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1. Constraints on the structure and seasonal variations of Triton’s atmosphere from the 5 October 2017 stellar occultation and previous observations

Author: J. Marques Oliveira, B. Sicardy, A. R. Gomes-Júnior, J. L. Ortiz, D. F. Strobel, T. Bertrand, F. Forget, E. Lellouch, J. Desmars, D. Bérard, A. Doressoundiram, J. Lecacheux, R. Leiva, E. Meza, F. Roques, D. Souami, T. Widemann, P. Santos-Sanz, N. Morales, R. Duffard, E. Fernández-Valenzuela, A. J. Castro-Tirado, F. Braga-Ribas, B. E. Morgado, M. Assafin, J. I. B. Camargo, R. Vieira-Martins, G. Benedetti-Rossi, S. Santos-Filho, M. V. Banda-Huarca, F. Quispe-Huaynasi, C. L. Pereira, F. L. Rommel, G. Margoti, A. Dias-Oliveira, F. Colas, J. Berthier, S. Renner, R. Hueso, S. Pérez-Hoyos, A. Sánchez-Lavega, J. F. Rojas, W. Beisker, M. Kretlow, D. Herald, D. Gault, K.-L. Bath, H.-J. Bode, E. Bredner, K. Guhl, T. V. Haymes, E. Hummel, B. Kattentidt, O. Klös, A. Pratt, B. Thome, C. Avdellidou, K. Gazeas, E. Karampotsiou, L. Tzouganatos, E. Kardasis, A. A. Christou, E. M. Xilouris, I. Alikakos, A. Gourzelas, A. Liakos, V. Charmandaris, M. Jelínek, J. Štrobl, A. Eberle, K. Rapp, B. Gährken, B. Klemt, S. Kowollik, R. Bitzer, M. Miller, G. Herzogenrath, D. Frangenberg, L. Brandis, I. Pütz, V. Perdelwitz, G. M. Piehler, P. Riepe, K. von Poschinger, P. Baruffetti, D. Cenadelli, J.-M. Christille, F. Ciabattari, R. Di Luca, D. Alboresi, G. Leto, R. Zanmar Sanchez, P. Bruno, G. Occhipinti, L. Morrone, L. Cupolino, A. Noschese, A. Vecchione, C. Scalia, R. Lo Savio, G. Giardina, S. Kamoun, R. Barbosa, R. Behrend, M. Spano, E. Bouchet, M. Cottier, L. Falco, S. Gallego, L. Tortorelli, S. Sposetti, J. Sussenbach, F. Van Den Abbeel, P. André, M. Llibre, F. Pailler, J. Ardissone, M. Boutet, J. Sanchez, M. Bretton, A. Cailleau, V. Pic, L. Granier, R. Chauvet, M. Conjat, J. L. Dauvergne, O. Dechambre, P. Delay, M. Delcroix, L. Rousselot, J. Ferreira, P. Machado, P. Tanga, J.-P. Rivet, E. Frappa, M. Irzyk, F. Jabet, M. Kaschinski, A. Klotz, Y. Rieugnie, A. N. Klotz, O. Labrevoir, D. Lavandier, D. Walliang, A. Leroy, S. Bouley, S. Lisciandra, J.-F. Coliac, F. Metz, D. Erpelding, P. Nougayrède, T. Midavaine, M. Miniou, S. Moindrot, P. Morel, B. Reginato, E. Reginato, J. Rudelle, B. Tregon, R. Tanguy, J. David, W. Thuillot, D. Hestroffer, G. Vaudescal, D. Baba Aissa, Z. Grigahcene, D. Briggs, S. Broadbent, P. Denyer, N. J. Haigh, N. Quinn, G. Thurston, S. J. Fossey, C. Arena, M. Jennings, J. Talbot, S. Alonso, A. Román Reche, V. Casanova, E. Briggs, R. Iglesias-Marzoa, J. Abril Ibáñez, M. C. Díaz Martín, H. González, J. L. Maestre García, J. Marchant, I. Ordonez-Etxeberria, P. Martorell, J. Salamero, F. Organero, L. Ana, F. Fonseca, V. Peris, O. Brevia, A. Selva, C. Perello, V. Cabedo, R. Gonçalves, M. Ferreira, F. Marques Dias, A. Daassou, K. Barkaoui, Z. Benkhaldoun, M. Guennoun, J. Chouqar, E. Jehin, C. Rinner, J. Lloyd, M. El Moutamid, C. Lamarche, J. T. Pollock, D. B. Caton, V. Kouprianov, B. W. Timerson, G. Blanchard, B. Payet, A. Peyrot, J.-P. Teng-Chuen-Yu, J. Françoise, B. Mondon, T. Payet, C. Boissel, M. Castets, W. B. Hubbard, R. Hill, H. J. Reitsema, O. Mousis, L. Ball, G. Neilsen, S. Hutcheon, K. Lay, P. Anderson, M. Moy, M. Jonsen, I. Pink, R. Walters, B. Downs, Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Research Council, European Commission, Fundação para a Ciência e a Tecnologia (Portugal), 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), Universidade Estadual Paulista Júlio de Mesquita Filho = São Paulo State University (UNESP), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Johns Hopkins University (JHU), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut Polytechnique des Sciences Avancées (IPSA), 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-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Comisión Nacional de Investigación y Desarrollo Aeroespacial (CONIDA), Observatorio Astronómico de Moquegua, Florida Space Institute [Orlando] (FSI), University of Central Florida [Orlando] (UCF), Federal University of Technology - Paraná (UTFPR), Observatório Nacional [Rio de Janeiro] (ON), Ministério da Ciência, Tecnologia, Inovações e Comunicações (MCTIC), Universidade Federal do Rio de Janeiro (UFRJ), Polo Educacional Sesc [Rio de Janeiro], Université de Lille, Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), International Occultation Timing Association (IOTA), Internationale Amateursternwarte [Mittenwalde] (IAS), Société Astronomique de France (SAF), 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), Université Paris-Sud - Paris 11 (UP11), Analyse, ingénierie et contrôle des micro-organismes (MICROCOSME), Inria Grenoble - Rhône-Alpes, Institut National de Recherche en Informatique et en Automatique (Inria)-Institut National de Recherche en Informatique et en Automatique (Inria)-Université Grenoble Alpes (UGA), Laboratoire Ondes et Matière d'Aquitaine (LOMA), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS), 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), European Project: 669416,H2020,ERC-2014-ADG,LUCKY STAR(2015), and European Project: 687378,H2020,H2020-COMPET-2015,SBNAF(2016)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: atmospheres, planets and satellites: physical evolution, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], photometric [Techniques], FOS: Physical sciences, Astronomy and Astrophysics, methods: data analysis, techniques: photometric, Space and Planetary Science, [SDU]Sciences of the Universe [physics], atmospheres [Planets and satellites], observational [Methods], methods: observational, data analysis [Methods], physical evolution [Planets and satellites], Astrophysics - Earth and Planetary Astrophysics
Abstract: J.M.O. acknowledges financial support from the Portuguese Foundation for Science and Technology (FCT) and the European Social Fund (ESF) through the PhD grant SFRH/BD/131700/2017. The work leading to these results has received funding from the European Research Council under the European Community's H2020 2014-2021 ERC grant Agreement nffi 669416 "Lucky Star". We thank S. Para who supported some travels to observe the 5 October 2017 occultation. T.B. was supported for this research by an appointment to the National Aeronautics and Space Administration (NASA) Post-Doctoral Program at the Ames Research Center administered by Universities Space Research Association (USRA) through a contract with NASA. We acknowledge useful exchanges with Mark Gurwell on the ALMA CO observations. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. J.L.O., P.S.-S., N.M. and R.D. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709), they also acknowledge the financial support by the Spanish grant AYA-2017-84637-R and the Proyecto de Excelencia de la Junta de Andalucia J.A. 2012-FQM1776. The research leading to these results has received funding from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no. 687378, as part of the project "Small Bodies Near and Far" (SBNAF). P.S.-S. acknowledges financial support by the Spanish grant AYA-RTI2018-098657-J-I00 "LEO-SBNAF". The work was partially based on observations made at the Laboratorio Nacional de Astrofisica (LNA), Itajuba-MG, Brazil. The following authors acknowledge the respective CNPq grants: F.B.-R. 309578/2017-5; R.V.-M. 304544/2017-5, 401903/2016-8; J.I.B.C. 308150/2016-3 and 305917/2019-6; M.A. 427700/20183, 310683/2017-3, 473002/2013-2. This study was financed in part by the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior -Brasil (CAPES) -Finance Code 001 and the National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq grant 465376/2014-2). G.B.R. acknowledges CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016 and CAPES-PRINT/UNESP grant 88887.571156/2020-00, M.A. FAPERJ grant E26/111.488/2013 and A.R.G.Jr. FAPESP grant 2018/11239-8. B.E.M. thanks CNPq 150612/2020-6 and CAPES/Cofecub-394/2016-05 grants. Part of the photometric data used in this study were collected in the frame of the photometric observations with the robotic and remotely controlled telescope at the University of Athens Observatory (UOAO; Gazeas 2016). The 2.3 m Aristarchos telescope is operated on Helmos Observatory by the Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing of the National Observatory of Athens. Observations with the 2.3 m Aristarchos telescope were carried out under OPTICON programme. This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 730890. This material reflects only the authors views and the Commission is not liable for any use that may be made of the information contained therein. The 1. 2m Kryoneri telescope is operated by the Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing of the National Observatory of Athens. The Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVdA) is managed by the Fondazione Clement Fillietroz-ONLUS, which is supported by the Regional Government of the Aosta Valley, the Town Municipality of Nus and the "Unite des Communes valdotaines Mont-Emilius". The 0.81 m Main Telescope at the OAVdA was upgraded thanks to a Shoemaker NEO Grant 2013 from The Planetary Society. D.C. and J.M.C. acknowledge funds from a 2017 'Research and Education' grant from Fondazione CRT-Cassa di Risparmio di Torino. P.M. acknowledges support from the Portuguese Fundacao para a Ciencia e a Tecnologia ref. PTDC/FISAST/29942/2017 through national funds and by FEDER through COMPETE 2020 (ref. POCI010145 FEDER007672). F.J. acknowledges Jean Luc Plouvier for his help. S.J.F. and C.A. would like to thank the UCL student support observers: Helen Dai, Elise Darragh-Ford, Ross Dobson, Max Hipperson, Edward Kerr-Dineen, Isaac Langley, Emese Meder, Roman Gerasimov, Javier Sanjuan, and Manasvee Saraf. We are grateful to the CAHA, OSN and La Hita Observatory staffs. This research is partially based on observations collected at Centro Astronomico HispanoAleman (CAHA) at Calar Alto, operated jointly by Junta de Andalucia and Consejo Superior de Investigaciones Cientificas (IAA-CSIC). This research was also partially based on observation carried out at the Observatorio de Sierra Nevada (OSN) operated by Instituto de Astrofisica de Andalucia (CSIC). This article is also based on observations made with the Liverpool Telescope operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. Partially based on observations made with the Tx40 and Excalibur telescopes at the Observatorio Astrofisico de Javalambre in Teruel, a Spanish Infraestructura Cientifico-Tecnica Singular (ICTS) owned, managed and operated by the Centro de Estudios de Fisica del Cosmos de Aragon (CEFCA). Tx40 and Excalibur are funded with the Fondos de Inversiones de Teruel (FITE). A.R.R. would like to thank Gustavo Roman for the mechanical adaptation of the camera to the telescope to allow for the observation to be recorded. R.H., J.F.R., S.P.H. and A.S.L. have been supported by the Spanish projects AYA2015-65041P and PID2019-109467GB-100 (MINECO/FEDER, UE) and Grupos Gobierno Vasco IT1366-19. Our great thanks to Omar Hila and their collaborators in Atlas Golf Marrakech Observatory for providing access to the T60cm telescope. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege, and performed in collaboration with Cadi Ayyad University of Marrakesh. E.J. is a FNRS Senior Research Associate., Context. A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. Aims. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. Methods. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range similar to 8 km to similar to 190 km, corresponding to pressure levels from 9 mu bar down to a few nanobars. Results. (i) A pressure of 1.18 +/- 0.03 mu bar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 mu bar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude., Portuguese Foundation for Science and Technology SFRH/BD/131700/2017, European Social Fund (ESF) SFRH/BD/131700/2017, European Research Council under the European Community's H2020 2014-2021 ERC grant 669416, Spanish Government SEV-2017-0709 AYA-2017-84637-R AYA-RTI2018-098657-J-I00, Junta de Andalucia 2012-FQM1776, European Union's Horizon 2020 Research and Innovation Programme, as part of the project "Small Bodies Near and Far" (SBNAF) 687378, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ), Fundacao de Apoio a Pesquisa do Distrito Federal (FAPDF) 309578/2017-5 304544/2017-5 401903/2016-8 308150/2016-3 305917/2019-6 427700/2018-3 310683/2017-3 473002/2013-2, Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) 001, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ) 465376/2014-2 CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016 CAPES-PRINT/UNESP grant 88887.571156/2020-00, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ) E26/111.488/2013, Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) 2018/11239-8, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ) 150612/2020-6, European Union's Horizon 2020 research and innovation programme 730890, Regional Government of the Aosta Valley, Town Municipality of Nus, Unite des Communes valdotaines Mont-Emilius, Planetary Society, Fondazione CRT-Cassa di Risparmio di Torino, Portuguese Foundation for Science and Technology PTDC/FISAST/29942/2017, FEDER through COMPETE 2020 POCI010145 FEDER007672, UK Research & Innovation (UKRI), Science & Technology Facilities Council (STFC), Fondos de Inversiones de Teruel (FITE), Spanish Government AYA2015-65041P PID2019-109467GB-100, Grupos Gobierno Vasco IT1366-19, Fonds de la Recherche Scientifique - FNRS PDR T.0120.21, University of Liege, CAPES/Cofecub-394/2016-05
Published: 2022
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2. Stellar occultations enable milliarcsecond astrometry for Trans-Neptunian objects and Centaurs

Author: Josselin Desmars, A. Burtovoi, H. Mikuž, J. R. de Barros, Emmanuel Jehin, Marcelo Assafin, J. Fabrega Polleri, S. Sposetti, D. Herald, R. Szakats, A. R. Gomes-Júnior, Bruno Sicardy, D. W. Dunham, H. Tomioka, A. Ossola, Domenico Nardiello, F. L. Rommel, C. L. Pereira, A. Stechina, T. Hayamizu, Sohrab Rahvar, P. Sogorb, R. Vieira-Martins, Jose Luis Ortiz, Julio Camargo, J. B. Dunham, Luca Zampieri, P. Pravec, R. Komžík, J. Broughton, T. Janik, Anaëlle Maury, B. E. Morgado, P. M. Kilmartin, Pablo Santos-Sanz, G. Benedetti-Rossi, K. Hosoi, Rafael Sfair, Othon C. Winter, Nicolás Morales, D. Gault, András Pál, Y. Ueno, J. Tregloan-Reed, A. C. Gilmore, T. Carruthers, Estela Fernández-Valenzuela, P. B. Siqueira, J. Lecacheux, W. Hanna, Rhian H. Jones, Michele Fiori, Jeffrey A. Newman, Valerio Nascimbeni, Jonathan Bradshaw, K. Kitazaki, E. Pimentel, Rene Duffard, Felipe Braga-Ribas, Jan Maarten Winkel, S. Kerr, P. Nosworthy, A. Marciniak, D. Hooper, Giampiero Naletto, C. Jacques, Kamil Hornoch, Colin Snodgrass, Joseph Brimacombe, Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Fundação de Amparo à Pesquisa do Estado de São Paulo, Centre National D'Etudes Spatiales (France), National Research, Development and Innovation Office (Hungary), European Research Council, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), 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), Bairro Imperial de São Cristóvão, Federal University of Technology-Paraná (UTFPR/DAFIS), Institut Polytechnique des Sciences Avancées Ipsa, Univ. Lille, IAA-CSIC, Sorbonne Paris Cité, Universidade Federal do Rio de Janeiro (UFRJ), University of Central Florida, Universidade Estadual Paulista (Unesp), International Occultation Timing Association (IOTA), Trans-Tasman Occultation Alliance (TTOA), Canberra Astronomical Society, Samford Valley Observatory (Q79), Coral Towers Observatory, University of Padova, INAF-Astronomical Observatory of Padova, Jewel Box Observatory, Sonear Observatory, University of Canterbury, Academy of Sciences of the Czech Republic, Astronomical Association of Queensland, Lam, Swiss Astronomical Society, Research Centre for Astronomy and Earth Sciences, Eötvös Loránd University, Institute of Physics, Centro de Amigos de la Astronomia Reconquista-CAAR, Japan Occultation Information Network (JOIN), Reedy Creek Observatory, Université de Liège, Slovak Academy of Sciences, Adam Mickiewicz University, San Pedro de Atacama Celestial Explorations-SPACE, Faculty of Mathematics and Physics, Panamanian Observatory in San Pedro de Atacama-OPSPA, Sharif University of Technology, Royal Observatory, Club d'Astronomie Luberon Sud Astro, and Universidad de Antofagasta
Subjects: 010504 meteorology & atmospheric sciences, general [Minor planets, asteroids], FOS: Physical sciences, Context (language use), Astrophysics, Ephemeris, 01 natural sciences, 0103 physical sciences, Trans-Neptunian object, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Earth and Planetary Astrophysics (astro-ph.EP), International Celestial Reference System, Astrometry, Kuiper belt: general, Minor planets, asteroids: general, Occultations, Minor planets, general [Kuiper belt], Astronomy and Astrophysics, Planetary system, asteroids: general, Space and Planetary Science, Asteroid, astro-ph.EP, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics, astro-ph.IM, Reference frame
Abstract: Full list of authors: Rommel, F. L.; Braga-Ribas, F.; Desmars, J.; Camargo, J. I. B.; Ortiz, J. L.; Sicardy, B.; Vieira-Martins, R.; Assafin, M.; Santos-Sanz, P.; Duffard, R.; Fernández-Valenzuela, E.; Lecacheux, J.; Morgado, B. E.; Benedetti-Rossi, G.; Gomes-Júnior, A. R.; Pereira, C. L.; Herald, D.; Hanna, W.; Bradshaw, J.; Morales, N. Brimacombe, J.; Burtovoi, A.; Carruthers, T.; de Barros, J. R.; Fiori, M.; Gilmore, A.; Hooper, D.; Hornoch, K.; Jacques, C.; Janik, T.; Kerr, S.; Kilmartin, P.; Winkel, Jan Maarten; Naletto, G.; Nardiello, D.; Nascimbeni, V.; Newman, J.; Ossola, A.; Pál, A.; Pimentel, E.; Pravec, P.; Sposetti, S.; Stechina, A.; Szakáts, R.; Ueno, Y.; Zampieri, L.; Broughton, J.; Dunham, J. B.; Dunham, D. W.; Gault, D.; Hayamizu, T.; Hosoi, K.; Jehin, E.; Jones, R.; Kitazaki, K.; Komžík, R.; Marciniak, A.; Maury, A.; Mikuž, H.; Nosworthy, P.; Fábrega Polleri, J.; Rahvar, S.; Sfair, R.; Siqueira, P. B.; Snodgrass, C.; Sogorb, P.; Tomioka, H.; Tregloan-Reed, J.; Winter, O. C., Context. Trans-Neptunian objects (TNOs) and Centaurs are remnants of our planetary system formation, and their physical properties have invaluable information for evolutionary theories. Stellar occultation is a ground-based method for studying these distant small bodies and has presented exciting results. These observations can provide precise profiles of the involved body, allowing an accurate determination of its size and shape. Aims. The goal is to show that even single-chord detections of TNOs allow us to measure their milliarcsecond astrometric positions in the reference frame of the Gaia second data release (DR2). Accurate ephemerides can then be generated, allowing predictions of stellar occultations with much higher reliability. Methods. We analyzed data from various stellar occultation detections to obtain astrometric positions of the involved bodies. The events published before the Gaia era were updated so that the Gaia DR2 stellar catalog is the reference, thus providing accurate positions. Events with detection from one or two different sites (single or double chord) were analyzed to determine the event duration. Previously determined sizes were used to calculate the position of the object center and its corresponding error with respectto the detected chord and the International Celestial Reference System propagated Gaia DR2 star position. Results. We derive 37 precise astrometric positions for 19 TNOs and four Centaurs. Twenty-one of these events are presented here for the first time. Although about 68% of our results are based on single-chord detection, most have intrinsic precision at the submilliarcsecond level. Lower limits on the diameter of bodies such as Sedna, 2002 KX14, and Echeclus, and also shape constraints on 2002 VE95, 2003 FF128, and 2005 TV189 are presented as valuable byproducts. Conclusions. Using the Gaia DR2 catalog, we show that even a single detection of a stellar occultation allows improving the object ephemeris significantly, which in turn enables predicting a future stellar occultation with high accuracy. Observational campaigns can be efficiently organized with this help, and may provide a full physical characterization of the involved object, or even the study of topographic features such as satellites or rings. © 2020 ESO., This study was financed in part by the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior - Brasil (CAPES) - Finance Code 001 and the National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq grant 465376/2014-2). The following authors acknowledge the respective CNPq grants: F.B.-R. 309578/2017-5; R.V.-M. 304544/2017-5, 401903/2016-8; J.I.B.C. 308150/2016-3; M.A. 427700/2018-3, 310683/2017-3, 473002/2013-2; O.C.W. 305210/2018-1. The following authors acknowledge the respective grants: B.E.M. thanks the CAPES/Cofecub-394/2016-05 grant; G.B-R. acknowledges CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016; M.A. acknowledges FAPERJ grant E-26/111.488/2013; A.R.G.Jr acknowledges FAPESP grant 2018/11239-8; O.C.W. and R.S. acknowledge FAPESP grant 2016/24561-0. D.N. acknowledges support from the French Centre National d'Etudes Spatiales (CNES). K.H. and P.P. were supported by the project R.V.O.: 67985815. A.P. and R.S. received support from the K-125015 grant of the National Research, Development and Innovation Office (NKFIH, Hungary). Partial funding of the computational infrastructure and database servers are received from the grant KEP-7/2018 of the Hungarian Academy of Sciences. Some of the results were based on observations taken at the 1.6m telescope on Pico dos Dias Observatory of the National Laboratory of Astrophysics (LNA/Brazil). Some data are based on observations collected at the Copernicus and Schmidt telescopes (Asiago, Italy) of the INAF-Astronomical Observatory of Padova. This work was carried out within the "Lucky Star" umbrella that agglomerates the efforts of the Paris, Granada and Rio teams, which is funded by the European Research Council under the European Community's H2020 (ERC Grant Agreement No. 669416). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. TRAPPIST is a project funded by the Belgian FNRS under grant FRFC 2.5.594.09.F and the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. E.J. is a FNRS Senior Research Associate. We would like to acknowledge financial support by the Spanish grant AYA-RTI2018-098657-JI00 "LEO-SBNAF" (MCIU/AEI/FEDER, U.E.) and the financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). Also, AYA2017-89637-R and FEDER funds are acknowledged. We are thankful to the following observers who participated and provided data for respective events as listed in Table B.1: Orlando A. Naranjo from Universidad de Los Andes, Merida/VEN; Faustino Organero from La Hita Observatory - Toledo/ESP.
Published: 2020
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3. The large trans-Neptunian object 2002 TC 302 from combined stellar occultation, photometry, and astrometry data

Author: G. Scarfi, T. Pribulla, J. C. Guirado, L. Buzzi, Grzegorz Dudziński, A. Farkas-Takács, L. Mazzei, E. Meza, A. Aletti, J. M. Christille, C. Perelló, L. Morrone, V. Peris, Valerio Nascimbeni, J. Lecacheux, J. M. Madiedo, Rene Duffard, F. Mancini, Bruno Sicardy, J. Alikakos, Vassilis Charmandaris, Cs. Kiss, M. Conjat, Raoul Behrend, R. Komžík, Frédéric Vachier, Martina Maestripieri, J. Skvarc, Paolo Bacci, T. G. Mueller, Domenico Nardiello, R. Iglesias-Marzoa, F. Colas, Aleksandar Cikota, András Pál, N. Paschalis, R. Szakats, A. Campo Bagatin, P. J. Gutierrez, Giacomo Succi, Pablo Santos-Sanz, A. R. Gomes-Júnior, Gábor Marton, M. Butkiewicz-Bak, E. Varga-Verebélyi, M. Masucci, Estela Fernández-Valenzuela, V. Tsamis, Victor Ali-Lagoa, Felipe Braga-Ribas, M. Alighieri, Roberto Vieira-Martins, F. Manzano, Julio Camargo, E. Dal Canto, S. Hellmich, F. Roques, A. Vecchione, A. Navarro, Stefano Mottola, A. Noschese, Albino Carbognani, F. Lavalade, Josselin Desmars, Mónica Vara-Lubiano, Nora Morales, C. Schnabel, Mauro Bachini, Kosmas Gazeas, J. M. Mari, Przemyslaw Bartczak, W. Beisker, S. Sposetti, F. Ciabattari, A. Alvarez-Candal, Stefan Cikota, J. L. Ortiz, Marcelo Assafin, A. Marciniak, G. Benedetti-Rossi, H. Mikuz, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Investigación Informática, Astronomía y Astrofísica, European Commission, Junta de Andalucía, Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Fundações de Amparo à Pesquisa (Brasil), National Research, Development and Innovation Office (Hungary), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, IAA-CSIC, Université de Paris, Laboratório Interinstitucional de E-Astronomia - LIneA, Federal University of Technology-Paraná (UTFPR / DAFIS), Observatório Nacional/MCTIC, University of Central Florida, 'G. Galilei' Universita Degli Studi di Padova, INAF - Osservatorio Astronomico di Padova, LAM, INAF - Osservatorio di Astrofisica e Scienza Dello Spazio, Schiaparelli Astronomical Observatory, Astronomical Observatory San Marcello Pistoiese CARA Project, Crni Vrh Observatory, University of Ljubljana, Osservatorio Astronomico di Monte Agliale, 55 Impasse de la Marjolaine, Observatorio Astronomico Iota-Scorpii, 1075 Avenue Saint Philippe, Observatoire de la Côte d'Azur, Gnosca Observatory, Osservatorio Astronomico di Tavolaia, 63 Boulevard de Brandebourg, UPMC Univ Paris 06, Universidade Federal do Rio de Janeiro (UFRJ), International Occultation Timing Association - European Section (IOTA-ES), Observatoire de Geneve, Max Planck Institut für Extraterrestrische Physik (MPE), Universidade Estadual Paulista (Unesp), Institute of Planetary Research, Universidad de Alicante, Unversidad de Alicante, Faculty of Electrical Engineering and Computing, E.O. Lawrence Berkeley National Laboratory, Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVdA), Research Centre for Astronomy and Earth Sciences, Institute of Physics, Slovak Academy of Sciences, MTA-ELTE Exoplanet Research Group, ELTE Gothard Astrophysical Observatory, National Observatory of Athens, University of Crete, Faculty of Science, A. Mickiewicz University, Nunki Observatory, Ellinogermaniki Agogi Observatory, Universidad de Valencia, Centro de Estudios de Física Del Cosmos de Aragón, Universidad de la Laguna, Agrupació Astronómica de Sabadell, Osservatorio Salvatore di Giacomo, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatorio Nacional [Rio de Janeiro], Universidad Politécnica Salesiana [Quito], Observatório Nacional/MCT, 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-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), 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: Absolute magnitude, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Kuiper belt objects: individual: 2002 TC302, 01 natural sciences, Occultation, law.invention, Telescope, Photometry (optics), law, Geometric albedo, Física Aplicada, 0103 physical sciences, Trans-Neptunian object, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Earth and Planetary Astrophysics (astro-ph.EP), photometric [Techniques], Astronomy and Astrophysics, general [Kuiper belt], Astrometry, individual: 2002 TC302 [Kuiper belt objects], Kuiper belt: general, Occultations, Techniques: photometric, Light curve, Space and Planetary Science, [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: All authors: Ortiz, J. L.; Santos-Sanz, P.; Sicardy, B.; Benedetti-Rossi, G.; Duffard, R.; Morales, N.; Braga-Ribas, F.; Fernández-Valenzuela, E.; Nascimbeni, V.; Nardiello, D.; Carbognani, A.; Buzzi, L.; Aletti, A.; Bacci, P.; Maestripieri, M.; Mazzei, L.; Mikuz, H.; Skvarc, J.; Ciabattari, F.; Lavalade, F. Scarfi, G.; Mari, J. M.; Conjat, M.; Sposetti, S.; Bachini, M.; Succi, G.; Mancini, F.; Alighieri, M.; Dal Canto, E.; Masucci, M.; Vara-Lubiano, M.; Gutiérrez, P. J.; Desmars, J.; Lecacheux, J.; Vieira-Martins, R.; Camargo, J. I. B.; Assafin, M.; Colas, F.; Beisker, W.; Behrend, R.; Mueller, T. G.; Meza, E.; Gomes-Junior, A. R.; Roques, F.; Vachier, F.; Mottola, S.; Hellmich, S.; Campo Bagatin, A.; Alvarez-Candal, A.; Cikota, S.; Cikota, A.; Christille, J. M.; Pál, A.; Kiss, C.; Pribulla, T.; Komžík, R.; Madiedo, J. M.; Charmandaris, V.; Alikakos, J.; Szakáts, R.; Farkas-Takács, A.; Varga-Verebélyi, E.; Marton, G.; Marciniak, A.; Bartczak, P.; Butkiewicz-Baķ, M.; Dudziński, G.; Alí-Lagoa, V.; Gazeas, K.; Paschalis, N.; Tsamis, V.; Guirado, J. C.; Peris, V.; Iglesias-Marzoa, R.; Schnabel, C.; Manzano, F.; Navarro, A.; Perelló, C.; Vecchione, A.; Noschese, A.; Morrone, L., Context. Deriving physical properties of trans-Neptunian objects is important for the understanding of our Solar System. This requires observational efforts and the development of techniques suitable for these studies. Aims. Our aim is to characterize the large trans-Neptunian object (TNO) 2002 TC302. Methods. Stellar occultations offer unique opportunities to determine key physical properties of TNOs. On 28 January 2018, 2002 TC302 occulted a mv ∼ 15.3 star with designation 593-005847 in the UCAC4 stellar catalog, corresponding to Gaia source 130957813463146112. Twelve positive occultation chords were obtained from Italy, France, Slovenia, and Switzerland. Also, four negative detections were obtained near the north and south limbs. This represents the best observed stellar occultation by a TNO other than Pluto in terms of the number of chords published thus far. From the 12 chords, an accurate elliptical fit to the instantaneous projection of the body can be obtained that is compatible with the near misses. Results. The resulting ellipse has major and minor axes of 543 ± 18 km and 460 ± 11 km, respectively, with a position angle of 3 ± 1 degrees for the minor axis. This information, combined with rotational light curves obtained with the 1.5 m telescope at Sierra Nevada Observatory and the 1.23 m telescope at Calar Alto observatory, allows us to derive possible three-dimensional shapes and density estimations for the body based on hydrostatic equilibrium assumptions. The effective diameter in equivalent area is around 84 km smaller than the radiometrically derived diameter using thermal data from Herschel and Spitzer Space Telescopes. This might indicate the existence of an unresolved satellite of up to ∼300 km in diameter, which is required to account for all the thermal flux, although the occultation and thermal diameters are compatible within their error bars given the considerable uncertainty of the thermal results. The existence of a potential satellite also appears to be consistent with other ground-based data presented here. From the effective occultation diameter combined with absolute magnitude measurements we derive a geometric albedo of 0.147 ± 0.005, which would be somewhat smaller if 2002 TC302 has a satellite. The best occultation light curves do not show any signs of ring features or any signatures of a global atmosphere. © ESO 2020., This research was partially based on data taken at the Sierra Nevada Observatory, which is operated by the Instituto de Astrofisica de Andalucia (CSIC). This research is also partially based on data taken at the German-Spanish Calar Alto observatory, which is jointly operated by the Max Planck Institute fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC). Part of the results were also based on observations taken at the 1.6m telescope on Pico dos Dias Observatory. This research was partially based on observations collected at the Schmidt telescope 67/92 cm (Asiago, Italy) of the INAF - Osservatorio Astronomico di Padova. Funding from Spanish projects AYA2014-56637-C2-1-P, AYA2017-89637-R, from FEDER, and Proyecto de Excelencia de la Junta de Andalucia 2012-FQM1776 is acknowledged. We would like to acknowledge financial support by the Spanish grant AYA-RTI2018-098657-JI00 "LEO-SBNAF" (MCIU/AEI/FEDER, UE) and the financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV- 2017-0709). Part of the research received funding from the European Union's Horizon 2020 Research and Innovation Programme, under grant agreement no. 687378 and from the ERC programme under Grant Agreement no. 669416 Lucky Star. The following authors acknowledge the respective CNPq grants: FB-R 309578/2017-5; RV-M 304544/2017-5, 401903/2016-8; J.I.B.C. 308150/2016-3; MA 427700/2018-3, 310683/2017-3, 473002/2013-2. This study was financed in part by the CoordenacAo de Aperfeiacoamento de Pessoal de Nivel Superior - Brasil (CAPES) - Finance Code 001 and the National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq grant 465376/2014-2). GBR acknowledges CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016, MA FAPERJ grant E-26/111.488/2013 and ARGJr FAPESP grant 2018/11239-8. E.F.-V. acknowledges support from the 2017 Preeminent Postdoctoral Program (P3) at UCF. C.K., R.S., A.F-T., and G.M. have been supported by the K-125015 and GINOP-2.3.2-15-2016-00003 grants of the Hungarian National Research, Development and Innovation Office (NKFIH), Hungary. G.M. was also supported by the Hungarian National Research, Development and Innovation Office (NKFIH) grant PD-128 360. R.K. and T.P. were supported by the VEGA 2/0031/18 grant. We acknowledge the use of Occult software by D. Herald.
Published: 2020
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4. Formation of Dusty Plasma Clouds at Meteoroid Impact on the Surface of the Moon

Author: E. S. Zubko, S. Sposetti, B. Atamaniuk, A. V. Zakharov, Lev Zelenyi, Sergey I. Popel, Alexey A. Berezhnoy, R. Lena, A. P. Golub, A. A. Tereshchenko, Yu. I. Velikodsky, and M. Iten
Subjects: Surface (mathematics), Physics, Shock wave, Dusty plasma, Physics and Astronomy (miscellaneous), Solid-state physics, Meteoroid, Astrophysics, Free space, 01 natural sciences, Regolith, Physics::Geophysics, 010305 fluids & plasmas, Physics::Space Physics, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The nature of two dusty plasma clouds appearing because of the impact of a meteoroid on the surface of the Moon has been discussed. It has been shown that one of the clouds is formed by particles (or fragments) of regolith ejected into free space by a shock wave induced by the meteoroid impact on the surface of the Moon and the second cloud is formed by solidified melt droplets. The main characteristics of these clouds, including the cloud expansion rates, the characteristic sizes of particles in both clouds, and the concentrations and charges of particles, have been calculated. The calculated cloud expansion rates are in qualitative agreement with the observational data.
Published: 2018
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5. Detection of impact-produced dust clouds near the lunar terminator

Author: A. A. Tereshchenko, A. P. Golub, Alexey A. Berezhnoy, M. Iten, Yu. I. Velikodsky, R. Lena, Sergey I. Popel, S. Sposetti, E. A. Feoktistova, and Evgenij Zubko
Subjects: Physics, Brightness, 010504 meteorology & atmospheric sciences, Meteoroid, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Regolith, Space and Planetary Science, 0103 physical sciences, Thermal, Lunar terminator, Ejecta, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Exosphere
Abstract: Analysis of observations of unique impact-produced flash near the lunar terminator was performed. Maximal brightness of detected thermal flash is 5.2–5.9m in R band, mass of impacted meteoroid is about 0.18–28 kg. Height of shadow in the place of meteoroid’s impact was only about 1 km, making it possible observations of impact-produced dust particles ejected to the lunar exosphere through their sunlight-scattering response. We detected two (fast and slow) clouds that were expanding with 3 km/s and 0.1 km/s, respectively. The maximal brightness reached by these fast and slow clouds in R band was 6.7m and 10m, respectively. Apparent mass of visible ejecta in fast and slow clouds is constrained to 80–8300 and 6–180 kg, respectively. Fast cloud consists of melt droplets and condensed grains while slow cloud consists of ejected lunar regolith dust particles.
Published: 2019
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6. 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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7. Physical models of ten asteroids from an observers' collaboration network

Author: R. Dymock, F. Manzini, S. Boroumand, Stephen M. Slivan, Robert D. Stephens, R. A. Koff, Greg Bolt, M. Fagas, R. Roy, Michael Fauerbach, Brian D. Warner, Josef Ďurech, Margaret Pan, A. Marciniak, M. Crow, Angel F. Lopez, Mikko Kaasalainen, Merideth Frey, Frederick Pilcher, Rita Pacheco, Thomas Bennett, S. Fauvaud, L. Crespo da Silva, C. Bembrick, W. Pych, Donald P. Pray, R. Crippa, Raoul Behrend, R. Poncy, S. Sposetti, Jérôme Berthier, T. Kwiatkowski, Marek Wolf, G. Santacana, R. Durkee, D. Jardine, Krzysztof Kamiński, Tadeusz Michalowski, W. H. Allen, Rui Soles Gonçalves, L. Bernasconi, R. Hirsch, Astronomical Institute, Charles University, Department of Mathematics and Statistics, Rolf Nevanlinna Institute, University of Helsinki, Astronomical Observatory, Adam Mickiewicz University, Vintage Lane Observatory, Observatoire Astronomique de l'Université de Genève, Mount Tarana Observatory, Florida Gulf Coast University, Observatoire des Engarouines, 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, Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Stazzione Astronomica di Sozzago, The WW Crow Observatory, Shed of Science Observatory, Association AstroQueyras, Groupe européen d’observation stellaire (GEOS), Department of Astronomy, Whitin Observatory, Wellesley College, Observatório Astronómico de Linhaceira, Illinois College, Antelope Hills Observatory, 980 Antelope Drive West, Bennett, Observatori Astronomic de Consell, Carbuncle Hill Observatory, Centrum Astronomiczne im. M. Kopernika, Warszawa (CAMK), Observatoire de Blauvac, Observatorio di Gnosca, Goat Mountain Astronomical Research Station, and Palmer Divide Observatory, Colorado Springs
Subjects: Physics, Physical model, 010504 meteorology & atmospheric sciences, Astronomy, Astronomy and Astrophysics, Inversion (meteorology), Astrophysics, 01 natural sciences, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Asteroid, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: International audience; Aims:We present physical models of ten asteroids obtained by means of lightcurve inversion. A substantial part of the photometric data was observed by amateur astronomers. We emphasize the importance of a coordinated network of observers that will be of extreme importance for future all-sky asteroid photometric surveys. Methods: The lightcurve inversion method was used to derive spin states and shape models of the asteroids. Results: We derived spin states and shape model for ten new asteroids: (110) Lydia, (125) Liberatrix, (130) Elektra, (165) Loreley, (196) Philomela, (218) Bianca, (306) Unitas, (423) Diotima, (776) Berbericia, and (944) Hidalgo. This increases the number of asteroid models up to nearly one hundred.
Published: 2007
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8. Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution

Author: J. Hanuš, J. Ďurech, M. Brož, A. Marciniak, B. D. Warner, F. Pilcher, R. Stephens, R. Behrend, B. Carry, D. Čapek, P. Antonini, M. Audejean, K. Augustesen, E. Barbotin, P. Baudouin, A. Bayol, L. Bernasconi, W. Borczyk, J.-G. Bosch, E. Brochard, L. Brunetto, S. Casulli, A. Cazenave, S. Charbonnel, B. Christophe, F. Colas, J. Coloma, M. Conjat, W. Cooney, H. Correira, V. Cotrez, A. Coupier, R. Crippa, M. Cristofanelli, Ch. Dalmas, C. Danavaro, C. Demeautis, T. Droege, R. Durkee, N. Esseiva, M. Esteban, M. Fagas, G. Farroni, M. Fauvaud, S. Fauvaud, F. Del Freo, L. Garcia, S. Geier, C. Godon, K. Grangeon, H. Hamanowa, N. Heck, S. Hellmich, D. Higgins, R. Hirsch, M. Husarik, T. Itkonen, O. Jade, K. Kamiński, P. Kankiewicz, A. Klotz, R. A. Koff, A. Kryszczyńska, T. Kwiatkowski, A. Laffont, A. Leroy, J. Lecacheux, Y. Leonie, C. Leyrat, F. Manzini, A. Martin, G. Masi, D. Matter, J. Michałowski, M. J. Michałowski, T. Michałowski, J. Michelet, R. Michelsen, E. Morelle, S. Mottola, R. Naves, J. Nomen, J. Oey, W. Ogłoza, A. Oksanen, D. Oszkiewicz, P. Pääkkönen, M. Paiella, H. Pallares, J. Paulo, M. Pavic, B. Payet, M. Polińska, D. Polishook, R. Poncy, Y. Revaz, C. Rinner, M. Rocca, A. Roche, D. Romeuf, R. Roy, H. Saguin, P. A. Salom, S. Sanchez, G. Santacana, T. Santana-Ros, J.-P. Sareyan, K. Sobkowiak, S. Sposetti, D. Starkey, R. Stoss, J. Strajnic, J.-P. Teng, B. Trégon, A. Vagnozzi, F. P. Velichko, N. Waelchli, K. Wagrez, H. Wücher, Astronomical Institute of Charles University, Charles University [Prague] (CU), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Palmer Divide Observatory, Organ Mesa Observatory, Goat Mountain Astronomical Research Station, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Observatoire de Bédoin, Observatoire de Chinon, Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), CdR & CdL group, Association T60, Observatoire Midi-Pyrénées, 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)-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, Harfleur Observatory, Observatoire des Engarouines, Collonges Observatory, Chercheur indépendant, Observatoire N°139 d'Antibes, Osservatorio Colleverde di Guidonia, Observatoire de Saint-Sulpice N°947, DPHY, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), 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), Observatorio de San Gervasi, Observatoire de Cabris, Blackberry Observatory, Centre d'Astronomie de Saint-Michel l'Observatoire, Observatoire de Sainte-Hélène, Observatorio Astronómico de Tradate, 138 Village-Neuf, The Amateur Sky Survey (TASS), The Amateur Sky Survey, Shed of Science Observatory, Association AstroQueyras, Association des Utilisateurs de Détecteurs Electroniques (AUDE), Association des Utilisateurs de Détecteurs Electroniques, Observatoire du Bois de Bardon, Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Nordic Optical Telescope (NOT), Instituto de Astrofisica de Canarias (IAC), Hamanowa Astronomical Observatory, DLR Institute of Planetary Research, German Aerospace Center (DLR), Hunters Hill Observatory, Skalnaté Pleso Observatory, A83 Jakokoski Observatory, Institute of Physics [Kielce], Jan Kochanowski University, 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), 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), Antelope Hills Observatory, 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), Stazione Astronomica di Sozzago, Forte Software, Scottish Universities Physics Alliance, Institute for Astronomy (SUPA), University of Edinburgh, Club d'Astronomie Lyon Ampéré [Vaulx-en-Velin] (CALA), Nyrölä Observatory (NYTT), Observatorio Montcabre, Observatorio Astronómico de Mallorca (OAM), Observatorio Astronómico de Mallorca, Kingsgrove Observatory, Mt. Suhora Observatory, Pedagogical University, Astronomy Department, Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), François-Xavier Bagnoud Observatory, Blauvac Obsevatory, Blauvac Observatory, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Gnosca Observatory, DeKalb Observatory, Observatoire astronomique des Makes, Laboratoire Kastler Brossel (LKB (Lhomond)), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institute of Astronomy [Kharkiv], V.N. Karazin Kharkiv National University (KhNU), University of Geneva [Switzerland], European Space Agency (ESA), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), 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), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), 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), University of Helsinki-University of Helsinki, Université Pierre et Marie Curie - Paris 6 (UPMC)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, photometry, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], media_common.quotation_subject, Population, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Inverse transform sampling, Astrophysics, 01 natural sciences, Photometry (optics), models, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Physical model, Minor planets, Astronomy and Astrophysics, Asteroids: general, 13. Climate action, Space and Planetary Science, Sky, Asteroid, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The larger number of models of asteroid shapes and their rotational states derived by the lightcurve inversion give us better insight into both the nature of individual objects and the whole asteroid population. With a larger statistical sample we can study the physical properties of asteroid populations, such as main-belt asteroids or individual asteroid families, in more detail. Shape models can also be used in combination with other types of observational data (IR, adaptive optics images, stellar occultations), e.g., to determine sizes and thermal properties. We use all available photometric data of asteroids to derive their physical models by the lightcurve inversion method and compare the observed pole latitude distributions of all asteroids with known convex shape models with the simulated pole latitude distributions. We used classical dense photometric lightcurves from several sources and sparse-in-time photometry from the U.S. Naval Observatory in Flagstaff, Catalina Sky Survey, and La Palma surveys (IAU codes 689, 703, 950) in the lightcurve inversion method to determine asteroid convex models and their rotational states. We also extended a simple dynamical model for the spin evolution of asteroids used in our previous paper. We present 119 new asteroid models derived from combined dense and sparse-in-time photometry. We discuss the reliability of asteroid shape models derived only from Catalina Sky Survey data (IAU code 703) and present 20 such models. By using different values for a scaling parameter cYORP (corresponds to the magnitude of the YORP momentum) in the dynamical model for the spin evolution and by comparing synthetics and observed pole-latitude distributions, we were able to constrain the typical values of the cYORP parameter as between 0.05 and 0.6., Accepted for publication in A&A, January 15, 2013
Published: 2013
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9. New and updated convex shape models of asteroids based on optical data from a large collaboration network

Author: J. Hanuš, J. Ďurech, D. A. Oszkiewicz, R. Behrend, B. Carry, M. Delbo, O. Adam, V. Afonina, R. Anquetin, P. Antonini, L. Arnold, M. Audejean, P. Aurard, M. Bachschmidt, B. Baduel, E. Barbotin, P. Barroy, P. Baudouin, L. Berard, N. Berger, L. Bernasconi, J-G. Bosch, S. Bouley, I. Bozhinova, J. Brinsfield, L. Brunetto, G. Canaud, J. Caron, F. Carrier, G. Casalnuovo, S. Casulli, M. Cerda, L. Chalamet, S. Charbonnel, B. Chinaglia, A. Cikota, F. Colas, J.-F. Coliac, A. Collet, J. Coloma, M. Conjat, E. Conseil, R. Costa, R. Crippa, M. Cristofanelli, Y. Damerdji, A. Debackère, A. Decock, Q. Déhais, T. Déléage, S. Delmelle, C. Demeautis, M. Dróżdż, G. Dubos, T. Dulcamara, M. Dumont, R. Durkee, R. Dymock, A. Escalante del Valle, N. Esseiva, R. Esseiva, M. Esteban, T. Fauchez, M. Fauerbach, M. Fauvaud, S. Fauvaud, E. Forné, C. Fournel, D. Fradet, J. Garlitz, O. Gerteis, C. Gillier, M. Gillon, R. Giraud, J.-P. Godard, R. Goncalves, Hiroko Hamanowa, Hiromi Hamanowa, K. Hay, S. Hellmich, S. Heterier, D. Higgins, R. Hirsch, G. Hodosan, M. Hren, A. Hygate, N. Innocent, H. Jacquinot, S. Jawahar, E. Jehin, L. Jerosimic, A. Klotz, W. Koff, P. Korlevic, E. Kosturkiewicz, P. Krafft, Y. Krugly, F. Kugel, O. Labrevoir, J. Lecacheux, M. Lehký, A. Leroy, B. Lesquerbault, M. J. Lopez-Gonzales, M. Lutz, B. Mallecot, J. Manfroid, F. Manzini, A. Marciniak, A. Martin, B. Modave, R. Montaigut, J. Montier, E. Morelle, B. Morton, S. Mottola, R. Naves, J. Nomen, J. Oey, W. Ogłoza, M. Paiella, H. Pallares, A. Peyrot, F. Pilcher, J.-F. Pirenne, P. Piron, M. Polińska, M. Polotto, R. Poncy, J. P. Previt, F. Reignier, D. Renauld, D. Ricci, F. Richard, C. Rinner, V. Risoldi, D. Robilliard, D. Romeuf, G. Rousseau, R. Roy, J. Ruthroff, P. A. Salom, L. Salvador, S. Sanchez, T. Santana-Ros, A. Scholz, G. Séné, B. Skiff, K. Sobkowiak, P. Sogorb, F. Soldán, A. Spiridakis, E. Splanska, S. Sposetti, D. Starkey, R. Stephens, A. Stiepen, R. Stoss, J. Strajnic, J.-P. Teng, G. Tumolo, A. Vagnozzi, B. Vanoutryve, J. M. Vugnon, B. D. Warner, M. Waucomont, O. Wertz, M. Winiarski, M. Wolf, Charles University [Prague] (CU), Astronomical Institute of Charles University, Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Bédoin, Observatoire de Chinon, Association des Utilisateurs de Détecteurs Electroniques, Laboratoire de Physique de la Matière Condensée - UR UPJV 2081 (LPMC), Université de Picardie Jules Verne (UPJV), Harfleur Observatory, Ressources des terroirs - UMR 8575, Centre National de la Recherche Scientifique (CNRS), Les Engarouines Observatory, Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Chercheur indépendant, Laboratoire d'optique des solides (LOS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Centre de Recherche Saint-Antoine (UMRS893), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM), Association T60, Observatoire Midi-Pyrénées, 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)-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, Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), CdR & CdL group, Physik-Institut, Universität Zürich [Zürich] = University of Zurich (UZH), Gestion environnementale et traitement biologique des déchets (UR GERE), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Observatorio de San Gervasi, Observatoire de Cabris, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronómico de Tradate, Observatoire N°139 d'Antibes, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), 138 Village-Neuf, Science et Ingénierie des Matériaux et Procédés (SIMaP ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Shed of Science Observatory, Association AstroQueyras, Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatoire du Bois de Bardon, Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Ciências Exatas e Tecnológicas [Viçosa], Universidade Federal de Viçosa = Federal University of Viçosa (UFV), Hamanowa Astronomical Observatory, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), European Southern Observatory (ESO), 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), 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 Chante-Perdrix, 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), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Stazione Astronomica di Sozzago, Milieux aquatiques, écologie et pollutions (UR MALY), German Aerospace Center (DLR), Observatorio Montcabre, Observatorio Astronómico de Mallorca (OAM), Observatorio Astronómico de Mallorca, Kingsgrove Observatory, Gestion Territoriale de l'Eau et de l'environnement (UMR GESTE), École Nationale du Génie de l'Eau et de l'Environnement de Strasbourg (ENGEES)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Organ Mesa Observatory, Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Association des Utilisateurs de Détecteurs Electroniques (AUDE), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon, Laboratoire de Recherche sur la Réactivité des Solides (LRRS), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'intégration, du matériau au système (IMS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Gnosca Observatory, DeKalb Observatory, Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Observatoire astronomique des Makes, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Institute of Neuropathology, University hospital of Zurich [Zurich], Charles University [Prague], University of Helsinki-University of Helsinki, University of Geneva [Switzerland], European Space Agency (ESA), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches Subatomiques (IReS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Cancéropôle du Grand Est-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de la Matière Condensée (EA 2081), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Université de Genève (UNIGE), Centre de Recherche Saint-Antoine (CR Saint-Antoine), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées, Universität Zürich [Zürich] (UZH), L2EP - Équipe Réseaux, Laboratoire d’Électrotechnique et d’Électronique de Puissance - EA 2697 (L2EP), Ecole Centrale de Lille-École Nationale Supérieure d'Arts et Métiers (ENSAM), Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Haute Etude d'Ingénieurs-Université de Lille-Ecole Centrale de Lille-École Nationale Supérieure d'Arts et Métiers (ENSAM), HESAM Université (HESAM)-HESAM Université (HESAM)-Haute Etude d'Ingénieurs-Université de Lille, Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Observatoire Midi-Pyrénées and Association T60, Laboratoire de photonique et de nanostructures (LPN), Universidade Federal de Vicosa (UFV), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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), Centre d'études de chimie métallurgique (CECM), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Laboratoire d’Électrotechnique et d’Électronique de Puissance - ULR 2697 (L2EP), Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), National Science Centre (Poland), Czech Science Foundation, Centre National D'Etudes Spatiales (France), Charles University [Prague] [CU], European Space Astronomy Centre [ESAC], Joseph Louis LAGRANGE [LAGRANGE], Institut de Recherches Subatomiques [IReS], Laboratoire d'Annecy de Physique des Particules [LAPP], Géosciences Paris Sud [GEOPS], Laboratoire d'optique des solides [LOS], Observatoire Astronomique de l'Université de Genève [ObsGE], Gestion environnementale et traitement biologique des déchets [UR GERE], Observatoire astronomique de Strasbourg [ObAS], Science et Ingénierie des Matériaux et Procédés [SIMaP], Laboratoire d’Optique Atmosphérique - UMR 8518 [LOA], Interactions et dynamique des environnements de surface [IDES], Laboratoire de photonique et de nanostructures [LPN], European Southern Observatory [ESO], Institut de recherche en astrophysique et planétologie [IRAP], Laboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA], Milieux aquatiques, écologie et pollutions [UR MALY], German Aerospace Center [DLR], Laboratoire de l'Accélérateur Linéaire [LAL], Université Claude Bernard Lyon 1 [UCBL], Laboratoire de Recherche sur la Réactivité des Solides [LRRS], Laboratoire de l'intégration, du matériau au système [IMS], Laboratoire de Physique Atmosphérique et Planétaire [LPAP], INAF - Osservatorio Astronomico di Padova [OAPD], Argelander Institute for Astronomy [AlfA], ITA, USA, GBR, FRA, DEU, and ESP
Subjects: Solar System, 010504 meteorology & atmospheric sciences, Computer science, media_common.quotation_subject, FOS: Physical sciences, Inverse transform sampling, 01 natural sciences, Gravitation, Photometry (optics), Methods: observational, 0103 physical sciences, QB Astronomy, observational [Methods], Shape optimization, asteroids: general / techniques: photometric / methods: observational / methods: numerical, 010303 astronomy & astrophysics, Scaling, QC, ComputingMilieux_MISCELLANEOUS, QB, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], numerical [Methods], Methods: numerical, photometric [Techniques], Minor planets, Astronomy, Astronomy and Astrophysics, 3rd-DAS, QC Physics, Minor planets, asteroids: general, Space and Planetary Science, Sky, Asteroid, Physics::Space Physics, minor planets, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [Asteroids], Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics, general [minor planets, asteroids]
Abstract: Context. Asteroid modeling efforts in the last decade resulted in a comprehensive dataset of almost 400 convex shape models and their rotation states. These efforts already provided deep insight into physical properties of main-belt asteroids or large collisional families. Going into finer detail (e.g., smaller collisional families, asteroids with sizes 20 km) requires knowledge of physical parameters of more objects. Aims. We aim to increase the number of asteroid shape models and rotation states. Such results provide important input for further studies, such as analysis of asteroid physical properties in different populations, including smaller collisional families, thermophysical modeling, and scaling shape models by disk-resolved images, or stellar occultation data. This provides bulk density estimates in combination with known masses, but also constrains theoretical collisional and evolutional models of the solar system. Methods. We use all available disk-integrated optical data (i.e., classical dense-in-time photometry obtained from public databases and through a large collaboration network as well as sparse-in-time individual measurements from a few sky surveys) as input for the convex inversion method, and derive 3D shape models of asteroids together with their rotation periods and orientations of rotation axes. The key ingredient is the support of more that 100 observers who submit their optical data to publicly available databases. Results. We present updated shape models for 36 asteroids, for which mass estimates are currently available in the literature, or for which masses will most likely be determined from their gravitational influence on smaller bodies whose orbital deflections will be observed by the ESA Gaia astrometric mission. Moreover, we also present new shape model determinations for 250 asteroids, including 13 Hungarias and three near-Earth asteroids. The shape model revisions and determinations were enabled by using additional optical data from recent apparitions for shape optimization. © 2016 ESO., J.H. greatly appreciates the CNES post-doctoral fellowship program. J.H. and M.D. were supported by the project under the contract 11-BS56-008 (SHOCKS) of the French Agence National de la Recherche (ANR), JD by grant GACR 15-04816S of the Czech Science Foundation, DO by the grant NCN 2012/S/ST9/00022 of Polish National Science Center, and A. Marciniak by grant 2014/13/D/ST9/01818 of Polish National Science Center.
Published: 2016
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10. 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
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11. THE SIZE, SHAPE, ALBEDO, DENSITY, AND ATMOSPHERIC LIMIT OF TRANSNEPTUNIAN OBJECT (50000) QUAOAR FROM MULTI-CHORD STELLAR OCCULTATIONS

Author: J. P. Colque, Alain Maury, R. Vieira-Martins, S. Roland, Paolo Tanga, Claudia V. Rodrigues, Leonardo A. Almeida, S. Sposetti, E. Frappa, Felipe Braga-Ribas, A. Amorim, P. Cacella, C. Jacques, Alain Klotz, Rodrigo Leiva, Gonzalo Tancredi, Joe Pollock, W. Beisker, L. Almenares, Estrella Álvarez, Jean Manfroid, William Schoenell, Marcelo Assafin, Michaël Gillon, Audrey Thirouin, François Colas, E. Pimentel, Julio Camargo, R. Salvo, Eduardo Unda-Sanzana, V. S. Magalhães, J. Capeche, Emmanuel Jehin, Ricardo Gil-Hutton, Emmanuel Lellouch, L. Vanzi, Frédéric Vachier, Breno L. Giacchini, Bruno Sicardy, C. Neves, Françoise Roques, Aaron P. LaCluyze, Rene Duffard, Thomas Widemann, Raoul Behrend, Sebastian Bruzzone, Daniel E. Reichart, A. Milone, K. M. Ivarsen, J. B. Haislip, C. E. Cedeño Montaña, Jose Luis Ortiz, Nicolás Morales, Marcelo Emilio, Jean Lecacheux, Ignacio Toledo, 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), Cátedra de Tecnología de la Madera. Departamento de Ingeniería Forestal (CTM-ETSIM), Universidad Politécnica de Madrid (UPM), Observatorio Nacional [Rio de Janeiro], 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), Observatório do Valongo/UFRJ [Rio de Janeiro], Universidade Federal do Rio de Janeiro (UFRJ), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), San Pedro de Atacama Celestial Explorations (SPACE), San Pedro de Atacama Celestial Explorations, Universidade Estadual de Ponta Grossa, Universidade Estadual de Ponta Grossa - State University of Ponta Grossa (UEPG), Institute Patology and Imunology Molecular, Fac Ciencias, Universidade do Porto, Instituto de Astronomıa, universidad catolica del Norte, Institut Parisien de Chimie Moléculaire (IPCM), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Observatório CEAMIG-REA, Universidad Nacional de San Juan (UNSJ), Instituto Nacional de Pesquisas Espaciais (INPE), Ministério da Ciência, Tecnologia e Inovação, European Southern Observatory (ESO), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Gnosca Observatory, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), 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), Euraster, Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Southwest Research Institute [Boulder] (SwRI), Joint ALMA Observatory (JAO), National Radio Astronomy Observatory (NRAO)-European Southern Observatory (ESO), International Occultation Timing Association European Section (IOTA ES), International Occultation Timing Association European Section, Department of Physics and Astronomy [Boone], Appalachian State University, University of North Carolina System (UNC)-University of North Carolina System (UNC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Universidade do Porto = University of Porto, Universidad Nacional de San Juan [Argentine] (UNSJ), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), and European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO)
Subjects: Kuiper belt objects: individual: 50000 Quaoar, 010504 meteorology & atmospheric sciences, Ciencias Físicas, Astrophysics, 7. Clean energy, 01 natural sciences, Planet, TRANSNEPTUNIAN OBJECT, occultations, 0103 physical sciences, Trans-Neptunian object, planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, KUIPER BELT OBJECTS, 0105 earth and related environmental sciences, planets and satellites: atmospheres, [PHYS]Physics [physics], Physics, Astronomy, Astronomy and Astrophysics, Astronomía, Stars, Space and Planetary Science, OCCULTATIONS, Chord (music), ATMOSPHERES, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], CIENCIAS NATURALES Y EXACTAS
Abstract: We present results derived from the first multi-chord stellar occultations by the transneptunian object (50000) Quaoar, observed on 2011 May 4 and 2012 February 17, and from a single-chord occultation observed on 2012 October 15. If the timing of the five chords obtained in 2011 were correct, then Quaoar would possess topographic features (crater or mountain) that would be too large for a body of this mass. An alternative model consists in applying time shifts to some chords to account for possible timing errors. Satisfactory elliptical fits to the chords are then possible, yielding an equivalent radius Requiv = 555±2.5 km and geometric visual albedo pV = 0.109±0.007. Assuming that Quaoar is a Maclaurin spheroid with an indeterminate polar aspect angle, we derive a true oblateness of = 0.087+0.0268 −0.0175, an equatorial radius of 569+24 −17 km, and a density of 1.99 ± 0.46 g cm−3. The orientation of our preferred solution in the plane of the sky implies that Quaoar’s satellite Weywot cannot have an equatorial orbit. Finally, we detect no global atmosphere around Quaoar, considering a pressure upper limit of about 20 nbar for a pure methane atmosphere. Fil: Braga Ribas, F.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil; . Laboratoire d; Fil: Sicardy, B.. Laboratoire d; . Universite Pierre Et Marie Curie; Francia; Fil: Ortiz, J. L.. Consejo Superior de Investigaciones Científicas. Instituto de Astrofísica de Andalucía; España; Fil: Lellouch, E.. Laboratoire d; Fil: Tancredi, G.. Observatorio Astronomico Los Molinos; Uruguay; Fil: Lecacheux, J.. Laboratoire d; Fil: Vieira Martins, R.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil; . L; . Universidade Federal Rural do Rio de Janeiro. Observatorio do Valongo; Brasil; Fil: Camargo, J. I. B.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil; Fil: Assafin, M.. Universidade Federal Rural do Rio de Janeiro. Observatorio do Valongo; Brasil; Fil: Behrend, R.. Observatoire de Geneve; Suiza; Fil: Vachier, F.. L; Fil: Colas, F.. L; Fil: Morales, N.. Consejo Superior de Investigaciones Científicas. Instituto de Astrofísica de Andalucía; España; Fil: Maury, A.. San Pedro de Atacama Celestial Explorations, Chile; Fil: Emilio, M.. Universidad Stadual de Ponta Grossa; Brasil; Fil: Amorim, A.. Universidade Federal Da Santa Catarina; Brasil; Fil: Unda Sanzana, E.. Universidad de Antofagasta. Unidad de Astronomía; Chile; Fil: Roland, S.. Observatorio Astronomico Los Molinos; Uruguay; Fil: Bruzzone, S.. Observatorio Astronomico Los Molinos; Uruguay; Fil: Almeida, L. A.. Centro de Previsao de Tempo e Estudos Climaticos. Instituto Nacional de Pesquisas Espaciais; Brasil; Fil: Rodrigues, C. V.. Centro de Previsao de Tempo e Estudos Climaticos. Instituto Nacional de Pesquisas Espaciais; Brasil; Fil: Jacques, C.. Centro de Estudos Astronomicos de Minas Gerais; Brasil; Fil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico - CONICET - San Juan. Complejo Astronómico; Argentina Fil: Vanzi, L.. Pontificia Universidad Católica de Chile. Department of Electrical Engineering and Center of Astro-Engineering; Chile; Fil: Milone, A. C.. Centro de Previsao de Tempo e Estudos Climaticos. Instituto Nacional de Pesquisas Espaciais; Brasil; Fil: Schoenell, W.. Consejo Superior de Investigaciones Científicas. Instituto de Astrofísica de Andalucía; España; . Universidade Federal Da Santa Catarina; Brasil; Fil: Salvo, R.. Observatorio Astronomico Los Molinos; Uruguay; Fil: Almenares, L.. Observatorio Astronomico Los Molinos; Uruguay; Fil: Jehin, E. Université de Liège. Institut d’Astrophysique; Belgica; Fil: Manfroid, J.. Université de Liège. Institut d’Astrophysique; Belgica; Fil: Sposetti, S.. Gnosca Observatory, Suiza; Fil: Tanga, P.. Observatoire de la Cote D; . Universite de Sophia Antipolis. Laboratoire Lagrange; Francia; Fil: Klotz, A.. Université Toulouse III “Paul Sabatier”. Observatoire Midi-Pyrénées. Institut de Recherche en Astrophysique et Planétologie; Francia; Fil: Frappa, E.. Euraster, Francia; Fil: Cacella, P.. Rede de Astronomia Observacional; Brasil; Fil: Colque, J. P.. Universidad de Antofagasta. Unidad de Astronomía; Chile; Fil: Neves, C.. Universidad Stadual de Ponta Grossa; Brasil; Fil: Alvarez, E. M.. Observatorio Los Algarrobos, Uruguay; Fil: Gillon, M.. Université de Liège. Institut d’Astrophysique; Belgica; Fil: Pimentel, E.. Centro de Estudos Astronomicos de Minas Gerais; Brasil; Fil: Giacchini, B.. Centro de Estudos Astronomicos de Minas Gerais; Brasil; Fil: Roques, F.. Laboratoire d; Fil: Widemann, T.. Laboratoire d; Fil: Magalhães, V. S.. Centro de Previsao de Tempo e Estudos Climaticos. Instituto Nacional de Pesquisas Espaciais; Brasil; Fil: Thirouin, A.. Consejo Superior de Investigaciones Científicas. Instituto de Astrofísica de Andalucía; España; Fil: Duffard, Rene Damian. Centro Informático Científico de Andalucía; España; . Consejo Superior de Investigaciones Científicas. Instituto de Astrofísica de Andalucía; España; Fil: Leiva, R.. Pontificia Universidad Católica de Chile. Department of Electrical Engineering and Center of Astro-Engineering; Chile; Fil: Toledo, I.. Joint Atacama Large Millimeter/submillimeter Array Observatory; Chile; Fil: Capeche, J.. Observatorio Astronomico Los Molinos; Uruguay; Fil: Beisker, W.. International Occultation Timing Association European Section; Alemania; Fil: Pollock, J.. Appalachian State University. Department of Physics and Astronomy; Estados Unidos; Fil: Cedeno Montaña, C. E.. Centro de Previsao de Tempo e Estudos Climaticos. Instituto Nacional de Pesquisas Espaciais; Brasil; Fil: Ivarsen, K. University of North Carolina. Physics and Astronomy Department; Estados Unidos; Fil: Reichart, D.. University of North Carolina. Physics and Astronomy Department; Estados Unidos; Fil: Haislip, J.. University of North Carolina. Physics and Astronomy Department; Estados Unidos; Fil: Lacluyze, A.. University of North Carolina. Physics and Astronomy Department; Estados Unidos
Published: 2013
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12. Study of the Plutino Object (208996) 2003 AZ 84 from Stellar Occultations: Size, Shape, and Topographic Features

Author: A. Klotz, Julio Camargo, T. Hayamizu, Shashikiran Ganesh, Noah Brosch, Felipe Braga-Ribas, Avishay Gal-Yam, Paolo Tanga, J. L. Ortiz, J. Bradshaw, S. Andersson, G. Dangl, H. Tomioka, Rodrigo Leiva, Marcelo Assafin, A. Sharma, Andrea Richichi, Emmanuel Jehin, S. Sposetti, Tapas Baug, Frédéric Vachier, Zhao Ergang, T. Chandrasekhar, Zhu Liying, H. Yamamura, Shai Kaspi, Hayato Watanabe, Puji Irawati, E. Frappa, R. Naves, Eran O. Ofek, Thomas Widemann, Zouhair Benkhaldoun, Nora Morales, C. Rinner, Qian Shengbang, Alain Maury, Pablo Santos-Sanz, Ilan Manulis, Rene Duffard, Yasukazu Ikari, S. Kerr, A. Dias-Oliveira, Raoul Behrend, Jean Manfroid, Vishnu Mohan, J. Jain, Audrey Thirouin, G. Wortmann, A. Daassou, A. R. Gomes-Junior, Michaël Gillon, Hiroyuki Watanabe, Jean Lecacheux, G. Benedetti-Rossi, P. Mahasena, M. Owada, Josselin Desmars, Roberto Vieira-Martins, A. Asai, R. Garcia-Lozano, Bruno Sicardy, T. Haymes, 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), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatorio Nacional [Rio de Janeiro], Observatório Nacional/MCT, Observatório do Valongo/UFRJ [Rio de Janeiro], Universidade Federal do Rio de Janeiro (UFRJ), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Physical Research Laboratory [Ahmedabad] (PRL), and Indian Space Research Organisation (ISRO)
Subjects: Rotation period, Chord (geometry), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], Astrophysics, Rotation, 01 natural sciences, Occultation, law.invention, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Geometric albedo, law, 0103 physical sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [PHYS]Physics [physics], Astronomy and Astrophysics, Light curve, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Amplitude, Space and Planetary Science, Hydrostatic equilibrium, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [PHYS.PHYS.PHYS-DATA-AN]Physics [physics]/Physics [physics]/Data Analysis, Statistics and Probability [physics.data-an], Astrophysics - Earth and Planetary Astrophysics
Abstract: We present results derived from four stellar occultations by the plutino object (208996) 2003~AZ$_{84}$, detected at January 8, 2011 (single-chord event), February 3, 2012 (multi-chord), December 2, 2013 (single-chord) and November 15, 2014 (multi-chord). Our observations rule out an oblate spheroid solution for 2003~AZ$_{84}$'s shape. Instead, assuming hydrostatic equilibrium, we find that a Jacobi triaxial solution with semi axes $(470 \pm 20) \times (383 \pm 10) \times (245 \pm 8)$~km % axis ratios $b/a= 0.82 \pm 0.05$ and $c/a= 0.52 \pm 0.02$, can better account for all our occultation observations. Combining these dimensions with the rotation period of the body (6.75~h) and the amplitude of its rotation light curve, we derive a density $��=0.87 \pm 0.01$~g~cm$^{-3}$ a geometric albedo $p_V= 0.097 \pm 0.009$. A grazing chord observed during the 2014 occultation reveals a topographic feature along 2003~AZ$_{84}$'s limb, that can be interpreted as an abrupt chasm of width $\sim 23$~km and depth $> 8$~km or a smooth depression of width $\sim 80$~km and depth $\sim 13$~km (or an intermediate feature between those two extremes).
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11. THE SIZE, SHAPE, ALBEDO, DENSITY, AND ATMOSPHERIC LIMIT OF TRANSNEPTUNIAN OBJECT (50000) QUAOAR FROM MULTI-CHORD STELLAR OCCULTATIONS

12. Study of the Plutino Object (208996) 2003 AZ 84 from Stellar Occultations: Size, Shape, and Topographic Features

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