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1. Interconnection between adolescents’ and family members’ sleep

Author: E. Reynaud, J. Berthier, E. Louis, E. Eyuboğlu, R. Scelles, and C. M. Schröder
Subjects: Medicine, Science
Abstract: Abstract Deficient sleep has been linked to a broad range of physical, cognitive and mental health impacts, in particular during adolescence. It is thus essential to understand its underlying mechanisms, including family factors. The goal of our study was to assess through combined subjective and objective assessments, how family members’ daily variations in sleep are interconnected, between parents and siblings of adolescents. A total of 111 participants within 30 families were included, of whom 30 adolescents (14.5 years +/− 2.1 years, 46.7% boys), 30 siblings (12.8 years + /− 3.8, 40% boys), 30 mothers (43.5 years +/− 5.5) and 21 fathers (47.5 years +/− 7.6). Sleep was objectively assessed using parallel actigraphy recordings during a single week for all family members. Adolescents’ daily variation in sleep duration and timing displayed many concordances with their siblings’ and their mothers’ sleep, but not with their fathers’ sleep. Adolescents whose parents did not set limits on sleep time or screen use went to bed over an hour later (p
Published: 2024
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2. Evidence for differentiation of the most primitive small bodies

Author: Carry, B., Vernazza, P., Vachier, F., Neveu, M., Hanus, J. Berthier J., Ferrais, M., Jorda, L., Marsset, M., Viikinkoski, M., Bartczak, P., Behrend, R., Benkhaldoun, Z., Birlan, M., Castillo-Rogez, J., Cipriani, F., Colas, F., Drouard, A., Dudzinski, G. P., Desmars, J., Dumas, C., Durech, J., Fetick, R., Fusco, T., Grice, J., Jehin, E., Kaasalainen, M., Kryszczynska, A., Lamy, P., Marchis, F., Marciniak, A., Michalowski, T., Michel, P., Pajuelo, M., Podlewska-Gaca, E., Rambaux, N., Santana-Ros, T., Storrs, A., Tanga, P., Vigan, A., Warner, B., Wieczorek, M., Witasse, O., and Yang, B.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Dynamical models of Solar System evolution have suggested that P-/D-type volatile-rich asteroids formed in the outer Solar System and may be genetically related to the Jupiter Trojans, the comets and small KBOs. Indeed, their spectral properties resemble that of anhydrous cometary dust. High-angular-resolution images of P-type asteroid (87) Sylvia with VLT/SPHERE were used to reconstruct its 3D shape, and to study the dynamics of its two satellites. We also model Sylvia's thermal evolution. The shape of Sylvia appears flattened and elongated. We derive a volume-equivalent diameter of 271 +/- 5 km, and a low density of 1378 +/- 45 kg.m-3. The two satellites orbit Sylvia on circular, equatorial orbits. The oblateness of Sylvia should imply a detectable nodal precession which contrasts with the fully-Keplerian dynamics of the satellites. This reveals an inhomogeneous internal structure, suggesting that Sylvia is differentiated. Sylvia's low density and differentiated interior can be explained by partial melting and mass redistribution through water percolation. The outer shell would be composed of material similar to interplanetary dust particles (IDPs) and the core similar to aqueously altered IDPs or carbonaceous chondrite meteorites such as the Tagish Lake meteorite. Numerical simulations of the thermal evolution of Sylvia show that for a body of such size, partial melting was unavoidable due to the decay of long-lived radionuclides. In addition, we show that bodies as small as 130-150 km in diameter should have followed a similar thermal evolution, while smaller objects, such as comets and the KBO Arrokoth, must have remained pristine, in agreement with in situ observations of these bodies. NASA Lucy mission target (617) Patroclus (diameter~140 km) may, however, be differentiated., Comment: Accepted for publication in A&A
Published: 2021
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3. Gaia Data Release 3: The Solar System survey

Author: P. Tanga, T. Pauwels, F. Mignard, K. Muinonen, A. Cellino, P. David, D. Hestroffer, F. Spoto, J. Berthier, J. Guiraud, W. Roux, B. Carry, M. Delbo, A. Dell'Oro, C. Fouron, L. Galluccio, A. Jonckheere, S.A. Klioner, Y. Lefustec, and L. Liberato...
Subjects: Space and Planetary Science, Astronomy and Astrophysics
Published: 2022
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4. (704) Interamnia: a transitional object between a dwarf planet and a typical irregular-shaped minor body

Author: J. Hanuš, P. Vernazza, M. Viikinkoski, M. Ferrais, N. Rambaux, E. Podlewska-Gaca, A. Drouard, L. Jorda, E. Jehin, B. Carry, M. Marsset, F. Marchis, B. Warner, R. Behrend, V. Asenjo, N. Berger, M. Bronikowska, T. Brothers, S. Charbonnel, C. Colazo, J.-F. Coliac, R. Duffard, A. Jones, A. Leroy, A. Marciniak, R. Melia, D. Molina, J. Nadolny, M. Person, O. Pejcha, H. Riemis, B. Shappee, K. Sobkowiak, F. Soldán, D. Suys, R. Szakats, J. Vantomme, M. Birlan, J. Berthier, P. Bartczak, C. Dumas, G. Dudziński, J. Ďurech, J. Castillo-Rogez, F. Cipriani, R. Fetick, T. Fusco, J. Grice, M. Kaasalainen, A. Kryszczynska, P. Lamy, T. Michalowski, P. Michel, T. Santana-Ros, P. Tanga, F. Vachier, A. Vigan, O. Witasse, and B. Yang
Published: 2020
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5. SsODNet: The Solar system Open Database Network

Author: J. Berthier, B. Carry, M. Mahlke, J. Normand, 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), 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, and 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)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract: The sample of Solar system objects has dramatically increased over the last decades. The amount of measured properties (e.g., diameter, taxonomy, rotation period, thermal inertia) has grown even faster. The benefit of all these developments has, however, not come to full fruition. While some catalogs are publicly available in machine-readable formats on, e.g., the Planetary Data System (PDS), or the Centre de Données astronomiques de Strasbourg (CDS), a significant fraction of results are only tabulated within articles. Furthermore, the designation of small bodies often evolves with time, from potentially several provisional designations, to a single number and finally an official name. Hence, the same object can be referred to by different labels in different studies, making its cross-identification over several sources a complex task. Accessing to all the characteristics of a given body, or a population, can thus be tedious, or even impractical. A universal access point for all measured properties of Solar system objects available in the literature and online databases is thus required. We provide a practical solution to the identification of Solar system objects from any of their multiple names/designations. We also compile and rationalize their properties to provide an easy access to them. We aim to continuously update the database as new measurements become available. We built a Web Service, SsODNet, that offers four interfaces, each corresponding to an identified typical need in the community: name resolution (quaero), compilation of a large corpus of properties (datacloud), determination of the best estimates among compiled values (ssoCard), and statistical description of the population (BFT). The name resolver quaero translates any of the 5 million designations of objects into their current official designation in a fraction of second. The datacloud compiles about a 100 million measurements of many parameters (osculating and proper element, pair and family membership, diameter, albedo, mass, density, spin, phase function, color taxonomy, thermal inertia, and Yarkovsky drift) from over 2,900 articles. Each parameter is associated with an object, and a complete bibliographic reference is linked with it. For each of the 1.2 million objects in the system, a ssoCard providing a single best-estimate for each parameter is available, and delivered in json format, again in a fraction of a second. Finally, the BFT large table compiles all these best-estimates into a single eCSV file for population-wide studies. The four interfaces of SsODNet have a Web service with an application programming interface (API). The SsODNet interfaces are fully operational and freely accessible to everyone (https://ssp.imcce.fr/webservices/ssodnet/). We also propose a python package and command-line tool to acces the service: rocks (https://rocks.readthedocs.io/).
Published: 2022
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6. 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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7. 545 Skin Organoids derived from NCSTN mutated patient-induced pluripotent stem cells recapitulate Hidradenitis Suppurativa pathogenic hallmarks

Author: C. Nait Meddour, P.M. Tricarico, S. Garcovich, J. Berthier, G. Marianne, S. Jamain, and M. Boniotto
Subjects: Cell Biology, Dermatology, Molecular Biology, Biochemistry
Published: 2022
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8. An advanced multipole model for (216) Kleopatra triple system

Author: Laurent Jorda, Josef Hanus, François Colas, Alexis Drouard, J. Grice, Julie Castillo-Rogez, Patrick Michel, Philippe Lamy, Pierre Vernazza, Josef Ďurech, Miroslav Brož, Bin Yang, Matti Viikinkoski, Franck Marchis, Tadeusz Michalowski, Marin Ferrais, Fabrice Cipriani, Thierry Fusco, Nicolas Rambaux, Olivier Witasse, Przemyslaw Bartczak, Arthur Vigan, David Vokrouhlický, Emmanuel Jehin, E. Podlewska-Gaca, Toni Santana-Ros, Frédéric Vachier, M. Pajuelo, Paolo Tanga, S. Benseguane, Romain Fétick, Christophe Dumas, Grzegorz Dudziński, Mirel Birlan, Agnieszka Kryszczyńska, S. Fauvaud, Anna Marciniak, Benoit Carry, J. Berthier, Michael Marsset, Institute of Astronomy [Prague], Charles University [Prague] (CU), Search for Extraterrestrial Intelligence Institute (SETI), 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), 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), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Tampere University of Technology [Tampere] (TUT), Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, SETI Institute, Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire du Bois de Bardon, Astronomical Institute of Romanian Academy, Romanian Academy, Thirty Meter Telescope Observatory, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Pontificia Universidad Católica del Perú = Pontifical Catholic University of Peru (PUCP), Universidad de Alicante, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Czech Science Foundation, Charles University (Czech Republic), National Science Foundation (US), National Aeronautics and Space Administration (US), Generalitat Valenciana, Ministerio de Ciencia, Innovación y Universidades (España), Fédération Wallonie-Bruxelles, and Belgian Science Policy Office
Subjects: 010504 meteorology & atmospheric sciences, fundamental parameters [Planets and satellites], Library science, FOS: Physical sciences, Astrophysics, 01 natural sciences, methods: numerical, Física Aplicada, 0103 physical sciences, Celestial mechanics, planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], numerical [Methods], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Minor planets, Astronomy and Astrophysics, Astrometry, celestial mechanics, asteroids: individual: (216) Kleopatra, individual: (216) Kleopatra [Asteroids], Space and Planetary Science, individual: (216) Kleopatra [Minor planets, asteroids], minor planets, astrometry, TRAPPIST, Christian ministry, Earth and Planetary Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: [Aims] To interpret adaptive-optics observations of (216) Kleopatra, we need to describe an evolution of multiple moons orbiting an extremely irregular body and include their mutual interactions. Such orbits are generally non-Keplerian and orbital elements are not constants. [Methods] Consequently, we used a modified N-body integrator, which was significantly extended to include the multipole expansion of the gravitational field up to the order ℓ = 10. Its convergence was verified against the 'brute-force' algorithm. We computed the coefficients Cℓ m, Sℓ m for Kleopatra's shape, assuming a constant bulk density. For Solar System applications, it was also necessary to implement a variable distance and geometry of observations. Our χ2 metric then accounts for the absolute astrometry, the relative astrometry (second moon with respect to the first), angular velocities, and silhouettes, constraining the pole orientation. This allowed us to derive the orbital elements of Kleopatra's two moons. [Results] Using both archival astrometric data and new VLT/SPHERE observations (ESO LP 199.C-0074), we were able to identify the true periods of the moons, P1 = (1.822359 ± 0.004156) d, P2 = (2.745820 ± 0.004820) d. They orbit very close to the 3:2 mean-motion resonance, but their osculating eccentricities are too small compared to other perturbations (multipole, mutual), meaning that regular librations of the critical argument are not present. The resulting mass of Kleopatra, m1 = (1.49 ± 0.16) × 10-12 M· or 2.97 × 1018 kg, is significantly lower than previously thought. An implication explained in the accompanying paper is that (216) Kleopatra is a critically rotating body., Broz, M. et al., This work has been supported by the Czech Science Foundation through grant 21-11058S (M. Brož, D. Vokrouhlický), 20-08218S (J. Hanuš, J. Ďurech), and by the Charles University Research program No. UNCE/SCI/023. This material is partially based upon work supported by the National Science Foundation under Grant No. 1743015. P.V., A.D., M.F. and B.C. were supported by CNRS/INSU/PNP. M.M. was supported by the National Aeronautics and Space Administration under grant No. 80NSSC18K0849 issued through the Planetary Astronomy Program. The work of TSR was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE). The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant FRFC 2.5.594.09.F. TRAPPIST-North is a project funded by the University of Liège, and performed in collaboration with Cadi Ayyad University of Marrakesh. E. Jehin is a FNRS Senior Research Associate.
Published: 2021
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9. ESASky SSOSS: Solar System Object Search Service and the case of Psyche

Author: E. Racero, Bruno Merín, Deborah Baines, J. González Núñez, P. Rodriguez, M. López-Caniego, Sebastien Besse, I. de la Calle, Elena Puga, Fabrizio Giordano, Th. Müller, Michael Küppers, N. Álvarez Crespo, Benoit Carry, S. Kruk, Max Mahlke, B. López-Martí, M. Wrangblad, Ivan Valtchanov, Henrik Norman, J. Berthier, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), asteroids: individual: Pysche, Physics, Solar System, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, asteroids: general, Psyche, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Limiting magnitude, Observatory, Asteroid, Thermal, minor planets, Emissivity, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract: We introduce in this work the Solar System Object Search Service (SSOSS), a service aimed at providing the scientific community with a search service for all potential detections of SSOs among the ESA astronomy archival imaging data. We illustrate its functionalities using the case of asteroid (16) Psyche, for which no information in the far-IR (70-500 {\mu}m) has previously been reported, to derive its thermal properties in preparation for the upcoming NASA Psyche mission. This service performs a geometrical cross-match of the orbital path of each object with respect to the public high-level imaging footprints stored in the ESA archives. For this first release, three missions were chosen: XMM-Newton, the Hubble Space Telescope (HST), and Herschel Observatory. We present a catalog listing all potential detections of asteroids within estimated limiting magnitude or flux limit in Herschel, XMM-Newton, and HST archival imaging data, including 909 serendipitous detections in Herschel images, 985 in XMM-Newton Optical Monitor camera images, and over 32,000 potential serendipitous detections in HST images. We also present a case study: the analysis of the thermal properties of Psyche from four serendipitous Herschel detections, combined with previously published thermal IR measurements. We see strong evidence for an unusual drop in (hemispherical spectral) emissivity, from 0.9 at 100 {\mu}m down to about 0.6 at 350 {\mu}m, followed by a possible but not well-constrained increase towards 500 {\mu}m, comparable to what was found for Vesta. The combined thermal data set puts a strong constraint on Psyche's thermal inertia (between 20 to 80$J m^{-2} s^{-1/2} K^{-1}$) and favours an intermediate to low level surface roughness (below 0.4 for the rms of surface slopes)., Comment: 21 pages, 17 figures
Published: 2022
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10. A multi-chord stellar occultation by the large trans-Neptunian object (174567) Varda

Author: G. Benedetti-Rossi, R. C. Boufleur, C. Lara, D. Oesper, Benoit Carry, R. Showers, C. J. Anderson, Felipe Braga-Ribas, T. George, Marcelo Emilio, Jose Luis Ortiz, H. Pavlov, K. Thomason, Marcelo Assafin, Josselin Desmars, Marc W. Buie, F. Vachier, J. Berthier, Matthew Kehrli, E. Self, D. Souami, Julio Camargo, P. D. Maley, E. Frappa, Nicolás Morales, R. Vieira-Martins, A. R. Gomes-Júnior, B. E. Morgado, G. Margoti, Bruno Sicardy, Juan M. Cota, R. Dunford, C. Spencer, W. Thomas, J. Bardecker, Keitha McCandless, Pablo Santos-Sanz, J. Lecacheux, Maria L. Garcia, Rene Duffard, Rodrigo Leiva, D. W. Dunham, C. L. Pereira, John Keller, Sorbonne Paris Cité, University of Namur, Federal University of Technology - Paraná (UTFPR / DAFIS), Observatório Nacional/MCTIC, Laboratório Interinstitucional de E-Astronomia - LineA, IAA-CSIC, Institut Polytechnique des Sciences Avancées Ipsa, Sorbonne Université, Laboratoire Lagrange, International Occultation Timing Association (IOTA), College of Southern Idaho, Nasa Johnson Space Center Astronomical Society, Southwest Research Institute, University of Colorado, Universidade Federal do Rio de Janeiro (UFRJ), Universidade Estadual Paulista (Unesp), Tangra Observatory (E24), California Polytechnic State University, Calipatria High School, Euraster, Jimginny Observatory (W08), Universidade Estadual de Ponta Grossa (UEPG), 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), 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), 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), Zoological Research Museum Alexander Koenig (ZFMK), Centre for Molecular Biodiversity Research, Uppsala University, Observatorio Nacional [Rio de Janeiro], Observatório do Valongo/UFRJ [Rio de Janeiro], ENVIRONMENTAL CHANGE INSTITUTE OXFORD GBR, Partenaires IRSTEA, Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Préhistoire et Technologie (PréTech), Université Paris Nanterre (UPN)-Centre National de la Recherche Scientifique (CNRS), Universidade Estadual de Ponta Grossa, Universidade Estadual de Ponta Grossa - State University of Ponta Grossa (UEPG), 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), 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, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Research Council, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Fundação de Amparo à Pesquisa do Estado de São Paulo, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, and National Science Foundation (US)
Subjects: Absolute magnitude, individual: Varda [Kuiper belt objects], 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Occultation, Geometric albedo, 0103 physical sciences, occultations, observational [Methods], Trans-Neptunian object, education, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, Astronomy and Astrophysics, Radius, Albedo, Kuiper belt objects: individual: Varda, Space and Planetary Science, Occultations, methods: observational, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: Full list of authors: Souami, D.; Braga-Ribas, F.; Sicardy, B.; Morgado, B.; Ortiz, J. L.; Desmars, J.; Camargo, J. I. B.; Vachier, F.; Berthier, J.; Carry, B.; Anderson, C. J.; Showers, R.; Thomason, K.; Maley, P. D.; Thomas, W.; Buie, M. W.; Leiva, R.; Keller, J. M.; Vieira-Martins, R.; Assafin, M.; Santos-Sanz, P.; Morales, N.; Duffard, R.; Benedetti-Rossi, G.; Gomes-Júnior, A. R.; Boufleur, R.; Pereira, C. L.; Margoti, G.; Pavlov, H.; George, T.; Oesper, D.; Bardecker, J.; Dunford, R.; Kehrli, M.; Spencer, C.; Cota, J. M.; Garcia, M.; Lara, C.; McCandless, K. A.; Self, E.; Lecacheux, J.; Frappa, E.; Dunham, D.; Emilio, M. .--Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Context. We present results from the first recorded stellar occultation by the large trans-Neptunian object (174567) Varda that was observed on September 10, 2018. Varda belongs to the high-inclination dynamically excited population, and has a satellite, Ilmarë, which is half the size of Varda. Aims. We determine the size and albedo of Varda and constrain its 3D shape and density. Methods. Thirteen different sites in the USA monitored the event, five of which detected an occultation by the main body. A best-fitting ellipse to the occultation chords provides the instantaneous limb of the body, from which the geometric albedo is computed. The size and shape of Varda are evaluated, and its bulk density is constrained using Varda's mass as is known from previous works. Results. The best-fitting elliptical limb has semi-major (equatorial) axis of (383 ± 3) km and an apparent oblateness of 0.066 ± 0.047, corresponding to an apparent area-equivalent radius R′equiv = (370±7) km and geometric albedo pv = 0.099 ± 0.002 assuming a visual absolute magnitude HV = 3.81 ± 0.01. Using three possible rotational periods for the body (4.76, 5.91, and 7.87 h), we derive corresponding MacLaurin solutions. Furthermore, given the low-amplitude (0.06 ± 0.01) mag of the single-peaked rotational light-curve for the aforementioned periods, we consider the double periods. For the 5.91 h period (the most probable) and its double (11.82 h), we find bulk densities and true oblateness of ρ = (1.78 ± 0.06) g cm-3, ϵ = 0.235 ± 0.050, and ρ = (1.23 ± 0.04) g cm-3, ϵ = 0.080 ± 0.049. However, it must be noted that the other solutions cannot be excluded just yet. © D. Souami et al. 2020., This campaign was carried out within the "Lucky Star" umbrella that agglomerates the efforts of the Paris, Granada and Rio teams. It is funded by the European Research Council under the European Community's H2020 (2014-2020/ERC Grant Agreement No. 669416). 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. 427700/2018-3, 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, MA FAPERJ grant E-26/111.488/2013 and ARGJr FAPESP grant 2018/11239-8. 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 for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). P.S.-S. acknowledges financial support by the Spanish grant AYA-RTI2018-098657-J-I00 "LEO-SBNAF" (MCIU/AEI/FEDER, UE). Observations from the RECON network were provided by students, teachers, and community members, including Xavier Banaga, Jesus Bustos, Amanda Carrillo, Dorey W. Conway, Kenneth Conway, Danielle D. Laguna, Andrew E. McCandless, Kaitlin McArdle, and Jared T. White, Jr. The observers listed in this paper are but a small fraction of the total RECON network and their dedication to this project is deeply appreciated. Funding for RECON was provided by grants from NSF AST-1413287, AST-1413072, AST-1848621, and AST-1212159. 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. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France (DOI: 10.26093/cds/vizier). The original description of the VizieR service was published in Ochsenbein et al. (2000).
Published: 2020
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11. The shape of (7) Iris as evidence of an ancient large impact?

Author: Miroslav Brož, Philippe Lamy, Anna Marciniak, Josef Ďurech, J. Grice, M. Pajuelo, Paolo Tanga, Patrick Michel, Benoit Carry, Marin Ferrais, Emmanuel Jehin, Bin Yang, Alexis Drouard, Toni Santana-Ros, Frédéric Vachier, Franck Marchis, Michael Marsset, Matti Viikinkoski, Josef Hanus, Romain Fétick, Olivier Witasse, Christophe Dumas, J. Berthier, François Colas, Julie Castillo-Rogez, Agnieszka Kryszczyńska, Tadeusz Michalowski, Mikko Kaasalainen, Grzegorz Dudziński, Pierre Vernazza, Przemyslaw Bartczak, E. Podlewska-Gaca, Mirel Birlan, Thierry Fusco, H. Le Coroller, Arthur Vigan, Laurent Jorda, Fabrice Cipriani, Astronomical Institute of Charles University, Charles University [Prague] (CU), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), 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), Department of Mathematics [Tampere], Tampere University of Technology [Tampere] (TUT), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-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), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Search for Extraterrestrial Intelligence Institute (SETI), 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), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), West Pomeranian University of Technology in Szczecin (ZUT), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, The Open University [Milton Keynes] (OU), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), TMT International Observatory, Pontificia Universidad Católica del Perú = Pontifical Catholic University of Peru (PUCP), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), 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, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Technical University of Szczecin (TUNIV), Technical university of Szczecin, European Space Agency (ESA), TMT Observatory, and Pontificia Universidad Católica del Perú (PUCP)
Subjects: Solar System, Planetesimal, 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, methods: numerical, Impact crater, Angular diameter, 0103 physical sciences, medicine, Iris (anatomy), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Collisional family, Astronomy and Astrophysics, 15. Life on land, medicine.anatomical_structure, 13. Climate action, Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], minor planets, asteroids: individual: 7 Iris, methods: observational, Astrophysics - Earth and Planetary Astrophysics
Abstract: Asteroid (7) Iris is an ideal target for disk-resolved imaging owing to its brightness (V$\sim$7-8) and large angular size of 0.33 arcsec during its apparitions. Iris is believed to belong to the category of large unfragmented asteroids that avoided internal differentiation, implying that its current shape and topography may record the first few 100 Myr of the solar system's collisional evolution. We recovered information about the shape and surface topography of Iris from disk-resolved VLT/SPHERE/ZIMPOL images acquired in the frame of our ESO large program. We used the All-Data Asteroid Modeling (ADAM) shape reconstruction algorithm to model the 3D shape of Iris, using optical disk-integrated data and disk-resolved images from SPHERE as inputs. We analyzed the SPHERE images to infer the asteroid's global shape and the morphology of its main craters. We present the volume-equivalent diameter D$_{{\rm eq}}$=214$\pm$5 km, and bulk density $\rho$=2.7$\pm$0.3 g cm$^{-3}$ of Iris. Its shape appears to be consistent with that of an oblate spheroid with a large equatorial excavation. We identified eight putative surface features 20--40 km in diameter detected at several epochs, which we interpret as impact craters. Craters on Iris have depth-to-diameter ratios that are similar to those of analogous 10 km craters on Vesta. The bulk density of Iris is consistent with that of its meteoritic analog, namely LL ordinary chondrites. Considering the absence of a collisional family related to Iris and the number of large craters on its surface, we suggest that its equatorial depression may be the remnant of an ancient (at least 3 Gyr) impact. Iris's shape further opens the possibility that large planetesimals formed as almost perfect oblate spheroids. Finally, we attribute the difference in crater morphology between Iris and Vesta to their different surface gravities., Comment: Accepted for publication in Astronomy and Astrophysics
Published: 2019
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12. Closing the gap between Earth-based and interplanetary mission observations: Vesta seen by VLT/SPHERE

Author: Olivier Witasse, Tadeusz Michalowski, Anna Marciniak, J. Berthier, Benoit Carry, Benoit Neichel, Arthur Vigan, Michael Marsset, E. Podlewska-Gaca, Marin Ferrais, P. Lamy, Laurent Jorda, Pierre Vernazza, Toni Santana-Ros, Bin Yang, Josef Hanus, Matti Viikinkoski, Franck Marchis, Frédéric Vachier, Przemyslaw Bartczak, Christophe Dumas, Mirel Birlan, R. Jl. Fétick, François Colas, Julie Castillo-Rogez, Patrick Michel, Laurent M. Mugnier, Agnieszka Kryszczyńska, M. Pajuelo, Paolo Tanga, H. Le Coroller, Fabrice Cipriani, Thierry Fusco, Alexis Drouard, Mikko Kaasalainen, Grzegorz Dudziński, Emmanuel Jehin, 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), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Joseph Louis LAGRANGE (LAGRANGE), 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), Fundació Privada Observatori Esteve Duran, Charles University [Prague], Tampere University of Technology [Tampere] (TUT), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Adam Mickiewicz University in Poznań (UAM), Laboratoire d'Electronique et des Technologies de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS), Université de Liège, Institut d'Astrophysique et de Géophysique [Liège], Department of Mathematics [Tampere], Astronomical Observatory [Poznan], 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), Amgen (Europe) GmbH, Galaxies, Etoiles, Physique, Instrumentation (GEPI), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Pontificia Universidad Católica del Perú (PUCP), Universisty of Szczecin (Szczecin) (Institute of Physics), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Tampere University, Computing Sciences, DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), 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, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Charles University [Prague] (CU), 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), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of Szczecin, 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), Agence Spatiale Européenne = European Space Agency (ESA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), 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), Pontificia Universidad Católica del Perú = Pontifical Catholic University of Peru (PUCP), European Space Astronomy Centre (ESAC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Nanophysique Magnétisme et Optoélectronique (LNMO), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), and Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)
Subjects: Point spread function, [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], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Context (language use), techniques: image processing, Astrophysics, 01 natural sciences, Interplanetary mission, Observatory, 0103 physical sciences, 111 Mathematics, 010303 astronomy & astrophysics, Image resolution, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Earth and Planetary Astrophysics (astro-ph.EP), techniques: high angular resolution, Astronomy and Astrophysics, asteroids: individual: Vesta, Albedo, 13. Climate action, Space and Planetary Science, Asteroid, minor planets, methods: observational, Interplanetary spaceflight, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: International audience; Context. Over the past decades, several interplanetary missions have studied small bodies in situ, leading to major advances in our understanding of their geological and geophysical properties. These missions, however, have had a limited number of targets. Among them, the NASA Dawn mission has characterised in detail the topography and albedo variegation across the surface of asteroid (4) Vesta down to a spatial resolution of 20 m pixel-1 scale. Aims: Here our aim was to determine how much topographic and albedo information can be retrieved from the ground with VLT/SPHERE in the case of Vesta, having a former space mission (Dawn) providing us with the ground truth that can be used as a benchmark. Methods: We observed Vesta with VLT/SPHERE/ZIMPOL as part of our ESO large programme (ID 199.C-0074) at six different epochs, and deconvolved the collected images with a parametric point spread function (PSF). We then compared our images with synthetic views of Vesta generated from the 3D shape model of the Dawn mission, on which we projected Vesta's albedo information. Results: We show that the deconvolution of the VLT/SPHERE images with a parametric PSF allows the retrieval of the main topographic and albedo features present across the surface of Vesta down to a spatial resolution of 20-30 km. Contour extraction shows an accuracy of 1 pixel (3.6 mas). The present study provides the very first quantitative estimate of the accuracy of ground-based adaptive-optics imaging observations of asteroid surfaces. Conclusions: In the case of Vesta, the upcoming generation of 30-40 m telescopes (ELT, TMT, GMT) should in principle be able to resolve all of the main features present across its surface, including the troughs and the north-south crater dichotomy, provided that they operate at the diffraction limit. Reduced images of Table A.1 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/623/A6Based on observations made with ESO Telescopes at the Paranal Observatory under programme ID 199.C-0074 (PI: P. Vernazza).
Published: 2019
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13. Finite Element Method for Micro- and Nano-Systems for Biotechnology

Author: J. Berthier
Subjects: Materials science, Nano, Nanotechnology, Finite element method
Published: 2017
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14. 3D shape of asteroid (6) Hebe from VLT/SPHERE imaging: Implications for the origin of ordinary H chondrites

Author: Christophe Dumas, Marco Delbo, Pierre Vernazza, J. Grice, Thierry Fusco, J. Berthier, Emmanuel Jehin, T. G. Müller, Josef Hanus, Michaël Gillon, Michael Marsset, F. Kugel, Raoul Behrend, Matti Viikinkoski, J. Caron, Sarah M. Sonnett, Bin Yang, Benoit Carry, Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), 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), TMT Observatory, Astronomical Institute of Charles University, Charles University [Prague] (CU), Tampere University of Technology [Tampere] (TUT), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Max-Planck-Institut für Extraterrestrische Physik (MPE), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, The Open University [Milton Keynes] (OU), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Planetary Science Institute [Tucson] (PSI), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Tampere University, Mathematics, Research group: Inverse Problems, 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), TMT International Observatory, 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), Université de Genève = University of Geneva (UNIGE), Astrophysics Research Centre, Queen's University Belfast, 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), Astéroïdes, comètes, météores et éphémérides (ACME), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Astronomical Institute, Charles University, Department of Mathematics, Tampere University of Technology, Max-Planck-Institut fur extraterrestrische Physik, University of Liège, Open University, European Southern Observatory, ONERA, Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, and CdR & CdL Group: Lightcurves of Minor Planets and Variable Stars
Subjects: Rotation period, 010504 meteorology & atmospheric sciences, ASTEROIDE, FOS: Physical sciences, Context (language use), Astrophysics, OPTIQUE ADAPTATIVE, 01 natural sciences, VLT, MINOR PLANETS, Chondrite, 0103 physical sciences, TECHNIQUES, 111 Mathematics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), biology, METEORITES, Hebe, HIGH ANGULAR RESOLUTION, Astronomy and Astrophysics, Light curve, biology.organism_classification, ASTEROIDS INDIVIDUAL (6) HEBE, METEORS, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], METEOROIDS, Meteorite, 13. Climate action, Space and Planetary Science, Asteroid, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, Asteroid belt, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. The high-angular-resolution capability of the new-generation ground-based adaptive-optics camera SPHERE at ESO VLT allows us to assess, for the very first time, the cratering record of medium-sized (D~100-200 km) asteroids from the ground, opening the prospect of a new era of investigation of the asteroid belt's collisional history. Aims. We investigate here the collisional history of asteroid (6) Hebe and challenge the idea that Hebe may be the parent body of ordinary H chondrites, the most common type of meteorites found on Earth (~34% of the falls). Methods. We observed Hebe with SPHERE as part of the science verification of the instrument. Combined with earlier adaptive-optics images and optical light curves, we model the spin and three-dimensional (3D) shape of Hebe and check the consistency of the derived model against available stellar occultations and thermal measurements. Results. Our 3D shape model fits the images with sub-pixel residuals and the light curves to 0.02 mag. The rotation period (7.274 47 h), spin (343 deg,+47 deg), and volume-equivalent diameter (193 +/- 6km) are consistent with previous determinations and thermophysical modeling. Hebe's inferred density is 3.48 +/- 0.64 g.cm-3 , in agreement with an intact interior based on its H-chondrite composition. Using the 3D shape model to derive the volume of the largest depression (likely impact crater), it appears that the latter is significantly smaller than the total volume of close-by S-type H-chondrite-like asteroid families. Conclusions. Our results imply that (6) Hebe is not the most likely source of H chondrites. Over the coming years, our team will collect similar high-precision shape measurements with VLT/SPHERE for ~40 asteroids covering the main compositional classes, thus providing an unprecedented dataset to investigate the origin and collisional evolution of the asteroid belt., Comment: 11 pages, 13 figures, accepted for publication in A&A
Published: 2017
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15. Gaia Data Release 1, Pre-processing and source list creation

Author: C. Fabricius, U. Bastian, J. Portell, J. Castañeda, M. Davidson, N. C. Hambly, M. Clotet, M. Biermann, A. Mora, D. Busonero, A. Riva, A. G. A. Brown, R. Smart, U. Lammers, J. Torra, R. Drimmel, G. Gracia, W. Löffler, A. Spagna, L. Lindegren, S. Klioner, A. Andrei, N. Bach, L. Bramante, T. Brüsemeister, G. Busso, J. M. Carrasco, M. Gai, N. Garralda, J. J. González-Vidal, R. Guerra, M. Hauser, S. Jordan, C. Jordi, H. Lenhardt, F. Mignard, R. Messineo, A. Mulone, I. Serraller, U. Stampa, P. Tanga, A. van Elteren, W. van Reeven, H. Voss, U. Abbas, W. Allasia, M. Altmann, S. Anton, C. Barache, U. Becciani, J. Berthier, L. Bianchi, A. Bombrun, S. Bouquillon, G. Bourda, B. Bucciarelli, A. Butkevich, R. Buzzi, R. Cancelliere, T. Carlucci, P. Charlot, R. Collins, G. Comoretto, N. Cross, M. Crosta, F. de Felice, A. Fienga, F. Figueras, E. Fraile, R. Geyer, J. Hernandez, D. Hobbs, W. Hofmann, S. Liao, E. Licata, M. Martino, P. J. McMillan, D. Michalik, R. Morbidelli, P. Parsons, M. Pecoraro, M. Ramos-Lerate, M. Sarasso, H. Siddiqui, I. Steele, H. Steidelmüller, F. Taris, A. Vecchiato, A. Abreu, E. Anglada, S. Boudreault, M. Cropper, B. Holl, N. Cheek, C. Crowley, J. M. Fleitas, A. Hutton, J. Osinde, N. Rowell, E. Salguero, E. Utrilla, N. Blagorodnova, M. Soffel, J. Osorio, D. Vicente, J. Cambras, H.-H. Bernstein, Nelson Mandela Metropolitan University [Port Elizabeth, South Africa], Zentrum für astronomie, Universität Heidelberg [Heidelberg], Open University of Israël, Department of nuclear medicine, Haukeland University Hospital, University of Bergen (UiB)-University of Bergen (UiB), Department of Clinical Medicine, University of Bergen (UiB), Departamento de Microbiología y Parasitología [Lugo, Spain], Laboratorio de Referencia de E. coli [Lugo, Spain] (LREC), Universidade de Santiago de Compostela [Spain] (USC )-Universidade de Santiago de Compostela [Spain] (USC ), Institute of Hepatology, Birkbeck College [University of London]-Foundation for Liver Research, INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Agence Spatiale Européenne (ESA), European Space Agency (ESA), ARHEOINVEST, Universitatea Alexandru Ioan Cuza [Lasi], Department of Medicine, Icahn School of Medicine at Mount Sinai [New York] (MSSM), CICEnergigune, Astrometry, Istituto Nazionale di Astrofisica (INAF)-Istituto Nazionale di Astrofisica (INAF), Laboratorio de Inmunologıa y Virologıa, Facultad de Ciencias Biológicas, Universidad Autónoma de Nuevo León, San Nicolas de los Garza, Laboratório de Ictiologia e Pesca, Universidade Federal de Rondônia [Brésil] (UNIR), Department of Pathology and Cell Biology, Columbia University [New York], AUTRES, EURIX (.), Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Récepteurs et Canaux Ioniques Membranaires (RCIM), Université d'Angers (UA)-Institut National de la Recherche Agronomique (INRA), 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 Grenoble Alpes - UFR Langage, lettres et arts du spectacle, information et communication - Dpt Lettres et arts du spectacle (UGA UFR LLASIC LAS), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut de Chimie Moléculaire de Reims - UMR 7312 (ICMR), SFR Condorcet, Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Centre National de la Recherche Scientifique (CNRS)-Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Centre National de la Recherche Scientifique (CNRS)-SFR CAP Santé (Champagne-Ardenne Picardie Santé), Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), M2A 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Biological, Environmental and Rural Sciences (IBERS), Géoazur (GEOAZUR 7329), Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Solvay (France), Chinese Academy of Sciences [Beijing] (CAS), Human Cancer Genetics Program, Comprehensive Cancer Center-College of Medicine and Public Health [Colombus], Astrophysics Research Institute [Liverpool] (ARI), Liverpool John Moores University (LJMU), Instituto Superior de Engenharia de Lisboa (ISEL), Centre of Technology and Systems (CTS), Faculdade de Ciências e Tecnologia = School of Science & Technology (FCT NOVA), Universidade Nova de Lisboa = NOVA University Lisbon (NOVA)-Universidade Nova de Lisboa = NOVA University Lisbon (NOVA), Departamento de Fisica de la Materia Condensada [Madrid] (FMC), Facultad de Ciencas [Madrid], Universidad Autonoma de Madrid (UAM)-Universidad Autonoma de Madrid (UAM), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Heckscher-Klinikum, University of Las Palmas de Gran Canaria (ULPGC), Karl-Franzens-Universität Graz, University of Bergen (UIB)-University of Bergen (UIB), University of Bergen (UIB), Universidade Federal de Rondônia, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Récepteurs et Canaux Ioniques Membranaires (RCIM), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA), Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Université de Picardie Jules Verne (UPJV)-Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Faculty of Sciences and Technology (FCT NOVA), Universidade Nova de Lisboa (NOVA)-Universidade Nova de Lisboa (NOVA), Departamento de Fisica de la Materia Condensada, Universidad Autonoma de Madrid, Universidad Autonoma de Madrid (UAM), Nelson Mandela University [Port Elizabeth], Universität Heidelberg [Heidelberg] = Heidelberg University, Agence Spatiale Européenne = European Space Agency (ESA), EURIX Software Innovators, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Université de Reims Champagne-Ardenne (URCA)-Institut de Chimie du CNRS (INC)-SFR CAP Santé (Champagne-Ardenne Picardie Santé), Université de Reims Champagne-Ardenne (URCA)-Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS)-SFR Condorcet, Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS)-Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), 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)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Universidad Autónoma de Madrid (UAM)-Universidad Autónoma de Madrid (UAM), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), ITA, GBR, FRA, DEU, ESP, NLD, CHN, SWE, Universidade de Santiago de Compostela [A Coruña, Spain] (USC )-Universidade de Santiago de Compostela [A Coruña, Spain] (USC ), Mount Sinai School of Medicine, Géoazur (GEOAZUR), Université Nice Sophia Antipolis (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Ingénierie des Systèmes Biologiques et des Procédés (LISBP), Institut National de la Recherche Agronomique (INRA)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), and Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Astrometria, Computer science, FOS: Physical sciences, Star (graph theory), 01 natural sciences, Set (abstract data type), Astrometry, Methods: data analysis, Space vehicles: instruments, Astronomy and Astrophysics, Space and Planetary Science, 0103 physical sciences, Point (geometry), 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, QB, 010308 nuclear & particles physics, Payload, Galaxies, Galàxies, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cardinal point, Astrophysics - Instrumentation and Methods for Astrophysics, Algorithm
Abstract: International audience; Context. The first data release from the Gaia mission contains accurate positions and magnitudes for more than a billion sources, and proper motions and parallaxes for the majority of the 2.5 million Hipparcos and Tycho-2 stars. Aims: We describe three essential elements of the initial data treatment leading to this catalogue: the image analysis, the construction of a source list, and the near real-time monitoring of the payload health. We also discuss some weak points that set limitations for the attainable precision at the present stage of the mission. Methods: Image parameters for point sources are derived from one-dimensional scans, using a maximum likelihood method, under the assumption of a line spread function constant in time, and a complete modelling of bias and background. These conditions are, however, not completely fulfilled. The Gaia source list is built starting from a large ground-based catalogue, but even so a significant number of new entries have been added, and a large number have been removed. The autonomous onboard star image detection will pick up many spurious images, especially around bright sources, and such unwanted detections must be identified. Another key step of the source list creation consists in arranging the more than 1010 individual detections in spatially isolated groups that can be analysed individually. Results: Complete software systems have been built for the Gaia initial data treatment, that manage approximately 50 million focal plane transits daily, giving transit times and fluxes for 500 million individual CCD images to the astrometric and photometric processing chains. The software also carries out a successful and detailed daily monitoring of Gaia health.
Published: 2016
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16. Near-infrared spatially resolved spectroscopy of (136108) Haumea’s multiple system

Author: Frédéric Vachier, Christophe Dumas, Benoit Carry, Maria Antonieta Barucci, Florian Gourgeot, F. Merlin, Pedro Lacerda, J. Berthier, European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), 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), Institut de biologie et chimie des protéines [Lyon] (IBCP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), 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), Queens University Belfast, European Space Agency (ESA), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, and 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)
Subjects: Physics, Orbital elements, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Solar System, Very Large Telescope, 010504 meteorology & atmospheric sciences, Near-infrared spectroscopy, Haumea, Dwarf planet, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, 01 natural sciences, Far infrared, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: The transneptunian region of the solar system is populated by a wide variety of icy bodies showing great diversity. The dwarf planet (136108) Haumea is among the largest TNOs and displays a highly elongated shape and hosts two moons, covered with crystalline water ice like Hamuea. Haumea is also the largest member of the sole TNO family known to date. A catastrophic collision is likely responsible for its unique characteristics. We report here on the analysis of a new set of observations of Haumea obtained with SINFONI at the ESO VLT. Combined with previous data, and using light-curve measurements in the optical and far infrared, we carry out a rotationally resolved spectroscopic study of the surface of Haumea. We describe the physical characteristics of the crystalline water ice present on the surface of Haumea for both regions, in and out of the Dark Red Spot (DRS), and analyze the differences obtained for each individual spectrum. The presence of crystalline water ice is confirmed over more than half of the surface of Haumea. Our measurements of the average spectral slope confirm the redder characteristic of the spot region. Detailed analysis of the crystalline water-ice absorption bands do not show significant differences between the DRS and the remaining part of the surface. We also present the results of applying Hapke modeling to our data set. The best spectral fit is obtained with a mixture of crystalline water ice (grain sizes smaller than 60 micron) with a few percent of amorphous carbon. Improvements to the fit are obtained by adding ~10% of amorphous water ice. Additionally, we used the IFU-reconstructed images to measure the relative astrometric position of the largest satellite Hi`iaka and determine its orbital elements. An orbital solution was computed with our genetic-based algorithm GENOID and our results are in full agreement with recent results., Comment: Accepted for publication in A&A
Published: 2016
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17. VLT/SPHERE- and ALMA-based shape reconstruction of asteroid (3) Juno (Corrigendum)

Author: Thierry Fusco, Matti Viikinkoski, Christophe Dumas, Pierre Kervella, Michael Marsset, William J. Merline, Mikko Kaasalainen, Bin Yang, Pierre Vernazza, Benoit Carry, J. Berthier, Josef Ďurech, Tampere University of Technology [Tampere] (TUT), Department of Mathematics and Statistics, Astronomical Institute of Charles University, Charles University [Prague] (CU), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), 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), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Laboratoire de Nanophysique Magnétisme et Optoélectronique (LNMO), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), European Southern Observatory (ESO), 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), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT), and 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)
Subjects: Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, Astronomy and Astrophysics, Astrophysics, Shape reconstruction, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 01 natural sciences, ComputingMilieux_MISCELLANEOUS
Abstract: 1 Department of Mathematics, Tampere University of Technology, PO Box 553, 33101 Tampere, Finland e-mail: matti.viikinkoski@tut.fi 2 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holesovickach 2, 18000 Prague, Czech Republic 3 ACME, IMCCE, UMR 8028 du CNRS, UPMC, Universite de Lille 1, 77 Av. Denfert-Rochereau, 75014 Paris, France 4 Laboratoire Lagrange, UMR 7293 CNRS, UNS, Observatoire de la Cote d’Azur, 06304 Nice, France 5 European Southern Observatory (ESO), Alonso de Cordova 3107, 1900 Casilla Vitacura, Santiago, Chile 6 Aix-Marseille University, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France 7 ONERA − Optics Department, 29 avenue de la Division Leclerc, 92322 Chatillon Cedex, France 8 Southwest Research Institute, 1050 Walnut St., #300 Boulder, CO 80302, USA 9 Unidad Mixta Internacional FCA (UMI 3386), CNRS/INSU & Universidad de Chile, Las Condes, Santiago, Chile 10 LESIA (UMR 8109), Observatoire de Paris, CNRS, UPMC, Univ. Paris-Diderot, PSL, 5 place Jules Janssen, 92195 Meudon, France
Published: 2015
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18. VLT/SPHERE- and ALMA-based shape reconstruction of asteroid (3) Juno

Author: Christophe Dumas, J. Berthier, Pierre Vernazza, William J. Merline, Matti Viikinkoski, Michael Marsset, Mikko Kaasalainen, Benoit Carry, Thierry Fusco, Pierre Kervella, Bin Yang, Josef Ďurech, Department of Mathematics [Tampere], Tampere University of Technology [Tampere] ( TUT ), Astronomical Institute of Charles University, Charles University [Prague], European Space Astronomy Centre, 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 ), ONERA - The French Aerospace Lab ( Chatillon ), ONERA, Centre de Formation et de Recherche sur les Environnements Méditérranéens ( CEFREM ), Université de Perpignan Via Domitia ( UPVD ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Space Studies [Boulder], Southwest Research Institute [Boulder] ( SwRI ), CNRS / Univ. de Chile, Laboratoire Franco-Chilien d'Astronomie ( LFCA ), Centre National de la Recherche Scientifique ( CNRS ), 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 Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Astrophysique de Marseille ( LAM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Aix Marseille Université ( AMU ) -Centre National d'Etudes Spatiales ( CNES ), Tampere University of Technology [Tampere] (TUT), Charles University [Prague] (CU), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), 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), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Centre de Formation et de Recherche sur les Environnements Méditérranéens (CEFREM), Université de Perpignan Via Domitia (UPVD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Southwest Research Institute [Boulder] (SwRI), Laboratoire Franco-Chilien d'Astronomie (LFCA), Universidad de Chile = University of Chile [Santiago] (UCHILE)-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción - University of Concepcion [Chile], 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), 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 Space Agency (ESA), 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 de Perpignan Via Domitia (UPVD)-Centre National de la Recherche Scientifique (CNRS), Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Chile, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Universidad de Chile-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Physics, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astronomy, Astronomy and Astrophysics, Astrophysics, Atacama Large Millimeter Array, 13. Climate action, Space and Planetary Science, Asteroid, [SDU]Sciences of the Universe [physics], Stellar occultation, Shape reconstruction, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Large size
Abstract: International audience; We use the recently released Atacama Large Millimeter Array (ALMA) and VLT/SPHERE science verification data, together with earlier adaptive-optics images, stellar occultation, and lightcurve data to model the 3D shape and spin of the large asteroid (3) Juno with the all-data asteroid modelling (ADAM) procedure. These data set limits on the plausible range of shape models, yielding reconstructions suggesting that, despite its large size, Juno has sizable unrounded features moulded by non-gravitational processes such as impacts.
Published: 2015
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19. Numerical modeling of superparamagnetic sub-micronic particles trajectories under the coupled action of 3D force fields

Author: J. Berthier, P. Pham, and P. Massé
Subjects: Physics, Classical mechanics, Computer simulation, Field (physics), Computation, Finite difference method, Vector field, Condensed Matter Physics, Instrumentation, Force field (chemistry), Finite element method, Action (physics), Electronic, Optical and Magnetic Materials
Abstract: Trajectories of superparamagnetic sub-micronic particles submitted to a multi-force field are modeled numerically by a Finite Element Method. The first step is the computation of the magnetic forces and the carrier fluid velocity field, the second step is the computation of the trajectories using a Finite Difference Method with a predictor-corrector scheme.
Published: 2000
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20. CCD photometry, spin and shape models of five asteroids: 225, 360, 416, 516, and 1223

Author: J. Boussuge, R. Baranowski, T. Kwiatkowski, W. Pych, S. Fauvaud, J. Berthier, P. Denchev, Agnieszka Kryszczyńska, and Tadeusz Michalowski
Subjects: Physics, Photometry (optics), Asteroid, General Physics and Astronomy, Astronomy, Astrophysics
Abstract: New CCD photometric observations for 225 Henrietta (1995), 360 Carlova (1996, 1997, 1998), 416 Vaticana (1995{96, 1998), 516 Amherstia (1995, 1996), and 1223 Neckar (1995{96) carried out at ve observa- tories are presented. New synodical periods for two as- teroids (225, 1223) have been obtained. Using all avail- able lightcurves, the spin vectors, senses of rotation, and triaxial elipsoid models of these ve asteroids have been determined or rened.
Published: 2000
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21. Photometric observations and modelling of the asteroid 85 Io in conjunction with data from an occultation event during the 1995–96 apparition fn2 fn2Partly based on observations collected at the European Southern Observatory, La Silla, Chile

Author: J. Piironen, Alan W. Harris, F. P. Velichko, Andreas Nathues, Z Ioannou, P. Denchev, Anders Erikson, J. Berthier, Claes-Ingvar Lagerkvist, Petr Pravec, Agnieszka Kryszczyńska, T. Michalowski, Lenka Šarounová, and P. Magnusson
Subjects: Physics, 010504 meteorology & atmospheric sciences, Astronomy, Astronomy and Astrophysics, Astrophysics, Orbital period, 01 natural sciences, Occultation, Photometry (optics), Space and Planetary Science, Asteroid, 0103 physical sciences, Derived value, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: The asteroid 85 Io has been observed using CCD and photoelectric photometry on 18 nights during its 1995–96 and 1997 apparitions. We present the observed lightcurves, determined colour indices and modelling of the asteroid spin vector and shape. The colour indices (U-B = 0.35±0.02, B-V = 0.66±0.02, V-R = 0.34±0.02, R-I = 0.36±0.02) are as expected for a C-type asteroid. The allowed spin vector solutions have the pole co-ordinates λ0 = 285±4°, β0 = −52±9° or λ0 = 108±10°, β0 = −46±10° and λ0 = 290±10°, β0 = −16±10° with a retrograde sense of rotation and a sidereal period Psid = 0d.286463±0d.000001. During the 1995–96 apparition the International Occultation Time Association (IOTA) observed an occultation event by 85 Io. The observations and modelling presented here were analysed together with the occultation data to develop improved constraints on the size of the asteroid. The derived value of 164 km is about 5% larger than the IRAS diameter. © 1999 Elsevier Science Ltd. All rights reserved.
Published: 1999
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22. A catalogue of the observations of the mutual phenomena of the Galilean satellites made in 1991 during the PHEMU91 campaign

Author: H. J. J. Bulder, J. J. Sacre, C. Ruatti, B. Morando, J. Vidal, J. M. Gomez-Forrellad, F. Sevre, T. Flatres, J. F. Mellilo, J. M. Desbats, A. Piersimoni, J. C. Le Floch, J. Arsenijevic, A. Dipaolantonio, F. Colas, V. Turcu, D. Hube, D. T. Vu, R. Burchi, O. Gherega, Y. Ito, J. Lecacheux, G. de Angelis, H. Takami, G. Oprescu, D. Przewozny, G. de Benedetto, D. Chis, B. Nitschelm, Patrice Bouchet, J. Colin, A. Mallama, Ricard Casas, G. Montignac, W. Thuillot, J. Barroso, V. Shkodrov, G. White, J. F. Le Campion, V. D'Ambrosio, F. Chauvet, M. Rapaport, J. Bourgeois, O. Hainaut, L. Farcas, J. E. Arlot, C. Blanco, C. Bauer, B. Nicolet, J. A. Cano, J. Guarro, A. Horvat, R. Taylor, B. E. Martin, H. Denzau, Mark R. Kidger, J. Souchay, J. Berthier, D. J. Tholen, M. Froeschle, A. Dumitrescu, V. Protitch-Benishek, R. Baptista, M. Federspiel, R. P. Wilds, S. Molau, A. Riou, G. Helmer, P. Descamps, R. Vasundhara, and C. Meyer
Subjects: Physics, Telescope, Jupiter, symbols.namesake, law, symbols, General Physics and Astronomy, Astronomy, Astrophysics, Astrometry, Galilean moons, law.invention
Abstract: In this paper, all the light-curves obtained during the PHEMU91 campaign of observations of the mutual phenomena of the Galilean satellites are presented. These observations give accurate astrometric positions of major interest for dynamical studies of the motion of the Galilean satellites. The aim of this work is to give obser- vational data directly usable for theoretical studies. We made 374 observations of 111 mutual events from 56 sites. The corresponding data are given in this paper 1 . The accu- racy of each observation has been deduced from a compar- ison with the theoretical predictions. For each observation, information is given about the telescope, the receptor, the site and the observational conditions.
Published: 1997
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23. Modélisation 3D des perturbations géomagnétiques induites. Validation du modèle éléments finis

Author: P. Massé, R. Blanpain, J. Vatry, and J. Berthier
Subjects: Physics, Computer software, General Engineering, General Physics and Astronomy, Geomorphology, Three dimensional model
Abstract: L'environnement magnetique tres basse frequence des zones cotieres resulte d'influences multiples. Entre autres, les phenomenes d'induction electromagnetique, fortement tridimensionnels, sont provoques par les variations temporelles du champ magnetique terrestre. Nous proposons une methode de resolution avec des elements finis nodaux en formulation quadrivecteur complexe pour des geometries tridimensionnelles, en utilisant le logiciel generateur Flux Expert. La premiere etape de validation de notre modele est effectuee par comparaison avec d'autres methodes pour des geometries simples de reference.
Published: 1997
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24. First Results of the PHESAT95 Campaign of Observation of the Phenomena of the Satellites of Saturn

Author: J.-E. Arlot, W. Thuillot, F. Colas, D.T. Vu, J. Berthier, P. Descamps, and CH. Ruatti
Subjects: Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract: From 1992 to 1999, the satellites of Saturn are involved in several phenomena: eclipses or occultations by the planet, transits in front of Saturn, or transits of their umbra. These phenomena occur thanks to the geometrical circumstances in 1995 when the Earth and the Sun went through the plane of the Saturnian ring and consequently through the orbital planes of the main satellites. These circumstances are also favorable to the observation of mutual phenomena occurring when the satellites eclipse or occult each other. These mutual phenomena and the eclipses by Saturn are rare as they occur only every 15 years. But, they are very useful to get highly accurate astrometric observations and they allowed us to estimate some physical parameters. We have organized the PHESAT95 campaign to observe these phenomena and a special effort was made to observe as many events as possible. At the present time, the observations are still being collected from different teams and different countries; this paper shows the first results which have been obtained in several sites, and the first comparison with the theory of the motions.
Published: 1997
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25. CCD Photometry of Seven Asteroids: New Spin Axis and Shape Determinations

Author: François Colas, Agnieszka Kryszczyńska, T. Michalowski, J. Berthier, and W. Pych
Subjects: Photometry (optics), Physics, Space and Planetary Science, Observatory, Asteroid, Sidereal time, Astronomy, Astronomy and Astrophysics, Spin axis
Abstract: New photometric observations of 31 Euphrosyne, 76 Freia, 196 Philomela, 218 Bianca, 291 Alice, 376 Geometria, and 5702 Morando carried out at Pic du Midi Observatory (France) and in Ostrowik (Poland) in 1994 are presented. The preliminary pole and shape determinations of 218, 291, and 376 are presented. New lightcurves of 31 and 196 allowed us to recalculate values for its poles, shapes, and sidereal periods. The first lightcurve of 5702 allowed us to estimate its synodical period.
Published: 1996
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26. Photometric Observations and Modeling of Asteroid 1620 Geographos

Author: T. Kwiatkowski, L. Jorda, Anders Erikson, E. Dotto, C. Blanco, W. Pych, F. P. Velichko, L. Sarounova, G. De Angelis, V. Ivanova, P. Denchev, Petr Pravec, Uwe Fink, Agnieszka Kryszczyńska, M. Dahlgren, M. Di Martino, N. M. Gaftonyuk, J.D. Drummond, Robert J. Whiteley, Wieslaw Z. Wisniewski, Walter J. Wild, R. P. Binzel, E. H. Geyer, William M. Grundy, J.F. Lahulla, Marek Wolf, Boris Komitov, P. Magnusson, Z. Donchev, D. F. Lupishko, Stefano Mottola, Michael J. Hoffmann, T. Bauer, Stephen M. Slivan, O. Mendez, David J. Tholen, Vasilij G. Chiorny, D. Riccioli, Yu. N. Krugly, François Colas, Maria Antonietta Barucci, Steven J. Ostro, Bonnie J. Buratti, Vasilij G. Shevchenko, Javier Licandro, J. Berthier, and Michael D. Hicks
Subjects: Physics, Amplitude, Space and Planetary Science, Asteroid, Ecliptic, Astronomy, Astronomy and Astrophysics, Angular velocity, Astrophysics, Albedo, Variation (astronomy), Rotation, Orbital period
Abstract: Photometric observations of 1620 Geographos in 1993 and 1994 are presented and, in combination with previously published data, are used to derive models of Geographos. We estimate that the sidereal period of rotation is 0.21763860 ± 0.00000003 days (5h13m23.975s± 0.003s). The sense of rotation is retrograde. The ecliptic coordinates of the spin angular velocity vector are estimated to λp= 56° ± 6° and βp= −47° ± 4° (equinox J2000.0). The lightcurve amplitudes are well-explained by an ellipsoidal model with axis ratiosa/b= 2.58 ± 0.16 andb/c= 1.00 ± 0.15. Models that have one or both ends more sharply pointed than the ellipsoid improve the fit to the observations. There are no significant indications of albedo variegation, but non-geometric scattering effects are tentatively suggested based on significant rotational color variation.
Published: 1996
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27. Three dimensional finite element modeling of streaming potential and associated magnetic field in porous media

Author: P. Masse and J. Berthier
Subjects: business.product_category, Materials science, Mechanics, Horizontal plane, Streaming current, Finite element method, Physics::Geophysics, Electronic, Optical and Magnetic Materials, Magnetic field, Fluid dynamics, Electrical and Electronic Engineering, Inclined plane, business, Anisotropy, Porous medium
Abstract: Electro-magnetic modeling of electrofiltration phenomena requires coupled modeling of fluid flow, electric (streaming) potential and magnetic field. We present a finite element method for solving 3-dimensional problems in anisotropic porous media based on the code Flux-Expert. Numerical results are given for the case of water flowing at a constant rate through a window in the wall of a borehole drilled into sandstone. Two cases of anisotropy are examined: a horizontal plane and a 45 degree inclined plane.
Published: 1996
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28. Modelling of electromagnetic wakes of moving submerged bodies in stratified sea water

Author: R. Blanpain, J.J. Chaillout, and J. Berthier
Subjects: Physics, Finite volume method, Perturbation (astronomy), Mechanics, Wake, Electromagnetic radiation, Finite element method, Electronic, Optical and Magnetic Materials, Electromagnetic induction, symbols.namesake, Lorentz factor, Classical mechanics, Maxwell's equations, symbols, Electrical and Electronic Engineering
Abstract: Moving submerged bodies create wakes behind them. The motion of the sea water, because of its conductivity, induces an electromagnetic perturbation (b/spl I.oarr/, e/spl I.oarr/) in the Earth magnetic field B/spl I.oarr//sub T/. In this paper, we propose a numerical modelling of this perturbation. The water velocity field V(x,y,z) is first computed in two different cases: turbulent wake obtained using a finite volume method, wave field by a perturbation method. Then, the corresponding electromagnetic perturbation is obtained by solving the Maxwell equations including the Lorentz term. For that, we use a finite element method.
Published: 1996
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29. Finite element calculation of electromagnetic fields due to moving sea water

Author: J. Berthier, R. Blanpain, J.I. Chaillout, and V. Poulbot
Subjects: Electromagnetic field, Physics, Computer simulation, Mathematical analysis, Finite element method, Electronic, Optical and Magnetic Materials, Electromagnetic induction, Magnetic field, symbols.namesake, Classical mechanics, Maxwell's equations, symbols, Vector field, Electrical and Electronic Engineering, Linear combination
Abstract: The purpose of this work is to quantify the electromagnetic perturbation induced by a conductor subjected to a velocity field in the Earth's magnetic field, by using the finite element software Flux Expert. The resolution variables are chosen in order to reduce the number of unknowns and to improve the precision. Because of the possible orientations of the different fields the problem is a three-dimensional one. If a frame related to the perturbation is defined, one can get rid of the temporal dependence in the Maxwell equations. Because the problems are linear, a general problem is reconstructed by a linear combination of three elementary ones. The comparison of the results with analytical solutions obtained from simplified models confirm their validity. >
Published: 1995
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30. Integral-field spectroscopy of (90482) Orcus-Vanth

Author: Audrey Thirouin, Benoit Carry, Francesca E. DeMeo, David Farrelly, Thomas G. Müller, J. Berthier, Daniel Hestroffer, Pedro Lacerda, A. Doressoundiram, Bruno Sicardy, Christophe Dumas, 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), Agence Spatiale Européenne = European Space Agency (ESA), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), European Southern Observatory (ESO), Chemistry and biochemistry department, Utah State University (USU), Max-Planck-Institut für Extraterrestrische Physik (MPE), European Space Astronomy Centre (ESAC), 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), Université Paris Cité (UPCité), Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Instituto de Astrofisica de Andalucia, CSIC (IAA), Queen's University, Sorbonne Université (SU), European Southern Observatory, Utah State University, Max-Planck-Institut für Extraterrestriche Physik (MPE), Agence Spatiale Européenne (ESA), European Space Agency (ESA), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, and 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)
Subjects: 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Phase (waves), [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, Techniques: high angular resolution, Methods: observational, Techniques:imaging spectroscopy, Observatory, 0103 physical sciences, Field spectroscopy, 010303 astronomy & astrophysics, Spectrograph, 0105 earth and related environmental sciences, Orbital elements, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Kuiper belt objects: individual: (90482) Orcus, Very Large Telescope, Astronomy and Astrophysics, 13. Climate action, Space and Planetary Science, Absorption band, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: Aims. We seek to constrain the surface composition of the Trans-Neptunian Object (90482) Orcus and its small satellite Vanth, as well as their mass and density. Methods. We acquired near-infrared spectra (1.4-2.4 {\mu}m) of (90482) Orcus and its companion Vanth using the adaptive-optics-fed integral-field spectrograph SINFONI mounted on Yepun/UT4 at the European Southern Observatory Very Large Telescope. We took advantage of a very favorable appulse (separation of only 4") between Orcus and the UCAC2 29643541 star (R = 11.6) to use the adaptive optics mode of SINFONI, allowing both components to be spatially resolved and Vanth colors to be extracted independently from Orcus. Results. The spectrum of Orcus we obtain has the highest signal-to-noise ratio to date, and we confirm the presence of H2O ice in crystalline form, together with the presence of an absorption band at 2.2 {\mu}m. We set an upper limit of about 2% for the presence of methane, and 5% for ethane. Because the methane alone cannot account for the 2.2 {\mu}m band, the presence of ammonia is suggested to the level of a couple of percent. The colors of Vanth are found slightly redder than those of Orcus, but the large measurement uncertainties forbid us from drawing conclusions on the origin of the pair (capture or co-formation). Finally, we reset the orbital phase of Vanth around Orcus, and confirm the orbital parameters derived by Brown et al. (2010, AJ 139)., Comment: 9 pages, 6 figures, 6 tables, accepted for publication in A&A
Published: 2011
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31. Gaia spectroscopy: processing, performances and scientific returns

Author: F. Crifo, Eric Pierre Simon, Yassine Damerdji, A. E. Gomez, Leanne P. Guy, C. Parr, Daniel Hestroffer, David Hall, P. Sartoretti, C. Delle Luche, F. Thévenin, Mark Cropper, L. Chemin, Caroline Soubiran, A. Jean-Antoine, Stéphane Udry, C. Turon, J. Gerssen, F. Meynadier, S. G. Baker, C. Dolding, P. Ocvirk, Hans-Günter Ludwig, R. Blomme, Thierry Morel, C. Allende Prieto, L. Veltz, M. J. S. Smith, Gérard Jasniewicz, F. Royer, George M. Seabroke, A. Guerrier, Matthias Steinmetz, N. Gerbier, H. Huckle, P. David, Steve Boudreault, Christophe Martayan, K. Benson, Yves Fremat, Y. Viala, J. Berthier, M. David, D. Katz, Eric Gosset, Lionel Bigot, A.-T. Nguyen, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Physique des Lasers, Atomes et Molécules - UMR 8523 (PhLAM), Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), 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 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), inconnu, Inconnu, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory of Belgium [Brussels] (ROB), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, 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 de Recherche en Astronomie et Astrophysique du Languedoc (GRAAL), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg] = Heidelberg University, European Southern Observatory (ESO), 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)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Astrophysikalisches Institut Potsdam (AIP), Laboratoire Telecom Claude Chappe (LT2C), Université Jean Monnet - Saint-Étienne (UJM)-Ecole d'ingénieurs Télécom Saint-Etienne (TSE), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), 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), NASA Goddard Space Flight Center (GSFC), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Centre National de la Recherche Scientifique (CNRS)-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 Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, 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)-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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, 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), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Universität Heidelberg [Heidelberg], Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Institut National Polytechnique de Grenoble (INPG), Laboratoire Dispositifs et Instrumentation en Optoélecronique et Microondes – EA3523, Université Jean Monnet [Saint-Étienne] (UJM), Université Nice Sophia Antipolis (... - 2019) (UNS), Université de Genève (UNIGE), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Electronique et des Technologies de l'Information (CEA-LETI), Université Grenoble Alpes (UGA)-Direction de Recherche Technologique (CEA) (DRT (CEA)), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Royal Observatory of Belgium [Brussels], PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), 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), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Data processing, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Spectrometer, Astrophysics::Instrumentation and Methods for Astrophysics, General Engineering, Astronomy, Astronomy and Astrophysics, Celestial sphere, Astrophysics, 01 natural sciences, Galaxy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010309 optics, Radial velocity, Space and Planetary Science, 0103 physical sciences, Magnitude (astronomy), Astrophysics::Earth and Planetary Astrophysics, Spectroscopy, 010303 astronomy & astrophysics, Spectrograph
Abstract: International audience; During the five years of the mission, the Gaia spectrograph, the Radial Velocity Spectrometer (RVS) will repeatedly survey the celestial sphere down to magnitude V ~ 17-18. This talk presents: (i) the system which is currently developed within the Gaia Data Processing and Analysis Consortium (DPAC) to reduce and calibrate the spectra and to derive the radial and rotational velocities, (ii) the RVS expected performances and (iii) scientific returns.
Published: 2010
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32. Electrically actuated sacrificial membranes for valving in microsystems

Author: J Berthier, P Pouteau, M. Allain, Skandar Basrour, Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Techniques de l'Informatique et de la Microélectronique pour l'Architecture des systèmes intégrés (TIMA), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Electronique et des Technologies de l'Information (CEA-LETI), Université Grenoble Alpes (UGA)-Direction de Recherche Technologique (CEA) (DRT (CEA)), Techniques of Informatics and Microelectronics for integrated systems Architecture (TIMA), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)
Subjects: Engineering, Microfluidics, electronic-systems, Nanotechnology, 02 engineering and technology, 010402 general chemistry, 01 natural sciences, chemistry.chemical_compound, Low energy, Microsystem, Electrical and Electronic Engineering, [SPI.NANO]Engineering Sciences [physics]/Micro and nanotechnologies/Microelectronics, microsystems, Electronic circuit, business.industry, Mechanical Engineering, 021001 nanoscience & nanotechnology, 0104 chemical sciences, Electronic, Optical and Magnetic Materials, Membrane, Silicon nitride, chemistry, Mechanics of Materials, PACS 85.42, Electrode, Silicon chip, 0210 nano-technology, business
Abstract: International audience; Valving is essential to microflow circuits and networks in microsystem technology. Many different types of valves have been designed and fabricated. Membranes of sacrificial material have already been designed for one-shot valving. However, the new design proposed here, based on sacrificial micro-membranes with embedded electrodes, has the advantages of being efficient, easily controllable and requiring very low energy levels. We have shown that a 100 µm × 100 µm × 500 nm Si3N4 membrane with a platinum electrode can be actuated to break up with an energy input of only 6 µJ, during an actuation time of 200 µs. At rest, in the absence of actuation, such membranes can withstand a pressure of 1 bar. The goal of the development of such membranes is to hydrodynamically connect, one by one, a series of initially isolated micro-chambers implemented in a silicon chip.
Published: 2010
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33. Titania's radius and an upper limit on its atmosphere from the September 8, 2001 stellar occultation

Author: Emmanuel Lellouch, F. Díaz, Ph. Dupouy, P. Figuereido, B. Mitchell, C. Birnbaum, W. Sutherland, H. Mendt, C. Labordena, C. Martinez, P. Valdes Sada, F. Schwartz, P. Burlot, E. van Ballegoij, C. Clarasso-Llauger, J.-F. Coliac, C. Sire, R. Jones, M. Kretlow, P. Maley, S. Rivaud, J. Lecacheux, J.M. Winkel, A. Cidadão, C. Saraiva, R. E. Hill, C. Marlot, S. Pau, F. Colas, F. Roques, E. López, C. Marciano, M. Gabaldá-Sánchez, C. Demeautis, P. Coelho, A. Roca, C. Schnabel, Jean-Eudes Arlot, Pedro Ré, R. Gonçalves, R. Hernández, C. Buil, A.J. Elliott, E. Masana, A. Ardanuy, C. Guillén, J.-F. Lecampion, F. Casarramona, William B. Hubbard, X. Simbaña, L. Rivas, L. Omar Porras, H. Callender, E. Brochard, J. L. Ortiz, M. Rapaport, D. Pulupa, A. Peña, J. Gonçalves, G. Sánchez, G. Rau, A. Hernández, B.M. Ewen-Smith, A. Arnal, Pascal Dubreuil, C. Lambin, C. R. Hills, E. Pallo, K. Daiffallah, X. Otazu-Porter, Richard Miles, Ch. Marlot, R. Cósias, S. Radaelli, B. Bayle, V. Ladino, C. Leyrat, P. Rodas, A. Klotz, R. Dusser, J. Clérigo, B. Wilson, E. Bredner, D. Cornwall, D. Ford, O. Labrevoir, D. Fernández, W. Barrow, Erika Castro, Bruno Sicardy, M. Mascaró, O. Chaptal, E. Simian, E. Recalde, B. Stephanus, Ricard Casas, F. Tonel, William Thuillot, V. Desnoux, J. Berthier, C. Oliveira, J. Laurindo Sobrinho, M. Rieugnié, P. Henriquet, J. Piraux, P. Rosenzweig, Steven N. Ward, G. Eleizalde, A. Yajamín, C. Sauzeaud, J. Aloy Doménech, K. Vieira, M. Lavayssière, P. Langlais, T. Rafaelli, G. Bouderand, J. Santiago, R. Delmas, M. Imbert, H. Denzau, J. A. Ros, A. Valencia, T. Lizardo, F. Teodoro de Gois, J. Porto, J. Fulgence, J.-P. Cazard, O. Contreras, F. Moreno, W. Beisker, J. Lockhart, T. Platt, F. Gorry, J. Afonso da Silva Mendes, R. Percz, R. Nunes, E. Guzmán, V. Ferrer, D. Dunham, S. Bumgarner, J. Fernández-Arozena, A.M. Blommers, C. Jasinski, O. Canales-Moreno, C. Reis, L.L. Martín-Rodríguez, M. Joaquim, O. Naranjo, D. Marchais, Thomas Widemann, C. Cremaschini, P.O. Pujat, and C. Cavadore
Subjects: Physics, 010504 meteorology & atmospheric sciences, Uranus, Astronomy, Astronomy and Astrophysics, Solar radius, Radius, Ephemeris, 01 natural sciences, Occultation, Atmosphere, 13. Climate action, Space and Planetary Science, Angular diameter, 0103 physical sciences, Physical Sciences, Polar, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: On September 8, 2001 around 2 h UT, the largest uranian moon, Titania, occulted Hipparcos star 106829 (alias SAO 164538, a V = 7.2 , K0 III star). This was the first-ever observed occultation by this satellite, a rare event as Titania subtends only 0.11 arcsec on the sky. The star's unusual brightness allowed many observers, both amateurs or professionals, to monitor this unique event, providing fifty-seven occultations chords over three continents, all reported here. Selecting the best 27 occultation chords, and assuming a circular limb, we derive Titania's radius: R T = 788.4 ± 0.6 km ( 1 - σ error bar). This implies a density of ρ = 1.711 ± 0.005 g cm −3 using the value G M = ( 2.343 ± 0.006 ) × 10 11 m 3 s −2 derived by Taylor [Taylor, D.B., 1998. Astron. Astrophys. 330, 362–374]. We do not detect any significant difference between equatorial and polar radii, in the limit r eq − r po = − 1.3 ± 2.1 km , in agreement with Voyager limb image retrieval during the 1986 flyby. Titania's offset with respect to the DE405 + URA027 (based on GUST86 theory) ephemeris is derived: Δ α T cos ( δ T ) = − 108 ± 13 mas and Δ δ T = − 62 ± 7 mas (ICRF J2000.0 system). Most of this offset is attributable to a Uranus' barycentric offset with respect to DE405, that we estimate to be: Δ α U cos ( δ U ) = − 100 ± 25 mas and Δ δ U = − 85 ± 25 mas at the moment of occultation. This offset is confirmed by another Titania stellar occultation observed on August 1st, 2003, which provides an offset of Δ α T cos ( δ T ) = − 127 ± 20 mas and Δ δ T = − 97 ± 13 mas for the satellite. The combined ingress and egress data do not show any significant hint for atmospheric refraction, allowing us to set surface pressure limits at the level of 10–20 nbar. More specifically, we find an upper limit of 13 nbar ( 1 - σ level) at 70 K and 17 nbar at 80 K, for a putative isothermal CO2 atmosphere. We also provide an upper limit of 8 nbar for a possible CH4 atmosphere, and 22 nbar for pure N2, again at the 1 - σ level. We finally constrain the stellar size using the time-resolved star disappearance and reappearance at ingress and egress. We find an angular diameter of 0.54 ± 0.03 mas (corresponding to 7.5 ± 0.4 km projected at Titania). With a distance of 170 ± 25 parsecs, this corresponds to a radius of 9.8 ± 0.2 solar radii for HIP 106829, typical of a K0 III giant.
Published: 2009
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34. A model for the determination of the dimensions of dents for jagged electrodes in electrowetting on dielectric microsystems

Author: J. Berthier and C. Peponnet
Subjects: Fluid Flow and Transfer Processes, Materials science, business.industry, Physics::Instrumentation and Detectors, Microfluidics, Biomedical Engineering, Nanotechnology, Dielectric, Condensed Matter Physics, Colloid and Surface Chemistry, Physics::Plasma Physics, Microsystem, Electrode, Electrowetting, Optoelectronics, General Materials Science, Electrohydrodynamics, business, Dimensioning, Microfabrication, Regular Articles
Abstract: The motion of a droplet from one electrode to the next in electrowetting on dielectric microsystems is not straightforward. Microfabrication imposes a gap separating the electrodes. This hydrophobic gap has the effect of pinning the triple contact line, preventing the motion of the microdrop. To avoid such a drawback, jagged electrodes, i.e., electrodes with crenellated side boundaries have been designed. In this work, an analytical model for dimensioning the size of the dents of the electrodes is derived based on the contact line elasticity theory. This model determines a lower limit for the nondimensional ratio of the length of a dent to its width. The designs of jagged electrodes in the literature have been verified to satisfy the condition, but with very different safety margins.
Published: 2006

35. Studying binary asteroids with NGS and LGS AO systems

Author: Donald T. Gavel, J. Berthier, Conor Laver, Frédéric Vachier, Daniel Hestroffer, P. Descamps, Imke de Pater, Franck Marchis, University of California/Berkeley, USA, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), University of California Observatoires/Lick Observatory, USA, Bonaccini Calia, Domenico, Ellerbroek, Brent L., Ragazzoni, and Roberto
Subjects: Orbital elements, Physics, education.field_of_study, Population, Astronomy, Orbital mechanics, Ephemeris, Astrobiology, Laser guide star, Trojan, Neptune, Asteroid, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], education
Abstract: International audience; Since the discovery of Dactyl orbiting around Ida by the Galileo spacecraft in 1993, over twenty-five binary asteroid systems have been discovered using radar, direct imaging and Adaptive Optics observations. Asteroidal moon discoveries dramatically increased with the advent of this last technique on ground based telescopes. Our group focuses on the search and study of double asteroids in the main-belt, in the Trojan population and beyond Neptune's orbit. We have been using several of the AO systems available (Lick-3m, Palomar-5m, VLT-8m, Keck-10m) and related techniques such as Appulse and Laser Guide Star observations to broaden the sample of asteroids observed from the main-belt out to the Kuiper Belt. We will present a quality comparison between various techniques and different AO systems with NGS and will detail our first successful observations with the Lick LGS system. Precise orbital elements of the secondary can be determined by multiple observations spanning large periods of time (several months). Our group developed a method to predict the ephemeris of a secondary companion. Without any assumptions, this method, tested successfully on 22 Kalliope and 121 Hermione binary systems, leads to the direct determination of important physical parameters of the targets, such as their mass and the interior structure, as well as gives direct insights on their formation processes that may be otherwise only be speculated on from spacecraft mission flybys.
Published: 2004
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36. Measurement of the n_TOF beam profile with a micromegas detector

Author: Pancin, J. Abbondanno, U. Aerts, G. Alvarez, H. Andriamonje, S. Angelopoulos, A. Assimakopoulos, P. Bacri, C. Badurek, G. Baumann, P. Bečvář, F. Beer, H. Benlliure, J. Berthier, B. Berthoumieux, E. Boffi, S. Borcea, C. Boscolo-Marchi, E. Bustreo, N. Calvino, F. Cano-ott, D. Capote, R. Carlson, P. Cennini, P. Chepel, V. Chiaveri, E. Colonna, N. Cortes, G. Cortina, D. Couture, A. Cox, J. Dababneh, S. Dahlfors, M. David, S. Delbart, A. Derre, J. Dolfini, R. Domingo, C. Duran-Escribano, I. Eleftheriadis, C. Embid-Segura, M. Ferrant, L. Ferrari, A. Ferreira-Lourenco, L. Ferreiramarques, R. Frais-Koelbl, H. Furman, W. Giomataris, Y. Goncalves, I. Gonzalez-Romero, E. Goverdovski, A. Gramegna, F. Griesmayer, E. Gunsing, F. Haight, R. Heil, M. Herrera-Martinez, A. Ioannides, K. Janeva, N. Jeanneau, F. Jericha, E. Käppeler, F. Kadi, Y. Karamanis, D. Kelic, A. Ketlerov, V. Kitis, G. Koehler, P. Konovalov, V. Kossionides, E. Lacoste, V. Leeb, H. Lindote, A. Lopes, I. Lozano, M. Lukic, S. Markov, S. Marrone, S. Martinez-Val, J. Mastinu, P. Mengoni, A. Milazzo, P. Minguez, E. Molina-Coballes, A. Moreau, C. Neves, F. Oberhummer, H. O'brien, S. Papadopoulos, I. Papavengelou, T. Paradela, C. Pavlik, A. Pavlopoulos, P. Perez-Parra, A. Perlado, J. Peskov, V. Perrot, L. Peskov, V. Plag, R. Plompen, A. Plukis, A. Poch, A. Policarpo, A. Pretel, C. Quesada, J. Radici, M. Raman, S. Rapp, W. Reifarth, R. Rejmund, F. Rosetti, M. Rubbia, C. Rudolf, G. Rullhusen, P. Salgado, J. Savvidis, E. Stephan, C. Tagliente, G. Tain, J. Tapia, C. Tassan-Got, L. Tavora, L. Terlizzi, R. Terrani, M. Tsangas, N. Vannini, G. Vaz, P. Ventura, A. Villamarin-Fernandez, D. Vincente-Vincente, M. Vlachoudis, V. Vlastou, R. Voss, F. Wendler, H. Wiescher, M. Wisshak, K. Zanini, L.
Subjects: Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Nuclear Theory, Nuclear Experiment
Abstract: A Micromegas detector was used in the neutron Time-Of-Flight (n_TOF) facility at CERN to evaluate the spatial distribution of the neutron beam as a function of its kinetic energy. This was achieved over a large range of neutron energies by using two complementary processes: at low energy by capture of a neutron via the 6Li(n,α)t reaction, and at high energy by elastic scattering of neutrons on gas nuclei (argon+isobutane or helium+isobutane). Data are compared to Monte Carlo simulations and an analytic function fitting the beam profile has been calculated with a sufficient precision to use in neutron capture experiments at the n_TOF facility. © 2004 Elsevier B.V. All rights reserved.
Published: 2004

37. A low-mass neutron flux monitor for the n_TOF facility at CERN

Author: Mastinu, P.F. Abbondanno, U. Aerts, G. Alvarez, H. Andriamonje, S. Angelopoulos, A. Assimakopoulos, P. Bacri, C.O. Badurek, G. Baumann, P. Bečvář, F. Beer, H. Benlliure, J. Berthier, B. Berthomieux, E. Boffi, S. Borcea, C. Boscolo-Marchi, E. Bustreo, N. Calviño, P. Cano-Ott, D. Capote, R. Carlson, P. Cennini, P. Chepel, V. Chiaveri, E. Coceva, C. Colonna, N. Cortes, G. Cortina, D. Couture, A. Cox, J. Dababneh, S. Dahlfors, M. David, S. Dolfini, R. Domingo-Pardo, C. Duran, I. Eleftheriadis, C. Embid-Segura, M. Ferrant, L. Ferrari, A. Ferreira-Lourenco, L. Ferreira-Marques, R. Frais-Koelbl, H. Furman, W.I. Giomataris, Y. Goncalves, I.F. Gonzalez-Romero, E. Goverdovski, A. Gramegna, F. Griesmayer, E. Gunsing, F. Haight, R. Heil, M. Herrera-Martinez, A. Ioannides, K.G. Janeva, N. Jericha, E. Käppeler, F. Kadi, Y. Karamanis, D. Kelic, A. Ketlerov, V. Kitis, G. Koehler, P.E. Konovalov, V. Kossionides, E. Lacoste, V. Leeb, H. Lindote, A. Lopes, M.I. Loriggiola, M. Lozano, M. Lukic, S. Markov, S. Marigo, S. Marrone, S. Martinez-Val, J. Mengoni, A. Milazzo, P.M. Minguez, E. Molina-Coballes, A. Moreau, C. Neves, F. Oberhummer, H. O'Brien, S. Pancin, J. Papaevangelou, T. Paradela, C. Pavlik, A. Pavlopoulos, P. Perez-Parra, A. Perlado, J.M. Perrot, L. Peskov, V. Plag, R. Plompen, A. Plukis, A. Poch, A. Policarpo, A. Pretel, C. Quesada, J.M. Radici, M. Raman, S. Rapp, W. Rauscher, T. Reifarth, R. Rejmund, F. Rosetti, M. Rubbia, C. Rudolf, G. Rullhusen, P. Salgado, J. Savvidis, E. Soares, J.C. Stephan, C. Tagliente, G. Tain, J.L. Tapia, C. Tassan-Got, L. Tavora, L.M.N. Terlizzi, R. Terrani, M. Tsangas, N. Vannini, G. Vaz, P. Ventura, A. Villamarin-Fernandez, D. Vincente-Vincente, M. Vlachoudis, V. Vlastou, R. Voss, F. Wendler, H. Wiescher, M. Wisshak, K. Zanini, L.
Subjects: Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Physics::Accelerator Physics, Nuclear Experiment
Abstract: A small-mass system has been developed for monitoring the flux of neutrons with energy up to 1 MeV at the new time-of-flight facility at CERN, n_TOF. The monitor is based on a thin Mylar foil with a 6Li deposit, placed in the neutron beam, and an array of Silicon detectors, placed outside the beam, for detecting the products of the 6Li(n, α)3H reaction. The small amount of material on the beam ensures a minimal perturbation of the flux and minimizes the background related to scattered neutrons. Moreover, a further reduction of the γ-ray background has been obtained by constructing the scattering chamber hosting the device in carbon fibre. A detailed description of the flux monitor is here presented, together with the characteristics of the device, in terms of efficiency, resolution and induced background. The use of the monitor in the measurement of neutron capture cross-sections at n-TOF is discussed.
Published: 2004

38. New experimental validation of the pulse height weighting technique for capture cross-section measurements

Author: Abbondanno, U. Aerts, G. Alvarez, H. Andriamonje, S. Angelopoulos, A. Assimakopoulos, P. Bacri, C.O. Badurek, G. Baumann, P. Bečvář, F. Beer, H. Benlliure, J. Berthier, B. Berthomieux, E. Boffi, S. Borcea, C. Boscolo-Marchi, E. Bustreo, N. Calviño, P. Cano-Ott, D. Capote, R. Carlson, P. Cennini, P. Chepel, V. Chiaveri, E. Coceva, C. Colonna, N. Cortes, G. Cortina, D. Couture, A. Cox, J. Dababneh, S. Dahlfors, M. David, S. Dolfini, R. Domingo-Pardo, C. Duran, I. Eleftheriadis, C. Embid-Segura, M. Ferrant, L. Ferrari, A. Ferreira-Lourenco, L. Ferreira-Marques, R. Frais-Koelbl, H. Furman, W.I. Giomataris, Y. Goncalves, I.F. Gonzalez-Romero, E. Goverdovski, A. Gramegna, F. Griesmayer, E. Gunsing, F. Haight, R. Heil, M. Herrera-Martinez, A. Ioannides, K.G. Janeva, N. Jericha, E. Käppeler, F. Kadi, Y. Karamanis, D. Kelic, A. Ketlerov, V. Kitis, G. Koehler, P.E. Konovalov, V. Kossionides, E. Lacoste, V. Leeb, H. Lindote, A. Lopes, M.I. Lozano, M. Lukic, S. Markov, S. Marrone, S. Martinez-Val, J. Mastinu, P. Mengoni, A. Milazzo, P.M. Minguez, E. Molina-Coballes, A. Moreau, C. Neves, F. Oberhummer, H. O'Brien, S. Pancin, J. Papaevangelou, T. Paradela, C. Pavlik, A. Pavlopoulos, P. Perez-Parra, A. Perlado, J.M. Perrot, L. Peskov, V. Plag, R. Plompen, A. Plukis, A. Poch, A. Policarpo, A. Pretel, C. Quesada, J.M. Radici, M. Raman, S. Rapp, W. Rauscher, T. Reifarth, R. Rejmund, F. Rosetti, M. Rubbia, C. Rudolfh, G. Rullhusen, P. Salgado, J. Savvidis, E. Soares, J.C. Stephan, C. Tagliente, G. Tain, J.L. Tapia, C. Tassan-Got, L. Tavora, L.M.N. Terlizzi, R. Terrani, M. Tsangas, N. Vannini, G. Vaz, P. Ventura, A. Villamarin-Fernandez, D. Vincente-Vincente, M. Vlachoudis, V. Vlastou, R. Voss, F. Wendler, H. Wiescher, M. Wisshak, K. Zanini, L.
Abstract: The accuracy of the pulse height weighting technique for the determination of neutron capture cross-sections is investigated. The technique is applied to measurements performed with C6D6 liquid scintillation detectors of two different types using capture samples of various dimensions. The data for well-known (n,γ) resonances are analyzed using weighting functions obtained from Monte Carlo simulations of the experimental set-up. Several causes of systematic deviation are identified and their effect is quantified. In all the cases measured the reaction yield agrees with the standard value within 2%. © 2003 Elsevier B.V. All rights reserved.
Published: 2004

39. Electromagnetic fields due to moving sea water by finite element calculation

Author: R. Blanpain, J. Berthier, V. Poulbot, and J.J. Chaillout
Subjects: Electromagnetic field, Physics, symbols.namesake, Maxwell's equations, Mathematical analysis, symbols, Perturbation (astronomy), Vector field, Geophysics, Linear combination, Finite element method, Conductor, Magnetic field
Abstract: The purpose of this work is to quantify the electromagnetic perturbation induced by a conductor subjected to a velocity field in the Earth's magnetic field, by using the finite element software FLUX-EXPERT. The resolution variables are chosen in order to reduce the number of unknowns and to improve the precision. Because of the possible orientations of the different fields the problem is a three-dimensional one. If a frame related to the perturbation is defined, one can get rid of the temporal dependence in the Maxwell equations. Because the authors' problems are linear, a general problem is reconstructed by a linear combination of three elementary ones. The comparison of the results with analytical solutions obtained from simplified models confirm their validity. So the authors can study phenomena for which no easy analytical solution exists. >
Published: 2002
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40. A fast algorithm for the computation of induced geomagnetic field in the oceans using remote reference signals

Author: J. Berthier and R. Blanpain
Subjects: Electromagnetic field, Primary field, Earth's magnetic field, Spacetime, Basis (linear algebra), Computation, Geophysics, Linear combination, Geodesy, Transfer function, Geology, Physics::Geophysics
Abstract: The geomagnetic primary field external to the Earth induces a secondary field inside the Earth's crust and oceans. Using a remote reference located on shore for convenience, and precalculated transfer functions, the authors show that the time dependant electromagnetic field at any location is a linear combination of space only functions multiplied by time functions. This separation between space and time functions is the basis for a fast algorithm to compute the time dependant electromagnetic field at any location.
Published: 2002
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41. Adaptive optics observations of asteroid (216) Kleopatra

Author: Thierry Fusco, J. Berthier, Daniel Hestroffer, F. Marchis, 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), Department of Astronomy, University of California, ONERA - The French Aerospace Lab [Châtillon], and ONERA-Université Paris Saclay (COmUE)
Subjects: Physics, Binary Object, Astronomy, Astronomy and Astrophysics, Astrophysics, law.invention, Telescope, Amplitude, Space and Planetary Science, law, Asteroid, Deconvolution, Radar, Adaptive optics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Image resolution
Abstract: International audience; The large main-belt asteroid (216) Kleopatra has been for long suspected to be a binary object, mainly due to its large lightcurve amplitude. However, recent observations suggest that it is a single ``bone-shaped'' or bi-lobated body (Ostro et al. \cite{ostro00}; Tanga et al. \cite{tanga01}). We present results obtained from ground-based adaptive optics observations, and in agreement with the radar raw-observations, the images show two prominent lobes. Making use of the MISTRAL deconvolution technique, the restored images yield a well-separated binary object. Nevertheless, the spatial resolution of the 3.6 m ESO telescope is limited and a dumbbell-shaped body could yield similar features. Further simulations show that adaptive optics observations with an 8-meter class telescope analyzed with the powerful MISTRAL deconvolution technique could overcome this limitation. Based on observations collected at ESO-La Silla, Chile.
Published: 2002
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42. THE PUZZLING MUTUAL ORBIT OF THE BINARY TROJAN ASTEROID (624) HEKTOR

Author: H. Hamanowa, J. Berthier, Michael H. Wong, Frédéric Vachier, Gaspard Duchêne, Matija Ćuk, Matti Viikinkoski, Julie Castillo-Rogez, Josef Durech, Paul Kalas, M. A. van Dam, Franck Marchis, Carl Sagan Center, SETI Institute, 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), Astronomical Institute of Charles University, Charles University [Prague] (CU), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Flat Wavefronts, Hamanowa Astronomical Observatory, Department of Mathematics, Tampere University of Technology [Tampere] (TUT), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Charles University [Prague], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), NASA-California Institute of Technology (CALTECH), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Solar System, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Binary number, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Orbit, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Asteroid, Trojan, Primary (astronomy), 0103 physical sciences, Satellite, Ejecta, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: Asteroids with satellites are natural laboratories to constrain the formation and evolution of our solar system. The binary Trojan asteroid (624) Hektor is the only known Trojan asteroid to possess a small satellite. Based on W.M. Keck adaptive optics observations, we found a unique and stable orbital solution, which is uncommon in comparison to the orbits of other large multiple asteroid systems studied so far. From lightcurve observations recorded since 1957, we showed that because the large Req=125-km primary may be made of two joint lobes, the moon could be ejecta of the low-velocity encounter, which formed the system. The inferred density of Hektor's system is comparable to the L5 Trojan doublet (617) Patroclus but due to their difference in physical properties and in reflectance spectra, both captured Trojan asteroids could have a different composition and origin., 13 pages, 3 figures, 2 tables
Published: 2014
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43. [Mother and child in prison. Preserving their bond at any cost]

Author: J, Berthier, E, Draveny, and M N, Richard
Subjects: Adolescent, Child, Preschool, Prisoners, Humans, Female, Child, Mother-Child Relations
Published: 1998

44. First Results of The PHESAT95 Campaign of Observation of the Phenomena of the Satellites of Saturn

Author: P. Descamps, W. Thuillot, J. Berthier, François Colas, D. T. Vu, J. E. Arlot, and Ch. Ruatti
Subjects: Exploration of Saturn, Orbital plane, Planet, Celestial body, Saturn, Physics::Space Physics, Astronomy, Astrophysics::Earth and Planetary Astrophysics, Geology, Eclipse
Abstract: From 1992 to 1999, the satellites of Saturn are involved in several phenomena: eclipses or occultations by the planet, transits in front of Saturn, or transits of their umbra. These phenomena occur thanks to the geometrical circumstances in 1995 when the Earth and the Sun went through the plane of the Saturnian ring and consequently through the orbital planes of the main satellites. These circumstances are also favorable to the observation of mutual phenomena occurring when the satellites eclipse or occult each other. These mutual phenomena and the eclipses by Saturn are rare as they occur only every 15 years. But, they are very useful to get highly accurate astrometric observations and they allowed us to estimate some physical parameters. We have organized the PHESAT95 campaign to observe these phenomena and a special effort was made to observe as many events as possible. At the present time, the observations are still being collected from different teams and different countries; this paper shows the first results which have been obtained in several sites, and the first comparison with the theory of the motions.
Published: 1997
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45. Some examples of micro-devices for biotechnology developed at the Department of Technologies for Life Sciences and Healthcare of the LETI

Author: P. Pouteau, Christine Peponnet, Y. Fouillet, D. Jary, N. Sarrut, P. Caillat, V. Mourier, and J. Berthier
Subjects: Dna detection, Micro devices, Engineering, business.industry, Health care, Materials Chemistry, Bioengineering, Electrical and Electronic Engineering, Condensed Matter Physics, business, Biotechnology
Abstract: Biotechnology has been rapidly developing over the last 15 years. Its advantages in many medical and pharmaceutical domains are now obvious. Biotechnological microsystems are now widely encountered in the field of diagnostics, healthcare, life science and environment. This text relates a selection of developments performed at the CEA/LETI, in the Department of Biotechnology and Life Sciences. This selection encompasses digital microfluidic systems for DNA detection and identification, proteomic reactors, liquid-liquid extraction and smart tissues.
Published: 2010
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46. AFDM: An Advanced Fluid-Dynamics Model

Author: J Berthier, D Wilhelm, and W Bohl
Published: 1990
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47. AFDM: An Advanced Fluid-Dynamics Model

Author: F. R. Parker, W.R. Bohl, J. Berthier, L. Goutagny, Ninokata, and D. Wilhelm
Subjects: Momentum, Differential equation, Vaporization, Condensation, Heat transfer, Evaporation, Fluid dynamics, Thermodynamics, Fluid mechanics, Mathematics
Abstract: This report gives the Advanced Fluid-Dynamics Model (AFDM) solution algorithm describing vaporization/condensation (V/C) and melting/freezing processes. The finite-difference equations used are derived from the general AFDM differential equations with convection ignored. In two-phase cells, V/C is determined by a simultaneous iterative solution. The objective is to retain stability and energy conservation with consistent interfacial and bulk conditions describing vapor/liquid densities and temperatures. Particular attention is given in the special cases required to obtain a solution. In single-phase cells, the heat transfer is determined first; then, a vapor composition is updated for the {alpha}{sub 0} volume based on the saturation pressures for the individual liquids. Melting/freezing rates are determined based on equilibrium considerations. Mass-transfer-induced velocity changes are calculated implicitly so as to conserve momentum. In addition to the treatment of the standard models, a description is provided on the energy transfers used for the simplified NOPHASE option.
Published: 1990
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48. Massive physical and dynamical characterization of asteroids

Author: J. Berthier, Areg M. Mickaelian, William Thuillot, Lena A. Sargsyan, Guy Simon, Jesus Iglesias, Armand Sarkissian, Valery Lainey, and Mirel Birlan
Subjects: Physics, Space and Planetary Science, Asteroid, Astronomy, Astronomy and Astrophysics, Characterization (materials science), Astrobiology
Abstract: Numerous new Solar System objects, mainly asteroids, are still detected nowadays but their physical and dynamical characteristics remain not accurately determined, until dedicated observations and analysis are made. However, the Virtual Observatory is a perfect framework to search for this characterization by data mining. We are developing two studies for this goal by exploring the DENIS infrared and DFBS spectroscopic surveys. In order to scan the survey catalogues and to search for Solar System objects, we have developed a VO compliant workflow founded on the use of a recent VO tool labelled SkyBoT (Sky Bodies Tracker) (Berthier et al. 2005) and on the VizieR service provided by CDS. A public version of SkyBoT is implemented in the sky atlas Aladin since January 2006. It allows us to quickly get the precise coordinates of the asteroids, planets and natural satellites in any star field, provided we know its center, its size and the precise date of the exposure (between 1949 and 2009). Our data mining workflow performs cone search queries on SkyBoT and VizieR to extract all the known astronomical objects observed by the survey. Then the sources which are detected in the survey are correlated with the known objects to determine the matched and unmatched objects.
Published: 2006
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49. Observations From the Impact of Comet P/Shoe-Maker-Levy 9 in Jupiter From the Pic-Du-Midi Observatory, France

Author: D. Tiphène, P. Laques, D. Rouan, A. Sánchez-Lavega, J. Berthier, M. Roos-Serote, Jacques Crovisier, J. Lecacheux, Françoise Roques, A. Barucci, Marcello Fulchignoni, S. Pau, F. Deladerriere, Pierre Drossart, and François Colas
Subjects: Jupiter, MIDI, Observatory, Comet, Astronomy, computer.file_format, computer, Geology, Astrobiology
Published: 1995
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50. Lutypha sclerotiophila gen. et sp.nov. (Aphyllophorales) from India

Author: J. Berthier, I.P.S. Khurana, and K. S. Thind
Subjects: Aphyllophorales, biology, Botany, General Earth and Planetary Sciences, biology.organism_classification, General Environmental Science
Published: 1977
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