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1. Regional unit definition for the nucleus of comet 67P/Churyumov-Gerasimenko on the SHAP7 model

Author

Holger Sierks, J.-B. Vincent, F. Preusker, Giampiero Naletto, Francesco Marzari, Sonia Fornasier, Stubbe F. Hviid, M. A. Barucci, P. J. Gutierrez, Carsten Güttler, J. J. Lopez-Moreno, Jörg Knollenberg, Ivano Bertini, Stefano Debei, V. Da Deppo, P. L. Lamy, Frank Scholten, Detlef Koschny, Björn Davidsson, W-H. Ip, Marco Fulle, Nicolas Thomas, M. R. El Maarry, Cecilia Tubiana, Monica Lazzarin, Ekkehard Kührt, L. M. Lara, Raphael Marschall, J. L. Bertaux, H. U. Keller, Dennis Bodewits, R. Rodrigo, Laurent Jorda, G. Cremonese, M. De Cecco, P. Theologou, Olivier Groussin, ITA, USA, GBR, FRA, DEU, Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), 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), International Space Science Institute [Bern] (ISSI), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Università degli Studi di Padova = University of Padua (Unipd), Dipartimento di Fisica e Astronomia 'Galileo Galilei', CNR Istituto di Fotonica e Nanotecnologie [Padova] (IFN), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), 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), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), CNR Institute for Photonics and Nanotechnologies (IFN), Department of Industrial Engineering [Padova], University of Trento [Trento], INAF - Osservatorio Astronomico di Trieste (OAT), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institute of Astronomy [Taiwan] (IANCU), National Central University [Taiwan] (NCU), Space Science Institute [Macau] (SSI), Macau University of Science and Technology (MUST), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Universität Bern [Bern], 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), Universita degli Studi di Padova, Consiglio Nazionale delle Ricerche [Roma] (CNR), Max-Planck-Institut für Sonnensystemforschung (MPS), European Space Agency (ESA)-European Space Agency (ESA), California Institute of Technology (CALTECH)-NASA, 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), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), IMPEC - LATMOS, Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Technische Universität Braunschweig [Braunschweig], Swiss National Science Foundation, European Commission, and State Secretariat for Education, Research and Innovation (Switzerland)

Subjects
67P/Churyumov-Gerasimenko, Morphology, Surface (mathematics), 010504 meteorology & atmospheric sciences, Comet, Geometry, Surface finish, Table (information), 01 natural sciences, Nucleus, Computer graphics, Rosetta, 0103 physical sciences, medicine, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Subdivision, Astronomy and Astrophysics, Space and Planetary Science, business.industry, 520 Astronomy, 620 Engineering, medicine.anatomical_structure, es, [SDU]Sciences of the Universe [physics], business, Unit (ring theory), Geology
Abstract

Open Acces publication. This article is available under the Creative Commons CC-BY-NC-ND license and permits non-commercial use of the work as published, without adaptation or alteration provided the work is fully attributed., The previously defined regions on the nucleus of comet 67P/Churyumov-Gerasimenko have been mapped back onto the 3D SHAP7 model of the nucleus (Preusker et al., 2017). The resulting regional definition is therefore self-consistent with boundaries that are well defined in 3 dimensions. The facets belonging to each region are provided as supplementary material. The shape model has then been used to assess inhomogeneity of nucleus surface morphology within individual regions. Several regions show diverse morphology. We propose sub-division of these regions into clearly identifiable units (sub-regions) and a comprehensive table is provided. The surface areas of each sub-region have been computed and statistics based on grouping of unit types are provided. The roughness of each region is also provided in a quantitative manner using a technique derived from computer graphics applications. The quantitative method supports the sub-region definition by showing that differences between sub-regions can be numerically justified.© 2018 The Authors, The team from the University of Bern is supported through the Swiss National Science Foundation and through the NCCR PlanetS. The project has also received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 686709. This work was supported by the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number 16.0008-2.

Published
2018
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2. The geomorphology of (21) Lutetia: Results from the OSIRIS imaging system onboard ESA's Rosetta spacecraft

Author

Cesare Barbieri, Olivier Groussin, Ekkehard Kührt, M. Küppers, Matteo Massironi, Laurent Jorda, Jean-Baptiste Vincent, Simone Marchi, Holger Sierks, Stubbe F. Hviid, Mohamed Ramy El-Maarry, Colin Snodgrass, Elena Martellato, Hans Rickman, Richard Moissl, M. A. Barucci, R. Rodrigo, Cecilia Tubiana, Sonia Fornasier, Frank Scholten, Sebastien Besse, Katrin Stephan, K. P. Wenzel, H. U. Keller, F. Preusker, Detlef Koschny, Nicolas Thomas, Gabriele Cremonese, Francesco Marzari, P. L. Lamy, Physikalisches Institut [Bern], Universität Bern [Bern], 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), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Department of Physics and Astronomy [Uppsala], Uppsala University, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica, Dipartimento di Geoscienze [Padova], DLR Institute of Planetary Research, German Aerospace Center (DLR), 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), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre Jean Perrin [Clermont-Ferrand] (UNICANCER/CJP), UNICANCER, Imagerie Moléculaire et Thérapie Vectorisée (IMTV), Université d'Auvergne - Clermont-Ferrand I (UdA)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Cancéropôle CLARA-ITMO ' Technologies pour la Santé ', European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), European Space Astronomy Centre (ESAC), Universität Bern [Bern] (UNIBE), 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Università degli Studi di Padova = University of Padua (Unipd), Agence Spatiale Européenne = European Space Agency (ESA), and ITMO ' Technologies pour la Santé '-Cancéropôle CLARA-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université d'Auvergne - Clermont-Ferrand I (UdA)

Subjects
010504 meteorology & atmospheric sciences, Lineament, Data analysis, Terrain, 01 natural sciences, Imaging, Impact crater, Rosetta, 0103 physical sciences, Ejecta, 010303 astronomy & astrophysics, Geomorphology, 0105 earth and related environmental sciences, [PHYS]Physics [physics], geography, geography.geographical_feature_category, Asteroid, Astronomy and Astrophysics, Landslide, Geophysics, Radius, Lutetia, 13. Climate action, Space and Planetary Science, Ridge, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology
Abstract

International audience; The surface of (21) Lutetia is highly complex with significant interactions between ancient and more recent structures. This work attempts to summarize the surface geomorphology observed using the high resolution images from OSIRIS, the imaging system onboard the European Space Agency's Rosetta spacecraft. A wide range of surface morphologies are seen including heavily cratered terrain, extensive sets of lineaments, young impact craters, and a ridge, the height of which is more than 1/5th of the mean radius of the body. Very young and very old terrains (as inferred from crater densities) are seen in close proximity. The longest continuous lineament is over 80 km long. The lineaments show regional-dependent organization and structure. Several categories of lineament can be described. Lineaments radial to impact craters as seen on other asteroidal bodies are mostly absent. Although the lineaments may be of seismic origin (and possibly the result of several impact-induced events), impacts producing recent large craters place constraints on seismic phenomena. In particular, stronger attenuation of shocks than seen on other asteroidal bodies seems to be required. Inhomogeneous energy transport, possibly matching observed inhomogeneous ejecta deposition may offer explanations for some of the observed phenomena. Some impact craters show unusual forms, which are probably the result of impact into a surface with relief comparable to the resultant crater diameter and/or oblique impact. There is evidence that re-surfacing through landslides has occurred at several places on the object. (C) 2011 Elsevier Ltd. All rights reserved.

Published
2012

3. The advanced Moon micro-imager experiment (AMIE) on SMART-1: Scientific goals and expected results

Author

Karri Muinonen, Jean-Luc Josset, Yves Langevin, Pascale Ehrenfreund, Bernard Foing, P. Plancke, Stephane Beauvivre, M. C. De Sanctis, Beda A. Hofmann, Miguel Almeida, Zoran Sodnik, S. Chevrel, Patrick Pinet, M. Josset, Detlef Koschny, V. V. Shevchenko, Priscilla Cerroni, M. A. Barucci, Yu. G. Shkuratov, Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, Università degli Studi di Roma Tor Vergata [Roma], SPACE-X, Space Exploration Institute, Helsinki Observatory, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'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, 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), Astronomical Institute of Kharkov National University, Shternberg State Institute of Astronomy (SSIA), Power and Control Data division, ESA-ESTEC, Natural History Museum, Institut de Géologie de l'université de Neuchatel (IGUN), Leiden Observatory, and Space Science Department, European Space Agency

Subjects
geography, medicine.medical_specialty, geography.geographical_feature_category, Pixel, Detector, Astronomy and Astrophysics, South Pole–Aitken basin, Regolith, Spectral imaging, Volcano, Impact crater, Space and Planetary Science, medicine, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology, Remote sensing, Radio Science
Abstract

International audience; The advanced Moon micro-imager experiment (AMIE) is the imaging system on board ESA mission to the Moon SMART-1; it makes use of a miniaturised detector and micro-processor electronics developed by SPACE X in the frame of the ESA technical programme. The AMIE micro-imager will provide high resolution CCD images of selected lunar areas and it will perform colour imaging through three filters at 750, 915 and 960 nm with a maximum resolution of 46 m/pixel at the perilune of 500 km. Specific scientific objectives will include (1) imaging of high latitude regions in the southern hemisphere, in particular the South Pole Aitken basin (SPA) and the permanently shadowed regions close to the South Pole, (2) determination of the photometric properties of the lunar surface from observations at different phase angles (physical properties of the regolith), (3) multi-band imaging for constraining the chemical and mineral composition of the surface, (4) detection and characterisation of lunar non-mare volcanic units, (5) study of lithological variations from impact craters and implications for crustal heterogeneity. The AMIE micro-imager will also support a Laser-link experiment to Earth, an On Board Autonomous Navigation investigation and a Lunar libration experiment coordinated with radio science measurements.

Published
2005

4. Compositional type characterization of Rosetta asteroid candidates

Author

Alain Doressoundiram, C. A. Angeli, M. Florczak, Marcello Fulchignoni, Monica Lazzarin, and M. Antonietta Barucci

Subjects
Physics, Rosetta mission, Asteroid candidate, groundbased observations, Space and Planetary Science, Asteroid, Astronomy, Astronomy and Astrophysics, Characterization (materials science), Astrobiology
Abstract

The final selection of the two Rosetta target asteroids will be made in a successive phase of the Rosetta project development, when the engineering parameters will be frozen. In this paper we present spectroscopic observations of the possible Rosetta candidates and we discuss the results obtained, particularly the definition of their compositional type. We examine the possibility to select some more “primitive” candidates. On the basis of its size and spectral type, we suggest including the asteroid 140 Siwa as one of the asteroid targets of the Rosetta mission.

Published
1998

5. Rotational properties of main belt asteroids: photoelectric and CCD observations of 15 objects

Author

Mirel Birlan, Elisabetta Dotto, L. Perret, Andreas Nathues, M. Fulchignoni, Anders Erikson, M. Florczak, P. Thebault, and M. A. Barucci

Subjects
Physics, Space and Planetary Science, Asteroid, Astronomy and Astrophysics, Astrophysics, Remote sensing
Abstract

In this paper we present the results of several observational campaigns carried out during 1996 at the 1.2 m telescope of the Haute Provence Observatory (France) and at the 1.5m Danish, 0.9m Dutch, 0.6m Bochum and 0.5m telescopes of the European Southern Observatory (ESO, La Silla, Chile), in order to enlarge the available sample of know asteroid rotational periods. A total of 64 single night lightcurves for 15 asteroids were obtained. The rotational periods have been determined for 12 objects, with different quality code: 424 Gratia ( P syn = 19.47 h), 440 Theodora ( P syn = 4.828 h), 446 Aeternitas ( P syn = 15.85 h), 491 Carina ( P syn = 14.87 h), 727 Nipponia ( P syn = 4.6 h), 732 Tjilaki ( P syn = 12.34 h), 783 Nora ( P syn = 34.4 h), 888 Parysatis ( P syn = 5.49 h), 1626 Sadeya ( P syn = 3.438 h), 2209 Tianjin ( P syn = 9.47 h), 2446 Lunacharsky ( P syn = 3.613 h) and 3776 Vartiovuori ( P syn = 7.7 h). For 1246 Chaka, 1507 Vaasa and 1994 Shane the complete rotational phase was not covered and for two of them it was possible to find only an indication of the rotational period.

Published
1997

6. Rotational properties of asteroids: CCD observations of nine small asteroids

Author

M. Birlan, Alain Doressoundiram, M. A. Barucci, C. A. Angeli, and M. C. De Sanctis

Subjects
Telescope, Physics, Space and Planetary Science, Asteroid, law, Observatory, Astronomy, Astronomy and Astrophysics, law.invention
Abstract

The observational programme on small asteroids (diameter less than about 50 km) is continued to enlarge the available dataset of small asteroids. The results are presented of CCD observations of nine small asteroids ( D ≤23 km), performed in France with the 1.2 m telescope at Haute Provence Observatory and with the 2 m telescope at Pic du Midi Observatory. A total of 27 single night lightcurves for nine asteroids were obtained. All the objects were observed for the first time and rotational periods have been determined for all of the observed asteroids: 1992 Galvarino ( P syn = 7 h .004), 2419 Moldavia ( P syn = 2 h .412), 2921 Sophocles ( P syn = 4 h .778), 3247 Di Martino ( P syn = 5 h .445), 3623 Chaplin ( P syn = 8 h .361), 3986 Rozhkovskij ( P syn = 4 h .26), 4436 1983 EX ( P syn = 6 h .656), 5046 1981 DQ ( P syn = 6 h .050) and 1992 YG3 ( P syn = 8 h .91).

Published
1996

7. Fourier analysis of the lightcurves of 53 known pole asteroids

Author

M. A. Barucci, M. C. De Sanctis, M. Fulchignoni, and M. T. Capria

Subjects
ICARUS, Physics, education.field_of_study, Basis (linear algebra), Orientation (computer vision), business.industry, Population, Astronomy and Astrophysics, Astrophysics, Albedo, symbols.namesake, Optics, Space and Planetary Science, Asteroid, Fourier analysis, symbols, business, education, Fourier series
Abstract

The Fourier coefficients of 254 composite lightcurves of 53 asteroids are analysed, continuing a previous work (Barucci et al., Icarus 78 , 311–322, 1989), with the aim of inferring asteroidal shapes and possible albedo variegations. Coefficients are obtained only from good quality photometric data of asteroids for which a reliable estimate of the orientation of the spin axis is available. For each of the 53 asteroids an indicative shape is derived, on the basis of the coefficients resulting from the Fourier analysis. The shapes determined for 243 Ida and 951 Gaspra are confirmed by the Galileo images. Most of the analysed asteroids show a quasi-regular shape, probably due to a bias on the diameters of the sample; the remaining part, having smaller diameters, seems to show an irregular shape. The obtained results cannot be interpreted in a statistical sense but they can constitute a promising starting point for the understanding of the evolution of asteroidal population.

Published
1996

8. The slow rotation of 253 Mathilde

Author

Claes-Ingvar Lagerkvist, J.W. Young, Alan W. Harris, M. Antonietta Barucci, M. Dahlgren, Javier Licandro, J. Felix Lahulla, Gerhard Neukum, Beatrice E. A. Mueller, Stefano Mottola, Gil-Hutton Ricardo, C. A. Angeli, Gerhard Hahn, Anders Erikson, Bill Owen, and William D. Sears

Subjects
Rotation period, Physics, Photometry (astronomy), Amplitude, Slow rotation, Space and Planetary Science, Astronomy, Phase relation, Astronomy and Astrophysics, Astrophysics, Rotation, Color index
Abstract

CCD photometry of the NEAR mission fly-by target 253 Mathilde is presented. Measurements taken during 52 nights of observations, from February to June 1995, allow a rotation period of 17.406±0.010 days and a lightcurve amplitude of 0.45±0.02 mag to be determined. A B-V color index of 0.67±0.02 and a V-R of 0.35±0.02 are measured, which are compatible with C-type membership. The determination of the phase relation results in H = 10.28±0.03 and G = 0.12±0.06. Indications that the lightcurve is not strictly singly-periodic are found. A power-spectrum analysis detects a secondary frequency f 2 = 0.0322±0.0010 d −1 , which is interpreted as evidence for a complex rotation state.

Published
1995

9. A comparison of the G-mode and the three-parameter asteroid taxonomic classification techniques using a common data set

Author

M. Fulchignoni, M. Antonietta Barucci, and Edward F. Tedesco

Subjects
ICARUS, Data set, Astron, Space and Planetary Science, Asteroid, Yield (chemistry), Mode (statistics), Future application, Astronomy and Astrophysics, Biological classification, Algorithm, Mathematics
Abstract

A comparison of the G-mode (Barucci et al., Icarus 72, 304, 1987) and three-parameter (Tedesco et al., Astron. J. 97, 580, 1989) asteroid taxonomic classification systems is presented. Using a common data set we demonstrate that, at a 94% confidence level, the two methods yield the same classifications. We discuss the significance and future application of this result.

Published
1995

10. Ground-based Ida model: comparison with the first Galileo image

Author

M. Fulchignoni, Elisabetta Dotto, and M. A. Barucci

Subjects
ICARUS, Physics, Ground truth, Astronomy, Astronomy and Astrophysics, Astrobiology, Image (mathematics), Astron, symbols.namesake, Space and Planetary Science, Asteroid, Planet, Galileo (satellite navigation), symbols
Abstract

In this paper we present a model of the shape and surface features of the asteroid 243 Ida, second fly-by target of the Galileo mission. We obtained this model by applying the lightcurve inversion method (Fulchignoni and Barucci, B.A.A.S. 20, 866, 1988), already used for the model of 951 Gaspra (Barucci et al., Astron. Astrophys. 266, 385–394, 1992), on the whole sample of available lightcurves obtained during five oppositions between 1984 and 1993 (Binzel, Icarus 72, 135–208, 1987; Gonano-Beurer et al., Astron. Astrophys. 254, 393–396, 1992; Binzel et al., Icarus 105, 310–325, 1993; Mottola et al., Planet. Space Sci. 42, 21–25, 1994). The comparison of our model with the first Galileo image of 243 Ida gives another “ground truth” for the used method based on observations from the Earth.

Published
1995

11. Koronis family : reflectance spectra of 243 Ida, 1442 Corvina and 2226 Cunitza

Author

M. Lazzarin and M. A. Barucci

Subjects
asteroid family, Rotation period, Physics, spectroscopy, Reflection spectroscopy, Astronomy and Astrophysics, Astrophysics, space mission asteroid target, Reflectivity, Galileo spacecraft, Spectral line, Space and Planetary Science, Asteroid, Remote sensing
Abstract

Low-resolution spectra of the asteroids 243 Ida (target of the Galileo spacecraft on 28 August 1993), 1442 Corvina and 2226 Cunitza (other members of the Koronis family) were obtained. In the frame of a ground-based international campaign to observe Ida before the Galileo encounter (Binzel et al., Icarus, in press, 1993), we observed it spectroscopically in the visible at ESO-La Silla (Chile), obtaining four spectra covering the total rotational period (4.63 h). In one of these spectra, we observed a considerable variation in the depth of the absorption feature near 0.9 μ m, implying a different content of pyroxene and olivine on the surface of Ida. The spectra obtained for the other two objects are consistent with those of S-type asteroids and similar to that of Ida.

Published
1993

12. A spectroscopic survey of the small near-Earth asteroid population: Peculiar taxonomic distribution and phase reddening

Author

Irina Belskaya, Marcello Fulchignoni, Sonia Fornasier, Alain Doressoundiram, D. Perna, F. Merlin, M. A. Barucci, Marcel Popescu, C. Lantz, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Kharkiv], V.N. Karazin Kharkiv National University (KhNU), 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
Earth and Planetary Astrophysics (astro-ph.EP), Absolute magnitude, Solar System, education.field_of_study, Near-Earth object, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, New Technology Telescope, Early Earth, 01 natural sciences, Space and Planetary Science, Asteroid, Observatory, 0103 physical sciences, education, 010303 astronomy & astrophysics, Geology, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract

We present the results of the first-ever visible spectroscopic survey fully dedicated to the small (absolute magnitude H>20) near-Earth asteroid (NEA) population. Observations have been performed at the New Technology Telescope (NTT) of the European Southern Observatory (ESO), during a 30-night Guaranteed Time Observations programme, in the framework of the European Commission financed NEOShield-2 project. The visible spectra of 147 objects have been obtained and taxonomically classified. They show a peculiar taxonomic distribution, with respect to larger NEAs. In particular, olivine-rich A-types and organic-rich D-types are more abundant than what could be expected by extrapolating the taxonomic distribution of larger NEAs. Such results have implications for the investigation of the first phases of solar system history, including the delivery of prebiotic material on the early Earth. Having been obtained over a large range of solar phase angles, our data allowed us to evidence peculiar phase reddening behaviours for asteroids belonging to different taxonomic types. Low-albedo asteroids display no or limited phase reddening, compared to moderate- and high-albedo objects. This result suggests a promising novel way to distinguish primitive asteroids in the X-complex. In agreement with previous laboratory experiments, olivine-rich surfaces are the most affected by phase reddening., Accepted for publication in Planetary and Space Science. 22 pages, 6 figures

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