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1. New gravity field of comet 67P/C-G based on Rosetta's Doppler and optical data

Author

Laurent-Varin, Julien, James, Théo, Marty, Jean-Charles, Jorda, Laurent, Maistre, Sebastien Le, and Gaskell, Robert

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We provide a new gravity field of Comet 67P-C/G up to degree 4. We detect mass heterogeneity in the comet nucleus. The loss of mass is restimated at 0.28\% of the comet's total mass (3 times larger than previous estimate). Comparison of the gravity field between pre- and post-perihelion allowed us to measure a shift in the comet's center of gravity of 35 m northward, attributed to ice sublimation process.

Published
2024

2. Activity distribution of comet 67P/Churyumov-Gerasimenko from combined measurements of non-gravitational forces and torques

Author

Attree, Nicholas, Jorda, Laurent, Groussin, Olivier, Agarwal, Jessica, Manghi, Riccardo Lasagni, Tortora, Paolo, Zannoni, Marco, and Marschall, Raphael

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Aims. Understanding the activity is vital for deciphering the structure, formation, and evolution of comets. We investigate models of cometary activity by comparing them to the dynamics of 67P/Churyumov-Gerasimenko. Methods. We matched simple thermal models of water activity to the combined Rosetta datasets by fitting to the total outgassing rate and four components of the outgassing induced non-gravitational force and torque, with a final manual adjustment of the model parameters to additionally match the other two torque components. We parametrised the thermal model in terms of a distribution of relative activity over the surface of the comet, and attempted to link this to different terrain types. We also tested a more advanced thermal model based on a pebble structure. Results. We confirm a hemispherical dichotomy and non-linear water outgassing response to insolation. The southern hemisphere of the comet and consolidated terrain show enhanced activity relative to the northern hemisphere and dust-covered, unconsolidated terrain types, especially at perihelion. We further find that the non-gravitational torque is especially sensitive to the activity distribution, and to fit the pole-axis orientation in particular, activity must be concentrated (in excess of the already high activity in the southern hemisphere and consolidated terrain) around the south pole and on the body and neck of the comet over its head. This is the case for both the simple thermal model and the pebble-based model. Overall, our results show that water activity cannot be matched by a simple model of sublimating surface ice driven by the insolation alone, regardless of the surface distribution, and that both local spatial and temporal variations are needed to fit the data., Comment: Accepted for publication in A&A. 13 pages, 22 figures including appendix

Published
2023
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5. The Comet Interceptor Mission

Author

Jones, Geraint H., Snodgrass, Colin, Tubiana, Cecilia, Küppers, Michael, Kawakita, Hideyo, Lara, Luisa M., Agarwal, Jessica, André, Nicolas, Attree, Nicholas, Auster, Uli, Bagnulo, Stefano, Bannister, Michele, Beth, Arnaud, Bowles, Neil, Coates, Andrew, Colangeli, Luigi, Corral van Damme, Carlos, Da Deppo, Vania, De Keyser, Johan, Della Corte, Vincenzo, Edberg, Niklas, El-Maarry, Mohamed Ramy, Faggi, Sara, Fulle, Marco, Funase, Ryu, Galand, Marina, Goetz, Charlotte, Groussin, Olivier, Guilbert-Lepoutre, Aurélie, Henri, Pierre, Kasahara, Satoshi, Kereszturi, Akos, Kidger, Mark, Knight, Matthew, Kokotanekova, Rosita, Kolmasova, Ivana, Kossacki, Konrad, Kührt, Ekkehard, Kwon, Yuna, La Forgia, Fiorangela, Levasseur-Regourd, Anny-Chantal, Lippi, Manuela, Longobardo, Andrea, Marschall, Raphael, Morawski, Marek, Muñoz, Olga, Näsilä, Antti, Nilsson, Hans, Opitom, Cyrielle, Pajusalu, Mihkel, Pommerol, Antoine, Prech, Lubomir, Rando, Nicola, Ratti, Francesco, Rothkaehl, Hanna, Rotundi, Alessandra, Rubin, Martin, Sakatani, Naoya, Sánchez, Joan Pau, Simon Wedlund, Cyril, Stankov, Anamarija, Thomas, Nicolas, Toth, Imre, Villanueva, Geronimo, Vincent, Jean-Baptiste, Volwerk, Martin, Wurz, Peter, Wielders, Arno, Yoshioka, Kazuo, Aleksiejuk, Konrad, Alvarez, Fernando, Amoros, Carine, Aslam, Shahid, Atamaniuk, Barbara, Baran, Jędrzej, Barciński, Tomasz, Beck, Thomas, Behnke, Thomas, Berglund, Martin, Bertini, Ivano, Bieda, Marcin, Binczyk, Piotr, Busch, Martin-Diego, Cacovean, Andrei, Capria, Maria Teresa, Carr, Chris, Castro Marín, José María, Ceriotti, Matteo, Chioetto, Paolo, Chuchra-Konrad, Agata, Cocola, Lorenzo, Colin, Fabrice, Crews, Chiaki, Cripps, Victoria, Cupido, Emanuele, Dassatti, Alberto, Davidsson, Björn J. R., De Roche, Thierry, Deca, Jan, Del Togno, Simone, Dhooghe, Frederik, Donaldson Hanna, Kerri, Eriksson, Anders, Fedorov, Andrey, Fernández-Valenzuela, Estela, Ferretti, Stefano, Floriot, Johan, Frassetto, Fabio, Fredriksson, Jesper, Garnier, Philippe, Gaweł, Dorota, Génot, Vincent, Gerber, Thomas, Glassmeier, Karl-Heinz, Granvik, Mikael, Grison, Benjamin, Gunell, Herbert, Hachemi, Tedjani, Hagen, Christian, Hajra, Rajkumar, Harada, Yuki, Hasiba, Johann, Haslebacher, Nico, Herranz De La Revilla, Miguel Luis, Hestroffer, Daniel, Hewagama, Tilak, Holt, Carrie, Hviid, Stubbe, Iakubivskyi, Iaroslav, Inno, Laura, Irwin, Patrick, Ivanovski, Stavro, Jansky, Jiri, Jernej, Irmgard, Jeszenszky, Harald, Jimenéz, Jaime, Jorda, Laurent, Kama, Mihkel, Kameda, Shingo, Kelley, Michael S. P., Klepacki, Kamil, Kohout, Tomáš, Kojima, Hirotsugu, Kowalski, Tomasz, Kuwabara, Masaki, Ladno, Michal, Laky, Gunter, Lammer, Helmut, Lan, Radek, Lavraud, Benoit, Lazzarin, Monica, Le Duff, Olivier, Lee, Qiu-Mei, Lesniak, Cezary, Lewis, Zoe, Lin, Zhong-Yi, Lister, Tim, Lowry, Stephen, Magnes, Werner, Markkanen, Johannes, Martinez Navajas, Ignacio, Martins, Zita, Matsuoka, Ayako, Matyjasiak, Barbara, Mazelle, Christian, Mazzotta Epifani, Elena, Meier, Mirko, Michaelis, Harald, Micheli, Marco, Migliorini, Alessandra, Millet, Aude-Lyse, Moreno, Fernando, Mottola, Stefano, Moutounaick, Bruno, Muinonen, Karri, Müller, Daniel R., Murakami, Go, Murata, Naofumi, Myszka, Kamil, Nakajima, Shintaro, Nemeth, Zoltan, Nikolajev, Artiom, Nordera, Simone, Ohlsson, Dan, Olesk, Aire, Ottacher, Harald, Ozaki, Naoya, Oziol, Christophe, Patel, Manish, Savio Paul, Aditya, Penttilä, Antti, Pernechele, Claudio, Peterson, Joakim, Petraglio, Enrico, Piccirillo, Alice Maria, Plaschke, Ferdinand, Polak, Szymon, Postberg, Frank, Proosa, Herman, Protopapa, Silvia, Puccio, Walter, Ranvier, Sylvain, Raymond, Sean, Richter, Ingo, Rieder, Martin, Rigamonti, Roberto, Ruiz Rodriguez, Irene, Santolik, Ondrej, Sasaki, Takahiro, Schrödter, Rolf, Shirley, Katherine, Slavinskis, Andris, Sodor, Balint, Soucek, Jan, Stephenson, Peter, Stöckli, Linus, Szewczyk, Paweł, Troznai, Gabor, Uhlir, Ludek, Usami, Naoto, Valavanoglou, Aris, Vaverka, Jakub, Wang, Wei, Wang, Xiao-Dong, Wattieaux, Gaëtan, Wieser, Martin, Wolf, Sebastian, Yano, Hajime, Yoshikawa, Ichiro, Zakharov, Vladimir, Zawistowski, Tomasz, Zuppella, Paola, Rinaldi, Giovanna, and Ji, Hantao

Published
2024
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6. Interstellar comet 2I/Borisov as seen by MUSE: C$_2$, NH$_2$ and red CN detections

Author

Bannister, Michele T., Opitom, Cyrielle, Fitzsimmons, Alan, Moulane, Youssef, Jehin, Emmanuel, Seligman, Darryl, Rousselot, Philippe, Knight, Matthew M., Marsset, Michael, Schwamb, Megan E., Guilbert-Lepoutre, Aurélie, Jorda, Laurent, Vernazza, Pierre, and Benkhaldoun, Zouhair

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the clear detection of C$_2$ and of abundant NH$_2$ in the first prominently active interstellar comet, 2I/Borisov. We observed 2I on three nights in November 2019 at optical wavelengths 4800--9300 \AA with the Multi-Unit Spectroscopic Explorer (MUSE) integral-field spectrograph on the ESO/Very Large Telescope. These data, together with observations close in time from both 0.6-m TRAPPIST telescopes, provide constraints on the production rates of species of gas in 2I's coma. From the MUSE detection on all epochs of several bands of the optical emission of the C$_2$ Swan system, a rich emission spectrum of NH$_2$ with many highly visible bands, and the red (1-0) bandhead of CN, together with violet CN detections by TRAPPIST, we infer production rates of $Q$(C$_2$) = $1.1\times10^{24}$ mol s$^{-1}$, $Q$(NH$_2$) = $4.8\times10^{24}$ mol s$^{-1}$ and $Q$(CN) = $(1.8\pm0.2)\times 10^{24}$ mol s$^{-1}$. In late November at 2.03~au, 2I had a production ratio of C$_2$/CN$=0.61$, only barely carbon-chain depleted, in contrast to earlier reports measured further from the Sun of strong carbon-chain depletion. Thus, 2I has shown evolution in its C$_2$ production rate: a parent molecule reservoir has started sublimating. At $Q$(NH$_2$)/$Q$(CN) = 2.7, this second interstellar object is enriched in NH$_2$, relative to the known Solar System sample., Comment: 5 figures. Submitted to AAS Journals

Published
2020

7. Science objectives of the MMX rover

Author

Ulamec, Stephan, Michel, Patrick, Grott, Matthias, Böttger, Ute, Schröder, Susanne, Hübers, Heinz-Wilhelm, Cho, Yuichiro, Rull, Fernando, Murdoch, Naomi, Vernazza, Pierre, Prieto-Ballesteros, Olga, Biele, Jens, Tardivel, Simon, Arrat, Denis, Hagelschuer, Till, Knollenberg, Jörg, Vivet, Damien, Sunday, Cecily, Jorda, Laurent, Groussin, Olivier, Robin, Colas, and Miyamoto, Hirdy

Published
2023
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8. Development of observation strategies from mission design to operations: illustration with Mars moons Explorer infrared spectrometer (MIRS)

Author

Sawyer, Eric, Barucci, Maria Antonietta, Rocard, Francis, Fornasier, Sonia, Doressoundiram, Alain, Piou, Véronique, Bernardi, Pernelle, Nakamura, Tomoki, Nakagawa, Hiromu, Iwata, Takahiro, Le Du, Michel, Reess, Jean-Michel, Jorda, Laurent, Nicolas, Théret, Pons, Nathalie, Donny, Christophe, Goulet, Sébastien, Jesus Martins Carriço, Inês De, and Canalias, Elisabet

Published
2023
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9. Constraining models of activity on comet 67P/Churyumov-Gerasimenko with Rosetta trajectory, rotation, and water production measurements

Author

Attree, Nicholas, Jorda, Laurent, Groussin, Olivier, Mottola, Stefano, Thomas, Nick, Brouet, Yann, Kührt, Ekkehard, Knapmeyer, Martin, Preusker, Frank, Scholten, Frank, Knollenberg, Jorg, Hviid, Stubbe, Hartogh, Paul, and Rodrigo, Rafael

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Aims. We use four observational data sets, mainly from the Rosetta mission, to constrain the activity pattern of the nucleus of comet 67P/Churyumov-Gerasimenko. Methods. We develop a numerical model that computes the production rate and non-gravitational acceleration of the nucleus of comet 67P as a function of time, taking into account its complex shape with a shape model reconstructed from OSIRIS imagery. We use this model to fit three observational data sets: the trajectory data from flight dynamics; the rotation state, as reconstructed from OSIRIS imagery; and the water production measurements from ROSINA, of 67P. The two key parameters of our model, adjusted to fit the three data sets all together, are the activity pattern and the momentum transfer efficiency (i.e., the so-called "$\eta$ parameter" of the non-gravitational forces). Results. We find an activity pattern able to successfully reproduce the three data sets simultaneously. The fitted activity pattern exhibits two main features: a higher effective active fraction in two southern super-regions ($\sim 10$~\%) outside perihelion compared to the northern ones ($< 4$~\%), and a drastic rise of the effective active fraction of the southern regions ($\sim 25-35$~\%) around perihelion. We interpret the time-varying southern effective active fraction by cyclic formation and removal of a dust mantle in these regions. Our analysis supports moderate values of the momentum transfer coefficient $\eta$ in the range $0.6-0.7$; values $\eta\leq0.5$ or $\eta\geq0.8$ degrade significantly the fit to the three data sets. Our conclusions reinforce the idea that seasonal effects linked to the orientation of the spin axis play a key role in the formation and evolution of dust mantles, and in turn largely control the temporal variations of the gas flux., Comment: 12 pages, 17 figures. Accepted for publication in forthcoming Rosetta issue of Astronomy and Astrophysics

Published
2019
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10. Comet 67P/Churyumov-Gerasimenko rotation changes derived from sublimation induced torques

Author

Kramer, Tobias, Laeuter, Matthias, Hviid, Stubbe, Jorda, Laurent, Keller, Horst Uwe, and Kührt, Ekkehard

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

(Context) The change of the rotation period and the orientation of the rotation axis of comet 67P/Churyumov-Gerasimenko (67P/C-G) is deducible from images taken by the scientific imaging instruments on-board the Rosetta mission with high precision. Non gravitational forces are a natural explanation for these data. (Aims) We describe observed changes for the orientation of the rotation axis and the rotation period of 67P/C-G. For these changes we give an explanation based on a sublimation model with a best-fit for the surface active fraction (model P). Torque effects of periodically changing gas emissions on the surface are considered. (Methods) We solve the equation of state for the angular momentum in the inertial and the body-fixed frames and provide an analytic theory of the rotation changes in terms of Fourier coefficients, generally applicable to periodically forced rigid body dynamics. (Results) The torque induced changes of the rotation state constrain the physical properties of the surface, the sublimation rate and the local active fraction of the surface. (Conclusions) We determine a distribution of the local surface active fraction in agreement with the rotation properties, period and orientation, of 67P/C-G. The torque movement confirms that the sublimation increases faster than the insolation towards perihelion. The derived relatively uniform activity pattern is discussed in terms of related surface features., Comment: 11 pages

Published
2018
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11. The MMX rover: performing in situ surface investigations on Phobos

Author

Michel, Patrick, Ulamec, Stephan, Böttger, Ute, Grott, Matthias, Murdoch, Naomi, Vernazza, Pierre, Sunday, Cecily, Zhang, Yun, Valette, Rudy, Castellani, Romain, Biele, Jens, Tardivel, Simon, Groussin, Olivier, Jorda, Laurent, Knollenberg, Jörg, Grundmann, Jan Thimo, Arrat, Denis, Pont, Gabriel, Mary, Stephane, Grebenstein, Markus, Miyamoto, Hirdy, Nakamura, Tomoki, Wada, Koji, Yoshikawa, Kent, and Kuramoto, Kiyoshi

Published
2022
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13. The Philae lander reveals low-strength primitive ice inside cometary boulders

Author

O’Rourke, Laurence, Heinisch, Philip, Blum, Jürgen, Fornasier, Sonia, Filacchione, Gianrico, Van Hoang, Hong, Ciarniello, Mauro, Raponi, Andrea, Gundlach, Bastian, Blasco, Rafael Andrés, Grieger, Björn, Glassmeier, Karl-Heinz, Küppers, Michael, Rotundi, Alessandra, Groussin, Olivier, Bockelée-Morvan, Dominique, Auster, Hans-Ulrich, Oklay, Nilda, Paar, Gerhard, Perucha, Maria del Pilar Caballo, Kovacs, Gabor, Jorda, Laurent, Vincent, Jean-Baptiste, Capaccioni, Fabrizio, Biver, Nicolas, Parker, Joel Wm., Tubiana, Cecilia, and Sierks, Holger

Published
2020
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14. The violent collisional history of aqueously evolved (2) Pallas

Author

Marsset, Michaël, Brož, Miroslav, Vernazza, Pierre, Drouard, Alexis, Castillo-Rogez, Julie, Hanuš, Josef, Viikinkoski, Matti, Rambaux, Nicolas, Carry, Benoît, Jorda, Laurent, Ševeček, Pavel, Birlan, Mirel, Marchis, Franck, Podlewska-Gaca, Edyta, Asphaug, Erik, Bartczak, Przemyslaw, Berthier, Jérôme, Cipriani, Fabrice, Colas, François, Dudziński, Grzegorz, Dumas, Christophe, Ďurech, Josef, Ferrais, Marin, Fétick, Romain, Fusco, Thierry, Jehin, Emmanuel, Kaasalainen, Mikko, Kryszczynska, Agnieszka, Lamy, Philippe, Le Coroller, Hervé, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Richardson, Derek C., Santana-Ros, Toni, Tanga, Paolo, Vachier, Frédéric, Vigan, Arthur, Witasse, Olivier, and Yang, Bin

Published
2020
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15. MIRS: an imaging spectrometer for the MMX mission

Author

Barucci, Maria Antonietta, Reess, Jean-Michel, Bernardi, Pernelle, Doressoundiram, Alain, Fornasier, Sonia, Le Du, Michel, Iwata, Takahiro, Nakagawa, Hiromu, Nakamura, Tomoki, André, Yves, Aoki, Shohei, Arai, Takehiko, Baldit, Elisa, Beck, Pierre, Buey, Jean-Tristan, Canalias, Elisabet, Castelnau, Matthieu, Charnoz, Sebastien, Chaussidon, Marc, Chapron, Fréderic, Ciarletti, Valerie, Delbo, Marco, Dubois, Bruno, Gauffre, Stephane, Gautier, Thomas, Genda, Hidenori, Hassen-Khodja, Rafik, Hervet, Gilles, Hyodo, Ryuki, Imbert, Christian, Imamura, Takeshi, Jorda, Laurent, Kameda, Shingo, Kouach, Driss, Kouyama, Toru, Kuroda, Takeshi, Kurokawa, Hiroyuki, Lapaw, Laurent, Lasue, Jeremie, Le Deit, Laetitia, Ledot, Aurélien, Leyrat, Cedric, Le Ruyet, Bertrand, Matsuoka, Moe, Merlin, Frederic, Miyamoto, Hideaki, Moynier, Frederic, Nguyen Tuong, Napoleon, Ogohara, Kazunori, Osawa, Takahito, Parisot, Jérôme, Pistre, Laurie, Quertier, Benjamin, Raymond, Sean N., Rocard, Francis, Sakanoi, Takeshi, Sato, Takao M., Sawyer, Eric, Tache, Fériel, Trémolières, Sylvain, Tsuchiya, Fuminori, Vernazza, Pierre, and Zeganadin, Didier

Published
2021
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16. Pulsational analysis of V 588 Mon and V 589 Mon observed with the MOST and CoRoT satellites

Author

Zwintz, Konstanze, Kallinger, Thomas, Guenther, David B., Gruberbauer, Michael, Kuschnig, Rainer, Weiss, Werner W., Auvergne, Michel, Jorda, Laurent, Favata, Fabio, Matthews, Jaymie, and Fischer, Michael

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The two pulsating pre-main sequence (PMS) stars V 588 Mon and V 589 Mon were observed by CoRoT for 23.4 days in March 2008 during the Short Run SRa01 and in 2004 and 2006 by MOST for a total of ~70 days. We present their photometric variability up to 1000 $\mu$ Hz and down to residual amplitude noise levels of 23 and 10 ppm of the CoRoT data for V 588 Mon and V 589 Mon, respectively. The CoRoT imagette data as well as the two MOST data sets allowed for detailed frequency analyses using Period04 and SigSpec. We confirm all previously identified frequencies, improve the known pulsation spectra to a total of 21 frequencies for V 588 Mon and 37 for V 589 Mon and compare them to our PMS model predictions. No model oscillation spectrum with l = 0, 1, 2, and 3 p-modes matches all the observed frequencies. When rotation is included we find that the rotationally split modes of the slower rotating star, V 589 Mon, are addressable via perturbative methods while for the more rapidly rotating star, V 588 Mon, they are not and, consequently, will require more sophisticated modeling. The high precision of the CoRoT data allowed us to investigate the large density of frequencies found in the region from 0 to 300 $\mu$Hz. The presence of granulation appears to be a more attractive explanation than the excitation of high-degree modes. Granulation was modeled with a superposition of white noise, a sum of Lorentzian-like functions and a Gaussian. Our analysis clearly illustrates the need for a more sophisticated granulation model., Comment: accepted by ApJ

Published
2011
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17. The SARS algorithm: detrending CoRoT light curves with Sysrem using simultaneous external parameters

Author

Ofir, Aviv, Alonso, Roi, Bonomo, Aldo Stefano, Carone, Ludmila, Carpano, Stefania, Samuel, Benjamin, Weingrill, Jorg, Aigrain, Suzanne, Auvergne, Michel, Baglin, Annie, Barge, Pierre, Borde, Pascal, Bouchy, Francois, Deeg, Hans J., Deleuil, Magali, Dvorak, Rudolf, Erikson, Anders, Mello, Sylvio Ferraz, Fridlund, Malcolm, Gillon, Michel, Guillot, Tristan, Hatzes, Artie, Jorda, Laurent, Lammer, Helmut, Leger, Alain, Llebaria, Antoine, Moutou, Claire, Ollivier, Marc, Paetzold, Martin, Queloz, Didier, Rauer, Heike, Rouan, Daniel, Schneider, Jean, and Wuchterl, Guenther

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Surveys for exoplanetary transits are usually limited not by photon noise but rather by the amount of red noise in their data. In particular, although the CoRoT spacebased survey data are being carefully scrutinized, significant new sources of systematic noises are still being discovered. Recently, a magnitude-dependant systematic effect was discovered in the CoRoT data by Mazeh & Guterman et al. and a phenomenological correction was proposed. Here we tie the observed effect a particular type of effect, and in the process generalize the popular Sysrem algorithm to include external parameters in a simultaneous solution with the unknown effects. We show that a post-processing scheme based on this algorithm performs well and indeed allows for the detection of new transit-like signals that were not previously detected., Comment: MNRAS accepted. 5 pages, 3 figures

Published
2010
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18. Level-Set Based Algorithm for Automatic Feature Extraction on 3D Meshes: Application to Crater Detection on Mars

Author

Christoff, Nicole, Manolova, Agata, Jorda, Laurent, Viseur, Sophie, Bouley, Sylvain, Mari, Jean-Luc, Hutchison, David, Series Editor, Kanade, Takeo, Series Editor, Kittler, Josef, Series Editor, Kleinberg, Jon M., Series Editor, Mattern, Friedemann, Series Editor, Mitchell, John C., Series Editor, Naor, Moni, Series Editor, Pandu Rangan, C., Series Editor, Steffen, Bernhard, Series Editor, Terzopoulos, Demetri, Series Editor, Tygar, Doug, Series Editor, Weikum, Gerhard, Series Editor, Chmielewski, Leszek J., editor, Kozera, Ryszard, editor, Orłowski, Arkadiusz, editor, Wojciechowski, Konrad, editor, Bruckstein, Alfred M., editor, and Petkov, Nicolai, editor

Published
2018
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22. Rosetta lander Philae: Flight Dynamics analyses for landing site selection and post-landing operations

Author

Jurado, Eric, Martin, Thierry, Canalias, Elisabet, Blazquez, Alejandro, Garmier, Romain, Ceolin, Thierry, Gaudon, Philippe, Delmas, Cedric, Biele, Jens, Ulamec, Stephan, Remetean, Emile, Torres, Alex, Laurent-Varin, Julien, Dolives, Benoit, Herique, Alain, Rogez, Yves, Kofman, Wlodek, Jorda, Laurent, Zakharov, Vladimir, Crifo, Jean-François, Rodionov, Alexander, Heinish, P., and Vincent, Jean-Baptiste

Published
2016
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24. The equilibrium shape of (65) Cybele: primordial or relic of a large impact?

Author

Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Marsset, Michaël, Brož, Miroslav, Vermersch, Julie, Rambaux, Nicolas, Ferrais, Marin, Viikinkoski, Matti, Hanuš, Josef, Jehin, Emmanuel, Podlewska-Gaca, Edyta, Bartczak, Przemyslaw, Dudziński, Grzegorz, Carry, Benoît, Vernazza, Pierre, Szakáts, Róbert, Duffard, René, Jones, A., Molina, David, Santana-Ros, Toni, Benkhaldoun, Zouhair, Birlan, Mirel, Dumas, Christophe, Fétick, Romain, Fusco, Thierry, Jorda, Laurent, Marchis, Franck, Vachier, Frédéric, Yang, Bin, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Marsset, Michaël, Brož, Miroslav, Vermersch, Julie, Rambaux, Nicolas, Ferrais, Marin, Viikinkoski, Matti, Hanuš, Josef, Jehin, Emmanuel, Podlewska-Gaca, Edyta, Bartczak, Przemyslaw, Dudziński, Grzegorz, Carry, Benoît, Vernazza, Pierre, Szakáts, Róbert, Duffard, René, Jones, A., Molina, David, Santana-Ros, Toni, Benkhaldoun, Zouhair, Birlan, Mirel, Dumas, Christophe, Fétick, Romain, Fusco, Thierry, Jorda, Laurent, Marchis, Franck, Vachier, Frédéric, and Yang, Bin

Abstract

Context. Cybele asteroids constitute an appealing reservoir of primitive material genetically linked to the outer Solar System, and the physical properties (size and shape) of the largest members can be readily accessed by large (8m class) telescopes. Aims. We took advantage of the bright apparition of the most iconic member of the Cybele population, (65) Cybele, in July and August 2021 to acquire high-angular-resolution images and optical light curves of the asteroid with which we aim to analyse its shape and bulk properties. Methods. Eight series of images were acquired with VLT/SPHERE+ZIMPOL, seven of which were combined with optical light curves to reconstruct the shape of the asteroid using the ADAM, MPCD, and SAGE algorithms. The origin of the shape was investigated by means of N-body simulations. Results. Cybele has a volume-equivalent diameter of 263±3 km and a bulk density of 1.55 ± 0.19 g cm−3. Notably, its shape and rotation state are closely compatible with those of a Maclaurin equilibrium figure. The lack of a collisional family associated with Cybele and the higher bulk density of that body with respect to other large P-type asteroids suggest that it never experienced any large disruptive impact followed by rapid re-accumulation. This would imply that its present-day shape represents the original one. However, numerical integration of the long-term dynamical evolution of a hypothetical family of Cybele shows that it is dispersed by gravitational perturbations and chaotic diffusion over gigayears of evolution. Conclusions. The very close match between Cybele and an equilibrium figure opens up the possibility that D ≥ 260 km (M ≥ 1.5 × 1019 kg) small bodies from the outer Solar System all formed at equilibrium. However, we cannot currently rule out an old impact as the origin of the equilibrium shape of Cybele. Cybele itself is found to be dynamically unstable, implying that it was ‘recently’ (<1 Gyr ago) placed on its current orbit either through slow d

Published
2023

27. VLT/SPHERE imaging survey of D>100 km asteroids: Final results and synthesis

Author

Vernazza, Pierre, Carry, Benoit, Ferrais, Marin, Jorda, Laurent, Hanus, Josef, Marsset, Michael, Brož, Miroslav, Fetick, Roman, 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), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Charles University [Prague] (CU), and European Southern Observatory (ESO)

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

Until recently, only three large main belt asteroids, Ceres, Vesta and Lutetia, had been imaged with a high level of detail, as they were visited by the space missions Dawn and Rosetta of NASA and the European Space Agency, respectively. The previously small number of detailed observations of asteroids meant that, until now, key characteristics such as their 3D shape or density had remained largely unknown. Between 2017 and 2019, we have been filling this gap by conducting a high-angular-resolution imaging survey of 42 large main-belt asteroids with VLT/SPHERE (ESO large programme; PI: P. Vernazza; ID: 199.C-0074), sampling the main compositional classes. These observations have allowed to cast some light on the following fundamental questions: – What is the diversity in shape among large asteroids and are the shapes close to equilibrium?– How do large impacts affect asteroid shape?– What is the bulk density of large asteroids and is there a relationship with their surface composition? Is there any evidence of differentiation among those bodies?– Is the density of those bodies that are predicted to be implanted bodies from the outer Solar System (P/D-types) compatible with that of small (D ≤ 300 km) trans-Neptunian objects?– What physical properties drive the formation of companions around large asteroids? Importantly, our survey along with previous observations provides evidence in support of the possibility that some C-complex bodies could be intrinsically related to IDP-like P- and D-type asteroids, representing different layers of a same body (C: core; P/D: outer shell). We therefore propose that P/ D-types and some C-types may have the same origin in the primordial trans-Neptunian disk. The main belt would thus host a population of former TNOs much more important than the one previously considered, consisting solely of P and D-type bodies. Here, we will present an overview of the results obtained from this survey ([1]) with a specific focus on the origin of a large fraction of the asteroid belt (typically C, P and D-type bodies). References [1] Vernazza, P., Ferrais, M., Jorda, L., et al. VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. A&A 654, 2021.

Published
2023
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30. Constraining the shape and density of binary asteroid (121) Hermione

Author

Ferrais, Marin, primary, Vernazza, Pierre, additional, Marsset, Michaël, additional, Jorda, Laurent, additional, Carry, Benoit, additional, Hanus, Josef, additional, Brož, Miroslav, additional, Yang, Bin, additional, Fétick, Romain, additional, Marchis, Franck, additional, Vachier, Frederic, additional, Birlan, Mirel, additional, Jehin, Emmanuël, additional, Podlewska-Gaca, Edyta, additional, Bartczak, Przemyslaw, additional, Fusco, Thierry, additional, and Dudziński, Grzegorz, additional

Published
2022
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36. The PICOCAM Project at Pic du Midi

Author

Colas, Francois, Arlot, Jean Eudes, Berthier, Jerome, Fienga, Agnes, Gastineau, Michael, Hestroffer, Daniel, Jorda, Laurent, Lecacheux, Jean, Fitzsimmons, A., editor, Jewitt, D., editor, and West, R. M., editor

Published
2000
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39. Application of Implicit 3D Modelling to Reconstruct the Layered Structure of the Comet 67P

Author

Penasa, Luca, primary, Massironi, Matteo, additional, Simioni, Emanuele, additional, Franceschi, Marco, additional, Naletto, Giampiero, additional, Ferrari, Sabrina, additional, Bertini, Ivano, additional, Cambianica, Pamela, additional, Frattin, Elisa, additional, Forgia, Fiorangela La, additional, Lucchetti, Alice, additional, Pajola, Maurizio, additional, Preusker, Frank, additional, Scholten, Frank, additional, Jorda, Laurent, additional, Gaskell, Robert, additional, and Sierks, Holger, additional

Published
2022
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40. Comet 67P/Churyumov-Gerasimenko: Non-Gravitational Forces Based on its Detailed Shape

Author

Keller, Horst Uwe, Mottola, Stefano, Skorov, Yuri, Davidsson, Björn, Gutiérrez, Pedro, Jorda, Laurent, Maquet, Lucie, Laboratoire d'Astrophysique de Marseille (LAM), and 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)

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

International audience; Non-gravitational forces caused by sublimation on a cometary nucleus influence its orbital parameters and its rotational properties. Based on thermal models and rough estimates of the nucleus shape properties such as its mass and density can be derived [1, 2]. The uncertainty of the nucleus shape influences the quality of the results. Changes of the angular momentum of the nucleus rotation are more strongly influenced by details of the shape and surface. The long term observations of the nucleus of comet 67P/Churyumov-Gerasimenko by OSIRIS [3] during the rendezvous with ESA’s Rosetta spacecraft result in a very detailed shape model [3]. We use a shape model with > 105 facets to simulate the distributed forces due to sublimation and to calculate their exerted torques. The determination of the overall activity and its spatial and timely distribution over the nucleus remains a major challenge. Early observations revealed that the rotation period had changed from its last perihelion passage in 2009 [4]. The detailed shape model along with thermal modeling makes it possible to calculate the diurnal activity of the facets [6, 7]. The net torque integrated over the whole surface causes a change in the angular momentum. We also calculate the forces acting on the motion of the nucleus. This can be monitored by determinations of the spacecraft positions during the Rosetta mission. We will compare our results with the traditional approach to calculate the non-gravitational forces [8].[1, 2] Davidsson, B. J. R. & Gutiérrez, P. J., Icarus, 168, 392, 2004, Icarus, 176, 453, 2005[3] H. U. Keller, C. Barbieri, P. Lamy, H. Rickman, R. Rodrigo, K.-P. Wenzel, H. Sierks, M. A’Hearn, F. Angrilli, M. Angulo, et al., SSR, 128 (1-4): 433-506, 2007.[4] Preusker, F., Scholten, F., Matz, K.-D., et al., Astronomy & Astrophysics, accepted, 2015[5] S. Mottola, S. Lowry, C. Snodgrass, P. Lamy, I. Toth, et al. A&A, 569: L2, Sept. 2014.[6] H. U. Keller, S. Mottola, B. Davidsson, S. Schröder, Y. Skorov, E. Kührt, et al.. A&A, in press[7] H. U. Keller, S. Mottola, Y. V. Skorov, and L. Jorda, Astronomy and Astrophysics Letter , 2015.[8] B. G. Marsden, Z. Sekanina, and D. K. Yeomans, Astronomical Journal, 78: 211, Mar. 1973.

Published
2022

41. Meter-scale thermal contraction crack polygons on comet 67P/Churyumov-Gerasimenko

Author

Auger, Anne-Thérèse, Ramy El-Maarry, Mohamed, Groussin, Olivier, Jorda, Laurent, Bouley, Sylvain, Séjourné, Antoine, Capanna, Claire, Höfner, Sebastian, Sierks, Holger, Laboratoire d'Astrophysique de Marseille (LAM), and 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)

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

International audience; Since August 2014, high spatial resolution images of the nucleus of comet 67P/Churyumov-Gerasimenko have been acquired by the OSIRIS camera onboard Rosetta, enabling to identify meter-scale features on the surface (Thomas et al., 2015; El-Maary et al., 2015). Here, we report on the detection and characterization of thermal contraction polygons. We have identified more than 6000 polygons on 67P, using OSIRIS images with a spatial resolution down to 1.6 m/pixel. They are observed in consolidated terrains, from flat terrains to steep terrains such as cliffs and pit walls. The size of polygons is in the range 1 - 10 m, with a mean value of 3 m. Polygons detected on 67P show morphologies with an elevated center. Polygons are known to form on Mars and Earth when the thermal stress of the surface icy materials exceeds their tensile strength, therefore forming fractures (Lachenbruch, 1962; Mangold, 2005; Marchant & Head, 2007). The size, shape and spatial distribution of polygons across the surface provide constraints on their formation and evolution processes, the sub-surface water ice content, the thermal history of the surface and the mechanical properties of the surface material (e.g., Mellon et al., 2008; Levy et al., 2011).

Published
2022

42. 3D reconstruction of the final PHILAE landing site: Abydos

Author

Capanna, Claire, Jorda, Laurent, Lamy, Philippe, Gesquière, Gilles, Delmas, Cédric, Durand, Joëlle, Gaudon, Philippe, Jurado, Eric, Laboratoire d'Astrophysique de Marseille (LAM), and 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)

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

International audience; The Abydos region is the region of the final landing site of the PHILAE lander. The landing site has been potentially identified on images of this region acquired by the OSIRIS imaging system aboard the orbiter before (Oct 22, 2014) and after (Dec 6-13, 2014) the landing of PHILAE (Lamy et al., in prep.). Assuming that this identification is correct, we reconstructed the topography of Abydos in 3D using a method called ``multiresolution photoclinometry by deformation'' (MPCD, Capanna et al., The Visual Computer, 29(6-8): 825-835, 2013). The method works in two steps: (a) a DTM of this region is extracted from the global MPCD shape model, (b) the resulting triangular mesh is progressively deformed at increasing spatial resolution in order to match a set of 14 images of Abydos at pixel resolutions between 1 and 8 m. The method used to perform the image matching is the L-BFGS-b non-linear optimization (Morales et al., ACM Trans. Math. Softw., 38(1): 1-4, 2011).In spite of the very unfavourable illumination conditions, we achieve a vertical accuracy of about 3 m, while the horizontal sampling is 0.5 m. The accuracy is limited by high incidence angles on the images (about 60 deg on average) combined with a complex topography including numerous cliffs and a few overhangs. We also check the compatibility of the local DTM with the images obtained by the CIVA-P instrument aboard PHILAE. If the Lamy et al. identification is correct, our DTM shows that PHILAE landed in a cavity at the bottom of a small cliff of 8 m height.

Published
2022

43. Evidence for a precession of the nucleus of comet 67P/C-G from ROSETTA/OSIRIS images

Author

Jorda, Laurent, Gutierrez, Pedro, Davidsson, Bjoern, Gaskell, Robert, Hviid, Stubbe, Keller, Horst Uwe, Maquet, Lucie, Mottola, Stefano, Preusker, Frank, Scholten, Frank, Laboratoire d'Astrophysique de Marseille (LAM), and 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)

Subjects
[SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract

International audience; The retrieval of the rotational parameters of comet 67P/C-G is part of the shape reconstruction process conducted from data collected by the OSIRIS imaging system aboard ROSETTA. Among other parameters, this includes the reconstruction of the (RA,Dec) direction of the Z axis of the body-fixed frame and that of the angular momentum vector. The stereophotogrammetric solution (Preusker et al., A&A 2015, in press) obtained in Aug-Sep 2014 already showed evidence for a complex rotation of comet 67P/C-G. A subsequent analysis of the rotational data obtained using the stereophotoclinometry method (Gaskell et al., MP&S 43, 1049, 2008) up to April 2015 also revealed a precession with a likelihood greater than 99.99 %. The amplitude and period of the (RA,Dec) variations measured with both methods are fully compatible.We propose an interpretation of the measured period as a combination of torque free motions: a rotation combined with a precession of small amplitude. The modeling of this motion has implications on the value of the moments of inertia, from which it is possible to constrain the internal density distribution of comet 67P/C-G.

Published
2022

44. 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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45. 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, AʼHearn, Michael F., Auger, Anne-Thérèse, Barucci, M. Antonella, Bertaux, Jean-Loup, Bertini, Ivano, Capanna, Claire, Cremonese, Gabriele, Da Deppo, Vania, Davidsson, Björn, Debei, Stefano, De Cecco, Mariolino, El-Maarry, Mohamed Ramy, Ferri, Francesca, Fornasier, Sonia, Fulle, Marco, Gaskell, Robert, Giacomini, Lorenza, Groussin, Olivier, Guilbert-Lepoutre, Aurélie, Gutierrez-Marques, P., Gutiérrez, Pedro J., Güttler, Carsten, Hoekzema, Nick, Höfner, Sebastian, Hviid, Stubbe F., Ip, Wing-Huen, Jorda, Laurent, Knollenberg, Jörg, Kovacs, Gabor, Kramm, Rainer, Kührt, Ekkehard, Küppers, Michael, La Forgia, Fiorangela, Lara, Luisa M., Lazzarin, Monica, Lee, Vicky, Leyrat, Cédric, Lin, Zhong-Yi, Lopez Moreno, Josè J., Lowry, Stephen, Magrin, Sara, Maquet, Lucie, Marchi, Simone, Marzari, Francesco, Massironi, Matteo, Michalik, Harald, Moissl, Richard, Mottola, Stefano, Naletto, Giampiero, Oklay, Nilda, Pajola, Maurizio, Preusker, Frank, Scholten, Frank, Thomas, Nicolas, Toth, Imre, and Tubiana, Cecilia

Published
2015
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47. Evidence for scalloped terrains on 67P

Author

Bouquety, Axel, primary, Groussin, Olivier, additional, Jorda, Laurent, additional, Séjourné, Antoine, additional, Costard, François, additional, and Bouley, Sylvain, additional

Published
2021
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49. FRIPON: a worldwide network to track incoming meteoroids

Author

Marsset, Michaël, Brož, Miroslav, Castillo-Rogez, Julie, Hanuš, Josef, Viikinkoski, Matti, Ševeček, Pavel, Marchis, Franck, Podlewska-Gaca, Edyta, Asphaug, Erik, Bartczak, Przemyslaw, Berthier, Jérôme, Cipriani, Fabrice, Dudziński, Grzegorz, Dumas, Christophe, Ďurech, Josef, Ferrais, Marin, Fétick, Romain, Fusco, Thierry, Kaasalainen, Mikko, Kryszczynska, Agnieszka, Lamy, Philippe, Le Coroller, Hervé, Marciniak, Anna, Michalowski, Tadeusz, Michel, Patrick, Richardson, Derek, Santana-Ros, Toni, Vachier, Frédéric, Vigan, Arthur, Witasse, Olivier, Yang, Bin, Colas, François, Zanda, B., Bouley, S., Jeanne, S., Malgoyre, A., Birlan, Mirel, Blanpain, C., Gattacceca, J., Jorda, Laurent, Lecubin, J., Marmo, C., Rault, J., Vaubaillon, J., Vernazza, Pierre, Yohia, C., Gardiol, D., Nedelcu, A., Poppe, B., Rowe, J., Forcier, M., Trigo-Rodriguez, J., Lamy, H., Behrend, R., Ferrière, L., Barghini, D., Buzzoni, A., Carbognani, A., Di Carlo, M., Di Martino, M., Knapic, C., Londero, E., Pratesi, G., Rasetti, S., Riva, W., Stirpe, G., Valsecchi, G., Volpicelli, C., Zorba, S., Coward, D., Drolshagen, E., Drolshagen, G., Hernandez, O., Jehin, Emmanuel, Jobin, M., King, A., Nitschelm, C., Ott, T., Sanchez-Lavega, A., Toni, A., Abraham, P., Affaticati, F., Albani, M., Andreis, A., Andrieu, T., Anghel, S., Antaluca, E., Antier, K., Appéré, T., Armand, A., Ascione, G., Audureau, Y., Auxepaules, G., Avoscan, T., Baba Aissa, D., Bacci, P., Bǎdescu, O., Baldini, R., Baldo, R., Balestrero, A., Baratoux, D., Barbotin, E., Bardy, M., Basso, S., Bautista, O., Bayle, L., Beck, P., Bellitto, R., Belluso, R., Benna, C., Benammi, M., Beneteau, E., Benkhaldoun, Z., Bergamini, P., Bernardi, F., Bertaina, M., Bessin, P., Betti, L., Bettonvil, F., Bihel, D., Birnbaum, C., Blagoi, O., Blouri, E., Boacă, I., Boatǎ, R., Bobiet, B., Bonino, R., Boros, K., Bouchet, E., Borgeot, V., Bouchez, E., Boust, D., Boudon, V., Bouman, T., Bourget, P., Brandenburg, S., Bramond, Ph., Braun, E., Bussi, A., Cacault, P., Caillier, B., Calegaro, A., Camargo, J., Caminade, S., Campana, A., Campbell-Burns, P., Canal-Domingo, R., Carell, O., Carreau, S., Cascone, E., Cattaneo, C., Cauhape, P., Cavier, P., Celestin, S., Cellino, A., Champenois, M., Chennaoui Aoudjehane, H., Chevrier, S., Cholvy, P., Chomier, L., Christou, A., Cricchio, D., Coadou, P., Cocaign, J., Cochard, F., Cointin, S., Colombi, E., Colque Saavedra, J., Corp, L., Costa, M., Costard, F., COTTIER, M., Cournoyer, P., Coustal, E., Cremonese, G., Cristea, O., Cuzon, J., D’Agostino, G., Daiffallah, K., Dǎnescu, C., Dardon, A., Dasse, T., Davadan, C., Debs, V., Defaix, J., Deleflie, F., D’Elia, M., De Luca, P., De Maria, P., Deverchère, P., Devillepoix, H., Dias, A., Di Dato, A., Di Luca, R., Dominici, F., Drouard, Alexis, Dumont, J., Dupouy, P., Duvignac, L., Egal, A., Erasmus, N., Esseiva, N., Ebel, A., Eisengarten, B., Federici, F., Feral, S., Ferrant, G., Ferreol, E., Finitzer, P., Foucault, A., Francois, P., Frîncu, M., Froger, J., Gaborit, F., Gagliarducci, V., Galard, J., Gardavot, A., Garmier, M., Garnung, M., Gautier, B., Gendre, B., Gerard, D., Gerardi, A., Godet, J., Grandchamps, A., Grouiez, B., Groult, S., Guidetti, D., Giuli, G., Hello, Y., Henry, X., Herbreteau, G., Herpin, M., Hewins, P., Hillairet, J., Horak, J., Hueso, R., Huet, E., Huet, S., Hyaumé, F., Interrante, G., Isselin, Y., Jeangeorges, Y., Janeux, P., Jeanneret, P., Jobse, K., Jouin, S., Jouvard, J., Joy, K., Julien, J., Kacerek, R., Kaire, M., Kempf, M., Koschny, D., Krier, C., Kwon, M., Lacassagne, L., Lachat, D., Lagain, A., Laisné, E., Lanchares, V., Laskar, J., Lazzarin, M., Leblanc, M., Lebreton, J., Lecomte, J., Le Dû, P., LELONG, F., Lera, S., Leoni, J., Le-Pichon, A., Le-Poupon, P., Leroy, A., Leto, G., Levansuu, A., Lewin, E., Lienard, A., Licchelli, D., LOCATELLI, H., Loehle, S., Loizeau, D., Luciani, L., Maignan, M., Manca, F., Mancuso, S., Mandon, E., Mangold, N., Mannucci, F., Maquet, L., Marant, D., Marchal, Y., Marin, J., Martin-Brisset, J., Martin, D., Mathieu, D., Maury, A., Mespoulet, N., Meyer, F., Meyer, J., Meza, E., Moggi Cecchi, V., Moiroud, J., Millan, M., Montesarchio, M., Misiano, A., Molinari, E., Molau, S., Monari, J., Monflier, B., Monkos, A., Montemaggi, M., Monti, G., Moreau, R., Morin, J., Mourgues, R., Mousis, O., Nablanc, C., Nastasi, A., Niacşu, L., Notez, P., Ory, M., Pace, E., Paganelli, M., Pagola, A., Pajuelo, M., Palacián, J., Pallier, G., Paraschiv, P., Pardini, R., Pavone, M., Pavy, G., Payen, G., Pegoraro, A., Peña-Asensio, E., Perez, L., Pérez-Hoyos, S., Perlerin, V., Peyrot, A., Peth, F., Pic, V., Pietronave, S., Pilger, C., Piquel, M., Pisanu, T., Poppe, M., Portois, L., Prezeau, J., Pugno, N., Quantin, C., Quitté, G., Rambaux, Nicolas, Ravier, E., Repetti, U., Ribas, S., Richard, C., Richard, D., RIGONI, M., Rivet, J., Rizzi, N., Rochain, S., Rojas, J.F., Romeo, M., Rotaru, M., Rotger, M., Rougier, P., Rousselot, P., Rousset, J., Rousseu, D., Rubiera, O., Rudawska, R., Rudelle, J., Ruguet, J.P., Russo, P., Sales, S., Sauzereau, O., Salvati, F., Schieffer, M., Schreiner, D., Scribano, Y., Selvestrel, D., Serra, R., Shengold, L., Shuttleworth, A., Smareglia, R., Sohy, S., Soldi, M., Stanga, R., Steinhausser, A., Strafella, F., Sylla Mbaye, S., Smedley, A., Tagger, M., Tanga, Paolo, Taricco, C., Teng, J., Tercu, J., Thizy, O., Thomas, J., Tombelli, M., Trangosi, R., Tregon, B., Trivero, P., Tukkers, A., Turcu, V., Umbriaco, G., Unda-Sanzana, E., Vairetti, R., Valenzuela, M., Valente, G., Varennes, G., Vauclair, S., Vergne, J., Verlinden, M., Vidal-Alaiz, M., Vieira-Martins, R., Viel, A., Vîntdevarǎ, D., Vinogradoff, V., Volpini, P., Wendling, M., Wilhelm, P., Wohlgemuth, K., Yanguas, P., Zagarella, R., Zollo, A., l'Observatoire de Paris, Muséum national d'Histoire naturelle (France), Université Paris-Saclay, OSU Institut Pythéas, Istituto Nazionale di Astrofisica, Fondazione Cassa di Risparmio di Torino, Fondazione De Mari Savona, Diputación Foral de Bizkaia, Ministry of Research and Innovation (Romania), Museu de Astronomia e Ciências Afins (Brazil), Labex ESEP, Sorbonne Université, Universidad Pública de Navarra / Nafarroako Unibertsitate Publikoa. InaMat - Institute for Advanced Materials, Universidad Pública de Navarra. Departamento de Estadística, Informática y Matemáticas, Nafarroako Unibertsitate Publikoa. Estatistika, Informatika eta Matematika Saila, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Laboratoire d'Astrophysique de Marseille (LAM), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - 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L., Vaubaillon, J., Vernazza, P., Yohia, C., Gardiol, D., Nedelcu, A., Poppe, B., Rowe, J., Forcier, M., Koschny, D., Trigo-Rodriguez, J. M., Lamy, H., Behrend, R., Ferriere, L., Barghini, D., Buzzoni, A., Carbognani, A., Di Carlo, M., Di Martino, M., Knapic, C., Londero, E., Pratesi, G., Rasetti, S., Riva, W., Stirpe, G. M., Valsecchi, G. B., Volpicelli, C. A., Zorba, S., Coward, D., Drolshagen, E., Drolshagen, G., Hernandez, O., Jehin, E., Jobin, M., King, A., Nitschelm, C., Ott, T., Sanchez-Lavega, A., Toni, A., Abraham, P., Affaticati, F., Albani, M., Andreis, A., Andrieu, T., Anghel, S., Antaluca, E., Antier, K., Appere, T., Armand, A., Ascione, G., Audureau, Y., Auxepaules, G., Avoscan, T., Baba Aissa, D., Bacci, P., Badescu, O., Baldini, R., Baldo, R., Balestrero, A., Baratoux, D., Barbotin, E., Bardy, M., Basso, S., Bautista, O., Bayle, L. D., Beck, P., Bellitto, R., Belluso, R., Benna, C., Benammi, M., Beneteau, E., Benkhaldoun, Z., Bergamini, P., Bernardi, F., Bertaina, M. E., Bessin, P., Betti, L., Bettonvil, F., Bihel, D., Birnbaum, C., Blagoi, O., Blouri, E., Boaca, I., Boata, R., Bobiet, B., Bonino, R., Boros, K., Bouchet, E., Borgeot, V., Bouchez, E., Boust, D., Boudon, V., Bouman, T., Bourget, P., Brandenburg, S., Bramond, P., Braun, E., Bussi, A., Cacault, P., Caillier, B., Calegaro, A., Camargo, J., Caminade, S., Campana, A. P. C., Campbell-Burns, P., Canal-Domingo, R., Carell, O., Carreau, S., Cascone, E., Cattaneo, C., Cauhape, P., Cavier, P., Celestin, S., Cellino, A., Champenois, M., Chennaoui Aoudjehane, H., Chevrier, S., Cholvy, P., Chomier, L., Christou, A., Cricchio, D., Coadou, P., Cocaign, J. Y., Cochard, F., Cointin, S., Colombi, E., Colque Saavedra, J. P., Corp, L., Costa, M., Costard, F., Cottier, M., Cournoyer, P., Coustal, E., Cremonese, G., Cristea, O., Cuzon, J. C., D'Agostino, G., Daiffallah, K., Danescu, C., Dardon, A., Dasse, T., Davadan, C., Debs, V., Defaix, J. P., Deleflie, F., D'Elia, M., De Luca, P., De Maria, P., Deverchere, P., Devillepoix, H., Dias, A., Di Dato, A., Di Luca, R., Dominici, F. M., Drouard, A., Dumont, J. L., Dupouy, P., Duvignac, L., Egal, A., Erasmus, N., Esseiva, N., Ebel, A., Eisengarten, B., Federici, F., Feral, S., Ferrant, G., Ferreol, E., Finitzer, P., Foucault, A., Francois, P., Frincu, M., Froger, J. L., Gaborit, F., Gagliarducci, V., Galard, J., Gardavot, A., Garmier, M., Garnung, M., Gautier, B., Gendre, B., Gerard, D., Gerardi, A., Godet, J. P., Grandchamps, A., Grouiez, B., Groult, S., Guidetti, D., Giuli, G., Hello, Y., Henry, X., Herbreteau, G., Herpin, M., Hewins, P., Hillairet, J. J., Horak, J., Hueso, R., Huet, E., Huet, S., Hyaume, F., Interrante, G., Isselin, Y., Jeangeorges, Y., Janeux, P., Jeanneret, P., Jobse, K., Jouin, S., Jouvard, J. M., Joy, K., Julien, J. F., Kacerek, R., Kaire, M., Kempf, M., Krier, C., Kwon, M. 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Subjects
DYNAMICS, [INFO.INFO-AR]Computer Science [cs]/Hardware Architecture [cs.AR], Meteors, Computer science, Radio receiver, [INFO.INFO-DM]Computer Science [cs]/Discrete Mathematics [cs.DM], Surveys, 010502 geochemistry & geophysics, Track (rail transport), 01 natural sciences, Meteorites, meteors, meteoroids, law.invention, Planets and planetary system, [INFO.INFO-TS]Computer Science [cs]/Signal and Image Processing, Methods: observational, law, [INFO.INFO-RB]Computer Science [cs]/Robotics [cs.RO], meteoroids, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Observational methods, Earth and Planetary Astrophysics (astro-ph.EP), meteoroids -surveys -methods: observational -interplanetary medium, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ORIGIN, [INFO.INFO-AO]Computer Science [cs]/Computer Arithmetic, meteorites, meteors, meteoroids – surveys – methods: observational – interplanetary medium, Meteoroids, RECOVERY, ORBIT, Meteorite, Fully automated, Interplanetary medium, [INFO.INFO-TI]Computer Science [cs]/Image Processing [eess.IV], [INFO.INFO-DC]Computer Science [cs]/Distributed, Parallel, and Cluster Computing [cs.DC], Astrophysics - Instrumentation and Methods for Astrophysics, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing, FLUX, Real-time computing, fripon, [INFO.INFO-DS]Computer Science [cs]/Data Structures and Algorithms [cs.DS], FOS: Physical sciences, Context (language use), CAMERA, [INFO.INFO-SE]Computer Science [cs]/Software Engineering [cs.SE], [SPI.AUTO]Engineering Sciences [physics]/Automatic, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 0103 physical sciences, FIREBALL NETWORK, observational [Methods], meteors, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Meteoroid, INNISFREE METEORITE, [INFO.INFO-CV]Computer Science [cs]/Computer Vision and Pattern Recognition [cs.CV], Astronomy and Astrophysics, METEORITE FALL, Meteorites, meteors, meteoroid, Camera network, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Interplanetary spaceflight, meteroids tracking, meteoroids - surveys - methods: observational, SYSTEM, Astrophysics - Earth and Planetary Astrophysics, Meteorites
Abstract

Context. Until recently, camera networks designed for monitoring fireballs worldwide were not fully automated, implying that in case of a meteorite fall, the recovery campaign was rarely immediate. This was an important limiting factor as the most fragile - hence precious - meteorites must be recovered rapidly to avoid their alteration. Aims. The Fireball Recovery and InterPlanetary Observation Network (FRIPON) scientific project was designed to overcome this limitation. This network comprises a fully automated camera and radio network deployed over a significant fraction of western Europe and a small fraction of Canada. As of today, it consists of 150 cameras and 25 European radio receivers and covers an area of about 1.5 × 10km. Methods. The FRIPON network, fully operational since 2018, has been monitoring meteoroid entries since 2016, thereby allowing the characterization of their dynamical and physical properties. In addition, the level of automation of the network makes it possible to trigger a meteorite recovery campaign only a few hours after it reaches the surface of the Earth. Recovery campaigns are only organized for meteorites with final masses estimated of at least 500 g, which is about one event per year in France. No recovery campaign is organized in the case of smaller final masses on the order of 50 to 100 g, which happens about three times a year; instead, the information is delivered to the local media so that it can reach the inhabitants living in the vicinity of the fall. Results. Nearly 4000 meteoroids have been detected so far and characterized by FRIPON. The distribution of their orbits appears to be bimodal, with a cometary population and a main belt population. Sporadic meteors amount to about 55% of all meteors. A first estimate of the absolute meteoroid flux (mag < -5; meteoroid size ≥∼1 cm) amounts to 1250/yr/10km. This value is compatible with previous estimates. Finally, the first meteorite was recovered in Italy (Cavezzo, January 2020) thanks to the PRISMA network, a component of the FRIPON science project., FRIPON was initiated by funding from ANR (grant N.13- BS05-0009-03), carried by the Paris Observatory, Muséum National d’Histoire Naturelle, Paris-Saclay University and Institut Pythéas (LAM-CEREGE). VigieCiel was part of the 65 Millions d’Observateurs project, carried by the Muséum National d’Histoire Naturelle and funded by the French Investissements d’Avenir program. FRIPON data are hosted and processed at Institut Pythéas SIP (Service Informatique Pythéas), and a mirror is hosted at IMCCE (Institut de Mécanique Céleste et de Calcul des Éphémérides / Paris Observatory) with the help of IDOC (https://idoc.ias.u-psud.fr) (Integrated Data and Operation Center), supported by CNRS and CNES. PRISMA is the Italian Network for Systematic surveillance of Meteors and Atmosphere. It is a collaboration initiated and coordinated by the Italian National Institute for Astrophysics (INAF) that counts members among research institutes, associations and schools (http://www.prisma.inaf.it). PRISMA was partially funded by 2016 and 2020 Research and Education grants from Fondazione Cassa di Risparmio di Torino and by a 2016 grant from Fondazione Agostino De Mari (Savona). FRIPON-Bilbao is supported by a grant from Diputacion Foral Bizkaia (DFB/BFA). FRIPONMOROI was supported by a grant of the Romanian Ministery of Research and Innovation, CCCDI - UEFISCDI, project number PN-III-P1-1.2-PCCDI2017-0226/16PCCDI/2018 , within PNCDI III. Rio de Janeiro camera is hosted and partially maintained by MAST (Museum of Astronomy and Related Sciences)/MCTIC. The Meteorix project acknowledges supports from labex ESEP (Exploration Spatiale des Environnements Planétaires), DIM-ACAV+ Région Île-de-France, Janus CNES, IDEX Sorbonne Universités and Sorbonne Université.

Published
2020
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