, Green, Simon F., Grundmann, Jan Thimo, Herique, Alan, Hestroffer, Daniel, Hsieh, Henry, Kereszturi, Akos, Kueppers, Michael, Lewicki, Chris, Lin, Yangting, Mainzer, Amy, Michel, Patrick, Moon, Hong-Kyu, Nakamura, Tomoki, Penttila, Antti, Pursiainen, Sampsa, Raymond, Carol, Reddy, Vishnu, Rivkin, Andy, Sercel, Joel, Stickle, Angela, Tanga, Paolo, Takala, Mika, Wirtz, Tom, and Wu, YunZhao

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

In keeping with the Luxembourg government's initiative to support the future use of space resources, ASIME 2018 was held in Belval, Luxembourg on April 16-17, 2018. The goal of ASIME 2018: Asteroid Intersections with Mine Engineering, was to focus on asteroid composition for advancing the asteroid in-space resource utilisation domain. What do we know about asteroid composition from remote-sensing observations? What are the potential caveats in the interpretation of Earth-based spectral observations? What are the next steps to improve our knowledge on asteroid composition by means of ground-based and space-based observations and asteroid rendez-vous and sample return missions? How can asteroid mining companies use this knowledge? ASIME 2018 was a two-day workshop of almost 70 scientists and engineers in the context of the engineering needs of space missions with in-space asteroid utilisation. The 21 Questions from the asteroid mining companies were sorted into the four asteroid science themes: 1) Potential Targets, 2) Asteroid-Meteorite Links, 3) In-Situ Measurements and 4) Laboratory Measurements. The Answers to those Questions were provided by the scientists with their conference presentations and collected by A. Graps or edited directly into an open-access collaborative Google document or inserted by A. Graps using additional reference materials. During the ASIME 2018, first day and second day Wrap-Ups, the answers to the questions were discussed further. New readers to the asteroid mining topic may find the Conversation boxes and the Mission Design discussions especially interesting., Comment: Outcome from the ASIME 2018: Asteroid Intersections with Mine Engineering, Luxembourg. April 16-17, 2018. 65 Pages. arXiv admin note: substantial text overlap with arXiv:1612.00709

Published
2019

4. Space weathering acts strongly on the uppermost surface of Ryugu

Author

Matsuoka, Moe, Kagawa, Ei-ichi, Amano, Kana, Nakamura, Tomoki, Tatsumi, Eri, Osawa, Takahito, Hiroi, Takahiro, Milliken, Ralph, Domingue, Deborah, Takir, Driss, Brunetto, Rosario, Barucci, Antonella, Kitazato, Kohei, Sugita, Seiji, Fujioka, Yuri, Sasaki, Osamu, Kobayashi, Shiho, Iwata, Takahiro, Morota, Tomokatsu, Yokota, Yasuhiro, Kouyama, Toru, Honda, Rie, Kameda, Shingo, Cho, Yuichiro, Yoshioka, Kazuo, Sawada, Hirotaka, Hayakawa, Masahiko, Sakatani, Naoya, Yamada, Manabu, Suzuki, Hidehiko, Honda, Chikatoshi, Ogawa, Kazunori, Shirai, Kei, Lantz, Cateline, Rubino, Stefano, 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, Tomohiro, Yoshikawa, Makoto, Saiki, Takanao, Tanaka, Satoshi, Terui, Fuyuto, Nakazawa, Satoru, Watanabe, Sei-ichiro, and Tsuda, Yuichi

Published
2023
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5. GAUSS - genesis of asteroids and evolution of the solar system: A sample return mission to Ceres

Author

Shi, Xian, Castillo-Rogez, Julie, Hsieh, Henry, Hui, Hejiu, Ip, Wing-Huen, Lei, Hanlun, Li, Jian-Yang, Tosi, Federico, Zhou, Liyong, Agarwal, Jessica, Barucci, Antonella, Beck, Pierre, Bagatin, Adriano Campo, Capaccioni, Fabrizio, Coates, Andrew J., Cremonese, Gabriele, Duffard, Rene, Grande, Manuel, Jaumann, Ralf, Jones, Geraint H., Kallio, Esa, Lin, Yangting, Mousis, Olivier, Nathues, Andreas, Oberst, Jürgen, Sierks, Holger, Ulamec, Stephan, and Wang, Mingyuan

Published
2022
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6. Asteroid Ryugu Before the Hayabusa2 Encounter

Author

Wada, Koji, Grott, Matthias, Michel, Patrick, Walsh, Kevin J., Barucci, Antonella M., Biele, Jens, Blum, Jürgen, Ernst, Carolyn M., Grundmann, Jan T., Gundlach, Bastian, Hagermann, Axel, Hamm, Maximilian, Jutzi, Martin, Kim, Myung-Jin, Kührt, Ekkehard, Corre, Lucille Le, Libourel, Guy, Lichtenheldt, Roy, Maturilli, Alessandro, Messenger, Scott R., Michikami, Tatsuhiro, Miyamoto, Hideaki, Mottola, Stefano, Nakamura, Akiko M., Müller, Thomas, Nittler, Larry R., Ogawa, Kazunori, Okada, Tatsuaki, Palomba, Ernesto, Sakatani, Naoya, Schröder, Stefan, Senshu, Hiroki, Takir, Driss, and Zolensky, Michael E.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Asteroid (162173) Ryugu is the target object of Hayabusa2, an asteroid exploration and sample return mission led by Japan Aerospace Exploration Agency (JAXA). Ground-based observations indicate that Ryugu is a C-type near-Earth asteroid with a diameter of less than 1 km, but the knowledge of its detailed properties is still very limited. This paper summarizes our best understanding of the physical and dynamical properties of Ryugu based on remote sensing and theoretical modeling. This information is used to construct a design reference model of the asteroid that is used for formulation of mission operations plans in advance of asteroid arrival. Particular attention is given to the surface properties of Ryugu that are relevant to sample acquisition. This reference model helps readers to appropriately interpret the data that will be directly obtained by Hayabusa2 and promotes scientific studies not only for Ryugu itself and other small bodies but also for the Solar System evolution that small bodies shed light on., Comment: 62 pages, 10 figures, 8 tables. Submitted to Space Science Reviews, on 6 April 2018

Published
2018

7. The Mars system revealed by the Martian Moons eXploration mission

Author

Ogohara, Kazunori, Nakagawa, Hiromu, Aoki, Shohei, Kouyama, Toru, Usui, Tomohiro, Terada, Naoki, Imamura, Takeshi, Montmessin, Franck, Brain, David, Doressoundiram, Alain, Gautier, Thomas, Hara, Takuya, Harada, Yuki, Ikeda, Hitoshi, Koike, Mizuho, Leblanc, François, Ramirez, Ramses, Sawyer, Eric, Seki, Kanako, Spiga, Aymeric, Vandaele, Ann Carine, Yokota, Shoichiro, Barucci, Antonella, and Kameda, Shingo

Published
2022
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8. The global surface composition of 67P/CG nucleus by Rosetta/VIRTIS. I) Prelanding mission phase

Author

Filacchione, Gianrico, Capaccioni, Fabrizio, Ciarniello, Mauro, Raponi, Andrea, Tosi, Federico, De Sanctis, Maria Cristina, Erard, Stephane, Morvan, Dominique Bockelee, Leyrat, Cedric, Arnold, Gabriele, Schmitt, Bernard, Quirico, Eric, Piccioni, Giuseppe, Migliorini, Alessandra, Capria, Maria Teresa, Palomba, Ernesto, Cerroni, Priscilla, Longobardo, Andrea, Barucci, Antonella, Fornasier, Sonia, Carlson, Robert W., Jaumann, Ralf, Stephan, Katrin, Moroz, Lyuba V., Kappel, David, Rousseau, Batiste, Fonti, Sergio, Mancarella, Francesca, Despan, Daniela, and Faure, Mathilde

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

From August to November 2014 the Rosetta orbiter has performed an extensive observation campaign aimed at the characterization of 67P/CG nucleus properties and to the selection of the Philae landing site. The campaign led to the production of a global map of the illuminated portion of 67P/CG nucleus. During this prelanding phase the comet's heliocentric distance decreased from 3.62 to 2.93 AU while Rosetta was orbiting around the nucleus at distances between 100 to 10 km. VIRTIS-M, the Visible and InfraRed Thermal Imaging Spectrometer - Mapping channel (Coradini et al. 2007) onboard the orbiter, has acquired 0.25-5.1 micron hyperspectral data of the entire illuminated surface, e.g. the north hemisphere and the equatorial regions, with spatial resolution between 2.5 and 25 m/pixel. I/F spectra have been corrected for thermal emission removal in the 3.5-5.1 micron range and for surface's photometric response. The resulting reflectance spectra have been used to compute several Cometary Spectral Indicators (CSI): single scattering albedo at 0.55 micron, 0.5-0.8 micron and 1.0-2.5 micron spectral slopes, 3.2 micron organic material and 2.0 micron water ice band parameters (center, depth) with the aim to map their spatial distribution on the surface and to study their temporal variability as the nucleus moved towards the Sun. Indeed, throughout the investigated period, the nucleus surface shows a significant increase of the single scattering albedo along with a decrease of the 0.5-0.8 and 1.0-2.5 micron spectral slopes, indicating a flattening of the reflectance. We attribute the origin of this effect to the partial removal of the dust layer caused by the increased contribution of water sublimation to the gaseous activity as comet crossed the frost-line., Comment: 19 Figures, 5 Tables. Accepted for publication in Icarus journal on 29 February 2016

Published
2016
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9. OSS (Outer Solar System): A fundamental and planetary physics mission to Neptune, Triton and the Kuiper Belt

Author

Christophe, Bruno, Spilker, Linda J., Anderson, John D., André, Nicolas, Asmar, Sami W., Aurnou, Jonathan, Banfield, Don, Barucci, Antonella, Bertolami, Orfeu, Bingham, Robert, Brown, Patrick, Cecconi, Baptiste, Courty, Jean-Michel, Dittus, Hansjörg, Fletcher, Leigh N., Foulon, Bernard, Francisco, Frederico, Gil, Paulo J. S., Glassmeier, Karl-Heinz, Grundy, Will, Hansen, Candice, Helbert, Jörn, Helled, Ravit, Hussmann, Hauke, Lamine, Brahim, Lämmerzahl, Claus, Lamy, Laurent, Lehoucq, Rolland, Lenoir, Benjamin, Levy, Agnès, Orton, Glenn, Páramos, Jorge, Poncy, Joël, Postberg, Frank, Progrebenko, Sergei V., Reh, Kim R., Reynaud, Serge, Robert, Clélia, Samain, Etienne, Saur, Joachim, Sayanagi, Kunio M., Schmitz, Nicole, Selig, Hanns, Sohl, Frank, Spilker, Thomas R., Srama, Ralf, Stephan, Katrin, Touboul, Pierre, and Wolf, Peter

Subjects
General Relativity and Quantum Cosmology, Astrophysics - Earth and Planetary Astrophysics, Physics - Instrumentation and Detectors
Abstract

The present OSS mission continues a long and bright tradition by associating the communities of fundamental physics and planetary sciences in a single mission with ambitious goals in both domains. OSS is an M-class mission to explore the Neptune system almost half a century after flyby of the Voyager 2 spacecraft. Several discoveries were made by Voyager 2, including the Great Dark Spot (which has now disappeared) and Triton's geysers. Voyager 2 revealed the dynamics of Neptune's atmosphere and found four rings and evidence of ring arcs above Neptune. Benefiting from a greatly improved instrumentation, it will result in a striking advance in the study of the farthest planet of the Solar System. Furthermore, OSS will provide a unique opportunity to visit a selected Kuiper Belt object subsequent to the passage of the Neptunian system. It will consolidate the hypothesis of the origin of Triton as a KBO captured by Neptune, and improve our knowledge on the formation of the Solar system. The probe will embark instruments allowing precise tracking of the probe during cruise. It allows to perform the best controlled experiment for testing, in deep space, the General Relativity, on which is based all the models of Solar system formation. OSS is proposed as an international cooperation between ESA and NASA, giving the capability for ESA to launch an M-class mission towards the farthest planet of the Solar system, and to a Kuiper Belt object. The proposed mission profile would allow to deliver a 500 kg class spacecraft. The design of the probe is mainly constrained by the deep space gravity test in order to minimise the perturbation of the accelerometer measurement., Comment: 43 pages, 10 figures, Accepted to Experimental Astronomy, Special Issue Cosmic Vision. Revision according to reviewers comments

Published
2011
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10. The ‘small’ asteroid population: a spectroscopic survey

Author

Michimani, Jonatan, primary, Rondón, Eduardo, additional, Perna, Davide, additional, Ieva, Simone, additional, Dotto, Elisabetta, additional, Mazzotta Epifani, Elena, additional, Barucci, Antonella, additional, Petropoulou, Vasiliki, additional, and Lazzaro, Daniela, additional

Published
2023
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12. Results from the ESO Large Program on Transneptunian Objects and Centaurs

Author

Boehnhardt, Hermann, Barucci, Antonella, Delsanti, Audrey, De Bergh, Catherine, Doressoundiram, Alain, Romon, Jennifer, Dotto, Elisabetta, Tozzi, Gianpaolo, Lazzarin, Monica, Fornasier, Sonia, Peixinho, Nuno, Hainaut, Olivier, Davies, John, Rousselot, Philippe, Barrera, Luis, Birkle, Kurt, Meech, Karen, Ortiz, Joseluis, Sekiguchi, Tomohiko, Watanabe, Jun-Ichi, Thomas, Nick, West, Richard, Davies, John K., editor, and Barrera, Luis H., editor

Published
2004
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13. GAUSS - genesis of asteroids and evolution of the solar system

Author

Shi, Xian, Castillo-Rogez, Julie, Hsieh, Henry, Hui, Hejiu, Ip, Wing-Huen, Lei, Hanlun, Li, Jian-Yang, Tosi, Federico, Zhou, Liyong, Agarwal, Jessica, Barucci, Antonella, Beck, Pierre, Campo Bagatin, Adriano, Capaccioni, Fabrizio, Coates, Andrew, Cremonese, Gabriele, Duffard, Rene, Grande, Manuel, Jaumann, Ralf, Jones, Geraint, Kallio, Esa, Lin, Yangting, Mousis, Olivier, Nathues, Andreas, Oberst, Jürgen, Sierks, Holger, Ulamec, Stephan, and Wang, Mingyuan

Subjects
habitability, Dwarf planet, ocean world, Ceres, voyage 2050, sample return
Published
2021

14. Two independent and primitive envelopes of the bilobate nucleus of comet 67P

Author

Massironi, Matteo, Simioni, Emanuele, Marzari, Francesco, Cremonese, Gabriele, Giacomini, Lorenza, Pajola, Maurizio, Jorda, Laurent, Naletto, Giampiero, Lowry, Stephen, El-Maarry, Mohamed Ramy, Preusker, Frank, Scholten, Frank, Sierks, Holger, Barbieri, Cesare, Lamy, Philippe, Rodrigo, Rafael, Koschny, Detlef, Rickman, Hans, Keller, Horst Uwe, AʼHearn, Michael F., Agarwal, Jessica, Auger, Anne-Thérèse, Barucci, Antonella M., Bertaux, Jean-Loup, Bertini, Ivano, Besse, Sebastien, Bodewits, Dennis, Capanna, Claire, Da Deppo, Vania, Davidsson, Björn, Debei, Stefano, De Cecco, Mariolino, Ferri, Francesca, Fornasier, Sonia, Fulle, Marco, Gaskell, Robert, Groussin, Olivier, Gutiérrez, Pedro J., Güttler, Carsten, Hviid, Stubbe F., Ip, Wing-Huen, Knollenberg, Jörg, Kovacs, Gabor, Kramm, Rainer, Kührt, Ekkehard, Küppers, Michael, La Forgia, Fiorangela, Lara, Luisa M., Lazzarin, Monica, Lin, Zhong-Yi, Lopez Moreno, Josè J., Magrin, Sara, Michalik, Harald, Mottola, Stefano, Oklay, Nilda, Pommerol, Antoine, Thomas, Nicolas, Tubiana, Cecilia, and Vincent, Jean-Baptiste

Published
2015
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15. TNOs are Cool: A Survey of the Transneptunian Region: A Herschel Open Time Key Programme

Author

Müller, Thomas G., Lellouch, Emmanuel, Böhnhardt, Hermann, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René, Fornasier, Sonia, Groussin, Olivier, Gutiérrez, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, Lara, Luisa, Lim, Tanya, Mueller, Michael, Moreno, Raphael, Ortiz, Jose-Luis, Rengel, Miriam, Santos-Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, and Trilling, David

Published
2009
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16. Spectrophotometric Properties of 162173 Ryugu’s Surface from the NIRS3 Opposition Observations

Author

Domingue, Deborah, primary, Kitazato, Kohei, additional, Matsuoka, Moe, additional, Yokota, Yasuhiro, additional, Tatsumi, Eri, additional, Iwata, Takahiro, additional, Abe, Masanao, additional, Ohtake, Makiko, additional, Matsuura, Shuji, additional, Schröder, Stefan, additional, Vilas, Faith, additional, Barucci, Antonella, additional, Brunetto, Rosario, additional, Takir, Driss, additional, Le Corre, Lucille, additional, and Moskovitz, Nicholas, additional

Published
2021
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17. GAUSS - genesis of asteroids and evolution of the solar system

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Shi, Xian, Castillo-Rogez, Julie, Hsieh, Henry, Hui, Hejiu, Ip, Wing-Huen, Lei, Hanlun, Li, Jian-Yang, Tosi, Federico, Zhou, Liyong, Agarwal, Jessica, Barucci, Antonella, Beck, Pierre, Campo Bagatin, Adriano, Capaccioni, Fabrizio, Coates, Andrew J., Cremonese, Gabriele, Duffard, René, Grande, Manuel, Jaumann, Ralf, Jones, Geraint H., Kallio, Esa, Lin, Yangting, Mousis, Olivier, Nathues, Andreas, Oberst, Jürgen, Sierks, Holger, Ulamec, Stephan, Wang, Mingyuan, The GAUSS Team, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Shi, Xian, Castillo-Rogez, Julie, Hsieh, Henry, Hui, Hejiu, Ip, Wing-Huen, Lei, Hanlun, Li, Jian-Yang, Tosi, Federico, Zhou, Liyong, Agarwal, Jessica, Barucci, Antonella, Beck, Pierre, Campo Bagatin, Adriano, Capaccioni, Fabrizio, Coates, Andrew J., Cremonese, Gabriele, Duffard, René, Grande, Manuel, Jaumann, Ralf, Jones, Geraint H., Kallio, Esa, Lin, Yangting, Mousis, Olivier, Nathues, Andreas, Oberst, Jürgen, Sierks, Holger, Ulamec, Stephan, Wang, Mingyuan, and The GAUSS Team

Abstract

The goal of Project GAUSS (Genesis of Asteroids and evolUtion of the Solar System) is to return samples from the dwarf planet Ceres. Ceres is the most accessible candidate of ocean worlds and the largest reservoir of water in the inner Solar System. It shows active volcanism and hydrothermal activities in recent history. Recent evidence for the existence of a subsurface ocean on Ceres and the complex geochemistry suggest past habitability and even the potential for ongoing habitability. GAUSS will return samples from Ceres with the aim of answering the following top-level scientific questions: - What is the origin of Ceres and what does this imply for the origin of water and other volatiles in the inner Solar System? - What are the physical properties and internal structure of Ceres? What do they tell us about the evolutionary and aqueous alteration history of dwarf planets? - What are the astrobiological implications of Ceres? Is it still habitable today? - What are the mineralogical connections between Ceres and our current collections of carbonaceous meteorites?

Published
2021

19. Results from the Eso Large Program on Transneptunian Objects and Centaurs

Author

Boehnhardt, Hermann, Barucci, Antonella, Delsanti, Audrey, De Bergh, Catherine, Doressoundiram, Alain, Romon, Jennifer, Dotto, Elisabetta, Tozzi, Gianpaolo, Lazzarin, Monica, Fornasier, Sonia, Peixinho, Nuno, Hainaut, Olivier, Davies, John, Rousselot, Philippe, Barrera, Luis, Birkle, Kurt, Meech, Karen, Ortiz, JoseLuis, Sekiguchi, Tomohiko, Watanabe, Jun-ichi, Thomas, Nick, and West, Richard

Published
2003
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20. Distinguishing carbonates and organics on OSIRIS-REx target asteroid Bennu using the 3.4-micron feature

Author

Ferrone, Salvatore, primary, Clark, Beth, additional, Kaplan, Hannah, additional, Zou, Xiao-Duan, additional, Li, Jian-Yang, additional, Barucci, Antonella, additional, Simon, Amy, additional, Hamilton, Elizabeth, additional, Reuter, Dennis, additional, Praet, Alice, additional, Deshapriya, Prasanna, additional, Poggiali, Giovanni, additional, Brucato, Jon, additional, and Lauretta, Dante, additional

Published
2020
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21. Hydration variations of Bennu’s surface: comparison of different methods.

Author

Praet, Alice, primary, Barucci, Antonella, additional, Kaplan, Hannah, additional, Merlin, Frédéric, additional, Clark, Beth, additional, Simon, Amy, additional, Hamilton, Victoria, additional, Emery, Joshua, additional, Howell, Ellen, additional, Lim, Lucy, additional, Zou, Xiao-Duan, additional, Reuter, Dennis, additional, Ferrone, Salvatore, additional, Deshapriya, Prasanna, additional, Fornasier, Sonia, additional, Hasselmann, Pedro, additional, Poggiali, Giovanni, additional, Brucato, John, additional, Takir, Driss, additional, and Lauretta, Dante, additional

Published
2020
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22. Tensile strength of 67P/Churyumov–Gerasimenko nucleus material from overhangs

Author

Attree, N., Groussin, O., Jorda, L., Nébouy, D., Thomas, N., Brouet, Y., Kührt, Ekkehard, Preusker, Frank, Scholten, Frank, Knollenberg, Jörg, Hartogh, P., Sierks, H., Barbieri, C., Lamy, P., Rodrigo, R., Koschny, D., Rickman, H., Keller, H. U., A’Hearn, M. F., Auger, A.-T., Barucci, Antonella, Bertaux, J.-L., Bertini, I., Bodewits, Dennis, Boudreault, S., Cremonese, G., Deppo, Vania Da, Davidsson, B., Debei, S., De Cecco, M., Deller, J., El-Maarry, M. R., Fornasier, S., Fulle, M., Gutierrez, P.J., Güttler, C., Hviid, Stubbe, Ip, W-H., Kovacs, G., Kramm, J. R., Küppers, M., Lara López, Luisa M., Lazzarin, M., Lopez Moreno, J., Lowry, S., Marchi, S., Marzari, F., Mottola, S., Naletto, G., Oklay, Nilda, Pajola, M., Toth, I., Tubiana, C., Vincent, Jean-Baptiste, Shi, X., 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), Physikalisches Institut [Bern], Universität Bern [Bern], DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Dipartimento di Fisica e Astronomia 'Galileo Galilei', Universita degli Studi di Padova, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), International Space Science Institute [Bern] (ISSI), European Space Agency Advanced Concepts and Science Payloads Office (ESA ESTEC), European Space Agency (ESA), ESA Scientific Support Office, Department of Physics and Astronomy [Uppsala], Uppsala University, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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 Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Laboratory for Ultraviolet and X-ray Optical Research [Padova] (LUXOR), CNR Institute for Photonics and Nanotechnologies (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR)-Consiglio Nazionale delle Ricerche [Roma] (CNR), Department of Industrial Engineering [Padova], University of Trento [Trento], Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institute of Space Science [Taiwan], National Central University [Taiwan] (NCU), Operations Department (ESAC), European Space Astronomy Centre (ESAC), European Space Agency (ESA)-European Space Agency (ESA), Centre for Astrophysics and Planetary Science [Canterbury] (CAPS), University of Kent [Canterbury], Solar System Exploration Research Virtual Institute (SSERVI), Southwest Research Institute [Boulder] (SwRI), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), NASA Ames Research Center (ARC), Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] ( DLR ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Centro de Astrobiologia [Madrid] ( CAB ), Instituto Nacional de Técnica Aeroespacial ( INTA ) -Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), International Space Science Institute ( ISSI ), Space Research Centre [Warsaw] ( CBK ), Polska Akademia Nauk ( PAN ), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] ( IGEP ), Technische Universität Braunschweig [Braunschweig], Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astronomico di Trieste ( OAT ), Istituto Nazionale di Astrofisica ( INAF ), Laboratory for Ultraviolet and X-ray Optical Research [Padova] ( LUXOR ), CNR Institute for Photonics and Nanotechnologies ( IFN ), Consiglio Nazionale delle Ricerche [Roma] ( CNR ) -Consiglio Nazionale delle Ricerche [Roma] ( CNR ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), National Central University [Taiwan] ( NCU ), European Space Astronomy Center ( ESAC ), European Space Agency ( ESA ) -European Space Agency ( ESA ), Centre for Astrophysics and Planetary Science [Canterbury] ( CAPS ), Solar System Exploration Research Virtual Institute ( SSERVI ), Southwest Research Institute [Boulder] ( SwRI ), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' ( CISAS ), NASA Ames Research Center ( ARC ), Hungarian Academy of Sciences [Budapest], Universität Bern [Bern] (UNIBE), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Università degli Studi di Padova = University of Padua (Unipd), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)-National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), ITA, USA, GBR, FRA, DEU, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Polska Akademia Nauk (PAN), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Consejo Superior de Investigaciones Científicas [Spain] (CSIC)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Comets: individual: Churyumov-Gerasimenko, FOS: Physical sciences, general [comets], Comets: general, Methods: observational, es, individual: Churyumov-Gerasimenko [comets], Astronomi, astrofysik och kosmologi, [SDU]Sciences of the Universe [physics], Astronomy, Astrophysics and Cosmology, observational [Methods], addenda, errata, ComputingMilieux_MISCELLANEOUS, [ SDU ] Sciences of the Universe [physics], Astrophysics - Earth and Planetary Astrophysics
Abstract

We directly measure twenty overhanging cliffs on the surface of comet 67P/Churyumov-Gerasimenko extracted from the latest shape model and estimate the minimum tensile strengths needed to support them against collapse under the comet's gravity. We find extremely low strengths of around one Pa or less (one to five Pa, when scaled to a metre length). The presence of eroded material at the base of most overhangs, as well as the observed collapse of two features and implied previous collapse of another, suggests that they are prone to failure and that true material strengths are close to these lower limits (although we only consider static stresses and not dynamic stress from, for example, cometary activity). Thus, a tensile strength of a few pascals is a good approximation for the tensile strength of 67P's nucleus material, which is in agreement with previous work. We find no particular trends in overhang properties with size, over the $\sim10-100$ m range studied here, or location on the nucleus. There are no obvious differences, in terms of strength, height or evidence of collapse, between the populations of overhangs on the two cometary lobes, suggesting that 67P is relatively homogenous in terms of tensile strength. Low material strengths are supportive of cometary formation as a primordial rubble pile or by collisional fragmentation of a small (tens of km) body., 13 pages, 11 figures. Accepted for publication in Astronomy & Astrophysics

Published
2018
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23. SHERMAN-Based Thermophysical Model of (101955) Bennu

Author

Crowell, Jenna, Howell, Ellen, Emery, Joshua, Trilling, David, Hergenrother, Carl, Hora, Joseph, Lim, Lucy F., Mueller, Michael, Delbo, Marco, Harris, Alan, Barucci, Antonella, Lauretta, Dante S., and Astronomy

Abstract

We apply our thermophysical model to derive regolith properties of (101955) Bennu constrained by Spitzer observations taken in 2007 (Emery et al. 2014) and 2012, before the arrival of the OSIRIS-REx spacecraft. From these observations, we will create a thermal curve and compare with photometric lightcurves, investigating physical characteristics. Our thermophysical model is described in detail by Magri et al. (2018) and treats surface roughness using a fractional coverage of hemispherical craters on each facet. In some cases we find that the thermal inertia in our models is lower than that calculated by other thermal models. This may be due to capturing inhomogeneity in our observations, or to observations at particular observing geometries (Crowell et al., 2017). (101955) Bennu, target of the OSIRIS-REx mission, will provide us with "ground-truth", allowing us to compare the results of our thermal model with the spatially resolved spacecraft measurements. This work will also allow us to interpret nonphysical parameters like crater fraction and relate them to the highly resolved measurements of the surface, soon to be available. References: Emery et al. 2014, Icarus 234, 17-35.; Magri et al. 2018, Icarus 303, 203-219; Crowell et al. 2017 ACM.

Published
2018

24. An efficient algorithm for prioritizing NEA physical observations

Author

Cortese, Matteo, Perozzi, Ettore, Micheli, Marco, Borgia, Barbara, Dotto, Elisabetta, Barucci, Antonella, Perna, Davide, Mazzotta, E., Epifani, and Ieva, S.

Subjects
NEOShield
Abstract

The present near-Earth asteroids (NEA) discovery rate has surpassed 1500 objects per year, thus calling for extensive observation campaigns devoted to physical characterization in order to define successful mitigation strategies in case of possible impactors. A tool is presented which, through a prioritization algorithm, aims to optimize the planning and the execution of NEA physical observations. Two ranking criteria are introduced, Importance and Urgency, accounting for the need of satisfying the two basic observational modes for physical characterization, that is, rapid response and large observing programs, aimed at selecting targets for exploration and mitigation space missions. The resulting tool generates a daily table of observable targets and it can also be run as a stand-alone tool in order to provide future observing opportunities at a specific date of interest. It has been developed and implemented within the framework of the NEOShield-2 EU/HORIZON 2020 Project; the output of the prioritization algorithm is publicly available, in tabular format, on the NEOShield-2 NEO Properties Portal (http://www.neoshield.net/the-neoshield-project/project-activities/neo-properties-portal), reachable from the main page of the Project website (http://www.neoshield.eu)., This work was also partially funded under ESA contract 4000112366 SSA P2-NEO-I NEO Precursor Services.

Published
2017
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25. Infrared detection of exposed Carbon Dioxide ice on 67P/CG nucleus surface by Rosetta-VIRTIS

Author

Filacchione, G., Raponi, A., Capaccioni, F., Barucci, Antonella, De Sanctis, M.C., Fornasier, S., Ciarniello, M., Migliorini, A., Erard, S., Bockelee-Morvan, D., Leyrat, C., Tosi, F., Piccioni, G., Palomba, E., Capria, M. T., Arnold, Gabriele, Schmitt, B., Quirico, E., Taylor, F.W., and Kappel, David

Subjects
Asteroiden und Kometen, 67P, composition, Leitungsbereich PF, Rosetta, VIRTIS
Abstract

In the period August 2014 - early May 2015 the heliocentric distance of the nucleus of 67P/CG decreased from 3.62 to 1.71 AU and the subsolar point moved towards the southern hemisphere. We investigated the IR spectra obtained by the Rosetta/VIRTIS instrument close to the newly illuminated regions, where colder conditions were present and consequently higher chances to observe highly volatility ices than water. We report about the discovery of CO2 ice identified in a region of the nucleus that recently passed through terminator. The quantitative abundance has been determined by means of spectral modeling of H2O-CO2 icy grains mixed to dark terrains as done in Filacchione et al., Nature, 10.1038/nature16190. The CO2 ice has been identified in an area in Anhur with abundance reaching up to 1.6% mixed with dark terrain. It is interesting to note that CO2 ice has been observed only for a short transient period of time, possibly demonstrating the seasonal nature of the presence of CO2 at the surface. A parallel study on the water and carbon dioxide gaseous emissions in the coma above this volatile-rich area is reported by Migliorini et al., this conference.

Published
2016

26. Composition of comet 67P/Churyumov-Gerasimenko refractory crust as inferred from VIRTIS-Spectro-Imager

Author

Quirico, E., Moroz, L.V., Beck, P., Schmitt, B., Arnold, Gabriele, Bonal, L., Capaccioni, F., Filacchione, G., Erard, S., Leyrat, C., Bockelee-Morvan, D., Tosi, F., Ciarnello, M., Raponi, A., Capria, M. T., De Sanctis, M.C., Piccioni, G., Barucci, Antonella, Drossart, P., and Markus, Kathrin

Subjects
67P, composition, Leitungsbereich PF, Rosetta, food and beverages, VIRTIS
Abstract

We report the interpretation of VIRTIS/ROSETTA spectra of comet 67P/CG, based on laboratory data collected on meteorites and series of analogs. We show that the crust is composed by a macromolecular carbonaceous material, mixed with minerals and likely more volatile molecules and possibly ammonium salts.

Published
2015

27. Spectral modeling in the VNIR range of 67P/Churyumov-Gerasimenko nucleus from VIRTIS-M onboard Rosetta

Author

Raponi, A., Ciarnello, M., Capaccioni, F., Filacchione, G., De Sanctis, M.C., Erard, S., Leyrat, C., Bockelee-Morvan, D., Tosi, F., Capria, M. T., Piccioni, G., Palomba, E., Longobardo, A, Drossart, P., Quirico, E., Beck, P., Schmitt, B., Barucci, Antonella, Arnold, Gabriele, and Blecka, M.

Subjects
67P, Rosetta, Leitungsbereich PF, spectral modeling, Astrophysics::Earth and Planetary Astrophysics, VIRTIS
Abstract

Topic of this work is the analysis of the surface composition of comet 67P/Churyumov-Gerasimenko using the data obtained by the VIRTIS instrument onboard the Rosetta spacecraft. We have focused on the VNIR spectral range (0.4 - 2.5 μm) which presents a nearly flat spectrum with quite uniform spectral slopes across the entire comet surface. In this work we report about the spectral modeling of CG VIS-IR spectra by means of Hapke’s radiative transfer model.

Published
2015

28. Compositional maps of 67P/CG nucleus after perihelion passage by VIRTIS-M aboard Rosetta

Author

Filacchione, G., Capaccioni, F., Ciarnello, M., Tosi, F., De Sanctis, M.C., Raponi, A., Erard, S., Bockelee-Morvan, D., Leyrat, C., Arnold, Gabriele, Schmitt, B., Quirico, E., Piccioni, G., Migliorini, A., Cerroni, P., Palomba, E., Bellucci, G., Longobardo, A, Jaumann, R., Stephan, K., Barucci, Antonella, Fornasier, S., McCord, Thomas B., Carlson, R. W., Ammannito, E., Despan, D., Blecka, M., Moroz, L.V., Mottola, S., Mennella, V., Beck, P., Bonal, L., Fonti, S., Orofino, V., Merlin, F., Markus, Kathrin, Noschese, R., Cartacci, M., Cicchetti, A., Politi, R., Henry, Florence, and Jacquinod, S.

Subjects
Asteroiden und Kometen, Planetengeologie, 67P, composition, Rosetta, Leitungsbereich PF, VIRTIS
Abstract

Comet 67P/Churyumov-Gerasimenko undergoes periherm transit at 1.2 AU in August 2015. During this passage the illumination conditions above the south hemisphere of the nucleus rapidly improve becoming optimal for the retrieval of the surface properties by VIRTIS-M onboard Rosetta. A similar mapping of the surface at about 12.5 m/pixel and at solar phases below 40 deg has been already performed during the Philae prelanding phase (August-September 2014, heliocentric distance 3.6 AU) allowing us to build compositional maps of the entire north hemisphere and equatorial regions down to latitudes -50 deg on a limited part of the Hapi, or the comet’s neck, region. One year after this first mapping campaign the illumination geometry becomes favorable to complete the coverage above the South polar region. Since comet’s activity is rapidly increasing and the Rosetta spacecraft cannot orbit on low trajectories like during the prelanding phase, the south hemisphere maps shall be reasonably observed by VIRTIS-M with a spatial resolution of about 25 m/pixel. Global scale data have shown that the nucleus’ double-lobe surface is characterized by morphologically different units uniformly covered by a very dark, low-albedo, dehydrated organic-rich material. Compositional properties across the different regions of the nucleus are mapped by measuring visible and infrared spectral slopes, calculated on the best linear fit to the reflectance spectra between 0.5-0.8 μm and 1-2.5 μm, respectively. As pre-landing data have clearly shown, spectral slopes are highly diagnostic to identify active areas, like in the Hapi area, and exposed water ice deposits where the spectra appear less red. As heliocentric distance decreases and diurnal temperatures increase, the 3-5 μm spectral range becomes affected by thermal emission from the surface. This emission is overlapping with the 3 μm feature previously observed by VIRTIS during the pre-landing period making more difficult to retrieve the distribution of the organic material. A summary of the spectral characteristics observed on the south hemisphere region during the perihelion passage is given. Activity-driven spectral changes observed before and after perihelion passage on some specific areas of the surface are discussed.

Published
2015

29. The nucleus and coma of 67P/Churyumov-Gerasimenko: highlights of the Rosetta-VIRTIS results

Author

Capaccioni, F., Filacchione, G., Erard, S., Arnold, Gabriele, Bockelee-Morvan, D., De Sanctis, M.C., Leyrat, C., Tosi, F., Schmitt, B., Quirico, E., Capria, M. T., Ciarnello, M., Raponi, A., Kührt, E., Piccioni, G., Palomba, E., Drossart, P., Cerroni, P., McCord, Thomas B., and Barucci, Antonella

Subjects
67P, Leitungsbereich PF, Rosetta, VIRTIS
Abstract

This paper will describe the major results obtained so far during the prelanding and initial escort phases (July 2014–February 2015) by the VIRTIS (Visible, Infrared and Thermal Imaging Spectrometer) dual channel spectrometer onboard Rosetta. The scientific goals of the VIRTIS instrument are related to the study of the nucleus surface composition and of its temperature and to the study of the gaseous and dust components of the coma. These are achieved by studying the reflected and emitted radiance of the comet in the spectral range 0.25-5.0 μm with a Mapping Spectrometer (VIRTIS-M) and a High Resolution Spectrometer (VIRTIS-H). The nucleus observations were performed with spatial resolution varying from the initial 500m down to 2.5m and have generated compositional maps of the illuminated areas. The nucleus integrated normal albedo has been calculated as 0.060 ± 0.003 at 0.55 μm, and reflectance spectra display distinct gradients in the VIS and IR regions (5-25 and 1.5-5 % kÅ-1 respectively). These results suggest a surface made of an association of carbon bearing species and opaque minerals such as sulfides. In addition a broad absorption feature in the 2.9-3.6μm range has been observed; this band is present across the entire illuminated surface and, its shape and width are compatible with absorptions due to non-volatile organic macromolecular materials, complex mixture of various types of C-H and/or O-H chemical groups. Ice rich regions of very limited extent, have also been observed. The surface temperature has been measured since the first distant observations of the nucleus in thermal emission. The highest surface temperature seen so far is 220K, which is an indication of a surface structure largely covered by a porous crust, mainly devoid of water ice. Water vapour and carbon dioxide molecules have been observed in the coma and their variability, as a function of altitude and geographic location has been studied. The molecules display an anti-correlated behaviour in their spatial distribution, which could suggest either intrinsic differences in the nucleus composition or insolation induced variability, which most probably will imply seasonal changes.

Published
2015

30. Composition of comet 67P/Churyumov-Gerasimenko refractory crust as inferred from VIRTIS-M/Rosetta Spectro-Imager

Author

Quirico, E., Moroz, L.V., Beck, P., Schmitt, B., Arnold, Gabriele, Bonal, L., Filacchione, G., Capaccioni, F., Leyrat, C., Bockelee-Morvan, D., Erard, S., Tosi, F., Ciarnello, M., Raponi, A., Capria, M. T., De Sanctis, M.C., Piccioni, G., Barucci, Antonella, Drossart, P., and Markus, Kathrin

Subjects
67P, composition, Leitungsbereich PF, Rosetta, VIRTIS
Abstract

VIRTIS reflectance spectra of comet 67P/CG point to the presence of a crust composed of refractory compounds as 1) polyaromatic organic solids mixed with 2) sulfides and Fe-Ni alloys. The presence of sulfides may also account for the red visible slope. The presence of OH chemical groups is inferred from the broad 3.2 μm band. Contributions from aliphatic or aromatic C-H groups is possible, as well as a contribution from salts (NH4+, possibly structural H2O). Salts are expected as minor constituents due to the very low reflectance of the comet surface, but the large absorption coefficient of ions may make their spectral contribution significant. Analysis from other instruments aboard ROSETTA orbiter and PHILAE lander will help constrain further the contribution of minor species.

Published
2015

31. Compositional maps of 67P/CG by Rosetta/VIRTIS-M

Author

Filacchione, G., Capaccioni, F., Tosi, F., Erard, S., De Sanctis, M.C., Ciarnello, M., Raponi, A., Palomba, E., Capria, M. T., Piccioni, G., Leyrat, C., Bockelee-Morvan, D., Drossart, P., Arnold, Gabriele, Jaumann, R., Barucci, Antonella, Ip, W-H., McCord, Thomas B., Schmitt, B., Quirico, E., Beck, P., Longobardo, A, Noschese, R., Cartacci, M., Cicchetti, A., Politi, R., Henry, Florence, and Jacquinod, S.

Subjects
Planetengeologie, 67P, composition, Rosetta, Leitungsbereich PF, VIRTIS
Abstract

The Visible InfraRed Thermal Imaging Spectrometer, VIRTIS onboard ESA’s Rosetta mission has completed two extensive mapping campaigns of the 67P/Churyumov-Gerasimenko comet nucleus in August-September 2014. After calibration and geometrical projection on nucleus shape model, VIRTIS data were processed to retrieve the distribution of several spectral indicators (spectral slopes, organic material band depths) from which compositional maps are built. Apart from being appropriate to map surface composition, those indicators allow us to correlate them with local morphological features (patches, boulders, scarps, terraces, active areas) and thermal properties.

Published
2015

32. The global surface composition of 67P/CG nucleus by Rosetta/VIRTIS. (I) Prelanding mission phase

Author

Filacchione, Gianrico, primary, Capaccioni, Fabrizio, additional, Ciarniello, Mauro, additional, Raponi, Andrea, additional, Tosi, Federico, additional, De Sanctis, Maria Cristina, additional, Erard, Stéphane, additional, Morvan, Dominique Bockelée, additional, Leyrat, Cedric, additional, Arnold, Gabriele, additional, Schmitt, Bernard, additional, Quirico, Eric, additional, Piccioni, Giuseppe, additional, Migliorini, Alessandra, additional, Capria, Maria Teresa, additional, Palomba, Ernesto, additional, Cerroni, Priscilla, additional, Longobardo, Andrea, additional, Barucci, Antonella, additional, Fornasier, Sonia, additional, Carlson, Robert W., additional, Jaumann, Ralf, additional, Stephan, Katrin, additional, Moroz, Lyuba V., additional, Kappel, David, additional, Rousseau, Batiste, additional, Fonti, Sergio, additional, Mancarella, Francesca, additional, Despan, Daniela, additional, and Faure, Mathilde, additional

Published
2016
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33. Comet 67P/Churyumov-Gerasimenko: First science results by Rosetta/OSIRIS

Author

Thomas, Nicolas, Sierks, Holger, Barbieri, Cesare, Lamy, Philippe, Rodrigo, Rafael, Koschny, Detlef, Rickman, Hans, Agarwal, Jessica, A Hearn, Michael, Angrilli, Francesco, Barucci, Antonella, Bertaux, Jean-Loup, Bertini, Ivano, Besse, Sebastien, Bodewits, Dennis, Capanna, Claire, Cremonese, Gabriele, Da Deppo, Vania, Davidsson, Björn, Debei, Stefano, Cecco, Mariolino, Ferri, Francesca, Fornasier, Sonia, marco fulle, Gaskell, Robert, Groussin, Olivier, Güttler, Carsten, Gutierrez, Pedroj, Hviid, Stubbe, Ip, Wing-Huen, Jorda, Laurent, Keller, Horst Uwe, Knollenberg, Jörg, Kramm, Rainer, Kührt, Ekkehard, Küppers, Michael, Laforgia, Fiorangela, Lara, Luisa, Lazzarin, Monica, Leyrat, Cedric, Lopez Moreno, Jose Juan, Lowry, Stephen, Magrin, Sara, Marchi, Simone, Marzari, Francesco, Michalik, Harald, Mottola, Stefano, Naletto, Giampiero, Oklay, Nilda, Pajola, Maurizio, Sabau, Lola, Snodgrass, Colin, Tubiana, Cecilia, Vincent, Jean-Baptiste, and Wenzel, Peter

Abstract

ESA's Rosetta mission arrived on August 6, 2014, at target comet 67P/Churyumov-Gerasimenko after 10 years of cruise. OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) is the scientific imaging system onboard Rosetta. It comprises a Narrow Angle Camera (NAC) for nucleus surface and dust studies and a Wide Angle Camera (WAC) for the wide field coma investigations.We present the first science results achieved by OSIRIS from the arrival at the comet throughout the mapping phase. The overview will cover surface morphology and activity of the nucleus as seen in gas, dust, and local jets.AcknowledgementsOSIRIS was built by a consortium led by the Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany, in collaboration with CISAS, University of Padova, Italy, the Laboratoire d'Astrophysique de Marseille, France, the Instituto de Astrofísica de Andalucia, CSIC, Granada, Spain, the Scientific Support Office of the European Space Agency, Noordwijk, The Netherlands, the Instituto Nacional de Técnica Aeroespacial, Madrid, Spain, the Universidad Politéchnica de Madrid, Spain, the Department of Physics and Astronomy of Uppsala University, Sweden, and the Institut für Datentechnik und Kommunikationsnetze der Technischen Universität Braunschweig, Germany. The support of the national funding agencies of Germany (DLR), France (CNES), Italy (ASI), Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is gratefully acknowledged. We thank the Rosetta Science Ground Segment at ESAC, the Rosetta Mission Operations Centre at ESOC and the Rosetta Project at ESTEC for their outstanding work enabling the science return of the Rosetta Mission.

Published
2014

35. TNOs are Cool: A Survey of the Trans-Neptunian Region

Author

Mommert, Michael, Müller, Thomas, Böhnhardt, Hermann, Lellouch, Emmanuel, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René D., Fornasier, Sonia, Groussin, Olivier, Guilbert, Aurelie, Gutiérrez Buenestado, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Henry, Florence, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, Lara López, Luisa M., Lim, Tanya, Mueller, Michael, Moreno, Raphael, Ortiz Moreno, Jose Luis, Pal, Andras, Protopapa, Silvia, Rengel, Miriam, Santos Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, Trilling, David, Vilenius, Esa, and Szalai, Nikolett

Subjects
thermal modeling, Herschel, TNO, thermophysical modeling
Published
2011

36. Large heterogeneities in comet 67P as revealed by active pits from sinkhole collapse

Author

Vincent, Jean-Baptiste, Bodewits, Dennis, Besse, Sébastien, Sierks, Holger, Barbieri, Cesare, Lamy, Philippe, Rodrigo, Rafael, Koschny, Detlef, Rickman, Hans, Keller, Horst Uwe, Agarwal, Jessica, A'Hearn, Michael F., Auger, Anne Thérese, Barucci, Antonella, Bertaux, Jean-Loup, Bertini, Ivano, Capanna, Claire, Cremonese, Gabriele, Da Deppo, Vania, Davidson, Björn, Debei, Stefano, De Cecco, Mariolino, El-Maarry, Mohamed Ramy, Ferri, Francesca, Fornasier, Sonia, Fulle, Marco, Gaskell, Robert, Giacomini, Lorenza, Giacomini, Olivier, Guilbert-Lepoutre, Aurélie, Gutierrez-Marques, P., Gutiérrez, Pedro J., Güttler, Caster, Hoekzem, Nick, Höfner, Sebastian, Hviid, Stubbe F., Ip, Wing-Huen, Jorda, Laurent, Knollenberg, Jörg, Kovacs, Gabor, Kramm, Rainer, Kührt, Ekkehard, Küppers, Michael, La Forgia, Fiona, Lara, Luisa M., Lazzarin, Monica, Lee, Vicky, Leyrat, Cédric, Lin, Zhong-Yi, Moreno, Josè J. Lopez, Lowry, S.C., Magrin, Sara, Maquet, Lucie, Marchi, Simone, Marzari, Francesco, Massironi, Matteo, Michalik, Harald, Moissl, Richard, Mottola, Stefano, Naletto, Giampiero, Oklay, Nilda, Pajola, Maurizio, Preusjer, Frank, Scholten, Frank, Thomas, Nicolas, Toth, Imre, Tubiana, Cecilia, Vincent, Jean-Baptiste, Bodewits, Dennis, Besse, Sébastien, Sierks, Holger, Barbieri, Cesare, Lamy, Philippe, Rodrigo, Rafael, Koschny, Detlef, Rickman, Hans, Keller, Horst Uwe, Agarwal, Jessica, A'Hearn, Michael F., Auger, Anne Thérese, Barucci, Antonella, Bertaux, Jean-Loup, Bertini, Ivano, Capanna, Claire, Cremonese, Gabriele, Da Deppo, Vania, Davidson, Björn, Debei, Stefano, De Cecco, Mariolino, El-Maarry, Mohamed Ramy, Ferri, Francesca, Fornasier, Sonia, Fulle, Marco, Gaskell, Robert, Giacomini, Lorenza, Giacomini, Olivier, Guilbert-Lepoutre, Aurélie, Gutierrez-Marques, P., Gutiérrez, Pedro J., Güttler, Caster, Hoekzem, Nick, Höfner, Sebastian, Hviid, Stubbe F., Ip, Wing-Huen, Jorda, Laurent, Knollenberg, Jörg, Kovacs, Gabor, Kramm, Rainer, Kührt, Ekkehard, Küppers, Michael, La Forgia, Fiona, Lara, Luisa M., Lazzarin, Monica, Lee, Vicky, Leyrat, Cédric, Lin, Zhong-Yi, Moreno, Josè J. Lopez, Lowry, S.C., Magrin, Sara, Maquet, Lucie, Marchi, Simone, Marzari, Francesco, Massironi, Matteo, Michalik, Harald, Moissl, Richard, Mottola, Stefano, Naletto, Giampiero, Oklay, Nilda, Pajola, Maurizio, Preusjer, Frank, Scholten, Frank, Thomas, Nicolas, Toth, Imre, and Tubiana, Cecilia

Abstract

Pits have been observed on many cometary nuclei mapped by spacecraft. It has been argued that cometary pits are a signature of endogenic activity, rather than impact craters such as those on planetary and asteroid surfaces. Impact experiments and models cannot reproduce the shapes of most of the observed cometary pits, and the predicted collision rates imply that few of the pits are related to impacts. Alternative mechanisms like explosive activity have been suggested, but the driving process remains unknown. Here we report that pits on comet 67P/Churyumov–Gerasimenko are active, and probably created by a sinkhole process, possibly accompanied by outbursts. We argue that after formation, pits expand slowly in diameter, owing to sublimation-driven retreat of the walls. Therefore, pits characterize how eroded the surface is: a fresh come- tary surface will have a ragged structure with many pits, while an evolved surface will look smoother. The size and spatial distribution of pits imply that large heterogeneities exist in the physical, structural or compositional properties of the first few hundred metres below the current nucleus surface.

Published
2015

37. TNOs are Cool: A Survey of the Trans-Neptunian Region: Radiometric properties of Trans-Neptunian Objects

Author

Mommert, Michael, Müller, Thomas, Böhnhardt, Hermann, Lellouch, Emmanuel, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René D., Fornasier, Sonia, Groussin, Olivier, Guilbert, Aurelie, Gutiérrez Buenestado, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Henry, Florence, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, Lara López, Luisa M., Lim, Tanya, Mueller, Michael, Moreno, Raphael, Ortiz Moreno, Jose Luis, Pal, Andras, Protopapa, Silvia, Rengel, Miriam, Santos Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, Trilling, David, and Vilenius, Esa

Subjects
Asteroiden und Kometen, thermal modeling, Herschel, TNO, thermophysical modeling
Abstract

The "TNOs are Cool: A Survey of the Trans-Neptunian Region" project is a Herschel Open Time Key Program awarded some 370 h of Herschel observing time. The observations include PACS and SPIRE point-source photometry on about 140 trans-Neptunian objects with known orbits. The goal is to characterize the individual objects and the full sample using radiometric techniques, in order to probe formation and evolution processes in the Solar System and to establish a benchmark for understanding the Solar System debris disk as well as extra-solar ones. We present results on a set of TNOs which were selected for the Science Demonstration and early mission phases and report on progress in deriving effective sizes, geometric albedos, and thermal characteristics. Our early sample also includes binary objects for which density estimates can be made on the basis of the derived diameters. TNO densities can provide insight into Solar-System formation scenarios.

Published
2010

38. TNO Modelling Aspects and First Radiometric Results from the ’TNOs are Cool’ Project

Author

Mommert, Michael, Müller, Thomas, Böhnhardt, Hermann, Lellouch, Emmanuel, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René D., Fornasier, Sonia, Groussin, Olivier, Guilbert, Aurelie, Gutiérrez Buenestado, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Henry, Florence, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, Lara López, Luisa M., Lim, Tanya, Mueller, Michael, Moreno, Raphael, Ortiz Moreno, Jose Luis, Pal, Andras, Protopapa, Silvia, Rengel, Miriam, Santos Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, Trilling, David, and Vilenius, Esa

Subjects
Asteroiden und Kometen, thermal modeling, Herschel, TNO, thermophysical modeling
Abstract

The "TNOs are Cool: A Survey of the Trans-Neptunian Region" project is a Herschel Open Time Key Program awarded some 370 h of Herschel observing time. The observations include PACS and SPIRE point-source photometry on about 140 trans-Neptunian objects with known orbits. The goal is to characterize the individual objects and the full sample using radiometric techniques, in order to probe formation and evolution processes in the Solar System and to establish a benchmark for understanding the Solar System debris disk as well as extra-solar ones. We present results on a set of TNOs which were selected for the Science Demonstration and early mission phases and report on progress in deriving effective sizes, geometric albedos, thermal characteristics, and our different approaches using thermal and thermophysical models.

Published
2010

39. Consert for Asteroid - radar tomography of Near Earth Asteroid

Author

Herique, Alain, Plettemeier, Dirk, Kofman, Wlodek, Ulamec, Stephan, Biele, Jens, Goutail, Jean-Pierre, Beck, Pierre, Lassue, Jérémie, Barucci, Antonella, Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Technische Universität Dresden = Dresden University of Technology (TU Dresden), DLR Microgravity User Support Center (MUSC), Deutsches Zentrum für Luft- und Raumfahrt (DLR), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

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

International audience; Consert for Asteroid is a radar to instrument the Mascot lander, which is proposed in the frame of future Near Earth Asteroid missions. This low frequency radar is a unique opportunity to sound the internal structure of the target. Its objective is to achieve the tomography both in transmission and in reflexion of the asteroid in order to determine its fracturing, its stratigraphy and its heterogeneity at different scales, for a better understanding of accretion and evolution phenomena. This talk reviews all the aspects of the proposed experiment. The problematics of the NEA is reviewed in order to demonstrate the interest of low frequency radar sounding. A consert-like bistatic experiment solution is proposed to fulfil the low mass budget constraints. The concept of this tomography between the lander and the orbiter is detailed, including its different operation modes, the measurements, the inversions and the addressed NEA issues. In the second part, we present the preliminary design of our instrument. This review starts from the existing Consert instrument on board the Rosetta and Philae probes. The main instrument trade offs are presented from the mission characteristics and the proposed target. The electronics are revisited and the budgets are updated. So some antenna designs are proposed for both lander and orbiter spacecrafts. Finally, a preliminary experiment budget is shown.

Published
2010

40. The Marco Polo mission: a sample return from a low-albedo Near Earth Object in the ESA Cosmic Vision Program 2015-2025

Author

Michel, Patrick, Barucci, Antonella, Yoshikawa, Makoto, Koschny, Detlef, Boenhardt, Hermann, Brucato, John Robert, Coradini, Marcello, Dotto, Elisabetta, Franchi, Ian, Green, Simon F., Josset, Jean-Luc, Kawaguchi, Junichiro, Muinonen, Karri, Oberst, Jürgen, Yano, Hajime, Binzel, Rick, Agnolon, David, and Romstedt, Jens

Abstract

Marco Polo is a sample return mission to a Near-Earth Object (NEO) which was originally proposed as a joint European-Japanese mission for the scientific program Cosmic Vision 2015-2025 of the European Space Agency (ESA) in June 2007 and selected for an assessment study until fall 2009. The main goal of this mission is to return a sample from a dark taxonomic type (low albedo) NEO for detailed laboratory analysis in order to answer questions related to planetary formation, evolution and the origin of Life. In addition, it will provide detailed information on the physical and chemical properties of a body belonging to the population of potential Earth impactors, and therefore it is also directly relevant to the problems of risk assessment and mitigation. We review basic information on NEOs, potential targets for a sample return mission and the Marco Polo mission, with emphasis on their relevance to impact risk assessment and mitigation. More details on the Marco Polo mission and scientific objectives can be found in [1].

Published
2009

41. ESSC-ESF Position Paper: Science-Driven Scenario for Space Exploration: Report from the European Space Sciences Committee (ESSC)

Author

Worms, Jean-Claude, Lammer, Helmut, Barucci, Antonella, Beebe, Reta, Bibring, Jean-Pierre, Blamont, Jacques, Blanc, Michel, Bonnet, Roger, Brucato, John R, Chassefière, Eric, Coradini, Angioletta, Crawford, Ian, Ehrenfreund, Pascale, Falcke, Heino, Gerzer, Rupert, Grady, Monica, Grande, Manuel, Haerendel, Gerhard, Horneck, Gerda, Koch, Bernhard, Lobanov, Andreï, Lopez-Moreno, José J, Marco, Roberto, Norsk, Peter, Rothery, Dave, Swings, Jean-Pierre, Tropea, Cam, Ulamec, Stephan, Westall, Frances, Zarnecki, John, Worms, Jean-Claude, Lammer, Helmut, Barucci, Antonella, Beebe, Reta, Bibring, Jean-Pierre, Blamont, Jacques, Blanc, Michel, Bonnet, Roger, Brucato, John R, Chassefière, Eric, Coradini, Angioletta, Crawford, Ian, Ehrenfreund, Pascale, Falcke, Heino, Gerzer, Rupert, Grady, Monica, Grande, Manuel, Haerendel, Gerhard, Horneck, Gerda, Koch, Bernhard, Lobanov, Andreï, Lopez-Moreno, José J, Marco, Roberto, Norsk, Peter, Rothery, Dave, Swings, Jean-Pierre, Tropea, Cam, Ulamec, Stephan, Westall, Frances, and Zarnecki, John

Abstract

Udgivelsesdato: 2009-Feb-9, In 2005 the then ESA Directorate for Human Spaceflight, Microgravity and Exploration (D-HME) commissioned a study from the European Science Foundation's (ESF) European Space Sciences Committee (ESSC) to examine the science aspects of the Aurora Programme in preparation for the December 2005 Ministerial Conference of ESA Member States, held in Berlin. A first interim report was presented to ESA at the second stakeholders meeting on 30 and 31 May 2005. A second draft report was made available at the time of the final science stakeholders meeting on 16 September 2005 in order for ESA to use its recommendations to prepare the Executive proposal to the Ministerial Conference. The final ESSC report on that activity came a few months after the Ministerial Conference (June 2006) and attempted to capture some elements of the new situation after Berlin, and in the context of the reduction in NASA's budget that was taking place at that time; e.g., the postponement sine die of the Mars Sample Return mission. At the time of this study, ESSC made it clear to ESA that the timeline imposed prior to the Berlin Conference had not allowed for a proper consultation of the relevant science community and that this should be corrected in the near future. In response to that recommendation, ESSC was asked again in the summer of 2006 to initiate a broad consultation to define a science-driven scenario for the Aurora Programme. This exercise ran between October 2006 and May 2007. ESA provided the funding for staff support, publication costs, and costs related to meetings of a Steering Group, two meetings of a larger ad hoc group (7 and 8 December 2006 and 8 February 2007), and a final scientific workshop on 15 and 16 May 2007 in Athens. As a result of these meetings a draft report was produced and examined by the Ad Hoc Group. Following their endorsement of the report and its approval by the plenary meeting of the ESSC, the draft report was externally refereed, as is now normal prac

Published
2009

42. Marco Polo – A Mission to Return a Sample from a Near-Earth Object – Science Requirements and Operational Scenarios

Author

KOSCHNY, Detlef, primary, BARUCCI, Antonella, additional, YOSHIKAWA, Makoto, additional, BÖHNHARDT, Hermann, additional, BRUCATO, John, additional, CORADINI, Marcello, additional, DOTTO, Elisabetta, additional, FRANCHI, Ian, additional, F. GREEN, Simon, additional, JOSSET, Jean-Luc, additional, KAWAGUCHI, Junichiro, additional, MICHEL, Patrick, additional, MUINONEN, Karri, additional, OBERST, Jürgen, additional, YANO, Hajime, additional, BINZEL, Richard, additional, AGNOLON, David, additional, and ROMSTEDT, Jens, additional

Published
2010
Full Text
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43. ESSC-ESF Position Paper—Science-Driven Scenario for Space Exploration: Report from the European Space Sciences Committee (ESSC)

Author

Worms, Jean-Claude, primary, Lammer, Helmut, additional, Barucci, Antonella, additional, Beebe, Reta, additional, Bibring, Jean-Pierre, additional, Blamont, Jacques, additional, Blanc, Michel, additional, Bonnet, Roger, additional, Brucato, John R., additional, Chassefière, Eric, additional, Coradini, Angioletta, additional, Crawford, Ian, additional, Ehrenfreund, Pascale, additional, Falcke, Heino, additional, Gerzer, Rupert, additional, Grady, Monica, additional, Grande, Manuel, additional, Haerendel, Gerhard, additional, Horneck, Gerda, additional, Koch, Bernhard, additional, Lobanov, Andreï, additional, Lopez-Moreno, José J., additional, Marco, Roberto, additional, Norsk, Peter, additional, Rothery, Dave, additional, Swings, Jean-Pierre, additional, Tropea, Cam, additional, Ulamec, Stephan, additional, Westall, Frances, additional, and Zarnecki, John, additional

Published
2009
Full Text
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44. Coordinated observations of asteroids 1219 Britta and 1972 Yi Xing

Author

Binzel, Richard P, Cochran, Anita L, Barker, Edwin S, Tholen, David J, and Barucci, Antonella

Subjects
Astronomy
Abstract

A coordinated observational program conducted for asteroids 1219 Britta and 1972 Yi Xing has yielded a sidereal rotation period of 5.57497 + or - 0.00013 h for the former, which has retrograde rotation and may be classified as an S-type asteroid on the basis of its spectra and albedo. The 1972 Yi Xing synodic period is found to be 14.183 + or - 0.003 h, with an observed light-curve amplitude amplitude of 0.18 mag; its five-color measurements also appear consistent with an S-type classification. A light-curve maximum absolute magnitude of 13.32 + or - 0.01 is also obtained.

Published
1987
Full Text
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46. TNOs are Cool: A Survey of the Trans-Neptunian Region: Radiometric properties of Trans-Neptunian Objects

Author

Mommert, Michael, Müller, G., Bühnhardt, Hermann, Lellouch, Emmanuel, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Dores-Soundiram, Alain, Dotto, Elisabetta, Duffard, René, Fornasier, Sonia, Groussin, Olivier, Gutiérrez Buenestado, Pedro, Hainaut, Olivier, Harris, Alan, Hartogh, Paul, Henry, Florence, Daniel HESTROFFER, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, López, Luisa Lara, Lim, Tanya, Müller, Michael, Moreno, Raphael, Ortiz Moreno, Jose Luis, Protopapa, Silvia, Rengel, Miriam, Santos Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, Trilling, David, Astronomy, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-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 Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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, and 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)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The "TNOs are Cool: A Survey of the Trans-Neptunian Region" project is a Herschel Open Time Key Program awarded some 370 h of Herschel observing time. The observations include PACS and SPIRE point-source photometry on about 140 trans-Neptunian objects with known orbits. The goal is to characterize the individual objects and the full sample using radiometric techniques, in order to probe formation and evolution processes in the Solar System and to establish a benchmark for understanding the Solar System debris disk as well as extra-solar ones. We present results on a set of TNOs which were selected for the Science Demonstration and early mission phases and report on progress in deriving effective sizes, geometric albedos, and thermal characteristics. Our early sample also includes binary objects for which density estimates can be made on the basis of the derived diameters. TNO densities can provide insight into Solar-System formation scenarios.

47. TNOs are cool: a survey of the transneptunian region

Author

Müller, Thomas G., Lellouch, Emmanuel, Böhnhardt, Hermann, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René, Fornasier, Sonia, Groussin, Olivier, Gutiérrez, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, Lara, Luisa, Lim, Tanya, Mueller, Michael, Moreno, Raphael, Ortiz, Jose-Luis, Rengel, Miriam, Santos-Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, Trilling, David, Müller, Thomas G., Lellouch, Emmanuel, Böhnhardt, Hermann, Stansberry, John, Barucci, Antonella, Crovisier, Jacques, Delsanti, Audrey, Doressoundiram, Alain, Dotto, Elisabetta, Duffard, René, Fornasier, Sonia, Groussin, Olivier, Gutiérrez, Pedro J., Hainaut, Olivier, Harris, Alan W., Hartogh, Paul, Hestroffer, Daniel, Horner, Jonathan, Jewitt, Dave, Kidger, Mark, Kiss, Csaba, Lacerda, Pedro, Lara, Luisa, Lim, Tanya, Mueller, Michael, Moreno, Raphael, Ortiz, Jose-Luis, Rengel, Miriam, Santos-Sanz, Pablo, Swinyard, Bruce, Thomas, Nicolas, Thirouin, Audrey, and Trilling, David

Abstract

Over one thousand objects have so far been discovered orbiting beyond Neptune. These trans-Neptunian objects (TNOs) represent the primitive remnants of the planetesimal disk from which the planets formed and are perhaps analogous to the unseen dust parent-bodies in debris disks observed around other main-sequence stars. The dynamical and physical properties of these bodies provide unique and important constraints on formation and evolution models of the Solar System. While the dynamical architecture in this region (also known as the Kuiper Belt) is becoming relatively clear, the physical properties of the objects are still largely unexplored. In particular, fundamental parameters such as size, albedo, density and thermal properties are difficult to measure. Measurements of thermal emission, which peaks at far-IR wavelengths, offer the best means available to determine the physical properties. While Spitzer has provided some results, notably revealing a large albedo diversity in this population, the increased sensitivity of Herschel and its superior wavelength coverage should permit profound advances in the field. Within our accepted project we propose to perform radiometric measurements of 139 objects, including 25 known multiple systems. When combined with measurements of the dust population beyond Neptune (e.g. from the New Horizons mission to Pluto), our results will provide a benchmark for understanding the Solar debris disk, and extra-solar ones as well.

48. Marco Polo - a mission to return a sample from a Near-Earth Object - science requirements and operational scenarios

Author

Koschny, Detlef, Barucci, Antonella, Yoshikawa, Makoto, Böhnhardt, Hermann, Brucato, John, Coradini, Marcello, Dotto, Elisabetta, Franchi, Ian, Green, Simon F., Josset, Jean-Luc, Kawaguchi, Junichiro, Michel, Patrick, Muinonen, Karri, Oberst, Jürgen, Yano, Hajime, Binzel, Richard, Agnolon, David, Romstedt, Jens, Koschny, Detlef, Barucci, Antonella, Yoshikawa, Makoto, Böhnhardt, Hermann, Brucato, John, Coradini, Marcello, Dotto, Elisabetta, Franchi, Ian, Green, Simon F., Josset, Jean-Luc, Kawaguchi, Junichiro, Michel, Patrick, Muinonen, Karri, Oberst, Jürgen, Yano, Hajime, Binzel, Richard, Agnolon, David, and Romstedt, Jens

Abstract

Marco Polo is a mission to return a sample from a Near-Earth Object of primitive type (class C or D). It is foreseen as a collaborative effort between the Japanese Space Agency (JAXA) and the European Space Agency (ESA). Marco Polo is currently in a Phase-A study. This paper focuses on the scientific requirements provided to the industrial study consortia in Europe as well as the possible mission scenario at the target object in order to achieve the overall mission science objectives. The main scientific reasons for going to a Near-Earth Object are to understand the initial conditions and evolution history of the solar nebula, to understand how major events (e.g. agglomeration, heating) influence the history of planetesimals, whether primitive class objects contain presolar material, what the organics were in primitive materials, how organics could shed light on the origin of molecules necessary for life, and what the role of impacts by NEOs would be in the origin and evolution of life on Earth.

49. The Marco Polo mission: a sample return from a low-albedo Near Earth Object in the ESA Cosmic Vision Program 2015-2025

Author

Michel, Patrick, Barucci, Antonella, Yoshikawa, Makoto, Koschny, Detlef, Boenhardt, Hermann, Brucato, John Robert, Coradini, Marcello, Dotto, Elisabetta, Franchi, Ian, Green, Simon F., Josset, Jean-Luc, Kawaguchi, Junichiro, Muinonen, Karri, Oberst, Jürgen, Yano, Hajime, Binzel, Rick, Agnolon, David, Romstedt, Jens, Michel, Patrick, Barucci, Antonella, Yoshikawa, Makoto, Koschny, Detlef, Boenhardt, Hermann, Brucato, John Robert, Coradini, Marcello, Dotto, Elisabetta, Franchi, Ian, Green, Simon F., Josset, Jean-Luc, Kawaguchi, Junichiro, Muinonen, Karri, Oberst, Jürgen, Yano, Hajime, Binzel, Rick, Agnolon, David, and Romstedt, Jens

Abstract

Marco Polo is a sample return mission to a Near-Earth Object (NEO) which was originally proposed as a joint European-Japanese mission for the scientific program Cosmic Vision 2015-2025 of the European Space Agency (ESA) in June 2007 and selected for an assessment study until fall 2009. The main goal of this mission is to return a sample from a dark taxonomic type (low albedo) NEO for detailed laboratory analysis in order to answer questions related to planetary formation, evolution and the origin of Life. In addition, it will provide detailed information on the physical and chemical properties of a body belonging to the population of potential Earth impactors, and therefore it is also directly relevant to the problems of risk assessment and mitigation. We review basic information on NEOs, potential targets for a sample return mission and the Marco Polo mission, with emphasis on their relevance to impact risk assessment and mitigation. More details on the Marco Polo mission and scientific objectives can be found in [1].

50. The Marco Polo mission: a sample return from a low-albedo Near Earth Object in the ESA Cosmic Vision Program 2015-2025

Author

Michel, Patrick, Barucci, Antonella, Yoshikawa, Makoto, Koschny, Detlef, Boenhardt, Hermann, Brucato, John Robert, Coradini, Marcello, Dotto, Elisabetta, Franchi, Ian, Green, Simon F., Josset, Jean-Luc, Kawaguchi, Junichiro, Muinonen, Karri, Oberst, Jürgen, Yano, Hajime, Binzel, Rick, Agnolon, David, Romstedt, Jens, Michel, Patrick, Barucci, Antonella, Yoshikawa, Makoto, Koschny, Detlef, Boenhardt, Hermann, Brucato, John Robert, Coradini, Marcello, Dotto, Elisabetta, Franchi, Ian, Green, Simon F., Josset, Jean-Luc, Kawaguchi, Junichiro, Muinonen, Karri, Oberst, Jürgen, Yano, Hajime, Binzel, Rick, Agnolon, David, and Romstedt, Jens

Abstract

Marco Polo is a sample return mission to a Near-Earth Object (NEO) which was originally proposed as a joint European-Japanese mission for the scientific program Cosmic Vision 2015-2025 of the European Space Agency (ESA) in June 2007 and selected for an assessment study until fall 2009. The main goal of this mission is to return a sample from a dark taxonomic type (low albedo) NEO for detailed laboratory analysis in order to answer questions related to planetary formation, evolution and the origin of Life. In addition, it will provide detailed information on the physical and chemical properties of a body belonging to the population of potential Earth impactors, and therefore it is also directly relevant to the problems of risk assessment and mitigation. We review basic information on NEOs, potential targets for a sample return mission and the Marco Polo mission, with emphasis on their relevance to impact risk assessment and mitigation. More details on the Marco Polo mission and scientific objectives can be found in [1].

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