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Techniques for Asteroid Spectrocopy Marcel Popescu

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Techniques for asteroid spectrocopy Marcel Popescu To cite this version: Marcel Popescu. Techniques for asteroid spectrocopy. Earth and Planetary Astrophysics [astro- ph.EP]. Observatoire de Paris; Universitatea Politehnica din Bucuresti, Facultatea de Ştiinţe Aplicate, 2012. English. tel-00785991 HAL Id: tel-00785991 https://tel.archives-ouvertes.fr/tel-00785991 Submitted on 7 Feb 2013 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. OBSERVATOIRE DE PARIS ÉCOLE DOCTORALE D’ASTRONOMIE ET D’ASTROPHYSIQUE D’ÎLE-DE-FRANCE ∗ UNIVERSITATEA POLITHENICA BUCURE¸STI FACULTATEA DE ¸STIIN ¸TE APLICATE DOCTORAL THESIS by Marcel Popescu TECHNIQUES FOR ASTEROID SPECTROSCOPY Defended the 23 Octobre 2012 before the jury: Vasile IFTODE (Universitatea Polithenica Bucure¸sti) President Olivier GROUSSIN (Laboratoire d’Astrophysique de Marseille) Reviewer Petre POPESCU (Institutul Astronomic al Academiei Române) Reviewer Dan DUMITRA¸S (INFLPR, România) Reviewer Jean SOUCHAY (SYRTE - Observatoire de Paris) Examiner Mirel BIRLAN (IMCCE - Observatoire de Paris) Co-Advisor Constantin P. CRISTESCU (Universitatea Polithenica, Bucure¸sti) Co-Advisor [email protected] OBSERVATOIRE DE PARIS ÉCOLE DOCTORALE D’ASTRONOMIE ET D’ASTROPHYSIQUE D’ÎLE-DE-FRANCE ∗ UNIVERSITATEA POLITHENICA BUCURE¸STI FACULTATEA DE ¸STIIN ¸TE APLICATE THÈSE DE DOCTORAT par Marcel Popescu TECHNIQUES D’OBSERVATION SPECTROSCOPIQUE D’ASTÉROÏDES Soutenue le 23 Octobre 2012 devant un jury composé de : Vasile IFTODE (Universitatea Polithenica, Bucure¸sti) Présidente Olivier GROUSSIN (Laboratoire d’Astrophysique de Marseille) Rapporteur Petre POPESCU (Institutul Astronomic al Academiei Române) Rapporteur Dan DUMITRA¸S (INFLPR, România) Rapporteur Jean SOUCHAY (SYRTE - Observatoire de Paris) Examinateur Mirel BIRLAN (IMCCE - Observatoire de Paris) Co-Directeur de thèse Constantin P. CRISTESCU (Universitatea Polithenica, Bucure¸sti) Co-Directeur de thèse [email protected] OBSERVATOIRE DE PARIS ÉCOLE DOCTORALE D’ASTRONOMIE ET D’ASTROPHYSIQUE D’ÎLE-DE-FRANCE ∗ UNIVERSITATEA POLITHENICA BUCURE¸STI FACULTATEA DE ¸STIIN ¸TE APLICATE TEZA˘ DOCTORAT autor Marcel Popescu TEHNICI DE OBSERVA¸TIE SPECTROSCOPICA˘ PENTRU ASTEROIZI Sus¸tinut˘aîn 23 Octombrie 2012 în fa¸ta juriului: Vasile IFTODE (Universitatea Polithenica Bucure¸sti) President Olivier GROUSSIN (Laboratoire d’Astrophysique de Marseille) Reviewer Petre POPESCU (Institutul Astronomic al Academiei Române) Reviewer Dan DUMITRA¸S (INFLPR, România) Reviewer Jean SOUCHAY (SYRTE - Observatoire de Paris) Examiner Mirel BIRLAN (IMCCE - Observatoire de Paris) Co-Advisor Constantin P. CRISTESCU (Universitatea Polithenica, Bucure¸sti) Co-Advisor [email protected] Abstract: The fundamental goal of the planetary sciences is to understand the formation and evolution of the Solar System. For achieving this goal, the asteroids are of a special interest to the astronomical community as a possible window back to the beginning of the planetary for- mation. Being the only remnants of the early stages of planetary history they recorded the com- plex chemical and physical evolution that occurred in the solar nebula. Thus, the knowledge of both dynamical and physical properties of the current asteroid population brings valuable information for understanding the Solar System and more generally other planetary systems. In this thesis I present the project Modeling for Asteroids (acronym M4AST). M4AST is an on-line service that I developed for modeling surfaces of asteroids using several theoretical approaches. M4AST consists into a database containing more than 2,500 spectra of asteroids together with a library of routines which can model and extract several mineralogical param- eters. The database M4AST could be accessed via its own webpage interface as well as via the Virtual Observatory (VO-Paris) protocols. This service is available to the web address http://cardamine.imcce.fr/m4ast. It allows several routines for modeling spectra: taxonomic classification, space weathering effects modeling, comparison to laboratory spectra of mete- orites and minerals, band centers and band area computing. I have participated to more than 10 observational campaigns for observing both physical and orbital parameters of asteroids. The objective of spectral runs was to characterize the mineralogical properties of these bodies based on their reflectance spectra. Astrometry was mainly devoted to the confirmation and secures orbits of new discovered asteroid. During the thesis I observed and characterized near-infrared spectra of eight Near Earth Asteroids namely 1917, 8567, 16960, 164400, 188452, 2010 TD54, 5620, and 2001 SG286. These observations were obtained using the NASA telescope IRTF equipped with the spectro- imager SpeX, and the CODAM-Paris observatory facilities. Based on these spectra mineralog- ical solutions were proposed for each asteroid. The taxonomic classification of five of these objects was reviewed and a corresponding type was assigned to the other three asteroids that were not classified before. Four of the observed objects have delta - V lower than 7 km/sec, which make them suitable targets in terms of propulsion for a future spacecraft mission. The asteroid (5620) Jasonwheeler exhibits spectral behaviors similar to the carbonaceous chondrite meteorites. I observed and modeled six Main Belt Asteroids. (9147) Kourakuen, (854) Frostia, (10484) Hecht and (31569) 1999 FL18 show the characteristics of V-type objects, while (1333) Cevenola, (3623) Chaplin belong to S-complex. Some of them have some peculiar properties: (854) Fros- tia is a binary asteroid, (10484) Hecht and (31569) 1999 FL18 have pairs, (1333) Cevenola, (3623) Chaplin show large amplitude lightcurves. The taxonomic classification, the compar- isons to the meteorite spectra from the Relab database and the mineralogical analysis converged to the same solutions for each of these objects, allowing to find important details for the chem- ical compositions and resemblances to the Howardite-Eucrite-Diogenite class of meteorites. Résumé: L’objectif fondamental des sciences planétaires est la compréhension de la forma- tion et de l’évolution du Système Solaire. Pour atteindre cet objectif les astéroïdes présentent un intérêt tout particulier pour la communauté scientifique. En effet, nous pouvons regarder la population astéroïdale comme une fenêtre vers le passée, par laquelle nous regardons les débuts de la formation du système planétaire. Ils sont les témoins des premiers moments de la formation des planètes gardant dans leur structure la complexité chimique de la nébuleuse primordiale. Pour cette raison, les études physiques et dynamiques de ces corps nous appor- tent des informations essentielles sur l’histoire et l’évolution de notre Système Solaire et plus généralement sur la formation des systèmes planétaires. Pendant ma thèse j’ai développé l’application Modelling for Asteroids (acronyme M4AST). M4AST est un service en libre service sur internet permettant la modélisation des surfaces d’astéroïdes en utilisant plusieurs approches théoriques. M4AST est composé d’une base de données contenant quelques 2500 spectres d’astéroïdes et d’une bibliothèque de routines permettant la modélisation et l’obtention de plusieurs paramètres minéralogiques. La base de données est accessible aussi bien par les biais des protocoles de l’Observatoire Virtuel (OV-Paris) que par sa propre interface. Le service est accessible depuis l’adresse http:// cardamine.imcce.fr/m4ast. M4AST permet plusieurs types d’analyses : classifi- cation taxonomique, modélisation de l’altération spatiale, comparaison avec les spectres des météorites et des minéraux terrestres, calculs des centres et des surfaces des bandes. J’ai participé à plus de 10 campagnes d’observations pour la caractérisation physique et dynamique des astéroïdes. Les observations spectroscopiques ont servi à la caractérisation minéralogique des surfaces d’astéroïdes. L’astrométrie a plutôt servi à la confirmation et la sécurisation de nouvelles découvertes d’astéroïdes. Pendant la thèse, j’ai observé et carac- térisé les spectres en infrarouge proche de huit astéroïdes géocroiseurs : 1917, 8567, 16960, 164400, 188452, 2010 TD54, 5620, and 2001 SG286. Ces observations ont été obtenues avec le télescope IRTF et du spectrographe SpeX, en employant l’infrastructure CODAM de l’Observatoire de Paris. Pour chaque astéroïde j’ai proposé des solutions minéralogiques. Une révision de leur taxonomie a aussi été effectuée pour cinq astéroïdes de mon échantillon. Qua- tre des objets sont des objets à faible delta-V, qui sont des cibles souhaitables/possibles pour des missions spatiales. L’astéroïde (5620) Jasonwheeler montre un spectre similaire à ceux des météorites chondritiques. J’ai observé et modélisé six astéroïdes de la ceinture principale. (9147) Kourakuen, (854) Frostia, (10484) Hecht and (31569) 1999 FL18 montrent des caractéristiques des astéroïdes du type V; (1333) Cevenola, (3623) Chaplin sont du type taxonomique S. Quelques astéroïdes de cet échantillon sont particuliers : (854) Frostia
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    The Astronomical Journal, 140:770–784, 2010 September doi:10.1088/0004-6256/140/3/770 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. EXPLORENEOs. I. DESCRIPTION AND FIRST RESULTS FROM THE WARM SPITZER NEAR-EARTH OBJECT SURVEY D. E. Trilling1, M. Mueller2,J.L.Hora3, A. W. Harris4, B. Bhattacharya5, W. F. Bottke6, S. Chesley7, M. Delbo2, J. P. Emery8, G. Fazio3, A. Mainzer7, B. Penprase9,H.A.Smith3, T. B. Spahr3, J. A. Stansberry10, and C. A. Thomas1 1 Department of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ 86001, USA; [email protected] 2 Observatoire de la Coteˆ d’Azur, Universite´ de Nice Sophia Antipolis, CNRS, BP 4229, 06304 Nice Cedex 4, France 3 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-65, Cambridge, MA 02138, USA 4 DLR Institute of Planetary Research, Rutherfordstrasse 2, 12489 Berlin, Germany 5 NASA Herschel Science Center, Caltech, M/S 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA 6 Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA 7 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA 8 Department of Earth and Planetary Sciences, University of Tennessee, 1412 Circle Drive, Knoxville, TN 37996, USA 9 Department of Physics and Astronomy, Pomona College, 610 North College Avenue, Claremont, CA 91711, USA 10 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA Received 2009 December 18; accepted 2010 July 6; published 2010 August 9 ABSTRACT We have begun the ExploreNEOs project in which we observe some 700 Near-Earth Objects (NEOs) at 3.6 and 4.5 μm with the Spitzer Space Telescope in its Warm Spitzer mode.
  • Instrumental Methods for Professional and Amateur

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