Search

Your search keyword '"Jakokoski Observatory, University of Helsinki"' showing total 17 results
Start Over Author "Jakokoski Observatory, University of Helsinki"
17 results on '"Jakokoski Observatory, University of Helsinki"'

1. Olivine-rich asteroids in the main asteroid belt

Author

Demeo, Francesca E., Polishook, David, Benoit Carry, Moskovitz, Nick, Burt, Brian, Binzel, Rick, Massachusetts Institute of Technology, Jakokoski Observatory, University of Helsinki, 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), Astéroïdes, comètes, météores et éphémérides (ACME), 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, and Lowell Observatory, Flagstaff

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

International audience; Olivine-dominated asteroids, classified as A-types with near-infrared spectral measurements are largely thought to be the mantle remnants of disrupted differentiated small bodies. These A-type asteroids hold clues to asteroid differentiation and to the collisional history of those differentiated bodies. Preliminary studies of the abundance and distribution of A-type asteroids were performed by Carvano et al. (2010) and DeMeo & Carry (2013, 2014) using the Sloan Digital Sky Survey (SDSS). To confidently identify these olivine-dominated A-type asteroids, however, near-infrared spectral measurements are needed to identify the distinct broad and deep 1-micron olivine absorption feature. Using the Sloan Digital Sky Survey Moving Object Catalog to select A-type asteroid candidates, we have performed a near-infrared spectral survey of over 70 asteroids with SpeX on the IRTF. We present the abundance and distribution of A-type asteroids throughout the main asteroid belt and compare these results with similar surveys for basalt-rich V-type asteroids (e.g. Moskovitz et al. 2008). This work is supported by NASA under grant number NNX12AL26G issued through the Planetary Astronomy Program.

Published
2015

2. IAU Working Group for Numerical Standards of Fundamental Astronomy (NSFA): Past Efforts and Future Endeavors

Author

Luzum, Brian, Capitaine, Nicole, Fienga, Agnès, Folkner, William M., Fukushima, Toshio, Heinkelmann, Robert, Hilton, James L., Hohenkerk, Catherine, Petit, Gérard, Pitjeva, Elena V., Soffel, Michael, Wallace, Patrick, US Naval Observatory, Systèmes de Référence Temps Espace (SYRTE), 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)-Centre National de la Recherche Scientifique (CNRS), Rotation de la Terre et géodésie spatiale, 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)-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), 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), Astronomie et systèmes dynamiques (ASD), 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, Jet Propulsion Laboratory, California Institute of Technology (JPL), National Astronomical Observatory of Japan, European Southern Observatory (ESO), HM Nautical Almanac Office, Bureau International des Poids et Mesures (BIPM), Institute of Applied Astronomy RAS, Jakokoski Observatory, University of Helsinki, and STFC Rutherford Appleton Laboratory

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

International audience; In 2006, the International Astronomical Union (IAU) General Assembly (GA) established the Working Group (WG) for Numerical Standards of Fundamental Astronomy (NSFA). The NSFA WG Current Best Estimates (CBEs) were adopted at the 2009 IAU GA in Resolution B2 as the IAU (2009) System of Astronomical Constants. The IAU 2012 Resolution on the re-definition of the au was proposed by the NSFA WG. Since then, the WG has concentrated on establishing the process for maintaining the CBEs in an effort to provide a service for the IAU. The NSFA web presence documents both the IAU (2009) System of Astronomical Constants and the CBEs. All old pages of the CBEs are archived in order to document history of the CBEs. The CBE policy documents the procedures established for proposal, discussion, and voting for the adoption of new CBEs. The talk reviews the efforts of the WG and provides insight into future efforts.

Published
2015

3. Report of the IAU/IAG Working Group on Cartographic Coordinates and Rotational Elements: 2003

Author

Dale P. Cruikshank, Philip J. Stooke, David J. Tholen, James L. Hilton, Michael F. A'Hearn, P. K. Seidelmann, Peter C. Thomas, Juergen Oberst, J. L. Simon, Brent A. Archinal, H. U. Keller, University of Virginia, U.S. Geological Survey, University of Maryland, Stratospheric Observatory for Infrared Astronomy, Universities Space Research Association, NASA/Ames Research Center, Jakokoski Observatory, University of Helsinki, MPI Aeronomie, DLR Berlin Adlershof, 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), University of Western Ontario, University of Hawaii, and Center for Radiophysics and Space Research, Cornell University (CRSR)

Subjects
Astrophysics and Astronomy, Satellites, Planets, Rotation periods, Planet, Group (periodic table), Comets, Mathematical Physics, Web site, Geography, Applied Mathematics, Astronomy and Astrophysics, Mars Exploration Program, Asteroids, Computational Mathematics, Space and Planetary Science, Asteroid, Modeling and Simulation, Rotation axes, Reference surface, Sizes, Shapes, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cartographic coordinates, Cartography, Rotation (mathematics), Geology
Abstract

International audience; Every three years the IAU/IAG Working Group on Cartographic Coordinates and Rotational Elements revises tables giving the directions of the north poles of rotation and the prime meridians of the planets, satellites, and asteroids. This report introduces a system of cartographic coordinates for asteroids and comets. A topographic reference surface for Mars is recommended. Tables for the rotational elements of the planets and satellites and size and shape of the planets and satellites are not included, since there were no changes to the values. They are available in the previous report (Celest. Mech. Dyn. Astron., 82, 83 110, 2002), a version of which is also available on a web site.

Published
2005
Full Text
View/download PDF

4. Tidal Despinning of Iapetus, the Eighth Satellite of Saturn

Author

Efroimsky, Michael, Lainey, Valéry, Castillo-Rogez, Julie C., Williams, James G., Jakokoski Observatory, University of Helsinki, 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), and Jet Propulsion Laboratory, California Institute of Technology (JPL)

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

International audience; While currently Iapetus is locked into a 1:1 spin-orbit resonance with Saturn, its original state was likely one of rapid rotation. Simulations (Aleshkina 2009) have demonstrated that: (1) with a high arbitrariness in the initial conditions, Iapetus had passed without delay through the 5:2, 2:1, and 3:2 spin-orbit commensurabilities, and (2) its tidal-despinning time was about hundred billion years, an unphysical result for a moon in a spin-orbit lock. (For the other large satellites of Saturn these times are shorter by orders of magnitude.) Hence the necessity to seek efficient tidal-despinning mechanisms.

Published
2009

5. Polarimetry of the dwarf planet (136199) Eris

Author

Karri Muinonen, Irina Belskaya, Sonia Fornasier, Ludmilla Kolokolova, G. P. Tozzi, Stefano Bagnulo, Maria Antonietta Barucci, Astronomical Institute of Kharkov National University, 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), Armagh Observatory, College Hill, Jakokoski Observatory, University of Helsinki, INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), Université Paris Cité (UPCité), and University of Maryland

Subjects
Absolute magnitude, Brightness, Opposition surge, 010504 meteorology & atmospheric sciences, Dwarf planet, Polarimetry, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Eris, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, biology, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, biology.organism_classification, Pluto, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We investigate the surface characteristics of the large dwarf planet (136199) Eris. With the FORS1 instrument of the ESO VLT, we have obtained Bessell broadband R linear polarimetry and broadband V and I photometry. We have modelled the observations in terms of the coherent-backscattering mechanism to constrain the surface properties of the object. Polarimetric observations of Eris show a small negative linear polarization without opposition surge in the phase angle range of 0.15-0.5 degrees. The photometric data allow us to suppose a brightness opposition peak at phase angles below 0.2-0.3 degrees. The data obtained suggest possible similarity to the polarimetric and photometric phase curves of Pluto. The measured absolute magnitude and broadband colors of Eris are H_V=-1.15, V-R=0.41, and V-I=0.75., Accepted by A&A

Published
2007
Full Text
View/download PDF

6. Molecular oxygen in the rho Ophiuchi cloud

Author

Nicholas F. H Tothill, Alain Klotz, René Liseau, P. A. Feldman, Christine D. Wilson, Maryvonne Gerin, N. Biver, Steve Torchinsky, G. F. Gahm, Cathy Horellou, H. G. Floren, George F. Mitchell, Alain Lecacheux, Laurent Pagani, Urban Frisk, G. Olofsson, John H. Black, Georg Witt, V. Buat, E. Kyroelae, Gérard Mégie, G. Serra, Hans Rickman, Roy Booth, Tatsuhiko I. Hasegawa, L. Nordh, Aa. Hjalmarson, Peter F. Bernath, Anders Winnberg, Per Bergman, L.-Aa. Nyman, L. E. B. Johansson, Gustaf Rydbeck, A. O. H. Olofsson, P. J. Encrenaz, Kevin Volk, G. Persson, E. Falgarone, M. Fich, Michael Olberg, I. Ristorcelli, S. Lundin, Aa. Sandqvist, Fredrik von Schéele, Magnus Dahlgren, Rene Plume, Donal P. Murtagh, M. Hagstroem, Charles L. Curry, Bengt Larsson, Hans Olofsson, Sun Kwok, Jacques Crovisier, Tommy Wiklind, Kay Justtanont, E. J. Llewellyn, Jorma Harju, Mathias Fredrixon, T. Liljestroem, Stockholm Observatory, AlbaNova University Center, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Onsala Space Observatory, Chalmers University of Technology (OSO), Department of Physics, University of Waterloo, 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), Physique des plasmas, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), Laboratoire d'Astronomie Spatiale (LAS), Centre National de la Recherche Scientifique (CNRS), National Research Council of Canada (NRC), Swedish Space Corporation (SSC), Jakokoski Observatory, University of Helsinki, University of Calgary, Centre d'étude spatiale des rayonnements (CESR), 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), Finnish Meteorological Institute (FMI), Metsähovi Radio Observatory, University of Saskatchewan [Saskatoon] (U of S), Institut Pierre-Simon-Laplace (IPSL (FR_636)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Department of Astronomy and Physics, Saint Mary's University, Global Environmental Measurements Group, Swedish National Space Board (SNSB), APEX team, ESO, Santiago, Uppsala Astronomical Observatory, Canadian Space Agency (CSA), Department of Physics and Astronomy, McMaster University, and Department of Meteorology, Stockholm University

Subjects
Physics, Molecular cloud, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Spectral line, Interstellar medium, Chemical species, Space and Planetary Science, Satellite, Ground state, Spectroscopy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Line (formation)
Abstract

Molecular oxygen, O2 has been expected historically to be an abundant component of the chemical species in molecular clouds and, as such, an important coolant of the dense interstellar medium. However, a number of attempts from both ground and from space have failed to detect O2 emission. The work described here uses heterodyne spectroscopy from space to search for molecular oxygen in the interstellar medium. The Odin satellite carries a 1.1 m sub-millimeter dish and a dedicated 119 GHz receiver for the ground state line of O2. Starting in 2002, the star forming molecular cloud core rho Oph A was observed with Odin for 34 days during several observing runs. We detect a spectral line at v(LSR) = 3.5 km/s with dv(FWHM) = 1.5 km/s, parameters which are also common to other species associated with rho Ohp A. This feature is identified as the O2 (N_J = 1_1 - 1_0) transition at 118 750.343 MHz. The abundance of molecular oxygen, relative to H2,, is 5E-8 averaged over the Odin beam. This abundance is consistently lower than previously reported upper limits., Comment: 10 pages, 11 figures, accepted for publication in A&A

Published
2007
Full Text
View/download PDF

7. Exploring the surface properties of Transneptunian Objects and Centaurs with polarimetric FORS1/VLT observations

Author

Karri Muinonen, Maria Antonietta Barucci, Ludmilla Kolokolova, Hermann Boehnhardt, Stefano Bagnulo, Irina Belskaya, European Southern Observatory, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Jakokoski Observatory, University of Helsinki, University of Maryland, Astronomical Institute of Kharkov National University, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Physics, Solar System, Photon, 010504 meteorology & atmospheric sciences, Scattering, Astrophysics (astro-ph), Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Coherent backscattering, Astrophysics, Polarization (waves), 01 natural sciences, Regolith, Light scattering, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

Polarization is a powerful remote-sensing method to investigate solar system bodies. It is an especially sensitive diagnostic tool to reveal physical properties of the bodies whose observational characteristics are governed by small scatterers (dust, regolith surfaces). For these objects, at small phase angles, a negative polarization is observed, i.e., the electric vector E oscillates predominantly in the scattering plane, contrary to what is typical for rather smooth homogeneous surfaces. The behavior of negative polarization with phase angle depends on the size, composition and packing of the scatterers. These characteristics can be unveiled by modelling the light scattering by the dust or regolith in terms of the coherent backscattering mechanism. We have investigated the surface properties of TNOs and Centaurs by means of polarimetric observations with FORS1 of the ESO VLT. TNOs Ixion and Quaoar, and Centaur Chiron show a negative polarization surge. The Centaur Chiron has the deepest polarization minimum (-1.5 - 1.4%). The two TNOs show differing polarization curves: for Ixion, the negative polarization increases rapidly with phase; for Quaoar, the polarization is relatively small (~ -0.6%), and nearly constant at the observed phase angles. For all three objects, modelling results suggest that the surface contains an areal mixture of at least two components with different single-scatterer albedos and photon mean-free paths., 11 pages, 7 postscript figures, accepted by A&A; astro-ph abstract has been replaced with a more complete one

Published
2006
Full Text
View/download PDF

8. Multiplicity in the Jupiter Trojan Population: Low density of 617 Patroclus with Keck LGS AO and Perspective

Author

Marchis, Franck, Hestroffer, Daniel, Descamps, Pascal, Berthier, Jerôme, Bouchez, A. H., Campbell, Randall D., Chin, J. C. Y., van Dam, Marcos A., Hartman, Scott K., Johnasson, E. M., Lafon, Robert E., Le Mignant, David, de Pater, Imke, Stomski, Paul J., Summers, D. M., Wizinovich, Peter L., Wong, Michael H., UC-Berkeley, 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), 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, California Institute of Technology, Department of Astronomy (CALTECH), Jakokoski Observatory, University of Helsinki, and Henry, Florence

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

International audience; The system 617 Patroclus, the only binary Trojan known, was discovered in 2001 with the Hokupa'a Gemini-8m AO system. Because of their faintness (magnitude in visible mv>15.5), Trojan asteroids cannot be directly observed by most of the AO systems. In 2004, a Laser Guide Star (LGS) AO system was offered on the Keck-10m. We initiated an observing campaign, recording direct images of the 617 Patroclus double system in broadband filters with the NIRC2 near-infrared camera. The orbital parameters of the system were estimated using two methods and by including additional Gemini archive data (2001-2002), we obtained a consistent and accurate solution. The two components, separated by 680±20 km, revolve around their center of mass in 4.289±0.004 days in a roughly circular orbit (e ˜0.02-0.02). Using the thermal measurements by Fernandez et al. (2003), we derive (with a beaming parameter eta =0.94) a radius of R1= 60.9 km and R2= 56.3 km (with an error of 1.6 km and an Av= 0.04). Even considering the uncertainty in the volume of the components, the density of 617 Patroclus (rho = 0.8±0.15 g/cm3) is extremely low, if compared with the bulk-density of known binary C-type main-belt asteroids (rho 1.2 g/cm3, see Marchis et al., ACM, 2005). Assuming that the system is made of the same material as Ganymede or Callisto (uncompressed density of 1.6 g/cm3), the bulk density yields to a macro-porosity of ˜50%. A more realistic smaller porosity (p ˜15 different composition, such as more water ice in the interior of 617 Patroclus, suggesting a formation in the distant outer regions of the solar system (Morbidelli et al., Nature, 2005). The origin of this tightly bound system will be also discussed (Marchis et al., Nature, in press, 2005). We will present a quality comparison of the LGS Keck system with various techniques and different AO systems, discussing the interest of this technique to broaden the search for multiple asteroids in all minor planet populations.

Published
2006

9. Four new binary minor planets: (854) Frostia, (1089) Tama, (1313) Berna, (4492) Debussy

Author

A. Klotz, P. Antonini, M. Lavayssière, F. Colas, L. Bernasconi, F. Manzini, M. Vignand, E. Pimentel, A. Cazenave, Tommi Itkonen, Gianluca Masi, Felix Hormuth, R. Michelsen, A. Leroy, Ch. Demeautis, Donn R. Starkey, N. Waelchli, E. Brochard, S. Sposetti, Raoul Behrend, C. Cavadore, R. Durkee, J. M. Coloma, J. Nomen, L. Kurtze, H. Berrouachdi, R. Roy, J. Dorseuil, Donald P. Pray, Pertti Pääkkönen, Arto Oksanen, E. Barbotin, N. Berger, E. Frappa, V. Cotrez, K. Augustesen, C. Jacques, J. Lecacheux, A. Laffont, G. Dubos, S. Sanchez, R. Aoun, J. P. Teng, C. Rinner, S. Deconihout, R. Stoss, D. Matter, A. Peyrot, K. Sonnenberg, Observatoire Astronomique de l'Université de Genève, Association des Utilisateurs de Détecteurs Electroniques (AUDE), Association des Utilisateurs de Détecteurs Electroniques, Observatoire des Engarouines, Observatoire de Blauvac, Centre d'étude spatiale des rayonnements (CESR), 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), Observatoire de Haute-Provence (OHP), 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)-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), 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), Observatoire de Bédoin, Association T60, Observatoire Midi-Pyrénées, Observatoire Midi-Pyrénées (OMP), 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)-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, Astronomical Observatory, NBIfAFG, Observatoire de St-Jean de Bournay, Observatoire astronomique des Makes, Agrupación Astronómica de Sabadell, Shed of Science Observatory, Planétarium de Saint-Etienne, Max-Planck-Institut für Astronomie (MPIA), Jakokoski Observatory, University of Helsinki, Centro de Estudos Astronômicos de Minas Gerais (CEAMIG), Darmstadt University of Technology, Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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), Stazzione Astronomica di Sozzago, Università degli Studi di Roma Tor Vergata [Roma], Ørsted DTU, Technical University of Denmark, Elektrovej, Observatori Astronómico de Mallorca, Camí de l'Observatori, Nyrölä Observatory (NYTT), Carbuncle Hill Observatory, Sternwarte Weinheim, Observatorio di Gnosca, DeKalb Observatory, and Observatoire François-Xavier Bagnoud

Subjects
Physics, education.field_of_study, Scattering, Synodic day, Population, Astronomy, Binary number, Astronomy and Astrophysics, Astrophysics, Light curve, Rotation, Space and Planetary Science, Planet, Asteroid, education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Context. Aims.We present evidence that four minor planets of the main belt are binary systems. Methods.These discoveries are based on CCD photometric measurements made by many observers coordinated in a network of observatories. Results.Orbital and physical properties are derived from a total of 134 partial light curves involving 26 stations. (854) Frostia, (1089) Tama, (1313) Berna, and (4492) Debussy show mutual eclipses features on their light curves. In all cases, rotation and revolution are synchronous. Synodic periods are 37.728, 16.444, 25.464 and 26.606 h respectively. From a simple model, we have derived their bulk densities as follows: 0.89 ± 0.14, 2.52 ± 0.30, 1.22 ± 0.15 and 0.91 ± 0.10 g cm-3 respectively. Uncertainties in the bulk densities, arising from scattering and shadow effects are not taken into account. These could increase the density estimates by a factor up to 1.6. Our method of determining bulk density is completely independent of their mass and their diameter estimates. The low rotational periods and the low bulk densities clearly imply a collisional process to explain this kind of binary asteroid. Based on our database of a few thousand light curves of minor planets, the population of similar-sized objects in the main belt is estimated to 6± 3 percent in the 10-50 km diameter class. Conclusions.

Published
2006
Full Text
View/download PDF

10. The Orbit of 617 Patroclus Binary Trojan System from Keck LGS AO observations

Author

Marchis, Franck, Hestroffer, Daniel, Descamps, Pascal, Berthier, Jerôme, Bouchez, A. H., Campbell, Randall D., Chin, J. C. Y., van Dam, Marcos A., Hartman, Scott K., Johansson, Erik M., Lafon, Robert E., Le Mignant, David, de Pater, Imke, Stomski, Paul J., Summers, D. M., Wizinovich, Peter L., Wong, Michael H., UC-Berkeley, 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), 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, California Institute of Technology, Department of Astronomy (CALTECH), Jakokoski Observatory, University of Helsinki, and Henry, Florence

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

International audience; We report the results from Laser Guide Star Adaptive Optics observations in 2004-2005 of 617 Patroclus using the NIRC2 camera at the W. M. Keck Observatory. An observing campaign which focuses on this only known binary Trojan asteroid, was initiated by our group. Both components of the system were detected at 5 different epochs between Nov. 2004 and May 2005 with an angular separation between 45 and 190 mas and a Dm ˜0.17. The orbital parameters were estimated independently using two algorithms, a Monte-Carlo technique (Hestroffer and Vachier, IAU-ACM, 2005), and a visual binary method (Descamps, Cel. Mech., 2005): a= 685±40 km, e = 0.02±0.02, P = 4.287±0.002 or P= 2.391±0.003 corresponding to a total mass of 1.4 x 1018 or 4.3 x 1018 ± 0.2 kg. Considering recent radiometric measurements by Fernandez et al., (AJ, 126, 2003), the radii of components would be R1= 60.9 km and R2=56.3 km (error ˜1.6 km and with eta =0.94), leading to an averaged bulk density of 0.8 or 2.6 ±0.1 g/cm3. The factor of ˜2 uncertainty in the period will be removed using additional observations from CADC archive (in progress).

Published
2005

11. Gaia: an unprecedented tool for Solar System Science

Author

Cellino, A., Tanga, P., Mignard, F., Oro, A., Daniel HESTROFFER, Muinonen, K., Petit, J. M., Thuillot, W., Gaia Solar System Working Group Team, INAF/Osservatorio Astronomico di Torino, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), 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), Jakokoski Observatory, University of Helsinki, Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

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

International audience; Detailed investigations of the capabilities of the Gaia mission have revealed its strong potential for the exploration of scientific issues related to Solar System. This satellite will be placed in the Earth L2 and is expected to provide ˜ 70 observations (composed of ultra-precise astrometric measurements and magnitudes) of all the celestial bodies brighter than V 20, over 5 years of nominal operation. The observed objects will include ˜ 5x105 Main Belt Asteroids, ˜ 103 Near Earth Objects, the bright Trans-Neptunian Ojects, several comets, and many of the natural satellites of the major planets. Gaia observations will be characterized by an unprecedented astrometric accuracy (better than 1 mas per observation at V 15), the availability of multi-band photometry, and the virtually perfect knowledge of the attitude of the spaceraft relatively to a global astrometric reference. This points constitute the real strength of the mission, allowing to determine accurate sizes for ˜ 1000 asteroids and masses for > 100 objects, an improvement of a factor ˜ 100 in the orbital elements uncertainties, spin pole, shapes, and rotation periods for nearly all the observed objects, and a simultaneous determination of the PPN beta parameter and of the solar J2. The amount of physical data available, that will increase of several orders of magnitude relatively to the present situation, can be considered as a revolutionary step in Solar System science.

Published
2005

12. Dark Halo Baryons not in Ancient White Dwarfs?

Author

Annie C. Robin, Céline Reylé, Jean-Charles Cuillandre, Yannick Mellier, M. Creze, Vishnu Mohan, H. J. McCracken, O. Le Fevre, Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Université de Bretagne Sud (UBS), Jakokoski Observatory, University of Helsinki, Canada-France-Hawaii Telescope, 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), INAF-Osservatorio Astronomico di Bologna (OABO), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Sion, Edward M., Vennes, Stéphane, Shipman, Harry L., UP State Observatory, Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Observatoire Astronomique de Marseille Provence (OAMP), and Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Solar mass, Milky Way, Dark matter, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gravitational microlensing, Galaxy, Dark matter halo, Baryonic dark matter, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Massive compact halo object, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract

International audience; Microlensing experiments support the hypothesis that part of the Milky Way dark halo is made of MACHOs of 0.5-0.8 solar mass. Ancient white dwarfs are generally considered as the most plausible candidates for such MACHOs. We report the results of a proper motion survey of 0.16 deg2 at high galactic latitude and 1.6 deg2 at intermediate latitude (VIRMOS survey) using the CFH telescope. Both surveys are complete to I=23. No candidates were found within the colour-magnitude-proper motion range where halo white dwarfs can be safely discriminated from any standard population. A robust range of scenarii for a galaxy halo made of only 3 to 5% in mass of ancient white dwarfs predicts the detection of at least 3 such objects in our survey if the halo is at least 14 Gyr old (more if younger). The recent limit of 13.5 Gyr set by WMAP on the age of first stars forces one to disregard schemes with an older halo. We conclude that our observations rule out at the 95% significance level a fraction of ancient white dwarfs in the dark halo greater than 5%

Published
2005
Full Text
View/download PDF

13. Surface characterization of 28978 Ixion (2001 KX76)

Author

Boehnhardt, Hermann, Bagnulo, Stefano, Muinonen, Karri, Barucci, Maria Antonella, Kolokolova, L., Dotto, Elisabetta, Tozzi, Gian Paolo, Max-Planck-Institut für Astronomie (MPIA), European Southern Observatory, Jakokoski Observatory, University of Helsinki, 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), Department of Astronomy, University of Florida, INAF-Osservatorio Astronomico di Roma (INAF-OAR), and INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA)

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

International audience; The Plutino 28978 Ixion, one of the largest objects in the Kuiper Belt, is measured by R filter photometry and linear polarimetry over the phase angle range as well as by BVRI colours and visible spectroscopy. Ixion is a medium red object with spectral slope of 17.7%/100 nm (400-900 nm). While its opposition phase curve surge (0.2 mag/deg) is within the typical range found for other solar system objects, it displays unusually high negative polarization (min. -1.3%). Comparison with model spectra and numerical modeling of the opposition brightening and polarization effects suggest an areal mixture of absorbing (dark) and icy (bright) compounds on its surface: the mixing ratio is about 6:1 for dark and bright material of 0.21 and 0.79 single-scattering albedo and of 250 and 33 dimensionless mean free path (length multiplied by wave number), respectively.

Published
2004

14. Searching and Studying Binary Asteroids with AO Systems

Author

Marchis, Franck, Descamps, Pascal, Berthier, Jerôme, Hestroffer, Daniel, de Pater, Imke, Conrad, Al, Le Mignant, David, Chaffee, F., Gavel, Don T., UC-Berkeley, 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), 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, Jakokoski Observatory, University of Helsinki, and Moore Laboratory for AO at UCSC

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

International audience; Our group has conducted adaptive optics observations of asteroids since 2001. Our main goal is the search and study of binary asteroids using several AO systems (Lick, Keck, VLT) and related technique such as Appulse (Berthier and Marchis, 2002) and Laser Guide Star observations (Marchis et al., AGU-EGS, 2003) to broaden the sample of asteroids observed from the main-belt out to the Kuiper Belt. We focussed our program last year on Trojan Asteroids. Six of them were observed using Appulses with Keck AO ( ˜0.05-0.10", mv=15.4-18.5), 6 with the LGS at Lick ( ˜0.25-0.35", mv

Published
2003

15. Remote sensing of asteroids: large population sample from photometric and other data

Author

Kaasalainen, M., Alberto Cellino, Durech, J., Hestroffer, D., Michalowski, T., Pravec, P., Tanga, P., Torppa, J., Warner, B., Jakokoski Observatory, University of Helsinki, INAF-Osservatorio Astrofisico di Torino (INAF-OATo), Astron. Institute, Charles Univ., Prague, Czech Republic, 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), Adam Mickiewicz University in Poznań (UAM), Astron. Institute AS CR, Ondrejov, Czech Republic, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), and Palmer Divide Observatory, Colorado Springs

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

International audience; We review recent results of a project for building a large number of comprehensive physical asteroid models from combined photo- and interferometric observations, occultation timings, and other complementary data. Photometric data form the robust and stable basis for modelling, while particularly HST/FGS-interferometry and CW radar data can add local topographic information. We have built multidatainversion procedures that can efficiently combine such complementary data. We have also studied the specific characteristics and capabilities of the sources.

Published
2003

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

Author

Simon F. Green, Ian A. Franchi, M. Coradini, Jun'ichiro Kawaguchi, Elisabetta Dotto, Karri Muinonen, Jürgen Oberst, Hajime Yano, Jean-Luc Josset, John Robert Brucato, D. Agnolon, Hermann Böhnhardt, Antonella Barucci, Makoto Yoshikawa, J. Romstedt, Richard P. Binzel, Detlef Koschny, Patrick Michel, ESA-ESTEC, 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), JSPEC/ JAXA, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, INAF-Osservatorio Astrofisico di Arcetri (INAF-OAA), Agence Spatiale Européenne = European Space Agency (ESA), INAF-Osservatorio Astronomico di Roma (INAF-OAR), Open University, SPACE-X, Space Exploration Institute, Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Jakokoski Observatory, University of Helsinki, Institute for Planetary Sciences, DLR, and Massachusetts Institute of Technology, Cambridge

Subjects
Class (computer programming), Engineering, Near-Earth object, business.industry, Sample (statistics), Space (commercial competition), Object (philosophy), Astrobiology, Primitive data type, Mission design, Agency (sociology), Systems engineering, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business
Abstract

International audience; Marco Polo is a mission to return a sample from a near-Earth object of primitive type (class C or D). It is foreseen as a collaborative effort between the Japan Aerospace Exploration Agency (JAXA) and the European Space Agency (ESA). Marco Polo is currently in a Phase-A study (status as of summer 2009). This paper focuses on the scientific requirements provided to the industrial study consortia in Europe as well as the possible mission scenario at the target object in order to achieve the overall mission science objectives. The main scientific reasons for going to a near-Earth object are to understand the initial conditions and evolution history of the solar nebula, to understand how major events (e.g. agglomeration, heating) influence the history of planetesimals, whether primitive class objects contain presolar material, what the organics were in primitive materials, how organics could shed light on the origin of molecules necessary for life, and what the role of impacts by NEOs would be in the origin and evolution of life on Earth.

Published
2010
Full Text
View/download PDF

17. CCD photometry and model of MUSES-C target (25143) 1998 SF36

Author

Kaasalainen, M., Kwiatkowski, T., Piironen, J., Dermawan, B., Farnham, T., Colas, F., Lowry, S., Weissman, P., Whiteley, R. J., Tholen, D. J., Larson, S. M., Toth, I., Velichko, F. P., Abe, Masanao, Nakamura, T., Ohba, Yohei, Yoshikawa, Makoto, Jakokoski Observatory, University of Helsinki, Astronomical Observatory, Adam Mickiewicz University, The Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan, National Astronomical Observatory of Japan (NAOJ), Graduate School of Science, University of Tokyo, Department of Astronomy, University of Texas, 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), Jet Propulsion Laboratory, California Institute of Technology (JPL), Lunar and Planetary Laboratory [University of Arizona] (LPL), University of Arizona, Institute for Astronomy, University of Hawaii, Konkoly Observatory, Research Center for Astronomy and Earth Sciences, and Astronomical Institute of Kharkov National University

Subjects
Rotation period, Physics, 010504 meteorology & atmospheric sciences, Astronomy, Astronomy and Astrophysics, Astrophysics, Lambda, 01 natural sciences, Photometry (optics), Space and Planetary Science, Asteroid, Sidereal time, 0103 physical sciences, Elongation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

著者人数: 17名, Accepted: 2003-05-31, 資料番号: SA1003348000

Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results