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1. Asteroid phase curves using sparse Gaia DR2 data and differential dense light curves

Author: E Wilawer, D Oszkiewicz, A Kryszczyńska, A Marciniak, V Shevchenko, I Belskaya, T Kwiatkowski, P Kankiewicz, J Horbowicz, V Kudak, P Kulczak, V Perig, and K Sobkowiak
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract: The amount of sparse asteroid photometry being gathered by both space- and ground-based surveys is growing exponentially. This large volume of data poses a computational challenge owing to both the large amount of information to be processed and the new methods needed to combine data from different sources (e.g. obtained by different techniques, in different bands, and having different random and systematic errors). The main goal of this work is to develop an algorithm capable of merging sparse and dense data sets, both relative and differential, in preparation for asteroid observations originating from, for example, Gaia, TESS, ATLAS, LSST, K2, VISTA, and many other sources. We present a novel method to obtain asteroid phase curves by combining sparse photometry and differential ground-based photometry. In the traditional approach, the latter cannot be used for phase curves. Merging those two data types allows for the extraction of phase-curve information for a growing number of objects. Our method is validated for 26 sample asteroids observed by the Gaia mission., Comment: 10 pages, 7 figures (supplementary material: 20 pages, 58 figures)
Published: 2022

2. (704) Interamnia: a transitional object between a dwarf planet and a typical irregular-shaped minor body

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

Author: J. Strajnic, M. Pawłowski, Rene Duffard, Victor Ali-Lagoa, J.-G. Bosch, P. Pinel, Tamás Müller, Raoul Behrend, K. Wagrez, Dagmara Oszkiewicz, A. Pal, Brian A. Skiff, J. Krajewski, L. Brunetto, R. Szakats, T. Santana-Ros, F. Del Freo, E. Verebelyi, Paweł Kankiewicz, F. Richard, M. Evangelista-Santana, J. Michimani-Garcia, S. Fauvaud, T. Kundera, László Molnár, M. Butkiewicz Bąk, K. Sobkowiak, D. Lazzaro, Tom Polakis, J. Skrzypek, G. Farroni, S. Geier, Seitaro Urakawa, J. Golonka, R. Hirsch, P. Arcoverde, H. Medeiros, Eda Sonbas, Michał Żejmo, Doeon Kim, Frederick Pilcher, J. J. Sanabria, L. Bernasconi, Myung-Jin Kim, I. Konstanciak, Krzysztof Kamiński, M. Fauvaud, E. Pakštienė, V. Perig, E. Rondon, G. Stachowski, T. Rodrigues, Łukasz Tychoniec, Josef Ďurech, Cs. Kalup, V. Kecskeméthy, Zouhair Benkhaldoun, J. Grice, E. Podlewska-Gaca, F. Manzini, J. Horbowicz, Marin Ferrais, M. K. Kamińska, Jakub Nadolny, P. Julien, S. Brincat, Waldemar Ogloza, K. Żukowski, V. Kudak, A. Marciniak, Emmanuel Jehin, F. Monteiro, P. Kulczak, P. Trela, Nicolás Morales, Rupak Roy, Services communs OMP (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), National Science Centre (Poland), European Commission, Czech Science Foundation, National Research, Development and Innovation Office (Hungary), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), and Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal
Subjects: Rotation period, 010504 meteorology & atmospheric sciences, Infrared, FOS: Physical sciences, general [Minor planets, asteroids], Rotation, 7. Clean energy, 01 natural sciences, techniques: photometric, Física Aplicada, 0103 physical sciences, Thermal, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], photometric [Techniques], Astronomy and Astrophysics, Albedo, Light curve, asteroids: general, Computational physics, radiation mechanisms: thermal, Amplitude, 13. Climate action, Space and Planetary Science, Asteroid, Minor planets, asteroids: general, thermal [Radiation mechanisms], [SDU]Sciences of the Universe [physics], minor planets, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Full list of authors: Marciniak, A.; Ďurech, J.; Alí-Lagoa, V.; Ogłoza, W.; Szakáts, R.; Müller, T. G.; Molnár, L.; Pál, A.; Monteiro, F.; Arcoverde, P.; Behrend, R.; Benkhaldoun, Z.; Bernasconi, L.; Bosch, J.; Brincat, S.; Brunetto, L.; Butkiewicz-Bąk, M.; Del Freo, F.; Duffard, R.; Evangelista-Santana, M.; Farroni, G.; Fauvaud, S.; Fauvaud, M.; Ferrais, M.; Geier, S.; Golonka, J.; Grice, J.; Hirsch, R.; Horbowicz, J.; Jehin, E.; Julien, P.; Kalup, Cs.; Kamiński, K.; Kamińska, M. K.; Kankiewicz, P.; Kecskeméthy, V.; Kim, D. -H.; Kim, M. -J.; Konstanciak, I.; Krajewski, J.; Kudak, V.; Kulczak, P.; Kundera, T.; Lazzaro, D.; Manzini, F.; Medeiros, H.; Michimani-Garcia, J.; Morales, N.; Nadolny, J.; Oszkiewicz, D.; Pakštienė, E.; Pawłowski, M.; Perig, V.; Pilcher, F.; Pinel, P.; Podlewska-Gaca, E.; Polakis, T.; Richard, F.; Rodrigues, T.; Rondón, E.; Roy, R.; Sanabria, J. J.; Santana-Ros, T.; Skiff, B.; Skrzypek, J.; Sobkowiak, K.; Sonbas, E.; Stachowski, G.; Strajnic, J.; Trela, P.; Tychoniec, Ł.; Urakawa, S.; Verebelyi, E.; Wagrez, K.; Żejmo, M.; Żukowski, K., Context. Recent results for asteroid rotation periods from the TESS mission showed how strongly previous studies have underestimated the number of slow rotators, revealing the importance of studying those targets. For most slowly rotating asteroids (those with P > 12 h), no spin and shape model is available because of observation selection effects. This hampers determination of their thermal parameters and accurate sizes. Also, it is still unclear whether signatures of different surface material properties can be seen in thermal inertia determined from mid-infrared thermal flux fitting. Aims. We continue our campaign in minimising selection effects among main belt asteroids. Our targets are slow rotators with low light-curve amplitudes. Our goal is to provide their scaled spin and shape models together with thermal inertia, albedo, and surface roughness to complete the statistics. Methods. Rich multi-apparition datasets of dense light curves are supplemented with data from Kepler and TESS spacecrafts. In addition to data in the visible range, we also use thermal data from infrared space observatories (mainly IRAS, Akari and WISE) in a combined optimisation process using the Convex Inversion Thermophysical Model. This novel method has so far been applied to only a few targets, and therefore in this work we further validate the method itself. Results. We present the models of 16 slow rotators, including two updated models. All provide good fits to both thermal and visible data.The obtained sizes are on average accurate at the 5% precision level, with diameters found to be in the range from 25 to 145 km. The rotation periods of our targets range from 11 to 59 h, and the thermal inertia covers a wide range of values, from 2 to, This work was was initiated with the support from the National Science Centre, Poland, through grant no. 2014/13/D/ST9/01818; and from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no 687378 (SBNAF). The work of J.D. was supported by the grant 20-08218S of the Czech Science Foundation. A.P. and R.S. have been supported by the K-125015 grant of the National Research, Development and Innovation Office (NKFIH), Hungary. This project has been supported by the Lendulet grant LP2012-31 of the Hungarian Academy of Sciences. This project has been supported by the GINOP-2.3.2-15-2016-00003 grant of the Hungarian National Research, Development and Innovation Office (NKFIH). L.M. was supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences. The research leading to these results has received funding from the LP2018-7/2020 Lendulet grant of the Hungarian Academy of Sciences. The work of T.S.-R. was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE). E. P. acknowledges the Europlanet 2024 RI project funded by the European Union's Horizon 2020 Research and Innovation Programme (Grant agreement No. 871149). This article is based on observations obtained at the Observatorio Astronomico do Sertao de Itaparica (OASI, Itacuruba) of the Observatorio Nacional, Brazil. F.M. would like to thank the financial support given by FAPERJ (Process E-26/201.877/2020). E.R., P.A., H.M., M.E. and J.M. would like to thank CNPq and CAPES (Brazilian agencies) for their support through diverse fellowships. Support by CNPq (Process 305409/2016-6) and FAPERJ (Process E-26/202.841/2017) is acknowledged by D.L. The Joan Oro Telescope (TJO) of the Montsec Astronomical Observatory (OAdM) is owned by the Catalan Government and operated by the Institute for Space Studies of Catalonia (IEEC). This article is based on observations made in the Observatorios de Canarias del IAC with the 0.82 m IAC80 telescope operated on the island of Tenerife by the Instituto de Astrofisica de Canarias (IAC) in the Observatorio del Teide. This article is based on observations made with the SARA telescopes (Southeastern Association for Research in Astronomy), whose nodes are located at the Observatorios de Canarias del IAC on the island of La Palma in the Observatorio del Roque de los Muchachos; Kitt Peak, AZ under the auspices of the National Optical Astronomy Observatory (NOAO); and Cerro Tololo Inter-American Observatory (CTIO) in La Serena, Chile. This project uses data from the SuperWASP archive. The WASP project is currently funded and operated by Warwick University and Keele University, and was originally set up by Queen's University Belfast, the Universities of Keele, St. Andrews, and Leicester, the Open University, the Isaac Newton Group, the Instituto de Astrofisica de Canarias, the South African Astronomical Observatory, and by STFC. TRAPPIST-South is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege, in collaboration with the Cadi Ayyad University of Marrakech (Morocco). E. Jehin is FNRS Senior Research Associate. Funding for the Kepler and K2 missions are provided by the NASA Science Mission Directorate. The data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. Data from Pic du Midi Observatory have been obtained with the 0.6-m telescope, a facility operated by Observatoire Midi Pyrenees and Association T60, an amateur association. We acknowledge the contributions of the occultation observers who have provided the observations in the dataset. Most of those observers are affiliated with one or more of: European Asteroidal Occultation Network (EAON), International Occultation Timing Association (IOTA), International Occultation Timing Association European Section (IOTA/ES), Japanese Occultation Information Network (JOIN), and Trans Tasman Occultation Alliance (TTOA)., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.
Published: 2021

4. Physical parameters of selected Gaia mass asteroids

Author: Emmanuel Jehin, Neil Parley, E. Podlewska-Gaca, Anna Marciniak, Thomas G. Müller, Josep M. Bosch, Zouhair Benkhaldoun, Lawrence A. Molnar, L. Bernasconi, K. Sobkowiak, A. Farkas, Bojan Dintinjana, Grzegorz Dudziński, Rene Duffard, M. Audejean, Raoul Behrend, A. Chapman, K. Żukowski, Aled Jones, Erika Verebélyi, R. Poncy, Victor Ali-Lagoa, V. Asenjo, Nicolás Morales, Karolina Dziadura, J. Grice, Róbert Szakáts, R. Roy, M. Butkiewicz-Bąk, S. Geier, Bálint Seli, Przemyslaw Bartczak, D. Molina, Roman Hirsh, P. Antonini, Marin Ferrais, András Pál, Toni Santana-Ros, Herve Jacquinot, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, European Commission, National Aeronautics and Space Administration (US), Hungarian Academy of Sciences, Hungarian Scientific Research Fund, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Université de Liège, Generalitat Valenciana, and Université Cadi Ayyad
Subjects: Solar System, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, general [Minor planets, asteroids], Context (language use), Astrophysics, 7. Clean energy, 01 natural sciences, Occultation, Física Aplicada, 0103 physical sciences, Thermal, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), photometric [Techniques], Minor planets, Astronomy and Astrophysics, Radiation mechanisms: thermal, Asteroids: general, 13. Climate action, Space and Planetary Science, Asteroid, thermal [Radiation mechanisms], Physics::Space Physics, Stellar occultation, Satellite, Astrophysics::Earth and Planetary Astrophysics, Spin (aerodynamics), general [Asteroids], Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. Thanks to the Gaia mission, it will be possible to determine the masses of approximately hundreds of large main belt asteroids with very good precision. We currently have diameter estimates for all of them that can be used to compute their volume and hence their density. However, some of those diameters are still based on simple thermal models, which can occasionally lead to volume uncertainties as high as 20-30%. Aims. The aim of this paper is to determine the 3D shape models and compute the volumes for 13 main belt asteroids that were selected from those targets for which Gaia will provide the mass with an accuracy of better than 10%. Methods. We used the genetic Shaping Asteroids with Genetic Evolution (SAGE) algorithm to fit disk-integrated, dense photometric lightcurves and obtain detailed asteroid shape models. These models were scaled by fitting them to available stellar occultation and/or thermal infrared observations. Results. We determine the spin and shape models for 13 main belt asteroids using the SAGE algorithm. Occultation fitting enables us to confirm main shape features and the spin state, while thermophysical modeling leads to more precise diameters as well as estimates of thermal inertia values. Conclusions. We calculated the volume of our sample of main-belt asteroids for which the Gaia satellite will provide precise mass determinations. From our volumes, it will then be possible to more accurately compute the bulk density, which is a fundamental physical property needed to understand the formation and evolution processes of small Solar System bodies. © ESO 2020., 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 (SBNAF). Funding for the Kepler and K2 missions is provided by the NASA Science Mission directorate. L.M. was supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences. The research leading to these results has received funding from the LP2012-31 and LP2018-7 Lendulet grants of the Hungarian Academy of Sciences. This project has been supported by the Lendulet grant LP2012-31 of the Hungarian Academy of Sciences and by the GINOP-2.3.2-15-2016-00003 grant of the Hungarian National Research, Development and Innovation Office (NKFIH). TRAPPIST-South is a project funded by the Belgian Fonds de la Recherche Scientifique (F.R.S.-FNRS) under grant FRFC 2.5.594.09.F. TRAPPIST-North is a project funded by the University of Liege, and performed in collaboration with Cadi Ayyad University of Marrakesh. E.J. is a FNRS Senior Research Associate. "The Joan Oro Telescope (TJO) of the Montsec Astronomical Observatory (OAdM) is owned by the Catalan Government and operated by the Institute for Space Studies of Catalonia (IEEC)." "This article is based on observations made with the SARA telescopes (Southeastern Association for Research in Astronomy), whose node is located at the Kitt Peak National Observatory, AZ under the auspices of the National Optical Astronomy Observatory (NOAO)." "This project uses data from the SuperWASP archive. The WASP project is currently funded and operated by Warwick University and Keele University, and was originally set up by Queen's University Belfast, the Universities of Keele, St. Andrews, and Leicester, the Open University, the Isaac Newton Group, the Instituto de Astrofisica de Canarias, the South African Astronomical Observatory, and by STFC." "This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration." The work of TSR was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain)
Published: 2020

5. Against the biases in spins and shapes of asteroids

Author: F. Richard, Jakub Nadolny, E. Kosturkiewicz, K. Sobkowiak, A. Marciniak, Shin-ichiro Okumura, I. Konstanciak, Dagmara Oszkiewicz, Seitaro Urakawa, Magdalena Polińska, Krzysztof Kamiński, Łukasz Tychoniec, S. Fauvaud, Frederick Pilcher, Kota Nishiyama, M. Murawiecka, P. Trela, T. Sakamoto, Paweł Kankiewicz, M. Fauvaud, R. Hirsch, G. Stachowski, J. Horbowicz, and Toni Santana-Ros
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Brightness, 010504 meteorology & atmospheric sciences, Synodic day, Population, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Rotation, Orbital period, 01 natural sciences, Amplitude, Space and Planetary Science, Asteroid, Orientation (geometry), 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: Physical studies of asteroids depend on an availability of lightcurve data. Targets that are easy to observe and analyse naturally have more data available, so their synodic periods are confirmed from multiple sources. Also, thanks to availability of data from a number of apparitions, their spin and shape models can often be obtained. Almost half of bright (H12 hours) and are rarely chosen for photometric observations. There is a similar selection effect against asteroids with low lightcurve amplitudes (a_max, Published in Planetary and Space Science. 13 pages, 20 figures
Published: 2015

6. Shape and spin determination of Barbarian asteroids

Author: Jose Luis Ortiz, A. Kruszewki, R. Hirsch, Rodolfo Alfredo Artola, Paweł Kankiewicz, P. Antonini, Filip Berski, David Vernet, Josef Hanus, Orhan Erece, Myung-Jin Kim, I. Konstanciak, Hong-Kyu Moon, S. Pastor, E. Forne, Małgorzata Bronikowska, Krzysztof Kamiński, Young-Jun Choi, Murat Kaplan, K. Sobkowiak, Frederick Pilcher, P. Trela, Federico Manzini, Toni Santana-Ros, F. Reyes, Paul Hickson, Waldemar Ogloza, Paolo Tanga, J.-G. Bosch, T. Kwiatkowski, M. Murawiecka, Lyu Abe, Maxime Devogele, V. Kudak, F. Char, Jean Surdej, R. Durkee, Anna Marciniak, P. Bendjoya, J. M. Coloma, Dagmara Oszkiewicz, David Coward, Raoul Behrend, R. Poncy, J. Horbowicz, C. Colazo, J. P. Rivet, J.A. de los Reyes, M. C. Quiñones, Jakub Nadolny, Nuno Peixinho, Albino Carbognani, M. Audejean, H. Pallares, Natural Sciences and Engineering Research Council of Canada, European Commission, Fundação para a Ciência e a Tecnologia (Portugal), and National Science Centre (Poland)
Subjects: 010504 meteorology & atmospheric sciences, Polarimetry, FOS: Physical sciences, general [Minor planets, asteroids], Scale (descriptive set theory), Context (language use), Astrophysics, Rotation, 01 natural sciences, Methods: observational, 0103 physical sciences, observational [Methods], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Incidence (geometry), Physics, Earth and Planetary Astrophysics (astro-ph.EP), photometric [Techniques], Astronomy and Astrophysics, Photometry (astronomy), Space and Planetary Science, Sidereal time, Asteroid, Minor planets, asteroids: general, astro-ph.EP, Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. The so-called Barbarian asteroids share peculiar, but common polarimetric properties, probably related to both their shape and composition. They are named after (234) Barbara, the first on which such properties were identified. As has been suggested, large scale topographic features could play a role in the polarimetric response, if the shapes of Barbarians are particularly irregular and present a variety of scattering/incidence angles. This idea is supported by the shape of (234) Barbara, that appears to be deeply excavated by wide concave areas revealed by photometry and stellar occultations. Aims. With these motivations, we started an observation campaign to characterise the shape and rotation properties of Small Main-Belt Asteroid Spectroscopic Survey (SMASS) type L and Ld asteroids. As many of them show long rotation periods, we activated a worldwide network of observers to obtain a dense temporal coverage. Methods. We used light-curve inversion technique in order to determine the sidereal rotation periods of 15 asteroids and the convergence to a stable shape and pole coordinates for 8 of them. By using available data from occultations, we are able to scale some shapes to an absolute size. We also study the rotation periods of our sample looking for confirmation of the suspected abundance of asteroids with long rotation periods. Results. Our results show that the shape models of our sample do not seem to have peculiar properties with respect to asteroids with similar size, while an excess of slow rotators is most probably confirmed.© 2017 ESO., N.P. acknowledges funding from the Portuguese FCT - Foundation for Science and Technology. CI-TEUC is funded by National Funds through FCT - Foundation for Science and Technology (project: UID/ Multi/00611/2013) and FEDER - European Regional Development Fund through COMPETE 2020 - Operational Programme Competitiveness and Internationalisation (project: POCI-01-0145-FEDER-006922). SARA observations were obtained under the Chilean Telescope Allocation Committee program CNTAC 2015B-4. P.H. acknowledges financial support from the Natural Sciences and Engineering Research Council of Canada, and thanks the staff of Cerro Tololo Inter-American Observatory for technical support. The work of A.M. was supported by grant no. 2014/13/D/ST9/01818 from the National Science Centre, Poland. The research of V.K. is supported by the APVV-15-0458 grant and the VVGS-2016-72608 internal grant of the Faculty of Science, P.J. Safarik University in Kosice. M.K. and O.E. acknowledge TUBITAK National Observatory for a partial support in using T100 telescope with project number 14BT100-648.
Published: 2017

7. Photometric survey, modelling, and scaling of long-period and low-amplitude asteroids

Author: Toni Santana-Ros, Przemyslaw Bartczak, F. Manzini, Th. Müller, I. Konstanciak, Paweł Kankiewicz, J. J. Sanabria, R. Stoss, Krzysztof Kamiński, Waldemar Ogloza, Grzegorz Dudziński, Nicolás Morales, K. Sobkowiak, Rene Duffard, L. Jerosimic, K. Żukowski, Frederick Pilcher, M. Butkiewicz-Bąk, Raoul Behrend, R. Poncy, V. Kudak, E. Kosturkiewicz, L. Bernasconi, R. Hirsch, S. Fauvaud, Tom Polakis, Aleksandar Cikota, Michal Siwak, Brian A. Skiff, R. Crippa, S. Geier, J. Horbowicz, Victor Ali-Lagoa, Karolina Dziadura, Michał Żejmo, M. Hren, P. Korlevic, P. Antonini, Dagmara Oszkiewicz, Małgorzata Bronikowska, R. Ditteon, M. Murawiecka, A. Marciniak, National Science Centre (Poland), European Commission, and Slovak Research and Development Agency
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, photometric [Techniques], Inverse transform sampling, general [Minor planets, asteroids], FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Scale (descriptive set theory), Astrophysics, Albedo, Rotation, 01 natural sciences, Amplitude, Space and Planetary Science, Asteroid, Minor planets, asteroids: general, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Scaling, Techniques: photometric, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Marciniak, A. et. al..-- 33 p., The available set of spin and shape modelled asteroids is strongly biased against slowly rotating targets and those with low lightcurve amplitudes. This is due to the observing selection effects. As a consequence, the current picture of asteroid spin axis distribution, rotation rates, radiometric properties, or aspects related to the object's internal structure might be affected too. Aims. To counteract these selection effects, we are running a photometric campaign of a large sample of main belt asteroids omitted in most previous studies. Using least chi-squared fitting we determined synodic rotation periods and verified previous determinations. When a dataset for a given target was sufficiently large and varied, we performed spin and shape modelling with two different methods to compare their performance. Methods. We used the convex inversion method and the non-convex SAGE algorithm, applied on the same datasets of dense lightcurves. Both methods search for the lowest deviations between observed and modelled lightcurves, though using different approaches. Unlike convex inversion, the SAGE method allows for the existence of valleys and indentations on the shapes based only on lightcurves. Results. We obtain detailed spin and shape models for the first five targets of our sample: (159) Aemilia, (227) Philosophia, (329) Svea, (478) Tergeste, and (487) Venetia. When compared to stellar occultation chords, our models obtained an absolute size scale and major topographic features of the shape models were also confirmed. When applied to thermophysical modelling (TPM), they provided a very good fit to the infrared data and allowed their size, albedo, and thermal inertia to be determined. Conclusions. Convex and non-convex shape models provide comparable fits to lightcurves. However, some non-convex models fit notably better to stellar occultation chords and to infrared data in sophisticated thermophysical modelling (TPM). In some cases TPM showed strong preference for one of the spin and shape solutions. Also, we confirmed that slowly rotating asteroids tend to have higher-than-average values of thermal inertia, which might be caused by properties of the surface layers underlying the skin depth. © 2018 ESO., This work was supported by grant No. 2014/13/D/ST9/01818 from the National Science Centre, Poland. 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. V.K. was supported by the grant from the Slovak Research and Development Agency with number APVV-15-0458.
Published: 2017
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8. Photometry and models of selected main belt asteroids. VI. 160 Una, 747 Winchester, and 849 Ara

Author: A. Marciniak, Krzysztof Kamiński, R. Hirsch, K. Sobkowiak, Tadeusz Michalowski, L. Bernasconi, Magdalena Polińska, S. Starczewski, J. Michałowski, Agnieszka Kryszczyńska, M. Fagas, Raoul Behrend, and T. Kwiatkowski
Subjects: Rotation period, Physics, Photometry (optics), Space and Planetary Science, Planet, Asteroid, Asteroid belt, Astronomy, Astronomy and Astrophysics, Astrophysics, Light curve
Abstract: We present a set of new photometric observations of three main belt asteroids: 160 Una, 747 Winchester, and 849 Ara. This, combined with the available data, allowed us to construct their physical models. The lightcurve inversion method was used to obtain their spins and shapes. We have resolved problems with the rotation period of 160 Una, and found it to be 11.033176 ± 0.000011 h, almost twice the value given in the literature.
Published: 2009

9. 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

10. 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

11. 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

12. Photometry and models of selected main belt asteroids IX. Introducing interactive service for asteroid models (ISAM)

Author: Jari J. E. Kajava, K. Sobkowiak, F. Manzini, G. Santacana, C. Bembrick, A. Marciniak, R. Hirsch, Raoul Behrend, R. Poncy, Tayyaba Zafar, Desiree Della Monica Ferreira, Magdalena Polińska, Krzysztof Kamiński, S. Starczewski, Florent Colas, R. P. Hein Bertelsen, L. Bernasconi, S. Fauvaud, David Higgins, N. Esseiva, Michał J. Michałowski, R. Crippa, P. Antonini, T. Kwiatkowski, M. Fauvaud, F. P. Velichko, M. Fagas, A. Paschke, R. Roy, M. Stasik, J. M. Coloma, Tadeusz Michalowski, J. Michałowski, Agnieszka Kryszczyńska, Przemyslaw Bartczak, W. Borczyk, H. Wücher, Toni Santana-Ros, Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Observatoire de Bédoin, Geneva Observatory, University of Geneva [Switzerland], Observatoire des Engarouines, Service Interfaces et Capteurs (IFREMER), Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER), Observatorio de San Gervasi, Observatorio Astronómico de Tradate, Association AstroQueyras, Association T60, Observatoire 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Observatoire du Bois de Bardon, Hunters Hill Observatory, Stazione Astronomica di Sozzago, Groupe européen d’observation stellaire (GEOS), Chercheur indépendant, Laboratoire de Physique Nucléaire, Université Laval [Québec] (ULaval), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université de Genève = University of Geneva (UNIGE), Service Interfaces et capteurs (IC), 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, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute, and Astronomy
Subjects: 010504 meteorology & atmospheric sciences, Inverse transform sampling, Astrophysics, LIGHTCURVE INVERSION, minor planets, asteroids: general, 01 natural sciences, law.invention, Photometry, Photometry (optics), techniques: photometric, law, Radar imaging, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Radar, OPTIMIZATION METHODS, SHAPE DETERMINATION, Adaptive optics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], PHOTOELECTRIC PHOTOMETRY, Astronomy, Astronomy and Astrophysics, Inversion (meteorology), Stars, Asteroids, asteroids: general, Space and Planetary Science, Asteroid, POLE, minor planets, ROTATION, Astrophysics::Earth and Planetary Astrophysics
Abstract: Context. The shapes and spin states of asteroids observed with photometric techniques can be reconstructed using the lightcurve inversion method. The resultant models can then be confirmed or exploited further by other techniques, such as adaptive optics, radar, thermal infrared, stellar occultations, or space probe imaging.Aims. During our ongoing work to increase the set of asteroids with known spin and shape parameters, there appeared a need for displaying the model plane-of-sky orientations for specific epochs to compare models from different techniques. It would also be instructive to be able to track how the complex lightcurves are produced by various asteroid shapes.Methods. Basing our analysis on an extensive photometric observational dataset, we obtained eight asteroid models with the convex lightcurve inversion method. To enable comparison of the photometric models with those from other observing/modelling techniques, we created an on-line service where we allow the inversion models to be orientated interactively.Results. Our sample of objects is quite representative, containing both relatively fast and slow rotators with highly and lowly inclined spin axes. With this work, we increase the sample of asteroid spin and shape models based on disk-integrated photometry to over 200. Three of the shape models obtained here are confirmed by the stellar occultation data; this also allowed independent determinations of their sizes to be made.Conclusions. The ISAM service can be widely exploited for past and future asteroid observations with various, complementary techniques and for asteroid dimension determination.
Published: 2012

13. Photometry and models of selected main belt asteroids. VII. 350 Ornamenta, 771 Libera, and 984 Gretia

Author: A. Peyrot, T. Kwiatkowski, Magdalena Polińska, F. Colas, S. Fauvaud, Krzysztof Kamiński, Tadeusz Michalowski, A. Marciniak, K. Sobkowiak, P. Descamps, Regina Rudawska, J.-P. Teng-Chuen-Yu, G. Santacana, M. Fauvaud, Agnieszka Kryszczyńska, A. Bruno, L. Bernasconi, Raoul Behrend, R. Hirsch, Adam Mickiewicz University in Poznań (UAM), Observatoire Astronomique de l'Université de Genève, Observatoire des Engarouines, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Groupe Astrométrie et Planétologie (GAP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Observatoire du Bois de Bardon, 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, Université de Rennes (UR), and Observatoire astronomique des Makes
Subjects: Photometry (optics), Physics, Space and Planetary Science, Planet, Asteroid, Asteroid belt, Astronomy, Astronomy and Astrophysics, Astrophysics, Light curve, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; We analyze photometric observations of the three main-belt asteroids 350 Ornamenta, 771 Libera, and 984 Gretia, conducted over a twelve-year interval. Our data and those of other authors allow us to determine pole and shape models using the lightcurve inversion technique. In all three cases, a single pole solution was obtained without any significant mirror solution: Ornamenta - P = 9.180 414 h, lambdap = 184°, betap = -29° Libera - P = 5.890 423 h, lambdap = 64°, betap = -78° Gretia - P = 5.778 025 h, lambdap = 245°, betap = +52°. This analysis and the development of asteroid models increase the set of asteroids with known spin and shape parameters, which consists of only around 100 objects.
Published: 2009

14. Do Slivan states exist in the Flora family?

Author: Tadeusz Michalowski, Paweł Kankiewicz, V. Umlenski, Alain Maury, F. Manzini, Dagmara Oszkiewicz, Alain Klotz, Magdalena Polińska, B. Bilkina, Toni Santana-Ros, Raoul Behrend, R. Poncy, F. Colas, M. Fagas, L. Bernasconi, R. Crippa, A. Marciniak, G. Apostolovska, P. Antonini, T. Kwiatkowski, K. Sobkowiak, F. P. Velichko, Agnieszka Kryszczyńska, R. Hirsch, Krzysztof Kamiński, Frédéric Vachier, V. Ivanova, J. Lecacheux, W. Dimitrov, and W. Borczyk
Subjects: Physics, Flora, Younger age, 010504 meteorology & atmospheric sciences, Synodic day, Astronomy, Astronomy and Astrophysics, Context (language use), Astrophysics, 01 natural sciences, Space and Planetary Science, Asteroid, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Rotation (mathematics), 0105 earth and related environmental sciences, Spin-½
Abstract: Context. Recent studies have uncovered evidence that the statistical properties of asteroids’ physical parameters are a fundamental source of information on the physics of their collisions and evolution. The analysis of the spin rates and spin vector distributions helps us to understand the role of various known and new effects. The alignment of spin vectors and the correlation of spin rates are for the first time observed for ten members of the Koronis family. These unexpected non-random orientations of the spin axes and correlations of the spin rates, now known as Slivan states are interpreted in terms of a YORP effect and spin-orbit resonances. Aims. To study non-gravitational-effects, there appears to be a need for new observational campaigns devoted to determining the physical parameters of the asteroid families. Methods. We analysed the photometric observations of the asteroids, which are the most efficient method of studying asteroid physical parameters.Results. We report the results of a ten-year long observational survey of the light variations of objects in the Flora region. We present 544 individual lightcurves of 55 objects obtained at various observing geometries. These lightcurves yield new or refined synodic periods for 32 asteroids and confirm period determinations for 23 objects in our sample. To improve the statistics of the Flora family objects, we add to our dataset 91 objects with reliably determined periods. The distribution of rotation rates for the Flora family is non-Maxwellian at a confidence level of 94% and different from those of the Koronis and the Hungaria families. It seems to be consistent with the long-term influence of the YORP effect, although it is also indicative of a younger age for the Flora family compared to both the Koronis and the Hungaria families. Conclusions. Our new data is a foundation for the spin vector and shape determinations that will be the objectives of the second paper of the series. We search for spin vector and spin periods correlations in order to determine whether Slivan states exist in the Flora family.
Published: 2012

15. Photometry and models of selected main belt asteroids

Author: F. Manzini, H. Pallares, J.-G. Bosch, Tadeusz Michalowski, Magdalena Polińska, P. Bartczak, L. Brunetto, R. Hirsch, Krzysztof Kamiński, J. M. Coloma, Regina Rudawska, K. Sobkowiak, A. Marciniak, M. Conjat, Raoul Behrend, P. Ludick, F. Choisay, M. Fagas, R. Roy, S. Starczewski, G. Farroni, L. Bernasconi, J. Michałowski, Agnieszka Kryszczyńska, and T. Kwiatkowski
Subjects: Photometry (optics), North pole, Physics, Amplitude, Space and Planetary Science, Asteroid, Planet, Ecliptic, Asteroid belt, Astronomy, Astronomy and Astrophysics, Astrophysics, Light curve
Abstract: Context. The set of more than 100 asteroids, for which spin parameters have been modelled using an amplitude, magnitude or epoch methods, showed a pronounced gap in the distribution of the asteroid spin axes. These spin axes are rarely aligned with the ecliptic plane. Aims. The number of asteroids with known spin parameters should be increased to allow for statistical investigations. Methods. We gathered extensive photometric datasets on four selected main-belt asteroids to model their spin and shape parameters using the lightcurve inversion method. Our only criterion of selection was their observability for small telescopes. Results. All four of the modelled asteroids happened to have rotational poles that lie close to the ecliptic plane (periods and J2000 north pole coordinates): (94) Aurora − P = 7.226191 h, λp1 = 58 ◦ , βp1 =+ 16 ◦ ; λp2 = 242 ◦ , βp2 =+ 4 ◦ ; (174) Phaedra − P = 5.750249 h, λp = 265 ◦ , βp =+ 5 ◦ ; (679) Pax − P = 8.456016 h, λp1 = 42 ◦ , βp1 = −5 ◦ ; λp2 = 220 ◦ , βp2 =+ 32 ◦ (pole 2 preferred after comparison with AO-resolved observations); (714) Ulula − P = 6.998376 h, λp1 = 42 ◦ , βp1 = −9 ◦ ; λp2 = 227 ◦ , βp2 = −14 ◦ . Conclusions. This work suggests that asteroid spin axes do not avoid the ecliptic plane, contrary to what the classical modelling suggested.
Published: 2011

16. Thermal properties of slowly rotating asteroids: results from a targeted survey

Author: J. J. Sanabria, M. Feuerbach, Eda Sonbas, V. Kudak, V. Perig, J. Grice, O. Thizy, Seitaro Urakawa, R. Szakats, Victor Ali-Lagoa, E. Podlewska Gaca, Tom Polakis, I. Grześkowiak, J. Skrzypek, Dagmara Oszkiewicz, F. Manzini, S. Geier, Myung-Jin Kim, I. Konstanciak, Doeon Kim, Magdalena Polińska, Michał Żejmo, P. Kulczak, S. Fauvaud, P. Trela, K. Żukowski, R. Crippa, J. Horbowicz, Waldemar Ogloza, K. Sobkowiak, E. Barbotin, M. Butkiewicz Bąk, Rupak Roy, P. Antonini, László Molnár, Rene Duffard, Krzysztof Kamiński, Brian A. Skiff, Raoul Behrend, Frederick Pilcher, A. Marciniak, M. K. Kamińska, J. L. Maestre, N. Parley, J. Garlitz, R. Hirsch, Rui Soles Gonçalves, F. Monteiro, R. Ditteon, S. Marks, T. Santana-Ros, L. Bernasconi, Tamás Müller, A. Pal, National Science Centre (Poland), European Commission, Ministry of Education (Slovak Republic), Ministerio de Ciencia, Innovación y Universidades (España), and Hungarian Academy of Sciences
Subjects: Rotation period, 010504 meteorology & atmospheric sciences, Infrared, FOS: Physical sciences, Scale (descriptive set theory), Context (language use), Astrophysics, minor planets, asteroids: general, 01 natural sciences, photometric [techniques], Photometry (optics), techniques: photometric, 0103 physical sciences, Thermal, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Spin-½, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy and Astrophysics, radiation mechanisms: thermal, 13. Climate action, Space and Planetary Science, Asteroid, thermal [radiation mechanisms], Astrophysics::Earth and Planetary Astrophysics, general [minor planets, asteroids], Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. Earlier work suggests that slowly rotating asteroids should have higher thermal inertias than faster rotators because the heat wave penetrates deeper into the subsurface. However, thermal inertias have been determined mainly for fast rotators due to selection effects in the available photometry used to obtain shape models required for thermophysical modelling (TPM). Aims. Our aims are to mitigate these selection effects by producing shape models of slow rotators, to scale them and compute their thermal inertia with TPM, and to verify whether thermal inertia increases with the rotation period. Methods. To decrease the bias against slow rotators, we conducted a photometric observing campaign of main-belt asteroids with periods longer than 12 h, from multiple stations worldwide, adding in some cases data from WISE and Kepler space telescopes. For spin and shape reconstruction we used the lightcurve inversion method, and to derive thermal inertias we applied a thermophysical model to fit available infrared data from IRAS, AKARI, and WISE. Results. We present new models of 11 slow rotators that provide a good fit to the thermal data. In two cases, the TPM analysis showed a clear preference for one of the two possible mirror solutions. We derived the diameters and albedos of our targets in addition to their thermal inertias, which ranged between 3(-3)(+33) and 45(-30)(+60) Jm(-2) s(-1/2) K-1. Conclusions. Together with our previous work, we have analysed 16 slow rotators from our dense survey with sizes between 30 and 150 km. The current sample thermal inertias vary widely, which does not confirm the earlier suggestion that slower rotators have higher thermal inertias.© ESO 2019, This work was supported by the National Science Centre, Poland, through grant no. 2014/13/D/ST9/01818. 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 (SBNAF). The research of V.K. was supported by a grant from the Slovak Research and Development Agency, number APVV-15-0458. R. D. acknowledges 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). The Joan Oro Telescope (TJO) of the Montsec Astronomical Observatory (OAdM) is owned by the Catalan Government and operated by the Institute for Space Studies of Catalonia (IEEC). This article is based on observations made in the Observatorios de Canarias del IAC with the 0.82 m IAC80 telescope operated on the island of Tenerife by the Instituto de Astrofisica de Canarias (IAC) in the Observatorio del Teide. This article is based on observations made with the SARA telescopes (Southeastern Association for Research in Astronomy), whose nodes are located at the Observatorios de Canarias del IAC on the island of La Palma in the Observatorio del Roque de los Muchachos; Kitt Peak, AZ under the auspices of the National Optical Astronomy Observatory (NOAO); and Cerro Tololo Inter-American Observatory (CTIO) in La Serena, Chile. This project uses data from the SuperWASP archive. The WASP project is currently funded and operated by Warwick University and Keele University, and was originally set up by Queen's University Belfast, the Universities of Keele, St. Andrews, and Leicester, the Open University, the Isaac Newton Group, the Instituto de Astrofisica de Canarias, the South African Astronomical Observatory, and by STFC. Funding for the Kepler and K2 missions is provided by the NASA Science Mission Directorate. The data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This publication makes use of data products from theWide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The research leading to these results has received funding from the LP2012-31 and LP2018-7/2018 Lendulet grants of the Hungarian Academy of Sciences.
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17. Combined approach of selective and accelerated cloning for microfluidic chip-based system increases clone specific productivity.

Author: Desmurget C, Frentzel J, Strembitska A, Sobkowiak K, Perilleux A, Souquet J, Borth N, and Douet J
Subjects: CHO Cells, Animals, Immunoglobulin G genetics, Lab-On-A-Chip Devices, Flow Cytometry, Cricetulus
Abstract: Improving current cell line development workflows can either focus on increasing the specific productivity of the cell lines or shortening timelines to reach the clinic as fast as possible. In this work, using the Beacon platform, we have combined two distinct protocols - early cloning with low-viability pools, and IgG membrane staining-, to concomitantly reach both objectives, and generate highly productive CHO clones in shorter timelines. Fast-sorting approaches using low-viability pools in combination with the Beacon platform have recently been reported to shorten CLD timelines. However, the low recovery led to a drastic reduction in the clone number obtained postcloning. Here, we report a combined approach of fast-sorting and fluorescent membrane staining. With this new protocol, the cells reach a correct recovery, allowing to fully exploit the Beacon screening capacities. In addition, by using a fluorescent staining recognizing the secreted IgG, we were able to enrich the fraction of highly secreting cells prior to cloning and we obtained significant increases in the cell's specific productivity. The combination of these two protocols has a synergistic effect, and as they help discarding the dead and nonproducing populations prior to cloning, they increase the throughput power of the Beacon platform and the detection of super productive clones., (© 2024 ARES Trading SA. Biotechnology Journal published by Wiley‐VCH GmbH.)
Published: 2024
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18. High-resolution mapping of mitotic DNA synthesis regions and common fragile sites in the human genome through direct sequencing.

Author: Macheret M, Bhowmick R, Sobkowiak K, Padayachy L, Mailler J, Hickson ID, and Halazonetis TD
Subjects: Cell Line, Tumor, Chromosome Breakage, DNA Replication Timing genetics, Genomic Instability, Humans, Molecular Sequence Annotation, Neoplasms genetics, Replication Origin genetics, Chromosome Fragile Sites genetics, DNA biosynthesis, Genome, Human, Mitosis genetics, Sequence Analysis, DNA
Abstract: DNA replication stress, a feature of human cancers, often leads to instability at specific genomic loci, such as the common fragile sites (CFSs). Cells experiencing DNA replication stress may also exhibit mitotic DNA synthesis (MiDAS). To understand the physiological function of MiDAS and its relationship to CFSs, we mapped, at high resolution, the genomic sites of MiDAS in cells treated with the DNA polymerase inhibitor aphidicolin. Sites of MiDAS were evident as well-defined peaks that were largely conserved between cell lines and encompassed all known CFSs. The MiDAS peaks mapped within large, transcribed, origin-poor genomic regions. In cells that had been treated with aphidicolin, these regions remained unreplicated even in late S phase; MiDAS then served to complete their replication after the cells entered mitosis. Interestingly, leading and lagging strand synthesis were uncoupled in MiDAS, consistent with MiDAS being a form of break-induced replication, a repair mechanism for collapsed DNA replication forks. Our results provide a better understanding of the mechanisms leading to genomic instability at CFSs and in cancer cells.
Published: 2020
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19. Effect of exogenous butyrate on the gastrointestinal tract of sheep. II. Hydrolytic activity in the rumen and structure and function of the small intestine.

Author: Górka P, Śliwiński B, Flaga J, Olszewski J, Nawrocka P, Sobkowiak K, Miltko R, Godlewski MM, Zabielski R, and Kowalski ZM
Published: 2020
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20. Effect of exogenous butyrate on the gastrointestinal tract of sheep. II. Hydrolytic activity in the rumen and structure and function of the small intestine.

Author: Górka P, Sliwinski B, Flaga J, Olszewski J, Nawrocka P, Sobkowiak K, Miltko R, Godlewski MM, Zabielski R, and Kowalski ZM
Subjects: Animal Feed, Animals, Diet veterinary, Gastrointestinal Tract drug effects, Gastrointestinal Tract metabolism, Hydrolysis, Intestinal Mucosa drug effects, Intestinal Mucosa metabolism, Intestine, Small drug effects, Intestine, Small metabolism, Male, Random Allocation, Rumen drug effects, Rumen metabolism, Butyric Acid pharmacology, Sheep physiology
Abstract: The aim of this study was to determine the effect of exogenous butyrate on the activity of carbohydrate-digesting enzymes in the reticuloruminal digesta and structure and selected functions of the small intestine in sheep. Eighteen rams (30.8 ± 2.1 kg; 12 to 15 mo of age) were fed for 14 d a diet without (CTRL) or with sodium butyrate (BUT; 36 g/kg of offered DM). Butyrate concentration in the reticuloruminal fluid and proximal small intestinal digesta was greater for BUT compared with CTRL (P ≤ 0.05). Amylolytic activity was greater, whereas cellulolytic and xylanolytic activity in the reticuloruminal digesta was less for BUT compared with CTRL (P ≤ 0.04). Relative to BW, small intestinal tissue mass and small intestine length did not differ between treatments (P ≥ 0.15); however, absolute length of the small intestine was greater for BUT compared with CTRL (P = 0.04). In the duodenum, crypt depth tended (P = 0.10) to be greater, whereas in the ileum, crypt depth and muscularis thickness tended (P = 0.10) to be less for BUT compared with CTRL. Mitosis-to-apoptosis ratio in the proximal jejunum was greater for CTRL compared with BUT (P = 0.02). Expression of G-protein-coupled receptor 43 mRNA in the duodenal epithelium was greater for BUT compared with CTRL (P < 0.01). On the other hand, peptide transporter 1 mRNA expression in the distal sections of the small intestine, as well as activity of aminopeptidase A and dipeptidylpeptidase IV, were greater for CTRL (P ≤ 0.05). In summary, exogenous butyrate supplementation in feed affects hydrolytic activity in the rumen, and increased butyrate flow out of the reticulorumen affects both proximal and distal sections of the small intestine in sheep.
Published: 2018
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21. 2012 QG42: A SLOW ROTATOR NEA.

Author: Warner BD, Baker RE, Bartczak P, Marciniak A, Sobkowiak K, Hirsch R, Kaminski K, Bacci P, Franco L, Vorobjov T, and Holmes RE Jr
Abstract: CCD photometric observations of the near-Earth asteroid 2012 QG42 were made by a collaboration of observers in the U.S. and Europe. The asteroid was found to be a slow rotator, having a synodic period of 24.22 ± 0.01 h based on a data set spanning nearly two weeks. The amplitude of the lightcurve was 1.18 ± 0.03 mag.
Published: 2013

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21 results on '"K. Sobkowiak"'

1. Asteroid phase curves using sparse Gaia DR2 data and differential dense light curves

2. (704) Interamnia: a transitional object between a dwarf planet and a typical irregular-shaped minor body

3. Properties of slowly rotating asteroids from the Convex Inversion Thermophysical Model

4. Physical parameters of selected Gaia mass asteroids

5. Against the biases in spins and shapes of asteroids

6. Shape and spin determination of Barbarian asteroids

7. Photometric survey, modelling, and scaling of long-period and low-amplitude asteroids

8. Photometry and models of selected main belt asteroids. VI. 160 Una, 747 Winchester, and 849 Ara

9. The small binary asteroid (939) Isberga

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

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

12. Photometry and models of selected main belt asteroids IX. Introducing interactive service for asteroid models (ISAM)

13. Photometry and models of selected main belt asteroids. VII. 350 Ornamenta, 771 Libera, and 984 Gretia

14. Do Slivan states exist in the Flora family?

15. Photometry and models of selected main belt asteroids

16. Thermal properties of slowly rotating asteroids: results from a targeted survey

17. Combined approach of selective and accelerated cloning for microfluidic chip-based system increases clone specific productivity.

18. High-resolution mapping of mitotic DNA synthesis regions and common fragile sites in the human genome through direct sequencing.

19. Effect of exogenous butyrate on the gastrointestinal tract of sheep. II. Hydrolytic activity in the rumen and structure and function of the small intestine.

20. Effect of exogenous butyrate on the gastrointestinal tract of sheep. II. Hydrolytic activity in the rumen and structure and function of the small intestine.

21. 2012 QG42: A SLOW ROTATOR NEA.

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21 results on '"K. Sobkowiak"'

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