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1. The EPN-TAP protocol for the Planetary Science Virtual Observatory

Author

N. Bourrel, P. Le Sidaner, Marco Giardino, Jérôme Berthier, Marco Molinaro, F. Henry, Nathalie André, Stéphane Erard, C. Jacquey, Baptiste Cecconi, M. Gangloff, F. Topf, 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, Université Paris sciences et lettres (PSL), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Laboratoire GEOSITLAB Dipartimento delle Scienze della Terra, Università degli studi di Torino = University of Turin (UNITO), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-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 -Institut de Recherche pour le Développement (IRD)-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 -Centre National de la Recherche Scientifique (CNRS), Archéologies d'Orient et d'Occident et Sciences des textes (AOROC), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Università degli studi di Torino (UNITO), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École pratique des hautes études (EPHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Laboratoire d’Océanologie et de Géosciences (LOG) - UMR 8187 (LOG), Université de Lille-Université du Littoral Côte d'Opale-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE)-École normale supérieure - Paris (ENS Paris)

Subjects
Standards, 010504 meteorology & atmospheric sciences, Computer science, FOS: Physical sciences, Virtual observatory, 01 natural sciences, Set (abstract data type), 0103 physical sciences, Data services, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Protocol (object-oriented programming), 0105 earth and related environmental sciences, [PHYS]Physics [physics], Information retrieval, Astronomy and Astrophysics, Virtual Observatory, Computer Science Applications, Planetary science, Data access, Data model, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Table (database), Solar System, Data as a service, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Planetary Science
Abstract

A Data Access Protocol has been set up to search and retrieve Planetary Science data in general. This protocol will allow the user to select a subset of data from an archive in a standard way, based on the IVOA Table Access Protocol (TAP). The TAP mechanism is completed by an underlying Data Model and reference dictionaries. This paper describes the principle of the EPN- TAP protocol and interfaces, underlines the choices that have been made, and discusses possible evolutions., 21 pages. Submitted to Astronomy & Computing, S.I. Virtual Observatory

Published
2014
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2. Physical and dynamical properties of the main belt triple Asteroid (87) Sylvia

Author

Jérôme Berthier, Benoit Carry, Josef Ďurech, F. Marchis, F. Vachier, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), SETI Institute, Astronomical Institute of Charles University, Charles University [Prague] (CU), Based on observations collected at the European Southern Observatory, Paranal, Chile (089.C-0944, 087.C-0014, 385.C-0089, 085.C-0480, 077.C-0422, 074.C-0052), at the Gemini North Observatory in Hawaii, and at the W. M. Keck Observatory. The Keck observatory was made possible by the generous financial support of the W. M. Keck Foundation., Université Pierre et Marie Curie - Paris 6 (UPMC)-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 de Lille-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Epoch (astronomy), [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, 01 natural sciences, Occultation, Orbit determination, Photometry, Photometry (optics), Position (vector), Primary (astronomy), 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Mass distribution, Astronomy, Astronomy and Astrophysics, Satellites of asteroids, Asteroids, Space and Planetary Science, Asteroid, Occultations, Adaptive optics, Astrophysics - Earth and Planetary Astrophysics
Abstract

International audience; We present the analysis of high angular resolution observations of the triple Asteroid (87) Sylvia collected with three 8-10 m class telescopes (Keck, VLT, Gemini North) and the Hubble Space Telescope. The moons' mutual orbits were derived individually using a purely Keplerian model. We computed the position of Romulus, the outer moon of the system, at the epoch of a recent stellar occultation which was successfully observed at less than 15 km from our predicted position, within the uncertainty of our model. The occultation data revealed that the Moon, with a surface-area equivalent diameter Ds=23.1±0.7km, is strongly elongated (axes ratio of 2.7±0.32.7±0.3), significantly more than single asteroids of similar size in the main-belt. We concluded that its shape is probably affected by the tides from the primary. A new shape model of the primary was calculated combining adaptive-optics observations with this occultation and 40 archived light-curves recorded since 1978. The difference between the J2=0.024-0.009+0.016 derived from the 3-D shape model assuming an homogeneous distribution of mass for the volume equivalent diameter Dv=273±10km primary and the null J2 implied by the Keplerian orbits suggests a non-homogeneous mass distribution in the asteroid's interior.

Published
2014
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3. New insights on the binary Asteroid 121 Hermione

Author

Mikko Kaasalainen, P. Baudouin, Pascal Descamps, Franck Marchis, Raoul Behrend, Marcelo Assafin, Melissa C. Nysewander, J. B. Haislip, F. Manzini, Josh Emery, S. Sposetti, A. Peyrot, Daniel E. Reichart, Julio Camargo, Felipe Braga-Ribas, Alan W. Harris, Joe Pollock, K. M. Ivarsen, Roberto Vieira-Martins, F. Colas, Frédéric Vachier, L. Hutton, J. Greene, J. Lecacheux, L. Brunetto, Jérôme Berthier, Aaron P. LaCluyze, J. Durech, R. Roy, J. A. Crain, J.-P. Teng-Chuen-Yu, L. Bernasconi, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, SETI Institute, Astronomical Institute of Charles University, Charles University [Prague] (CU), Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], DLR Institute of Planetary Research, German Aerospace Center (DLR), Department of Mathematics and Statistics, Makes Observatory, Department of Physics and Astronomy [Boone], Appalachian State University, University of North Carolina System (UNC)-University of North Carolina System (UNC), Observatório do Valongo/UFRJ [Rio de Janeiro], Universidade Federal do Rio de Janeiro (UFRJ), Observatório Nacional/MCT, Observatório do Valongo, Universidade Federal do Rio de Janeiro Ladeira do Pedro Antônio, Department of Physics and Astronomy [Chapel Hill], University of North Carolina [Chapel Hill] (UNC), Geneva Observatory, University of Geneva [Switzerland], 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), Les Engarouines Observatory, Blauvac Observatory, Harfleur Observatory, Chercheur indépendant, Gnosca Observatory, Stazione Astronomica di Sozzago, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Université de Genève = University of Geneva (UNIGE), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Astronomy Department [Berkeley], Charles University [Prague], German Aerospace Center ( DLR ), Department of Physics and Astronomy, Universidade Federal do Rio de Janeiro [Rio de Janeiro] ( UFRJ ), The University of North Carolina at Chapel Hill, Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), and 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 )

Subjects
Solar System, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Eclipses, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Asteroids: rotation, Equinox, surfaces, eclipses, rotation, 01 natural sciences, law.invention, Photometry, Photometry (optics), Telescope, satellites, Spitzer Space Telescope, law, 0103 physical sciences, Adaptive optics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy, Astronomy and Astrophysics, Light curve, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Asteroids, [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Space and Planetary Science, Asteroid, Satellites of Asteroids, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report on the results of a six-month photometric study of the main-belt binary C-type asteroid 121 Hermione, performed during its 2007 opposition. We took advantage of the rare observational opportunity afforded by one of the annual equinoxes of Hermione occurring close to its opposition in June 2007. The equinox provides an edge-on aspect for an Earth-based observer, which is well suited to a thorough study of Hermione's physical characteristics. The catalog of observations carried out with small telescopes is presented in this work, together with new adaptive optics (AO) imaging obtained between 2005 and 2008 with the Yepun 8-m VLT telescope and the 10-m Keck telescope. The most striking result is confirmation that Hermione is a bifurcated and elongated body, as suggested by Marchis et al., (2005). A new effective diameter of 187 +/- 6 km was calculated from the combination of AO, photometric and thermal observations. The new diameter is some 10% smaller than the hitherto accepted radiometric diameter based on IRAS data. The reason for the discrepancy is that IRAS viewed the system almost pole-on. New thermal observations with the Spitzer Space Telescope agree with the diameter derived from AO and lightcurve observations. On the basis of the new AO astrometric observations of the small 32-km diameter satellite we have refined the orbit solution and derived a new value of the bulk density of Hermione of 1.4 +0.5/-0.2 g cm-3. We infer a macroscopic porosity of ~33 +5/-20%., Comment: 39 pages, 4 Tables, 8 figures

Published
2009
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4. New determination of the size and bulk density of the binary Asteroid 22 Kalliope from observations of mutual eclipses

Author

Magdalena Polińska, A. Devyatkin, A.W. Harris, F. Marchis, J.-F. Coliac, E. M. Cooper, D. Gorshanov, Jérôme Berthier, P. Descamps, Mikko Kaasalainen, Joe Pollock, Agnieszka Kryszczyńska, Michael H. Wong, Frédéric Vachier, M. Birlan, P. Wiggins, K. A. Kettner, W. Romanishin, I. Verestchagina, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, SETI Institute, Department of Physics and Astronomy [Boone], Appalachian State University, University of North Carolina System (UNC)-University of North Carolina System (UNC), Department of Mathematics and Statistics, DLR Institute of Planetary Research, German Aerospace Center (DLR), H. L. Dodge Department of Physics and Astronomy [Norman], University of Oklahoma (OU), Wiggins Observatory, Central Astronomical Observatory, Russian Academy of Sciences [Moscow] (RAS), Observatoire de la Farigourette, 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 de Lille-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)

Subjects
Asteroid surfaces, Solar System, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Eclipses, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Binary number, Eclipse season, Astrophysics, Orbit plane, rotation, 01 natural sciences, Photometry, Photometry (optics), Asteroids surfaces, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Line-of-sight, Astrophysics (astro-ph), Astronomy, Astronomy and Astrophysics, Satellites of asteroids, Bulk density, Asteroids, Space and Planetary Science, Asteroid
Abstract

In 2007, the M-type binary asteroid 22 Kalliope reached one of its annual equinoxes. As a consequence, the orbit plane of its small moon, Linus, was aligned closely to the Sun's line of sight, giving rise to a mutual eclipse season. A dedicated international campaign of photometric observations, based on amateur-professional collaboration, was organized and coordinated by the IMCCE in order to catch several of these events. The set of the compiled observations is released in this work. We developed a relevant model of these events, including a topographic shape model of Kalliope refined in the present work, the orbit solution of Linus as well as the photometric effect of the shadow of one component falling on the other. By fitting this model to the only two full recorded events, we derived a new estimation of the equivalent diameter of Kalliope of 166.2+/-2.8km, 8% smaller than its IRAS diameter. As to the diameter of Linus, considered as purely spherical, it is estimated to 28+/-2 km. This substantial "shortening" of Kalliope gives a bulk density of 3.35+/-0.33g/cm3, significantly higher than past determinations but more consistent with its taxonomic type. Some constraints can be inferred on the composition., 59 pages, 8 tables, 15 figures submitted to Icarus

Published
2008
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5. Mass and density of Asteroid 121 Hermione from an analysis of its companion orbit

Author

Jérôme Berthier, Conor Laver, Daniel Hestroffer, P. Descamps, I. de Pater, Franck Marchis, Department of Astronomy, University of California, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Groupe Astrométrie et Planétologie (GAP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
Physics, Orbital elements, Solar System, Space and Planetary Science, Asteroid, Planet, Synchronous orbit, Equator, Ecliptic, Astronomy, Astronomy and Astrophysics, Circular orbit, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We report on Adaptive Optics observations of the satellite of Asteroid 121 Hermione with the ESO-Paranal UT4 VLT and the Keck AO telescopes. The binary system, belonging to the Cybele family, was observed during two observing campaigns in January 2003 and January 2004 aiming to confirm its trajectory and accurately determine its orbital elements. A precessing Keplerian model was used to describe the motion of S/2002 (121) 1. We find that the satellite of Hermione revolves at a = 768 ± 11 km from the primary in P = 2.582 ± 0.002 days with a roughly circular and prograde orbit (e = 0.001 ± 0.001, i = 3 ± 2 ◦ w.r.t. equator primary). These extensive astrometric measurements enable us to determine the mass of Hermione to be 0.54 ± 0.03 × 10 19 kg and its pole solution (λ0 = 1.5 ◦ ± 2.00, β0 = 10 ◦ ± 2.0 in ecliptic J2000). Additional Keck AO observations taken close to the asteroid opposition in December 2003 give us direct insight into the structure of the primary which presents a bilobated shape. Since the angular resolution is limited to the theoretical angular resolution of the telescope (43 mas corresponding to a spatial resolution of 80 km), two shape models (called snowman and peanut) are proposed based on the images which were deconvolved with MISTRAL deconvolution process. Assuming a purely synchronous orbit and knowing the mass of the primary, the peanut shape composed of two separated components is quite unlikely. Additionally the J2 calculated from the analysis of the secondary orbit is not in agreement with the peanut model, but close to the snowman shape. The bulk density of the primary as derived from the observed size of the snowman shape is estimated to ρ ∼ 1.8 ± 0. 2g /cm 3 implying a porosity ∼14% for this C-type asteroid, corresponding to a fractured asteroid. Considering the IRAS diameter, the density is lower ( ρ = 1.1 ± 0. 3g /cm 3 ) leading to a high porosity (p = 30–60%) with a nominal value of p = 48%, which indicates a completely loose rubble-pile structure for the primary. Further work is necessary to better constrain the size, shape, and then internal structure of Hermione’s primary.  2005 Elsevier Inc. All rights reserved.

Published
2005
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6. First ground-based astrometric observations of Puck

Author

Claude Le Guyader, Franck Marchis, Pascal Descamps, Jérôme Berthier, R. Prange, and Thierry Fusco

Subjects
Physics, Orbital elements, media_common.quotation_subject, General Engineering, Uranus, Energy Engineering and Power Technology, Astronomy, Astrometry, Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Natural satellite, Astrophysics::Earth and Planetary Astrophysics, Eccentricity (behavior), Adaptive optics, media_common
Abstract

The ten small inner moons of Uranus, discovered in 1986, have so far only been studied from space (Voyager 2, HST). The orbital elements derived from the observations indicate very weakly eccentric orbits for all of them but one (Ophelia). We present here the first ground-based astrometric observations of Puck, performed using an Adaptive Optics system. The long observing sequences permitted by ground-based facilities at ESO-La Silla, Chile (64.S-0289) revealed an eccentricity 100 times larger than previously believed. Such a disagreement with the actual theory may arise from the reduction itself based on the bright moons of Uranus, considered until now as precise astrometric references. To cite this article: P. Descamps et al., C. R. Physique 3 (2002) 121–128

Published
2002
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