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1. The multichord stellar occultation by the centaur Bienor on January 11, 2019

Author: E. Fernández-Valenzuela, N. Morales, M. Vara-Lubiano, J. L. Ortiz, G. Benedetti-Rossi, B. Sicardy, M. Kretlow, P. Santos-Sanz, B. Morgado, D. Souami, F. Organero, L. Ana, F. Fonseca, A. Román, S. Alonso, R. Gonçalves, M. Ferreira, R. Iglesias-Marzoa, J. L. Lamadrid, A. Alvarez-Candal, M. Assafin, F. Braga-Ribas, J. I. B. Camargo, F. Colas, J. Desmars, R. Duffard, J. Lecacheux, A. R. Gomes-Júnior, F. L. Rommel, R. Vieira-Martins, C. L. Pereira, V. Casanova, A. Selva, C. Perelló, S. Mottola, S. Hellmich, J. L. Maestre, A. J. Castro-Tirado, A. Pal, J. M. Trigo-Rodriguez, W. Beisker, A. Laporta, M. Garcés, L. Escaned, M. Bretton, Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Research Council, European Commission, National Research, Development and Innovation Office (Hungary), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), 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), Pôle Planétologie du LESIA, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut Polytechnique des Sciences Avancées (IPSA), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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), Minor planets, asteroids: individual: Bienor, Stellar occultations, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astronomy and Astrophysics, general [Kuiper belt], Trans-Neptunian Objects – Kuiper Belt objects: individual: Bienor – Photometry – Stellar occultations, Trans-Neptunian Objects, individual: Bienor [Minor planets, asteroids], Kuiper Belt objects: individual: Bienor, Planets and satellites: composition, Photometry, Planets and satellites: formation, Space and Planetary Science, composition [Planets and satellites], Kuiper belt: general, formation [Planets and satellites], Astrophysics - Earth and Planetary Astrophysics
Abstract: Within our program of physical characterization of trans-Neptunian objects and centaurs, we predicted a stellar occultation by the centaur (54598) Bienor to occur on January 11, 2019, with good observability potential. We obtained high accuracy astrometric data to refine the prediction, resulting in a shadow path favorable for the Iberian Peninsula. This encouraged us to carry out an occultation observation campaign that resulted in five positive detections from four observing sites. This is the fourth centaur for which a multichord (more than two chords) stellar occultation has been observed so far, the other three being (2060) Chiron, (10199) Chariklo, and (95626) 2002 GZ32. From the analysis of the occultation chords, combined with the rotational light curve obtained shortly after the occultation, we determined that Bienor has an area-equivalent diameter of 150 ± 20 km. This diameter is ∼30 km smaller than the one obtained from thermal measurements. The position angle of the short axis of the best fitting ellipse obtained through the analysis of the stellar occultation does not match that of the spin axis derived from long-term photometric models. We also detected a strong irregularity in one of the minima of the rotational light curve that is present no matter the aspect angle at which the observations were done. We present different scenarios to reconcile the results from the different techniques. We did not detect secondary drops related to potential rings or satellites. Nonetheless, similar rings in size to that of Chariklo’s cannot be discarded due to low data accuracy., European Research Council (ERC) 669416, Space Research Initiative from State of Florida, Spanish grant (MCIU/AEI/FEDER, UE) AYA-2017-84637-R, National Research, Development & Innovation Office (NRDIO) - Hungary K-138962 CAPES-PRINT/UNESP 88887.310463/2018-00 88887.571156/2020-00, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ) 427700/2018-3 310683/2017-3 473002/2013-2 314772/2020-0 308150/2016-3 305917/2019-6 150612/2020-6, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ) E-26/111.488/2013, Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) 2018/11239-8, Spanish Government PGC2018-097374-B-I00, Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) 001, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ), Fundacao de Apoio a Pesquisa do Distrito Federal (FAPDF) 465376/2014-2, Spanish Government AYA-2017-84637-R SEV-2017-0709, Junta de Andalucia PY20_01309, Agencia Estatal de Investigacion PID2020-112789GB-I00, Fondos de Inversiones de Teruel (FITE)
Published: 2023

2. Selfcare in Healthcare – Fehlender Fokus auf Ärztliche Gesundheit?

Author: S. Hellmich
Subjects: Ökonomie, Medicine and health, Selfcare, Arbeitsverdichtung, Arbeitsbedingungen
Abstract: Fragestellung: Der Krankenhausalltag ist in den letzten Jahren komplexer und schnelllebiger geworden. Vielfältige Aufgaben müssen in immer kürzerer Zeit erledigt werden. Die Behandlung von Patienten soll besser, gleichzeitig aber auch effizienter werden. Unter diesem ökonomischen [zum vollständigen Text gelangen Sie über die oben angegebene URL]
Published: 2022
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3. The 2017 May 20 stellar occultation by the elongated centaur (95626) 2002 GZ32

Author: V. Peris, A Fuambuena Leiva, G. Benedetti-Rossi, Victor Ali-Lagoa, Felipe Braga-Ribas, Fernando Fonseca, S. Moindrot, Rene Duffard, P Delincak, T Haymes, Mónica Vara-Lubiano, András Pál, Kosmas Gazeas, T. Pribulla, Albino Carbognani, B Kattentidt, J. Alikakos, Marcelo Assafin, M Bretton, F. Ciabattari, Luis Fernando Acosta Pérez, R. Komžík, A. Alvarez-Candal, Eda Sonbas, J. C. Guirado, F Signoret, J. L. Ortiz, S. Hellmich, J L Lamadrid, J. Horbowicz, H González, C. Schnabel, Josselin Desmars, N. Paschalis, L Ana-Hernández, R. Iglesias-Marzoa, Bruno Sicardy, M Jennings, Estela Fernández-Valenzuela, Y Jiménez-Teja, Vassilis Charmandaris, A. Marciniak, N Maícas, Cs. Kiss, A Selva, Julio Camargo, J. Lecacheux, Nora Morales, C. Perelló, M Boutet, Fernando J. Ballesteros, Stefano Mottola, S. Pastor, Pablo Santos-Sanz, J A Reyes, F. Organero, J Sanchez, Roberto Vieira-Martins, C Ratinaud, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Junta de Andalucía, European Research Council, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, University of Florida, National Research, Development and Innovation Office (Hungary), Slovak Research and Development Agency, CSIC - Unidad de Recursos de Información Científica para la Investigación (URICI), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), 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 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 Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), and Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)
Subjects: Rotation period, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Ellipse, 01 natural sciences, Occultation, law.invention, techniques: photometric, law, Geometric albedo, 0103 physical sciences, occultations, observational [Methods], individual: 2002 GZ(32) [Kuiper Belt objects], methods: observational – techniques: photometric – occultations – Kuiper Belt objects: individual: 2002 GZ32, 010303 astronomy & astrophysics, Kuiper Belt objects: individual: 2002 GZ(32), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], photometric [Techniques], Astronomy and Astrophysics, Centaur, Albedo, Light curve, Kuiper Belt objects: individual: 2002 GZ32, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Occultations, Hydrostatic equilibrium, methods: observational, Astrophysics - Earth and Planetary Astrophysics
Abstract: Full list of authors: Santos-Sanz, P.; Ortiz, J. L.; Sicardy, B.; Benedetti-Rossi, G.; Morales, N.; Fernández-Valenzuela, E.; Duffard, R.; Iglesias-Marzoa, R.; Lamadrid, J. L.; Maícas, N.; Pérez, L.; Gazeas, K.; Guirado, J. C.; Peris, V.; Ballesteros, F. J.; Organero, F.; Ana-Hernández, L.; Fonseca, F.; Alvarez-Candal, A.; Jiménez-Teja, Y. Vara-Lubiano, M.; Braga-Ribas, F.; Camargo, J. I. B.; Desmars, J.; Assafin, M.; Vieira-Martins, R.; Alikakos, J.; Boutet, M.; Bretton, M.; Carbognani, A.; Charmandaris, V.; Ciabattari, F.; Delincak, P.; Fuambuena Leiva, A.; González, H.; Haymes, T.; Hellmich, S.; Horbowicz, J.; Jennings, M.; Kattentidt, B.; Kiss, Cs; Komžík, R.; Lecacheux, J.; Marciniak, A.; Moindrot, S.; Mottola, S.; Pal, A.; Paschalis, N.; Pastor, S.; Perello, C.; Pribulla, T.; Ratinaud, C.; Reyes, J. A.; Sanchez, J.; Schnabel, C.; Selva, A.; Signoret, F.; Sonbas, E.; Alí-Lagoa, V.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We predicted a stellar occultation of the bright star Gaia DR1 4332852996360346368 (UCAC4 385-75921) (mV = 14.0 mag) by the centaur 2002 GZ32 for 2017 May 20. Our latest shadow path prediction was favourable to a large region in Europe. Observations were arranged in a broad region inside the nominal shadow path. Series of images were obtained with 29 telescopes throughout Europe and from six of them (five in Spain and one in Greece) we detected the occultation. This is the fourth centaur, besides Chariklo, Chiron, and Bienor, for which a multichord stellar occultation is reported. By means of an elliptical fit to the occultation chords, we obtained the limb of 2002 GZ32 during the occultation, resulting in an ellipse with axes of 305 ± 17 km × 146 ± 8 km. From this limb, thanks to a rotational light curve obtained shortly after the occultation, we derived the geometric albedo of 2002 GZ32 (pV = 0.043 ± 0.007) and a 3D ellipsoidal shape with axes 366 km × 306 km × 120 km. This shape is not fully consistent with a homogeneous body in hydrostatic equilibrium for the known rotation period of 2002 GZ32. The size (albedo) obtained from the occultation is respectively smaller (greater) than that derived from the radiometric technique but compatible within error bars. No rings or debris around 2002 GZ32 were detected from the occultation, but narrow and thin rings cannot be discarded. © 2020 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society., P.S-S. acknowledges financial support by the Spanish grant AYA-RTI2018-098657-J-I00 'LEO-SBNAF' (MCIU/AEI/FEDER, UE). PS-S, JLO, NM, and RD 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), 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. We acknowledge support of the publication fee by the CSIC Open Access Publication Support Initiative through its Unit of Information Resources for Research (URICI). 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). Part of the research leading to these results has received funding from the European Research Council under the European Community's H2020 (2014-2020/ERC Grant Agreement no. 669416 `LUCKY STAR'). E.F-V. acknowledges funding through the Preeminant Postdoctoral Program of the University of Central Florida. Part of the data were collected during the photometric monitoring observations with the robotic and remotely controlled observatory at the University of Athens Observatory -UOAO (Gazeas 2016). F.J.B. acknowledges financial support by the Spanish grant AYA2016-81065-C2-2-P. A.A-C. acknowledges support from FAPERJ (grant E26/203.186/2016) and CNPq (grants 304971/20162 and 401669/2016-5). A.C. acknowledges the use of the main telescope of theAstronomical Observatory of the Autonomous Region of the Aosta Valley (OAVdA). C.K. has been supported by the grants K125015 and GINOP-2.3.2-15-2016-00003 of the National Research, Development and Innovation Office, Hungary (NKFIH). T.P. and R.K. acknowledge support from the project ITMS No. 26220120029, based on the Research and development program financed from the European Regional Development Fund and from the Slovak Research and Development Agency -the contract No. APVV-150458. We are grateful to the CAHA and OSN staffs. This research is partially based on observations collected at Centro Astronomico Hispano-Aleman (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 the Instituto de Astrofisica de Canarias in the Spanish Roque de losMuchachos Observatory. Partially based on observations made with the Tx40 telescope 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 Arag on (CEFCA). Tx40 is funded with the Fondos de Inversiones de Teruel (FITE). 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.
Published: 2021
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4. Convex Shape and Rotation Model of Lucy Target (11351) Leucus from Lightcurves and Occultations

Author: Simone Marchi, Harold F. Levison, Stefano Mottola, Marc W. Buie, Amanda M. Zangari, S. Hellmich, and Michael E. Brown
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Rotation period, Asteroiden und Kometen, Ecliptic coordinate system, Planetengeodäsie, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Phase curve, Light curves, Light curve, Stellar occultation, Occultation, Jupiter trojans, Geophysics, Space and Planetary Science, Sidereal time, Geometric albedo, Orientation (geometry), Earth and Planetary Sciences (miscellaneous), Astrophysics::Earth and Planetary Astrophysics, CCD photometry, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report new photometric lightcurve observations of the Lucy Mission target (11351) Leucus acquired during the 2017, 2018, and 2019 apparitions. We use these data in combination with stellar occultations captured during five epochs to determine the sidereal rotation period, the spin axis orientation, a convex shape model, the absolute scale of the object, its geometric albedo, and a model of the photometric properties of the target. We find that Leucus is a prograde rotator with a spin axis located within a sky-projected radius of 3° (1σ) from J2000 Ecliptic coordinates (λ = 208°, β = +77°) or J2000 Equatorial Coordinates (R.A. = 248°, decl. = +58°). The sidereal period is refined to P sid = 445.683 ± 0.007 h. The convex shape model is irregular, with maximum dimensions of 60.8, 39.1, and 27.8 km. The convex model accounts for global features of the occultation silhouettes, although minor deviations suggest that local and global concavities are present. We determine a geometric albedo of p V = 0.043 ± 0.002. The derived phase curve supports a D-type classification for Leucus.
Published: 2020

5. Study of the physical properties of selected active objects in the main belt and surrounding regions by broadband photometry

Author: E. Kuehrt, S. Hellmich, Stefano Mottola, Alexander Baransky, Karen J. Meech, and Serhii Borysenko
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, photometric observations, Comet, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, law.invention, dust activity, Telescope, Photometry (optics), Space and Planetary Science, law, Asteroid, Observatory, quasi-Hilda comets, 0103 physical sciences, Broadband, Asteroid belt, main belt comets, 010303 astronomy & astrophysics, Geology, active asteroids, Astrophysics - Earth and Planetary Astrophysics
Abstract: Dynamically different groups of comets and active asteroids with orbits at 2 - 5 a. u. show dust activity in varying degrees and forms. Photometric study and comparison of physical parameters can help to classify mechanisms and nature of the activity for such objects. We present new observations using broadband photometry of 15 active objects in the main asteroid belt and surrounding regions obtained during 2012 - 2016. The study aims to compare the physical properties of main-belt comets (MBCs), quasi-Hilda comets (QHCs), and active asteroids (AAs). The observations were carried out with the 0.7-m telescope of the Kyiv Comet Station, Ukraine, and with the 1.23-m telescope at the Calar Alto Observatory, Spain, using BVR broadband filters. Upper limits for the nuclear radii, Afrho parameters, and color indices were measured. The results of 2012 - 2016 observations suggest that there exist systematic differences in the physical parameters of MBCs and QHCs., 10 pages, 3 figures, 4 tables. Accepted for publication in Astronomische Nachrichten
Published: 2020

6. The large trans-Neptunian object 2002 TC 302 from combined stellar occultation, photometry, and astrometry data

Author: G. Scarfi, T. Pribulla, J. C. Guirado, L. Buzzi, Grzegorz Dudziński, A. Farkas-Takács, L. Mazzei, E. Meza, A. Aletti, J. M. Christille, C. Perelló, L. Morrone, V. Peris, Valerio Nascimbeni, J. Lecacheux, J. M. Madiedo, Rene Duffard, F. Mancini, Bruno Sicardy, J. Alikakos, Vassilis Charmandaris, Cs. Kiss, M. Conjat, Raoul Behrend, R. Komžík, Frédéric Vachier, Martina Maestripieri, J. Skvarc, Paolo Bacci, T. G. Mueller, Domenico Nardiello, R. Iglesias-Marzoa, F. Colas, Aleksandar Cikota, András Pál, N. Paschalis, R. Szakats, A. Campo Bagatin, P. J. Gutierrez, Giacomo Succi, Pablo Santos-Sanz, A. R. Gomes-Júnior, Gábor Marton, M. Butkiewicz-Bak, E. Varga-Verebélyi, M. Masucci, Estela Fernández-Valenzuela, V. Tsamis, Victor Ali-Lagoa, Felipe Braga-Ribas, M. Alighieri, Roberto Vieira-Martins, F. Manzano, Julio Camargo, E. Dal Canto, S. Hellmich, F. Roques, A. Vecchione, A. Navarro, Stefano Mottola, A. Noschese, Albino Carbognani, F. Lavalade, Josselin Desmars, Mónica Vara-Lubiano, Nora Morales, C. Schnabel, Mauro Bachini, Kosmas Gazeas, J. M. Mari, Przemyslaw Bartczak, W. Beisker, S. Sposetti, F. Ciabattari, A. Alvarez-Candal, Stefan Cikota, J. L. Ortiz, Marcelo Assafin, A. Marciniak, G. Benedetti-Rossi, H. Mikuz, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Investigación Informática, Astronomía y Astrofísica, European Commission, Junta de Andalucía, Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Fundações de Amparo à Pesquisa (Brasil), National Research, Development and Innovation Office (Hungary), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, IAA-CSIC, Université de Paris, Laboratório Interinstitucional de E-Astronomia - LIneA, Federal University of Technology-Paraná (UTFPR / DAFIS), Observatório Nacional/MCTIC, University of Central Florida, 'G. Galilei' Universita Degli Studi di Padova, INAF - Osservatorio Astronomico di Padova, LAM, INAF - Osservatorio di Astrofisica e Scienza Dello Spazio, Schiaparelli Astronomical Observatory, Astronomical Observatory San Marcello Pistoiese CARA Project, Crni Vrh Observatory, University of Ljubljana, Osservatorio Astronomico di Monte Agliale, 55 Impasse de la Marjolaine, Observatorio Astronomico Iota-Scorpii, 1075 Avenue Saint Philippe, Observatoire de la Côte d'Azur, Gnosca Observatory, Osservatorio Astronomico di Tavolaia, 63 Boulevard de Brandebourg, UPMC Univ Paris 06, Universidade Federal do Rio de Janeiro (UFRJ), International Occultation Timing Association - European Section (IOTA-ES), Observatoire de Geneve, Max Planck Institut für Extraterrestrische Physik (MPE), Universidade Estadual Paulista (Unesp), Institute of Planetary Research, Universidad de Alicante, Unversidad de Alicante, Faculty of Electrical Engineering and Computing, E.O. Lawrence Berkeley National Laboratory, Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVdA), Research Centre for Astronomy and Earth Sciences, Institute of Physics, Slovak Academy of Sciences, MTA-ELTE Exoplanet Research Group, ELTE Gothard Astrophysical Observatory, National Observatory of Athens, University of Crete, Faculty of Science, A. Mickiewicz University, Nunki Observatory, Ellinogermaniki Agogi Observatory, Universidad de Valencia, Centro de Estudios de Física Del Cosmos de Aragón, Universidad de la Laguna, Agrupació Astronómica de Sabadell, Osservatorio Salvatore di Giacomo, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatorio Nacional [Rio de Janeiro], Universidad Politécnica Salesiana [Quito], Observatório Nacional/MCT, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Absolute magnitude, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Kuiper belt objects: individual: 2002 TC302, 01 natural sciences, Occultation, law.invention, Telescope, Photometry (optics), law, Geometric albedo, Física Aplicada, 0103 physical sciences, Trans-Neptunian object, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Earth and Planetary Astrophysics (astro-ph.EP), photometric [Techniques], Astronomy and Astrophysics, general [Kuiper belt], Astrometry, individual: 2002 TC302 [Kuiper belt objects], Kuiper belt: general, Occultations, Techniques: photometric, Light curve, Space and Planetary Science, [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: All authors: Ortiz, J. L.; Santos-Sanz, P.; Sicardy, B.; Benedetti-Rossi, G.; Duffard, R.; Morales, N.; Braga-Ribas, F.; Fernández-Valenzuela, E.; Nascimbeni, V.; Nardiello, D.; Carbognani, A.; Buzzi, L.; Aletti, A.; Bacci, P.; Maestripieri, M.; Mazzei, L.; Mikuz, H.; Skvarc, J.; Ciabattari, F.; Lavalade, F. Scarfi, G.; Mari, J. M.; Conjat, M.; Sposetti, S.; Bachini, M.; Succi, G.; Mancini, F.; Alighieri, M.; Dal Canto, E.; Masucci, M.; Vara-Lubiano, M.; Gutiérrez, P. J.; Desmars, J.; Lecacheux, J.; Vieira-Martins, R.; Camargo, J. I. B.; Assafin, M.; Colas, F.; Beisker, W.; Behrend, R.; Mueller, T. G.; Meza, E.; Gomes-Junior, A. R.; Roques, F.; Vachier, F.; Mottola, S.; Hellmich, S.; Campo Bagatin, A.; Alvarez-Candal, A.; Cikota, S.; Cikota, A.; Christille, J. M.; Pál, A.; Kiss, C.; Pribulla, T.; Komžík, R.; Madiedo, J. M.; Charmandaris, V.; Alikakos, J.; Szakáts, R.; Farkas-Takács, A.; Varga-Verebélyi, E.; Marton, G.; Marciniak, A.; Bartczak, P.; Butkiewicz-Baķ, M.; Dudziński, G.; Alí-Lagoa, V.; Gazeas, K.; Paschalis, N.; Tsamis, V.; Guirado, J. C.; Peris, V.; Iglesias-Marzoa, R.; Schnabel, C.; Manzano, F.; Navarro, A.; Perelló, C.; Vecchione, A.; Noschese, A.; Morrone, L., Context. Deriving physical properties of trans-Neptunian objects is important for the understanding of our Solar System. This requires observational efforts and the development of techniques suitable for these studies. Aims. Our aim is to characterize the large trans-Neptunian object (TNO) 2002 TC302. Methods. Stellar occultations offer unique opportunities to determine key physical properties of TNOs. On 28 January 2018, 2002 TC302 occulted a mv ∼ 15.3 star with designation 593-005847 in the UCAC4 stellar catalog, corresponding to Gaia source 130957813463146112. Twelve positive occultation chords were obtained from Italy, France, Slovenia, and Switzerland. Also, four negative detections were obtained near the north and south limbs. This represents the best observed stellar occultation by a TNO other than Pluto in terms of the number of chords published thus far. From the 12 chords, an accurate elliptical fit to the instantaneous projection of the body can be obtained that is compatible with the near misses. Results. The resulting ellipse has major and minor axes of 543 ± 18 km and 460 ± 11 km, respectively, with a position angle of 3 ± 1 degrees for the minor axis. This information, combined with rotational light curves obtained with the 1.5 m telescope at Sierra Nevada Observatory and the 1.23 m telescope at Calar Alto observatory, allows us to derive possible three-dimensional shapes and density estimations for the body based on hydrostatic equilibrium assumptions. The effective diameter in equivalent area is around 84 km smaller than the radiometrically derived diameter using thermal data from Herschel and Spitzer Space Telescopes. This might indicate the existence of an unresolved satellite of up to ∼300 km in diameter, which is required to account for all the thermal flux, although the occultation and thermal diameters are compatible within their error bars given the considerable uncertainty of the thermal results. The existence of a potential satellite also appears to be consistent with other ground-based data presented here. From the effective occultation diameter combined with absolute magnitude measurements we derive a geometric albedo of 0.147 ± 0.005, which would be somewhat smaller if 2002 TC302 has a satellite. The best occultation light curves do not show any signs of ring features or any signatures of a global atmosphere. © ESO 2020., This research was partially based on data taken at the Sierra Nevada Observatory, which is operated by the Instituto de Astrofisica de Andalucia (CSIC). This research is also partially based on data taken at the German-Spanish Calar Alto observatory, which is jointly operated by the Max Planck Institute fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC). Part of the results were also based on observations taken at the 1.6m telescope on Pico dos Dias Observatory. This research was partially based on observations collected at the Schmidt telescope 67/92 cm (Asiago, Italy) of the INAF - Osservatorio Astronomico di Padova. Funding from Spanish projects AYA2014-56637-C2-1-P, AYA2017-89637-R, from FEDER, and Proyecto de Excelencia de la Junta de Andalucia 2012-FQM1776 is acknowledged. We would like to acknowledge financial support by the Spanish grant AYA-RTI2018-098657-JI00 "LEO-SBNAF" (MCIU/AEI/FEDER, UE) and the financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV- 2017-0709). Part of the research received funding from the European Union's Horizon 2020 Research and Innovation Programme, under grant agreement no. 687378 and from the ERC programme under Grant Agreement no. 669416 Lucky Star. The following authors acknowledge the respective CNPq grants: FB-R 309578/2017-5; RV-M 304544/2017-5, 401903/2016-8; J.I.B.C. 308150/2016-3; MA 427700/2018-3, 310683/2017-3, 473002/2013-2. This study was financed in part by the CoordenacAo de Aperfeiacoamento de Pessoal de Nivel Superior - Brasil (CAPES) - Finance Code 001 and the National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq grant 465376/2014-2). GBR acknowledges CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016, MA FAPERJ grant E-26/111.488/2013 and ARGJr FAPESP grant 2018/11239-8. E.F.-V. acknowledges support from the 2017 Preeminent Postdoctoral Program (P3) at UCF. C.K., R.S., A.F-T., and G.M. have been supported by the K-125015 and GINOP-2.3.2-15-2016-00003 grants of the Hungarian National Research, Development and Innovation Office (NKFIH), Hungary. G.M. was also supported by the Hungarian National Research, Development and Innovation Office (NKFIH) grant PD-128 360. R.K. and T.P. were supported by the VEGA 2/0031/18 grant. We acknowledge the use of Occult software by D. Herald.
Published: 2020
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7. Spitzer Albedos of Near-Earth Objects

Author: Annika Gustafsson, S. Hellmich, Joseph L. Hora, David E. Trilling, Stefano Mottola, Michael Mommert, Alan W. Harris, Andrew McNeill, and Howard A. Smith
Subjects: Astronomical Reference Material: Surveys, 010504 meteorology & atmospheric sciences, Visible Astronomy, Monte Carlo method, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, Geometric albedo, Astronomical Techniques: Photometry, 0103 physical sciences, Astronomical Methods: Infrared Astronomy, education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Near-Earth object, Sampling (statistics), Astronomy and Astrophysics, asteroids: Near-Earth Objects, Albedo, Meteorite, Space and Planetary Science, Asteroid, Astrophysics - Earth and Planetary Astrophysics
Abstract: Thermal infrared observations are the most effective way to measure asteroid diameter and albedo for a large number of near-Earth objects. Major surveys like NEOWISE, NEOSurvey, ExploreNEOs, and NEOLegacy find a small fraction of high albedo objects that do not have clear analogs in the current meteorite population. About 8% of Spitzer-observed near-Earth objects have nominal albedo solutions greater than 0.5. This may be a result of lightcurve variability leading to an incorrect estimate of diameter or inaccurate absolute visual magnitudes. For a sample of 23 high albedo NEOs we do not find that their shapes are significantly different from the McNeill et al. (2019) near-Earth object shape distribution. We performed a Monte Carlo analysis on 1505 near-Earth objects observed by Spitzer, sampling the visible and thermal fluxes of all targets to determine the likelihood of obtaining a high albedo erroneously. Implementing the McNeill shape distribution for near-Earth objects, we provide an upper-limit on the geometric albedo of 0.5+/-0.1 for the near-Earth population., 19 pages, accepted by the Astronomical Journal
Published: 2019

8. Detailed Characterization of Low Activity Comet 49P/Arend-Rigaux

Author: Olivier Hainaut, Jacqueline V. Keane, Ekkehard Kührt, Laurie E.U. Chu, Tony L. Farnham, Karen J. Meech, Stefano Mottola, S. Hellmich, and Jan T. Kleyna
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Comet, Dust particles, Low activity, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, cometary activity, Light curve, 01 natural sciences, comet Arend-Rigaux, Jupiter, Outgassing, Dead state, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Minor planet, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Comet 49P/Arend-Rigaux is a well known low-activity Jupiter Family comet. Despite the low activity, we have witnessed outgassing activity in 1992, 2004, and 2012. In 2012 a broad tail-like feature (PA$\sim270^\circ, \sim2.3\times10^5$ km) and a narrow jet-like feature (PA$\sim180^\circ, \sim9.3\times10^4$ km) were seen simultaneously. Using Finson-Probstein (FP) dust dynamical models we determine: grain sizes released in each event; duration of activity; when activity peaked; and velocity of the dust particles, allowing us to make comparisons between the events. We find that the tail feature in 2012 is similar to the tail in 1992 with large grains (40-4000 $\mu$m) peaking in activity near perihelion with a long outgassing duration greater than 150 days. The jet feature from 2012, however, is more similar to the 2004 event which we model with small grains (1-8 $\mu$m) with a short duration of activity ($\sim$1 month). The main difference between these two features is that the 2004 event occurs prior to perihelion, while the 2012 event is post-perihelion. We use the grain sizes from the FP models to constrain ice sublimation models. Between 1985 and 2018 we cover 6 apparitions with 26 nights of our own observations plus data from the literature and the Minor Planet Center, which together, allow us to model the heliocentric light curve. We find that the models are consistent with H$_2$O ice sublimation as the volatile responsible for driving activity over most of the active phases and a combination of H$_2$O and CO$_2$ ices are responsible for driving activity near perihelion. We measure the fractional active area over time for H$_2$O and discover that the activity decreases from an average active area of $\sim3\%$ to $\sim0.2\%$. This secular decrease in activity implies that the comet is becoming depleted of volatiles and is in the process of transitioning to a dormant or dead state., Comment: 18 pages, 8 figures, Accepted for publication by Icarus
Published: 2019
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9. Influence of the Yarkovsky force on Jupiter Trojan asteroids

Author: Gerhard Hahn, D. de Niem, S. Hellmich, Stefano Mottola, and E. Kührt
Subjects: Asteroiden und Kometen, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Jupiter Trojan Asteroids, Population, Yarkovsky effect, FOS: Physical sciences, Astrophysics, Rotation, 01 natural sciences, Jupiter, 0103 physical sciences, Libration, Eccentricity (behavior), education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, Astronomy and Astrophysics, Amplitude, Space and Planetary Science, Trojan, Numerical integration, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Aims.We investigate the influence of the Yarkovsky force on the long-term orbital evolution of Jupiter Trojan asteroids.Methods.Clones of the observed population with different sizes and different thermal properties were numerically integrated for 1 Gyr with and without the Yarkovsky effect. The escape rate of these objects from the Trojan region as well as changes in the libration amplitude, eccentricity, and inclination were used as a metric of the strength of the Yarkovsky effect on the Trojan orbits.Results.Objects with radiiR≤ 1 km are significantly influenced by the Yarkovsky force. The effect causes a depletion of these objects over timescales of a few hundred million years. As a consequence, we expect the size-frequency distribution of small Trojans to show a shallower slope than that of the currently observable population (R≳ 1 km), with a turning point betweenR= 100 m andR= 1 km. The effect of the Yarkovsky acceleration on the orbits of Trojans depends on the sense of rotation in a complex way. The libration amplitude of prograde rotators decreases with time while the eccentricity increases. Retrograde rotators experience the opposite effect, which results in retrograde rotators being ejected faster from the 1:1 resonance region. Furthermore, for objects affected by the Yarkovsky force, we find indications that the effect tends to smooth out the differences in the orbital distribution between the two clouds.
Published: 2019
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10. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

Author: Valerio Nascimbeni, J. Lecacheux, Toni Santana-Ros, Agustín Sánchez-Lavega, Pablo Santos-Sanz, L. Nerli, D. T. Koseoglu, Frédéric Vachier, V. Peris, Przemyslaw Bartczak, R. Komžík, Eda Sonbas, Cs. Kiss, Gábor Marton, C. Ries, Yavuz Güney, Marcelo Assafin, Martina Maestripieri, Josselin Desmars, T. G. Mueller, Osman Demircan, O. Erece, V. Granata, A. R. Gomes-Júnior, Francesco Marzari, Ulrich Hopp, Cahit Yeşilyaprak, N. Paschalis, A. Campo Bagatin, B. Gaehrken, Paolo Bacci, V. Tsamis, O. Satir, F. Martinelli, F. L. Rommel, Santiago Pérez-Hoyos, F. Ciabattari, R. Iglesias-Marzoa, Stefano Mottola, Ricardo Hueso, Julio Camargo, Herman Mikuz, Françoise Roques, Mohammad Shameoni Niaei, Mauro Bachini, Vassilis Charmandaris, Jose Luis Ortiz, A. Takácsné Farkas, András Pál, A. Carbognani, L. Tzouganatos, Giuseppe Leto, Aleksandar Cikota, G. Benedetti-Rossi, Roberto Vieira-Martins, Nicolás Morales, José M. Madiedo, Bruno Sicardy, Róbert Szakáts, B. E. Morgado, Theodor Pribulla, Estela Fernández-Valenzuela, M. Butkiewicz-Bąk, Afşar Kabaş, Alvaro Alvarez-Candal, Giacomo Succi, Jérôme Berthier, J. Alikakos, Ç. Püsküllü, Kamil Hornoch, W. Beisker, E. Meza, Stefan Cikota, T. Ozisik, E. Varga-Verebélyi, J. M. Christille, J. C. Guirado, Grzegorz Dudziński, L. Mazzei, J. M. Ohlert, Rene Duffard, Raoul Behrend, S. Kalkan, A. Marciniak, N. Karaman, S. Hellmich, Kosmas Gazeas, Victor Ali-Lagoa, Ozan Ünsalan, Felipe Braga-Ribas, François Colas, Petr Pravec, Diane Berard, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Astronomía y Astrofísica, ITA, USA, GBR, FRA, 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), Observatorio Nacional [Rio de Janeiro], Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Observatório Nacional/MCT, Ludwig-Maximilians-Universität München (LMU), Dipartimento di Fisica, Università degli Studi di Padova = University of Padua (Unipd), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Centro Astronomico di Libbiano, Associazione Astrofili Alta Valdera, Istituto di Informatica e Telematica (IIT-CNR), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), 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), DLR Institute of Planetary Research, German Aerospace Center (DLR), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Physik-Institut, Universität Zürich [Zürich] = University of Zurich (UZH), 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), Observatório do Valongo/UFRJ [Rio de Janeiro], Universidade Federal do Rio de Janeiro (UFRJ), Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), International Occultation Timing Association European Section (IOTA ES), International Occultation Timing Association European Section, 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 (CEA), IESL, Osserv Astrofis Catania, Ist Nazl Astrofis, TKK Helsinki University of Technology (TKK), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Department of Astrophysics, Astronomy and Mechanics Panepistimiopolis (DAAMP), National and Kapodistrian University of Athens (NKUA), Astronomical Union of Sparta [Sparta], University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Departamento de Fı'sica Aplicada I, Escuela Tecnica Superior de Ingenieria Bilbao, Observatorio Astronomico de Valencia, Universitat de València (UV), Ondokuz Mayıs Üniversitesi, European Commission, European Research Council, Hungarian Academy of Sciences, Generalitat Valenciana, Junta de Andalucía, Ministerio de Economía, Industria y Competitividad (España), Universita degli Studi di Padova, Consiglio Nazionale delle Ricerche [Roma] (CNR), Université Nice Sophia Antipolis (... - 2019) (UNS), 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), 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), L2EP - Équipe Réseaux, Laboratoire d’Électrotechnique et d’Électronique de Puissance - ULR 2697 (L2EP), Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM), University of Geneva [Switzerland], University of the Basque Country [Bizkaia] (UPV/EHU), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Czech Academy of Sciences [Prague] (ASCR), 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), Universität Zürich [Zürich] (UZH), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Universidade Federal do Rio de Janeiro [Rio de Janeiro] (UFRJ), Laboratoire d’Électrotechnique et d’Électronique de Puissance - EA 2697 (L2EP), Ecole Centrale de Lille-École Nationale Supérieure d'Arts et Métiers (ENSAM), Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Haute Etude d'Ingénieurs-Université de Lille-Ecole Centrale de Lille-École Nationale Supérieure d'Arts et Métiers (ENSAM), HESAM Université (HESAM)-HESAM Université (HESAM)-Haute Etude d'Ingénieurs-Université de Lille, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Athens [Greece] (UOA), and Universitat de València (UV)-Observatorio Astronomico de Valencia
Subjects: 010504 meteorology & atmospheric sciences, European community, Trans Neptunian Object, Dwarf planet, Haumea, FOS: Physical sciences, Library science, shape, 01 natural sciences, size, dwarf planet, Neptune, Física Aplicada, 0103 physical sciences, media_common.cataloged_instance, European union, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [PHYS]Physics [physics], density, 2003 EL61, Kuiper-belt, photometric-observations, collisional family, object, bodies, albedo, satellites, Uranus, Dwarf planets, Multidisciplinary, European research, Asteroid, Trans-Neptunian, Astronomy, Stellar occultation, Moons of Haumea, stellar occultation, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ring, Astrophysics - Earth and Planetary Astrophysics
Abstract: Ortiz, José Luis et. al., Haumea-one of the four known trans-Neptunian dwarf planets- is a very elongated and rapidly rotating body1-3. In contrast to other dwarf planets4-6, its size, shape, albedo and density are not well constrained. The Centaur Chariklo was the first body other than a giant planet known to have a ring system7, and the Centaur Chiron was later found to possess something similar to Chariklo's rings8,9. Here we report observations from multiple Earth-based observatories of Haumea passing in front of a distant star (a multichord stellar occultation). Secondary events observed around the main body of Haumea are consistent with the presence of a ring with an opacity of 0.5, width of 70 kilometres and radius of about 2,287 kilometres. The ring is coplanar with both Haumea's equator and the orbit of its satellite Hi'iaka. The radius of the ring places it close to the 3:1 mean-motion resonance with Haumea's spin period-that is, Haumea rotates three times on its axis in the time that a ring particle completes one revolution. The occultation by the main body provides an instantaneous elliptical projected shape with axes of about 1,704 kilometres and 1,138 kilometres. Combined with rotational light curves, the occultation constrains the three-dimensional orientation of Haumea and its triaxial shape, which is inconsistent with a homogeneous body in hydrostatic equilibrium. Haumea's largest axis is at least 2,322 kilometres, larger than previously thought, implying an upper limit for its density of 1,885 kilograms per cubic metre and a geometric albedo of 0.51, both smaller than previous estimates1,10,11. In addition, this estimate of the density of Haumea is closer to that of Pluto than are previous estimates, in line with expectations. No global nitrogen- or methane-dominated atmosphere was detected.© 2017 Macmillan Publishers Limited, part of Springer Nature. All rights reserved., J.L.O. acknowledges funding from Spanish and Andalusian grants MINECO AYA-2014-56637-C2-1-P and J. A. 2012-FQM1776 as well as FEDER funds. Part of the research leading to these results received funding from the European Union's Horizon 2020 Research and Innovation Programme, under grant agreement no. 687378. B.S. acknowledges support from the French grants 'Beyond Neptune' ANR-08-BLAN-0177 and 'Beyond Neptune II' ANR-11-1S56-0002. Part of the research leading to these results has received funding from the European Research Council under the European Community's H2020 (2014-2020/ERG grant agreement no. 669416 'Lucky Star'). A.P. and R.S. have been supported by the grant LP2012-31 of the Hungarian Academy of Sciences. All of the Hungarian contributors acknowledge the partial support from K-125015 grant of the National Research, Development and Innovation Office (NKFIH). G.B.-R., F.B.-R., F.L.R., R.V.-M., J.I.B.C., M.A., A.R.G.-J. and B.E.M. acknowledge support from CAPES, CNPq and FAPERJ. J.C.G. acknowledges funding from AYA2015-63939-C2-2-P and from the Generalitat Valenciana PROMETEOII/2014/057. K.H. and P.P. were supported by the project RVO:67985815. The Astronomical Observatory of the Autonomous Region of the Aosta Valley acknowledges a Shoemaker NEO Grant 2013 from The Planetary Society. We acknowledge funds from a 2016 'Research and Education' grant from Fondazione CRT. We also acknowledge the Slovakian project ITMS no. 26220120029.
Published: 2017

11. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

Author: Ortiz, J.L. Santos-Sanz, P. Sicardy, B. Benedetti-Rossi, G. Bérard, D. Morales, N. Duffard, R. Braga-Ribas, F. Hopp, U. Ries, C. Nascimbeni, V. Marzari, F. Granata, V. Pál, A. Kiss, C. Pribulla, T. Komžík, R. Hornoch, K. Pravec, P. Bacci, P. Maestripieri, M. Nerli, L. Mazzei, L. Bachini, M. Martinelli, F. Succi, G. Ciabattari, F. Mikuz, H. Carbognani, A. Gaehrken, B. Mottola, S. Hellmich, S. Rommel, F.L. Fernández-Valenzuela, E. Bagatin, A.C. Cikota, S. Cikota, A. Lecacheux, J. Vieira-Martins, R. Camargo, J.I.B. Assafin, M. Colas, F. Behrend, R. Desmars, J. Meza, E. Alvarez-Candal, A. Beisker, W. Gomes, A.R. Morgado, B.E. Roques, F. Vachier, F. Berthier, J. Mueller, T.G. Madiedo, J.M. Unsalan, O. Sonbas, E. Karaman, N. Erece, O. Koseoglu, D.T. Ozisik, T. Kalkan, S. Guney, Y. Niaei, M.S. Satir, O. Yesilyaprak, C. Puskullu, C. Kabas, A. Demircan, O. Alikakos, J. Charmandaris, V. Leto, G. Ohlert, J. Christille, J.M. Szakáts, R. Farkas, A.T. Varga-Verebélyi, E. Marton, G. Marciniak, A. Bartczak, P. Santana-Ros, T. Butkiewicz-Bak, M. Dudzinski, G. Alí-Lagoa, V. Gazeas, K. Tzouganatos, L. Paschalis, N. Tsamis, V. Sánchez-Lavega, A. Pérez-Hoyos, S. Hueso, R. Guirado, J.C. Peris, V. Iglesias-Marzoa, R.
Abstract: Haumea-one of the four known trans-Neptunian dwarf planets- is a very elongated and rapidly rotating body1-3. In contrast to other dwarf planets4-6, its size, shape, albedo and density are not well constrained. The Centaur Chariklo was the first body other than a giant planet known to have a ring system7, and the Centaur Chiron was later found to possess something similar to Chariklo's rings8,9. Here we report observations from multiple Earth-based observatories of Haumea passing in front of a distant star (a multichord stellar occultation). Secondary events observed around the main body of Haumea are consistent with the presence of a ring with an opacity of 0.5, width of 70 kilometres and radius of about 2,287 kilometres. The ring is coplanar with both Haumea's equator and the orbit of its satellite Hi'iaka. The radius of the ring places it close to the 3:1 mean-motion resonance with Haumea's spin period-that is, Haumea rotates three times on its axis in the time that a ring particle completes one revolution. The occultation by the main body provides an instantaneous elliptical projected shape with axes of about 1,704 kilometres and 1,138 kilometres. Combined with rotational light curves, the occultation constrains the three-dimensional orientation of Haumea and its triaxial shape, which is inconsistent with a homogeneous body in hydrostatic equilibrium. Haumea's largest axis is at least 2,322 kilometres, larger than previously thought, implying an upper limit for its density of 1,885 kilograms per cubic metre and a geometric albedo of 0.51, both smaller than previous estimates1,10,11. In addition, this estimate of the density of Haumea is closer to that of Pluto than are previous estimates, in line with expectations. No global nitrogen- or methane-dominated atmosphere was detected. © 2017 Macmillan Publishers Limited, part of Springer Nature. All rights reserved.
Published: 2017

12. Binary asteroid population. 3. Secondary rotations and elongations

Author: Jozef Vilagi, Stefano Mottola, Robert D. Stephens, Jean Lecacheux, R. Inasaridze, Dirk Terrell, Z. Krzeminski, B. Macomber, Shantanu P. Naidu, Peter Brown, Petr Pravec, Agnieszka Kryszczyńska, Daniel E. Reichart, Kamil Hornoch, R. Dyvig, R. Montaigut, John Gross, O. Kvaratskhelia, David Higgins, Vasilij Rumyantsev, Vladimir Benishek, J. Žižka, V. R. Ayvazian, Vishnu Reddy, F. Marchis, A. Leroy, J. Vrastil, Igor Molotov, Yu. N. Krugly, R. Durkee, Adrian Galad, Aaron P. LaCluyze, Štefan Gajdoš, Vasilij G. Chiorny, Walter R. Cooney, Julian Oey, S. Hellmich, M. Baek, N. Gaftonyuk, J. G. Ries, J. B. Haislip, Leonard Kornoš, Peter Kusnirak, Marek Husárik, François Colas, P. Scheirich, Joe Pollock, Donald P. Pray, G. Masi, Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Physics Division [Oak Ridge], Oak Ridge National Laboratory [Oak Ridge] (ORNL), UT-Battelle, LLC-UT-Battelle, LLC, Sonoita Research Observatory, Department of Physics and Astronomy [Boone], Appalachian State University, University of North Carolina System (UNC)-University of North Carolina System (UNC), Skalnaté Pleso Observatory, Shed of Science Observatory, UND Department of Space Studies, University of North Dakota [Grand Forks] (UND), German Aerospace Center (DLR), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Kingsgrove Observatory, Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), 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), SETI Institute, 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), L2EP - Équipe Réseaux, Laboratoire d’Électrotechnique et d’Électronique de Puissance - ULR 2697 (L2EP), Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, and HESAM Université (HESAM)-HESAM Université (HESAM)
Subjects: 010504 meteorology & atmospheric sciences, Fission, Population, Orbital eccentricity, Astrophysics, Rotation, Near-Earth objects, 01 natural sciences, rotation, Photometry, 0103 physical sciences, education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], education.field_of_study, Near-Earth object, Astronomy, Astronomy and Astrophysics, dynamics, Asteroids, Astron, Space and Planetary Science, Asteroid, Tidal circularization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We collected data on rotations and elongations of 46 secondaries of binary and triple systems among near-Earth, Mars-crossing and small main belt asteroids. 24 were found or are strongly suspected to be synchronous (in 1:1 spin–orbit resonance), and the other 22, generally on more distant and/or eccentric orbits, were found or are suggested to have asynchronous rotations. For 18 of the synchronous secondaries, we constrained their librational angles, finding that their long axes pointed to within 20° of the primary on most epochs. The observed anti-correlation of secondary synchroneity with orbital eccentricity and the limited librational angles agree with the theories by Cuk and Nesvorný (Cuk, M., Nesvorný, D. [2010]. Icarus 207, 732–743) and Naidu and Margot (Naidu, S.P., Margot, J.-L. [2015]. Astron. J. 149, 80). A reason for the asynchronous secondaries being on wider orbits than synchronous ones may be longer tidal circularization time scales at larger semi-major axes. The asynchronous secondaries show relatively fast spins; their rotation periods are typically 10 h. An intriguing observation is a paucity of chaotic secondary rotations; with an exception of (35107) 1991 VH, the secondary rotations are single-periodic with no signs of chaotic rotation and their periods are constant on timescales from weeks to years. The secondary equatorial elongations show an upper limit of a 2 / b 2 ∼ 1.5 . The lack of synchronous secondaries with greater elongations appears consistent, considering uncertainties of the axis ratio estimates, with the theory by Cuk and Nesvorný that predicts large regions of chaotic rotation in the phase space for a 2 / b 2 ≳ 2 . Alternatively, secondaries may not form or stay very elongated in gravitational (tidal) field of the primary. It could be due to the secondary fission mechanism suggested by Jacobson and Scheeres (Jacobson, S.A., Scheeres, D.J. [2011]. Icarus 214, 161–178), as its efficiency is correlated with the secondary elongation. Sharma (Sharma, I. [2014]. Icarus 229, 278–294) found that rubble-pile satellites with a 2 / b 2 ≲ 1.5 are more stable to finite structural perturbations than more elongated ones. It appears that more elongated secondaries, if they originally formed in spin fission of parent asteroid, are less likely to survive intact and they more frequently fail or fission.
Published: 2016

13. Auswirkungen des Tabakrauchens aus gesundheits- und volkswirtschaftlicher Sicht

Author: S. Hellmich, L. Marek, and W. Marek
Subjects: Pulmonary and Respiratory Medicine, business.industry, Medicine, business
Published: 2009

14. Ground-based transit observations of the HAT-P-18, HAT-P-19, HAT-P-27/WASP40 and WASP-21 systems

Author: F. J. Aceituno, Diana P. Kjurkchieva, Martin Vaňko, T. O. B. Schmidt, A. Özdönmez, S. Buder, M. Haas, J. K. Guo, Ch. Adam, K. Werner, E. Güzel, Tansel Ak, A. Pannicke, M. Hackstein, Laurence A. Marschall, J. G. Schmidt, Rolf Chini, Markus Mugrauer, M. Kitze, C. Marka, Tolga Guver, Theodor Pribulla, A. Dathe, Wen Ping Chen, J. Budaj, V. Wolf, Xin Zhou, David H. Cohen, Eric L. N. Jensen, Ronny Errmann, S. Hellmich, M. Seeliger, Ralph Neuhäuser, Ersin Gogus, S. Richter, Ch. Ginski, D. Puchalski, A. Ide, Berk Aydin, J. M. Ohlert, Dinko Dimitrov, J. Greif, Raetz, Emil Kundra, Zhenyu Wu, M. Fernandez, Stefano Mottola, Matthias Mallonn, B. Dincel, and Ege Üniversitesi
Subjects: Orbital elements, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Planets and satellites: individual: WASP-21b, Planets and satellites: individual: HAT-P-27b/WASP-40b, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, HAT-P-18b HAT-P-19b HAT-P-27b/WASP-40b WASP-21b, Exoplanet, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, System parameters, Planets and satellites: individual: HAT-P-19b, Planets and satellites: individual: HAT-P-18b, Transit (astronomy), Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: As part of our ongoing effort to investigate transit timing variations (TTVs) of known exoplanets, we monitored transits of the four exoplanets HAT-P-18b, HAT-P-19b, HAT-P-27b/WASP-40b and WASP-21b. All of them are suspected to show TTVs due to the known properties of their host systems based on the respective discovery papers. During the past three years 46 transit observations were carried out, mostly using telescopes of the Young Exoplanet Transit Initiative. The analyses are used to refine the systems' orbital parameters. In all cases we found no hints for significant TTVs, or changes in the system parameters inclination, fractional stellar radius and planet-to-star radius ratio. However, comparing our results with those available in the literature shows that we can confirm the already published values. © 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Published: 2015

15. Proneurotensin 1–117, a stable neurotensin precursor fragment identified in human circulation

Author: S. Hellmich, A. Ernst, and A. Bergmann
Subjects: Physiology, Molecular Sequence Data, Prohormone, Neuropeptide, Peptide, Biochemistry, Chromatography, Affinity, Mass Spectrometry, Epitopes, Cellular and Molecular Neuroscience, chemistry.chemical_compound, Endocrinology, Affinity chromatography, medicine, Humans, Amino Acid Sequence, Intestinal Mucosa, Protein Precursors, Neurotensin, Immunoassay, chemistry.chemical_classification, Temperature, Biological activity, In vitro, Protein Structure, Tertiary, chemistry, Calibration, Neuromedin N, Peptides, medicine.drug
Abstract: Proneurotensin/neuromedin N (pro NT/NMN) is the common precursor of two biologically active peptides, neurotensin (NT) and neuromedin N (NMN). We have established antibodies against peptide sequences of the NT/NMN precursor and developed a sandwich immunoassay for the detection of pro NT/NMN immunoreactivity in human circulation. Endogenous pro NT/NMN immunoreactivity was enriched by affinity chromatography using antibodies against two different pro NT/NMN epitopes, and further purified by reversed phase HPLC. Mass spectrometry analysis revealed pro NT/NMN 1–117 as major pro NT/NMN immunoreactivity in human circulation. Pro NT/NMN 1–117 is detectable in serum from healthy individuals (n = 124; median 338.9 pmol/L). As known for NT, the release of pro NT/NMN 1–117 from the intestine into the circulation is stimulated by ingestion of an ordinary meal. Investigation of the pro NT/NMN 1–117 in vitro stability in human serum and plasma revealed that this molecule is stable for at least 48 h at room temperature. Since pro NT/NMN 1–117 is theoretically produced during precursor processing in stoichiometric amounts relative to NT and NMN, it could be a surrogate marker for the release of these bioactive peptides.
Published: 2006

16. The small binary asteroid (939) Isberga

Author: F. Richard, P. Scheirich, François Colas, E. Morelle, Lawrence A. Molnar, Emmanuel Jehin, M. Bonnardeau, A. Marciniak, M. Birlan, Richard P. Binzel, S. Fauvaud, Stefano Mottola, P. Farissier, M. Fauvaud, A. Leroy, Francesca E. DeMeo, R. Hirsch, C. Gillier, Jean Manfroid, F. Vachier, Marco Delbo, A. Carbognani, Michaël Gillon, Raoul Behrend, Benoit Carry, S. Hellmich, J. Strajnic, K. Sobkowiak, E. Barbotin, A. Matter, Petr Pravec, J. Montier, European Space Astronomy Centre (ESAC), 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, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), 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), Max-Planck-Institut für Radioastronomie (MPIFR), Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), Department of Physics and Astronomy [Grand Rapids), Calvin College Burton, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVDA), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, UNS-CNRS-Observatoire de la Côte d'Azur, Association des Utilisateurs de Détecteurs Electroniques, CdR & CdL group, Geneva Observatory, University of Geneva [Switzerland], Club d'Astronomie Lyon Ampéré [Vaulx-en-Velin] (CALA), Observatoire Midi-Pyrénées and Association T60, Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées, Observatoire du Bois de Bardon, 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-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), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Smithsonian Institution-Harvard University [Cambridge], Association T60, Observatoire Midi-Pyrénées, 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), Agence Spatiale Européenne = European Space Agency (ESA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), 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), Harvard University-Smithsonian Institution, Université de Genève = University of Geneva (UNIGE), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Binzel, Richard P, and DeMeo, Francesca E
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Ecliptic, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, dynamics, Albedo, Satellites of asteroids, Asteroids, Orbit determination, Space and Planetary Science, Asteroid, Planet, Orbit (dynamics), Satellite, Astrophysics - Earth and Planetary Astrophysics, Ordinary chondrite
Abstract: In understanding the composition and internal structure of asteroids, their density is perhaps the most diagnostic quantity. We aim here at characterizing the surface composition, mutual orbit, size, mass, and density of the small main-belt binary asteroid (939) Isberga. For that, we conduct a suite of multi-technique observations, including optical lightcurves over many epochs, near-infrared spectroscopy, and interferometry in the thermal infrared. We develop a simple geometric model of binary systems to analyze the interferometric data in combination with the results of the lightcurve modeling. From spectroscopy, we classify Ibserga as a Sq-type asteroid, consistent with the albedo of View the MathML source0.14[subscript -0.06][superscript +0.09] (all uncertainties are reported as 3-σ range) we determine (average albedo of S-types is 0.197 ± 0.153, see Pravec et al. (Pravec et al. [2012]. Icarus 221, 365–387). Lightcurve analysis reveals that the mutual orbit has a period of 26.6304 ± 0.0001 h, is close to circular (eccentricity lower than 0.1), and has pole coordinates within 7° of (225°, +86°) in Ecliptic J2000, implying a low obliquity of View the MathML source1.5[subscript -1.5][superscript +6.0]deg. The combined analysis of lightcurves and interferometric data allows us to determine the dimension of the system and we find volume-equivalent diameters of 12.4[subscript -1.2][superscript +2.5]km and 3.6[subscript -0.3][superscript +0.7]km for Isberga and its satellite, circling each other on a 33 km wide orbit. Their density is assumed equal and found to be 2.91[subscript -2.01][superscript +1].72gcm[superscript -3], lower than that of the associated ordinary chondrite meteorites, suggesting the presence of some macroporosity, but typical of S-types of the same size range (Carry [2012]. Planet. Space Sci. 73, 98–118). The present study is the first direct measurement of the size of a small main-belt binary. Although the interferometric observations of Isberga are at the edge of MIDI capabilities, the method described here is applicable to others suites of instruments (e.g., LBT, ALMA)., United States. National Aeronautics and Space Administration (09-NEOO009–0001)), National Science Foundation (U.S.) (0506716), National Science Foundation (U.S.) (0907766)
Published: 2014

17. The binary near-Earth asteroid (175706) 1996 FG3 - An observational constraint on its orbital evolution

Author: P. Scheirich, David Polishook, Josef Ďurech, James W. Brinsfield, Seth A. Jacobson, Kamil Hornoch, Donald P. Pray, V. R. Ayvazian, Adrian Galad, Igor Molotov, Yu. N. Krugly, Michaël Gillon, I. Slyusarev, Petr Pravec, Joe Pollock, Michael Mommert, R. Ya. Inasaridze, J. Pittichová, Javier Licandro, Emmanuel Jehin, S. Hellmich, Jean Manfroid, V. Alí-Lagoa, Stefano Mottola, O. Kvaratskhelia, and Peter Kusnirak
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, Near-Earth object, Population, Ecliptic, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, dynamics, Astrophysics, Mean anomaly, Near-Earth objects, Orbital period, Asteroids, Photometry, Orbital pole, Space and Planetary Science, Asteroid, Tidal force, education, Astrophysics - Earth and Planetary Astrophysics
Abstract: Using our photometric observations taken between 1996 and 2013 and other published data, we derived properties of the binary near-Earth asteroid (175706) 1996 FG3 including new measurements constraining evolution of the mutual orbit with potential consequences for the entire binary asteroid population. We also refined previously determined values of parameters of both components, making 1996 FG3 one of the most well understood binary asteroid systems. We determined the orbital vector with a substantially greater accuracy than before and we also placed constraints on a stability of the orbit. Specifically, the ecliptic longitude and latitude of the orbital pole are 266{\deg} and -83{\deg}, respectively, with the mean radius of the uncertainty area of 4{\deg}, and the orbital period is 16.1508 +/- 0.0002 h (all quoted uncertainties correspond to 3sigma). We looked for a quadratic drift of the mean anomaly of the satellite and obtained a value of 0.04 +/- 0.20 deg/yr^2, i.e., consistent with zero. The drift is substantially lower than predicted by the pure binary YORP (BYORP) theory of McMahon and Scheeres (McMahon, J., Scheeres, D. [2010]. Icarus 209, 494-509) and it is consistent with the theory of an equilibrium between BYORP and tidal torques for synchronous binary asteroids as proposed by Jacobson and Scheeres (Jacobson, S.A., Scheeres, D. [2011]. ApJ Letters, 736, L19). Based on the assumption of equilibrium, we derived a ratio of the quality factor and tidal Love number of Q/k = 2.4 x 10^5 uncertain by a factor of five. We also derived a product of the rigidity and quality factor of mu Q = 1.3 x 10^7 Pa using the theory that assumes an elastic response of the asteroid material to the tidal forces. This very low value indicates that the primary of 1996 FG3 is a 'rubble pile', and it also calls for a re-thinking of the tidal energy dissipation in close asteroid binary systems., Comment: Many changes based on referees comments
Published: 2014

18. Rotational properties of the Maria asteroid family

Author: Stefano Mottola, Young-Jun Choi, Noah Brosch, Jang-Hyun Park, Yong-Ik Byun, Joh-Na Yoon, Zeki Eker, Tobias C. Hinse, S. Hellmich, O. Uysal, Eda Guzel, Raoul Behrend, Murat Kaplan, Suleyman Kaynar, Myung-Jin Kim, Hong-Kyu Moon, and Ege Üniversitesi
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, asteroids, Solar System, Synodic day, FOS: Physical sciences, Resonance, Astronomy and Astrophysics, Astrophysics, Rotation, Asteroid family, asteroids: general, Mean motion, Amplitude, Space and Planetary Science, Asteroid, minor planets, Astrophysics - Earth and Planetary Astrophysics
Abstract: Maria family is regarded as an old-type (~3 +/- 1 Gyr) asteroid family which has experienced substantial collisional and dynamical evolution in the Main-belt. It is located nearby the 3:1 Jupter mean motion resonance area that supplies Near-Earth asteroids (NEAs) to the inner Solar System. We carried out observations of Maria family asteroids during 134 nights from 2008 July to 2013 May, and derived synodic rotational periods for 51 objects, including newly obtained periods of 34 asteroids. We found that there is a significant excess of fast and slow rotators in observed rotation rate distribution. The two-sample Kolmogorov-Smirnov test confirms that the spin rate distribution is not consistent with a Maxwellian at a 92% confidence level. From correlations among rotational periods, amplitudes of lightcurves, and sizes, we conclude that the rotational properties of Maria family asteroids have been changed considerably by non-gravitational forces such as the YORP effect. Using a lightcurve inversion method (Kaasalainen & Torppa 2001; Kaasalainen et al. 2001), we successfully determined the pole orientations for 13 Maria members, and found an excess of prograde versus retrograde spins with a ratio (N_p/N_r) of 3. This implies that the retrograde rotators could have been ejected by the 3:1 resonance into the inner Solar System since the formation of Maria family. We estimate that approximately 37 to 75 Maria family asteroids larger than 1 km have entered the near-Earth space every 100 Myr., 83 pages, 8 figures, 63 figures in Appendix A. Accepted for publication in The Astronomical Journal
Published: 2014

19. Ambulantes Operieren im Fachgebiet der Hals-Nasen-Ohren Heilkunde, Kopf- und Hals-Chirurgie

Author: K. Seifert, John-Martin Hempel, K. Jahnke, S. Hellmich, and U. Koch
Subjects: Otorhinolaryngology
Published: 2000

20. Septumplastik

Author: S. Hellmich
Subjects: Otorhinolaryngology
Published: 1997

21. Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution

Author: J. Hanuš, J. Ďurech, M. Brož, A. Marciniak, B. D. Warner, F. Pilcher, R. Stephens, R. Behrend, B. Carry, D. Čapek, P. Antonini, M. Audejean, K. Augustesen, E. Barbotin, P. Baudouin, A. Bayol, L. Bernasconi, W. Borczyk, J.-G. Bosch, E. Brochard, L. Brunetto, S. Casulli, A. Cazenave, S. Charbonnel, B. Christophe, F. Colas, J. Coloma, M. Conjat, W. Cooney, H. Correira, V. Cotrez, A. Coupier, R. Crippa, M. Cristofanelli, Ch. Dalmas, C. Danavaro, C. Demeautis, T. Droege, R. Durkee, N. Esseiva, M. Esteban, M. Fagas, G. Farroni, M. Fauvaud, S. Fauvaud, F. Del Freo, L. Garcia, S. Geier, C. Godon, K. Grangeon, H. Hamanowa, N. Heck, S. Hellmich, D. Higgins, R. Hirsch, M. Husarik, T. Itkonen, O. Jade, K. Kamiński, P. Kankiewicz, A. Klotz, R. A. Koff, A. Kryszczyńska, T. Kwiatkowski, A. Laffont, A. Leroy, J. Lecacheux, Y. Leonie, C. Leyrat, F. Manzini, A. Martin, G. Masi, D. Matter, J. Michałowski, M. J. Michałowski, T. Michałowski, J. Michelet, R. Michelsen, E. Morelle, S. Mottola, R. Naves, J. Nomen, J. Oey, W. Ogłoza, A. Oksanen, D. Oszkiewicz, P. Pääkkönen, M. Paiella, H. Pallares, J. Paulo, M. Pavic, B. Payet, M. Polińska, D. Polishook, R. Poncy, Y. Revaz, C. Rinner, M. Rocca, A. Roche, D. Romeuf, R. Roy, H. Saguin, P. A. Salom, S. Sanchez, G. Santacana, T. Santana-Ros, J.-P. Sareyan, K. Sobkowiak, S. Sposetti, D. Starkey, R. Stoss, J. Strajnic, J.-P. Teng, B. Trégon, A. Vagnozzi, F. P. Velichko, N. Waelchli, K. Wagrez, H. Wücher, Astronomical Institute of Charles University, Charles University [Prague] (CU), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Palmer Divide Observatory, Organ Mesa Observatory, Goat Mountain Astronomical Research Station, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Observatoire de Bédoin, Observatoire de Chinon, Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), CdR & CdL group, Association T60, Observatoire Midi-Pyrénées, Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, Harfleur Observatory, Observatoire des Engarouines, Collonges Observatory, Chercheur indépendant, Observatoire N°139 d'Antibes, Osservatorio Colleverde di Guidonia, Observatoire de Saint-Sulpice N°947, DPHY, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatorio de San Gervasi, Observatoire de Cabris, Blackberry Observatory, Centre d'Astronomie de Saint-Michel l'Observatoire, Observatoire de Sainte-Hélène, Observatorio Astronómico de Tradate, 138 Village-Neuf, The Amateur Sky Survey (TASS), The Amateur Sky Survey, Shed of Science Observatory, Association AstroQueyras, Association des Utilisateurs de Détecteurs Electroniques (AUDE), Association des Utilisateurs de Détecteurs Electroniques, Observatoire du Bois de Bardon, Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Nordic Optical Telescope (NOT), Instituto de Astrofisica de Canarias (IAC), Hamanowa Astronomical Observatory, DLR Institute of Planetary Research, German Aerospace Center (DLR), Hunters Hill Observatory, Skalnaté Pleso Observatory, A83 Jakokoski Observatory, Institute of Physics [Kielce], Jan Kochanowski University, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Antelope Hills Observatory, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Stazione Astronomica di Sozzago, Forte Software, Scottish Universities Physics Alliance, Institute for Astronomy (SUPA), University of Edinburgh, Club d'Astronomie Lyon Ampéré [Vaulx-en-Velin] (CALA), Nyrölä Observatory (NYTT), Observatorio Montcabre, Observatorio Astronómico de Mallorca (OAM), Observatorio Astronómico de Mallorca, Kingsgrove Observatory, Mt. Suhora Observatory, Pedagogical University, Astronomy Department, Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), François-Xavier Bagnoud Observatory, Blauvac Obsevatory, Blauvac Observatory, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Gnosca Observatory, DeKalb Observatory, Observatoire astronomique des Makes, Laboratoire Kastler Brossel (LKB (Lhomond)), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institute of Astronomy [Kharkiv], V.N. Karazin Kharkiv National University (KhNU), University of Geneva [Switzerland], European Space Agency (ESA), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Helsinki-University of Helsinki, Université Pierre et Marie Curie - Paris 6 (UPMC)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, photometry, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], media_common.quotation_subject, Population, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Inverse transform sampling, Astrophysics, 01 natural sciences, Photometry (optics), models, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Physical model, Minor planets, Astronomy and Astrophysics, Asteroids: general, 13. Climate action, Space and Planetary Science, Sky, Asteroid, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The larger number of models of asteroid shapes and their rotational states derived by the lightcurve inversion give us better insight into both the nature of individual objects and the whole asteroid population. With a larger statistical sample we can study the physical properties of asteroid populations, such as main-belt asteroids or individual asteroid families, in more detail. Shape models can also be used in combination with other types of observational data (IR, adaptive optics images, stellar occultations), e.g., to determine sizes and thermal properties. We use all available photometric data of asteroids to derive their physical models by the lightcurve inversion method and compare the observed pole latitude distributions of all asteroids with known convex shape models with the simulated pole latitude distributions. We used classical dense photometric lightcurves from several sources and sparse-in-time photometry from the U.S. Naval Observatory in Flagstaff, Catalina Sky Survey, and La Palma surveys (IAU codes 689, 703, 950) in the lightcurve inversion method to determine asteroid convex models and their rotational states. We also extended a simple dynamical model for the spin evolution of asteroids used in our previous paper. We present 119 new asteroid models derived from combined dense and sparse-in-time photometry. We discuss the reliability of asteroid shape models derived only from Catalina Sky Survey data (IAU code 703) and present 20 such models. By using different values for a scaling parameter cYORP (corresponds to the magnitude of the YORP momentum) in the dynamical model for the spin evolution and by comparing synthetics and observed pole-latitude distributions, we were able to constrain the typical values of the cYORP parameter as between 0.05 and 0.6., Accepted for publication in A&A, January 15, 2013
Published: 2013

22. New and updated convex shape models of asteroids based on optical data from a large collaboration network

Author: J. Hanuš, J. Ďurech, D. A. Oszkiewicz, R. Behrend, B. Carry, M. Delbo, O. Adam, V. Afonina, R. Anquetin, P. Antonini, L. Arnold, M. Audejean, P. Aurard, M. Bachschmidt, B. Baduel, E. Barbotin, P. Barroy, P. Baudouin, L. Berard, N. Berger, L. Bernasconi, J-G. Bosch, S. Bouley, I. Bozhinova, J. Brinsfield, L. Brunetto, G. Canaud, J. Caron, F. Carrier, G. Casalnuovo, S. Casulli, M. Cerda, L. Chalamet, S. Charbonnel, B. Chinaglia, A. Cikota, F. Colas, J.-F. Coliac, A. Collet, J. Coloma, M. Conjat, E. Conseil, R. Costa, R. Crippa, M. Cristofanelli, Y. Damerdji, A. Debackère, A. Decock, Q. Déhais, T. Déléage, S. Delmelle, C. Demeautis, M. Dróżdż, G. Dubos, T. Dulcamara, M. Dumont, R. Durkee, R. Dymock, A. Escalante del Valle, N. Esseiva, R. Esseiva, M. Esteban, T. Fauchez, M. Fauerbach, M. Fauvaud, S. Fauvaud, E. Forné, C. Fournel, D. Fradet, J. Garlitz, O. Gerteis, C. Gillier, M. Gillon, R. Giraud, J.-P. Godard, R. Goncalves, Hiroko Hamanowa, Hiromi Hamanowa, K. Hay, S. Hellmich, S. Heterier, D. Higgins, R. Hirsch, G. Hodosan, M. Hren, A. Hygate, N. Innocent, H. Jacquinot, S. Jawahar, E. Jehin, L. Jerosimic, A. Klotz, W. Koff, P. Korlevic, E. Kosturkiewicz, P. Krafft, Y. Krugly, F. Kugel, O. Labrevoir, J. Lecacheux, M. Lehký, A. Leroy, B. Lesquerbault, M. J. Lopez-Gonzales, M. Lutz, B. Mallecot, J. Manfroid, F. Manzini, A. Marciniak, A. Martin, B. Modave, R. Montaigut, J. Montier, E. Morelle, B. Morton, S. Mottola, R. Naves, J. Nomen, J. Oey, W. Ogłoza, M. Paiella, H. Pallares, A. Peyrot, F. Pilcher, J.-F. Pirenne, P. Piron, M. Polińska, M. Polotto, R. Poncy, J. P. Previt, F. Reignier, D. Renauld, D. Ricci, F. Richard, C. Rinner, V. Risoldi, D. Robilliard, D. Romeuf, G. Rousseau, R. Roy, J. Ruthroff, P. A. Salom, L. Salvador, S. Sanchez, T. Santana-Ros, A. Scholz, G. Séné, B. Skiff, K. Sobkowiak, P. Sogorb, F. Soldán, A. Spiridakis, E. Splanska, S. Sposetti, D. Starkey, R. Stephens, A. Stiepen, R. Stoss, J. Strajnic, J.-P. Teng, G. Tumolo, A. Vagnozzi, B. Vanoutryve, J. M. Vugnon, B. D. Warner, M. Waucomont, O. Wertz, M. Winiarski, M. Wolf, Charles University [Prague] (CU), Astronomical Institute of Charles University, Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Bédoin, Observatoire de Chinon, Association des Utilisateurs de Détecteurs Electroniques, Laboratoire de Physique de la Matière Condensée - UR UPJV 2081 (LPMC), Université de Picardie Jules Verne (UPJV), Harfleur Observatory, Ressources des terroirs - UMR 8575, Centre National de la Recherche Scientifique (CNRS), Les Engarouines Observatory, Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Chercheur indépendant, Laboratoire d'optique des solides (LOS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Centre de Recherche Saint-Antoine (UMRS893), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM), Association T60, Observatoire Midi-Pyrénées, Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), CdR & CdL group, Physik-Institut, Universität Zürich [Zürich] = University of Zurich (UZH), Gestion environnementale et traitement biologique des déchets (UR GERE), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Observatorio de San Gervasi, Observatoire de Cabris, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronómico de Tradate, Observatoire N°139 d'Antibes, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), 138 Village-Neuf, Science et Ingénierie des Matériaux et Procédés (SIMaP ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Shed of Science Observatory, Association AstroQueyras, Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatoire du Bois de Bardon, Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Ciências Exatas e Tecnológicas [Viçosa], Universidade Federal de Viçosa = Federal University of Viçosa (UFV), Hamanowa Astronomical Observatory, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), European Southern Observatory (ESO), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Observatoire Chante-Perdrix, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Stazione Astronomica di Sozzago, Milieux aquatiques, écologie et pollutions (UR MALY), German Aerospace Center (DLR), Observatorio Montcabre, Observatorio Astronómico de Mallorca (OAM), Observatorio Astronómico de Mallorca, Kingsgrove Observatory, Gestion Territoriale de l'Eau et de l'environnement (UMR GESTE), École Nationale du Génie de l'Eau et de l'Environnement de Strasbourg (ENGEES)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Organ Mesa Observatory, Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Association des Utilisateurs de Détecteurs Electroniques (AUDE), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon, Laboratoire de Recherche sur la Réactivité des Solides (LRRS), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'intégration, du matériau au système (IMS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Gnosca Observatory, DeKalb Observatory, Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Observatoire astronomique des Makes, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Institute of Neuropathology, University hospital of Zurich [Zurich], Charles University [Prague], University of Helsinki-University of Helsinki, University of Geneva [Switzerland], European Space Agency (ESA), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches Subatomiques (IReS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Cancéropôle du Grand Est-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de la Matière Condensée (EA 2081), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Université de Genève (UNIGE), Centre de Recherche Saint-Antoine (CR Saint-Antoine), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées, Universität Zürich [Zürich] (UZH), L2EP - Équipe Réseaux, Laboratoire d’Électrotechnique et d’Électronique de Puissance - EA 2697 (L2EP), Ecole Centrale de Lille-École Nationale Supérieure d'Arts et Métiers (ENSAM), Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Haute Etude d'Ingénieurs-Université de Lille-Ecole Centrale de Lille-École Nationale Supérieure d'Arts et Métiers (ENSAM), HESAM Université (HESAM)-HESAM Université (HESAM)-Haute Etude d'Ingénieurs-Université de Lille, Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Observatoire Midi-Pyrénées and Association T60, Laboratoire de photonique et de nanostructures (LPN), Universidade Federal de Vicosa (UFV), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre d'études de chimie métallurgique (CECM), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Laboratoire d’Électrotechnique et d’Électronique de Puissance - ULR 2697 (L2EP), Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), National Science Centre (Poland), Czech Science Foundation, Centre National D'Etudes Spatiales (France), Charles University [Prague] [CU], European Space Astronomy Centre [ESAC], Joseph Louis LAGRANGE [LAGRANGE], Institut de Recherches Subatomiques [IReS], Laboratoire d'Annecy de Physique des Particules [LAPP], Géosciences Paris Sud [GEOPS], Laboratoire d'optique des solides [LOS], Observatoire Astronomique de l'Université de Genève [ObsGE], Gestion environnementale et traitement biologique des déchets [UR GERE], Observatoire astronomique de Strasbourg [ObAS], Science et Ingénierie des Matériaux et Procédés [SIMaP], Laboratoire d’Optique Atmosphérique - UMR 8518 [LOA], Interactions et dynamique des environnements de surface [IDES], Laboratoire de photonique et de nanostructures [LPN], European Southern Observatory [ESO], Institut de recherche en astrophysique et planétologie [IRAP], Laboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA], Milieux aquatiques, écologie et pollutions [UR MALY], German Aerospace Center [DLR], Laboratoire de l'Accélérateur Linéaire [LAL], Université Claude Bernard Lyon 1 [UCBL], Laboratoire de Recherche sur la Réactivité des Solides [LRRS], Laboratoire de l'intégration, du matériau au système [IMS], Laboratoire de Physique Atmosphérique et Planétaire [LPAP], INAF - Osservatorio Astronomico di Padova [OAPD], Argelander Institute for Astronomy [AlfA], ITA, USA, GBR, FRA, DEU, and ESP
Subjects: Solar System, 010504 meteorology & atmospheric sciences, Computer science, media_common.quotation_subject, FOS: Physical sciences, Inverse transform sampling, 01 natural sciences, Gravitation, Photometry (optics), Methods: observational, 0103 physical sciences, QB Astronomy, observational [Methods], Shape optimization, asteroids: general / techniques: photometric / methods: observational / methods: numerical, 010303 astronomy & astrophysics, Scaling, QC, ComputingMilieux_MISCELLANEOUS, QB, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], numerical [Methods], Methods: numerical, photometric [Techniques], Minor planets, Astronomy, Astronomy and Astrophysics, 3rd-DAS, QC Physics, Minor planets, asteroids: general, Space and Planetary Science, Sky, Asteroid, Physics::Space Physics, minor planets, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [Asteroids], Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics, general [minor planets, asteroids]
Abstract: Context. Asteroid modeling efforts in the last decade resulted in a comprehensive dataset of almost 400 convex shape models and their rotation states. These efforts already provided deep insight into physical properties of main-belt asteroids or large collisional families. Going into finer detail (e.g., smaller collisional families, asteroids with sizes 20 km) requires knowledge of physical parameters of more objects. Aims. We aim to increase the number of asteroid shape models and rotation states. Such results provide important input for further studies, such as analysis of asteroid physical properties in different populations, including smaller collisional families, thermophysical modeling, and scaling shape models by disk-resolved images, or stellar occultation data. This provides bulk density estimates in combination with known masses, but also constrains theoretical collisional and evolutional models of the solar system. Methods. We use all available disk-integrated optical data (i.e., classical dense-in-time photometry obtained from public databases and through a large collaboration network as well as sparse-in-time individual measurements from a few sky surveys) as input for the convex inversion method, and derive 3D shape models of asteroids together with their rotation periods and orientations of rotation axes. The key ingredient is the support of more that 100 observers who submit their optical data to publicly available databases. Results. We present updated shape models for 36 asteroids, for which mass estimates are currently available in the literature, or for which masses will most likely be determined from their gravitational influence on smaller bodies whose orbital deflections will be observed by the ESA Gaia astrometric mission. Moreover, we also present new shape model determinations for 250 asteroids, including 13 Hungarias and three near-Earth asteroids. The shape model revisions and determinations were enabled by using additional optical data from recent apparitions for shape optimization. © 2016 ESO., J.H. greatly appreciates the CNES post-doctoral fellowship program. J.H. and M.D. were supported by the project under the contract 11-BS56-008 (SHOCKS) of the French Agence National de la Recherche (ANR), JD by grant GACR 15-04816S of the Czech Science Foundation, DO by the grant NCN 2012/S/ST9/00022 of Polish National Science Center, and A. Marciniak by grant 2014/13/D/ST9/01818 of Polish National Science Center.
Published: 2016

23. Stellar occultation by (119951) 2002 KX14on April 26, 2012

Author: Rene Duffard, S. Hellmich, A. Alvarez-Candal, J. L. Ortiz, Nora Morales, Stefano Mottola, S. P. Littlefair, T. R. Marsh, V. S. Dhillon, Bruno Sicardy, Yolanda Jiménez-Teja, T. Shahbaz, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), Department of Physics and Astronomy [Sheffield], University of Sheffield [Sheffield], DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), DLR Institute of Planetary Research, and German Aerospace Center (DLR)
Subjects: 010504 meteorology & atmospheric sciences, Context (language use), Astrophysics, 01 natural sciences, Occultation, law.invention, Atmosphere, Telescope, law, 0103 physical sciences, William Herschel Telescope, 010303 astronomy & astrophysics, methods: analytical – techniques: photometric – occultations – Kuiper belt objects: individual: (119951) 2002 KX14 –methods: observational, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [PHYS]Physics [physics], Physics, Observational techniques, Astronomy, Astronomy and Astrophysics, Astrometry, Albedo, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Context. Trans-Neptunian objects (TNOs) are important bodies, but very little is known about their basic physical properties such as size, density, and albedo. Aims. We intend to determine sizes, albedos, and even densities of a good sample of TNOs, especially those of the largest TNOs because they can be studied the best with different observational techniques. Methods. We took advantage of a stellar occultation by (119951) 2002 KX14 to obtain valuable information by means of high temporal resolution CCD imaging using ULTRACAM at the 4.2 m William Herschel Telescope on La Palma (Spain). Results. Thanks to the high time resolution of ULTRACAM and the large aperture provided by the telescope, we recorded the most accurate chord ever obtained for an occultation by a TNO, with a length of 415 ± 1 km. This is a lower limit to the diameter of (119951) 2002 KX14 assuming that it has a spherical shape. For ellipsoidal objects we developed a method for obtaining equivalent diameters by combining single-chord occultations and accurate astrometry at the time of occultation. By applying this method to (119951) 2002 KX14, we estimate an equal-area equivalent diameter of at least 365 +30 −21 km. A possible upper limit is 455 ± 27 km, obtained via thermal data. No atmosphere is detected. We obtain a surface temperature higher than 40 K, which precludes the existence of ices, other than water ice, upon the surface, which is consistent with the featureless spectrum of (119951) 2002 KX14 .T here are no secondary occultation events that could reveal whether there is a ring system, as recently found for the Centaur (10199) Chariklo.
Published: 2014

24. [Ambulatory surgery in the otorhinolaryngology, head and neck surgery specialty--combined scientific medical position of the German Society of Otorhinolaryngology, Head and Neck Surgery e.V., the German Professional Society of Otorhinolaryngologists e.V. and the Working Group of ENT Directors]

Author: U, Koch, J, Hempel, K, Jahnke, K, Seifert, and S, Hellmich
Subjects: Otolaryngology, Ambulatory Surgical Procedures, Germany, Humans, Societies, Medical
Published: 2001

25. [Septoplasty]

Author: S, Hellmich
Subjects: Adult, Humans, Rhinoplasty, Nasal Septum
Published: 1998

26. CONSTRAINTS ON A SECOND PLANET IN THE WASP-3 SYSTEM

Author: Matthew J. Holman, M. Raetz, Ronny Errmann, U. Kramm, G. Saral, Ch. Adam, Grzegorz Nowak, T. Pribulla, Andrzej Niedzielski, H. Gilbert, A. Wolszczan, M. Górecka, Dinko Dimitrov, M. Seeliger, F. J. Aceituno, B. Deka, V. Popov, J. M. Ohlert, S. Hellmich, Eric L. N. Jensen, Stefano Mottola, Monika Adamów, Markus Mugrauer, L. McKnight, D. W. Latham, R. Neuhaeuser, Ch. Ginski, G. A. Esquerdo, St. Raetz, Gracjan Maciejewski, J. N. Winn, T. O. B. Schmidt, M. Fernandez, Massachusetts Institute of Technology. Department of Physics, Winn, Joshua Nathan, and McKnight, Laura A.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Transit time, Star (graph theory), Orbital period, Light curve, Radial velocity, Orbit, Space and Planetary Science, Planet, planetary systems – planets and satellites: individual (WASP-3b) – stars: individual (WASP-3), Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy), Astrophysics - Earth and Planetary Astrophysics
Abstract: There have been previous hints that the transiting planet WASP-3b is accompanied by a second planet in a nearby orbit, based on small deviations from strict periodicity of the observed transits. Here we present 17 precise radial velocity (RV) measurements and 32 transit light curves that were acquired between 2009 and 2011. These data were used to refine the parameters of the host star and transiting planet. This has resulted in reduced uncertainties for the radii and masses of the star and planet. The RV data and the transit times show no evidence for an additional planet in the system. Therefore, we have determined the upper limit on the mass of any hypothetical second planet, as a function of its orbital period., United States. National Aeronautics and Space Administration (Origins program), Massachusetts Institute of Technology. Undergraduate Research Opportunities Program
Published: 2013

27. [The burn-out syndrome in nursing. An empirical study in a sociopsychological context]

Author: S, Hellmich and A, Reincke
Subjects: Age Factors, Humans, Nursing Staff, Social Environment, Burnout, Professional
Published: 1994

28. Hauptvortrag 8

Author: B. Lüderitz, S. Hellmich, J. Theissing, U. Ganzer, J. Helms, W. G. Hosemann, H. W. Mollenhauer, K. Ottmann, K. Seifert, and A. Wienke
Published: 1993

29. Book Reviews · Recensions · Buchbesprechungen

Author: Brandon Bentz, K. Seifert, T. Petzold, Chr. Dörr, Arthur G. Kristiansen, Michael J. McKenna, Corinna Nölle, K. Jahnke, U. Koch, Saumil N. Merchant, Bulent Mamikoglu, John-Martin Hempel, Gert Hofmann, Anke Tropitzsch, E. Klemm, J. Krüger, R. Hubert Laeng, Karl-Bernd Hüttenbrink, Uwe Vogel, J.D. Binnington, Thomas Zahnert, W.C. Lee, Richard J. Wiet, S. Koscielny, Michael Wunder, E.G. Thomaser, C. Mross, Arne Ernst, B. Bräuer, S. Hellmich, and Ijaz Ahmad
Subjects: Otorhinolaryngology
Published: 2000

30. Announcement · Annonce · Ankündigung

Author: W.C. Lee, Ijaz Ahmad, U. Koch, S. Koscielny, E.G. Thomaser, C. Mross, Karl-Bernd Hüttenbrink, Arne Ernst, K. Jahnke, John-Martin Hempel, Thomas Zahnert, J. Krüger, B. Bräuer, E. Klemm, Saumil N. Merchant, K. Seifert, S. Hellmich, Corinna Nölle, Anke Tropitzsch, Michael J. McKenna, J.D. Binnington, Arthur G. Kristiansen, R. Hubert Laeng, Richard J. Wiet, Michael Wunder, Brandon Bentz, T. Petzold, Chr. Dörr, Gert Hofmann, Bulent Mamikoglu, and Uwe Vogel
Subjects: Otorhinolaryngology
Published: 2000

31. Materialbedingte Gefahren der korrektiven Rhinoplastik

Author: S. Hellmich
Subjects: medicine.medical_specialty, Otorhinolaryngology, business.industry, Implant material, Head and neck surgery, medicine, Dentistry, General Medicine, Neurosurgery, Implant, business
Abstract: The fate of any implant depends decisively on the interaction between the implant bed and the implant material.
Published: 1979

32. Der Zwischenkieferknochen und Goethes Mephistopheles*

Author: J. Hellmich and S. Hellmich
Subjects: Otorhinolaryngology, media_common.quotation_subject, Art, media_common
Published: 1982

33. Elfenbein als Nasenimplantat bei Jacques Joseph

Author: O. Staindl, Alexander Berghaus, and S. Hellmich
Subjects: medicine.anatomical_structure, Otorhinolaryngology, business.industry, Implant material, Follow up studies, medicine, Dentistry, Implant, business, Biocompatible material, Late results, Nose
Abstract: A report is represented on late results of saddle-nose corrections in three patients who, more than 40 years ago, underwent surgery performed by Jacques Joseph in Berlin using an ivory chip. One patient showed a very good permanent result, while the two others had implant loss, which, in one case, was due to trauma. The case reports offer an opportunity to recall a few biographical data on Jacques Joseph and on his use of ivory as an implant material.
Published: 1989

34. Technische Verbesserungen der Kieferhöhlen-Endoskopie

Author: C. Herberhold and S. Hellmich
Subjects: medicine.medical_specialty, Otorhinolaryngology, Maxillary sinus endoscopy, business.industry, General surgery, medicine, Head and neck surgery, General Medicine, Neurosurgery, business
Published: 1972

35. Strahlenkonservierung von Bankknorpel mit Kobalt-60

Author: S. Hellmich
Subjects: medicine.medical_specialty, Otorhinolaryngology, business.industry, medicine, Head and neck surgery, General Medicine, Neurosurgery, business, Surgery
Published: 1972

36. Rekonstruktion des knorpeligen Septums

Author: S. Hellmich
Subjects: Columella, medicine.medical_specialty, business.industry, General Medicine, Anatomy, medicine.disease, Resection, Surgery, Otorhinolaryngology, otorhinolaryngologic diseases, Head and neck surgery, medicine, Nasal dorsum, Neurosurgery, Abscess, business
Abstract: Destruction of the cartilaginous septum is most commonly caused by trauma, septal abscess and inadequate septal resection. The typical findings — both cosmetic and functional — are characterized by a sunk-in lower nasal dorsum, rounded nostrils, a hidden columella, and severe valve problems due to pulled down upper lateral cartilages, creating a ballooning phenomenon.
Published: 1982

37. Die Verwendung von Kunststoff bei Nasenplastiken*

Author: S. Hellmich
Subjects: Otorhinolaryngology, business.industry, Medicine, business
Published: 1983

38. [The congenital laryngeal cyst in the newborn. Survey of literatur and case description (author's transl)]

Author: K, Korz, W, Hasselkus, and S, Hellmich
Subjects: Laryngeal Diseases, Male, Laryngoscopy, Cysts, Infant, Newborn, Humans, Punctures, Tracheotomy
Published: 1974

39. [Operative treatment of paranasal sinus diseases in childhood]

Author: S, Hellmich
Subjects: Meningomyelocele, Ethmoid Sinus, Child, Preschool, Acute Disease, Chronic Disease, Paranasal Sinus Diseases, Respiratory Hypersensitivity, Humans, Maxillary Sinus, Sinusitis, Child, Anti-Bacterial Agents
Abstract: An exact knowledge of the developing anatomy and physiology, and very conservative operative technique are the prerequisites for surgical therapy of the nose and the paranasal sinuses in children. These requirements are fulfilled by uncapping of the ethmoidal cells in chronic and especially acute ethmoid sinusitis. Intranasal antrostomy allows diagnosis to be made and limited local treatment to be given in acute and chronic maxillary sinusitis. More radical surgical procedures are not indicated in children, except in those cases, where severe orbital or endocranial complications have already developed. Uncapping of the ethmoidal cells and/or intranasal antrostomy combined with the elimination of mechanical obstruction of the upper respiratory tract are necessary, when conservative treatment of acute or chronic sinusitis is unsuccessful. Continuation of conservative therapy is then no longer indicated. The uncapping of the ethmoidal cells under antibiotic cover usually leads to a complete disappearance of the symptoms within a few days, even when orbital or periorbital complications of an acute ethmoiditis have already set in. Even after unsuccessful long-term treatment of a chronic maxillary sinusitis, intranasal antrostomy is successful in 75-90 per cent of cases. Complications did not occur in a personal series of 1,349 intranasal antrostomies in children in a period of 5 years.
Published: 1984

40. [The intermaxillary bone and Goethe's Mephistopheles]

Author: S, Hellmich and P, Camper
Subjects: Otolaryngology, Medicine in Literature, Germany, Poetry as Topic, Maxilla, Humans, History, 19th Century, History, 18th Century
Abstract: The greatest anatomist of the second half of the 18th century was considered to be Petrus Camper from Holland. His theory - widespread as a dogma - stated that the anatomical difference between man and animal was the missing intermaxillary bone in man, this being the distinguishing feature between man and monkey. Against this theory Goethe set hs own reflections and observations, and on March 27th 1784 he found, by "reflection and coincidence", the intermaxillary bone in the human skull. In order to present his exciting discovery to the famous anatomist, he wanted to use as an intermediary his good friend Johann Heinrich Merck from Darmstadt who was in contact with Petrus Camper. But Merck delayed the requested forwarding of the manuscript, belittled Goethe and the significance of his treatise considerably in an accompanying letter, did not forward Camper's replies, and in the meantime even took advantage of Goethe's treatise for his own publications. It as only late that Goethe became aware of the scheming and mean behaviour of his "good friend", and he felt disappointed and betrayed by Merck. In Goethe's dramatic poem "Faust", Dr. Faust is confronted with the figure of Mephistopheles--the spirit who always plans evil and always denies. There is enough evidence to believe that the person of J. H. Merck can be recognized in this figure, and that Goethe's discovery of the human intermaxillary bone had its part in creating the figure of Mephistopheles as we know it today.
Published: 1982

41. [Ivory as a nose implant performed by Jacques Joseph. Late results after more than 40 years]

Author: O, Staindl, S, Hellmich, and A, Berghaus
Subjects: Aged, 80 and over, Male, Postoperative Complications, Foreign-Body Reaction, Humans, Nose Deformities, Acquired, Biocompatible Materials, Female, Middle Aged, Nose, Rhinoplasty, Aged, Follow-Up Studies
Abstract: A report is represented on late results of saddle-nose corrections in three patients who, more than 40 years ago, underwent surgery performed by Jacques Joseph in Berlin using an ivory chip. One patient showed a very good permanent result, while the two others had implant loss, which, in one case, was due to trauma. The case reports offer an opportunity to recall a few biographical data on Jacques Joseph and on his use of ivory as an implant material.
Published: 1989

42. Kontrollierte Blutdrucksenkung mit Natriumnitroprussid — ein Vergleich unter verschiedenen Anaesthesieverfahren

Author: A. Mangos, G. Georgiadis, S. Hellmich, D. Schemmann, and R. Purschke
Abstract: Kunstliche Blutdrucksenkung fuhrt uber eine geringere Blutungsneigung zu ubersichtlicheren Operationsbedingungen, geringeren Blutverlusten und kurzeren Operationszeiten, und findet vor allem bei mikrochirurgischen Eingriffen am Ohr und in der plastischen Chirurgie zunehmende Verbreitung. Als besonders gunstiges Pharmakon hat sich dabei das Natriumnitroprussid wegen seiner guten Steuerbarkeit erwiesen. Allerdings ist dabei die verhaltnismasig geringe therapeutische Breite, die Moglichkeit einer Tachyphylaxie sowie die Gefahr einer Thiocyanatvergiftung bei hoher Dosierung zu berucksichtigen.
Published: 1981

43. Jacques Josephs Elfenbeinspäne für die Sattelnasenkorrektur — Spätergebnisse nach über 40 Jahren

Author: O. Staindl, Alexander Berghaus, and S. Hellmich
Published: 1989

44. [The use of synthetic materials in rhinoplasty]

Author: S, Hellmich
Subjects: Humans, Prostheses and Implants, Rhinoplasty
Abstract: The ideal implant does not yet exist. Generally, the use of plastic implants in rhino-surgery is of limited indication only. The use of plastic implants in septum surgery is contraindicated. Hard, rigid, insufficiently elastic and perforated implants should not be used in the nasal dorsum. The implantation of mesh material has proved a failure. Only in limited cases of a severely damaged and scarred nasal dorsum the implantation of plastic sponge is indicated. Experience teaches the critical surgeon that occasionally there are defects, which (also due to lack of suitable implant material) cannot be improved with a justifiable prospect of success.
Published: 1983

45. Surgical treatment of sinusitis

Author: S, Hellmich
Subjects: Adult, Male, Ethmoid Sinus, Chronic Disease, Methods, Frontal Sinus, Humans, Female, Maxillary Sinus, Sinusitis, Child
Abstract: There is no doubt that there is a considerable number of cases of acute and chronic sinusitis, which can be cured only by surgical intervention. The modern philosophy should be: to choose a surgical technique as conservative as possible and as radical as necessary according to the individual case. To achieve this goal, an exact knowledge of the anatomy and pathology of the paranasal sinuses, as well as a full command of the available diagnostic methods (including sinuscopy) are essential. The sometimes dangerous complications of acute ethmoiditis in children usually can be solved by simple displacement of the middle turbinate to the center and uncapping of the ethmoidal cells assisted by antibiotic and antiphlogistic treatment. The surgical treatment of choice in cases of acute recurrent or chronic maxillary sinusitis in children (often combined with bronchial or allergic problems) is the installation of a nasoantral window from the inferior meatus, to guarantee adequate drainage. In adults, the radical techniques of Caldwell-Luc (maxillary sinus) and Riedel (frontan sinus) should be used in selected cases only. They should be replaced--if possible--by osteoplastic methods or modified techniques (frontal and maxillary sinus) or bimeatal-transnasal approach under endoscopic control (maxillary and ethmoidal sinus). Healthy and reversibly damaged mucosa should be saved; but at the cost of sacrificing the nasal function instead.
Published: 1983

46. [Treatment of the acute septal abscess (author's transl)]

Author: S, Hellmich
Subjects: Cartilage, Postoperative Complications, Acute Disease, Humans, Nose Deformities, Acquired, Surgery, Plastic, Child, Transplantation, Autologous, Abscess, Nasal Septum
Published: 1974

47. Unanimity and diversity in nasal surgery

Author: E, Huizing, W, Pirsig, R, Wentges, S, Hellmich, E, Kern, A, van Olphen, G, Rettinger, and J, de Groot
Subjects: Otolaryngology, Cartilage, Education, Medical, Terminology as Topic, Nose Diseases, Methods, Humans, History, 20th Century, Nose, Bandages, Netherlands
Published: 1989

48. Die Bedeutung unterschiedlicher Lager für Knorpelimplantate in klinischen und experimentellen Untersuchungen

Author: S. Hellmich
Published: 1980

49. [The influence of different preservation methods upon the biological quality of cartilage implants (author's transl)]

Author: S, Hellmich
Subjects: Graft Rejection, Back, Time Factors, Transplantation, Heterologous, Ribs, Radiation Effects, Cartilage, Freeze Drying, Freezing, Anti-Infective Agents, Local, Animals, Transplantation, Homologous, Rabbits, Tissue Preservation, Cobalt Radioisotopes
Published: 1974

50. [Experience with preserved cartilage in nasal reconstruction]

Author: H, Masing and S, Hellmich
Subjects: Adult, Male, Cartilage, Postoperative Complications, Methods, Humans, Nose Deformities, Acquired, Transplantation, Homologous, Female, Tissue Preservation, Nose, Surgery, Plastic, Nasal Septum
Published: 1968

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