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43 results on '"Pulkovo Observatory"'

1. Astrometric observations of Uranian and Neptunian satellites with the Pulkovo and Crimean observatory telescopes in 2020

Author

S. V. Nazarov, Crimean astrophysical observatory, Yu. Khovritchev, Pulkovo Observatory, and D. A. Bikulova

Subjects
Observatory, Astronomy, Geology
Abstract

The paper presents the results of observations of the Uranian and Neptunian satellites performed in 2020 with the 1-meter mirror telescope ‘Saturn’ (Pulkovo observatory) and the 350-mm guide telescope of the ‘Sintez’ telescope (Crimean observatory). More than 8 thousand separate positions of the satellites were obtained in the Gaia EDR3 catalog system. The average values of standard errors of the satellite normal place in right ascension and declination for the entire observation period, demonstrating the internal convergence of the observation results, lie within 10—50 mas.

Published
2021
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8. SOLAR ACTIVITY AND CLIMATE OF THE EARTH

Author

Boian Kirov, Katya Georgieva, Yu.A. Nagovitsyn, Simeon Asenovski, and Pulkovo Observatory, Saint Petersburg, Russia

Subjects
Solar activity and climate, Environmental science, Earth (chemistry), Astrobiology
Published
2019
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14. PROPERTIES OF CLASSICAL Be STARS FROM ANALYSIS OF HIGH-RESOLUTION H PROFILES

Author

Miroshnichenko, A. S.; Ritter Observatory, University of Toledo, Toledo, Ohio, 43606, USA; Pulkovo Observatory, Saint-Petersburg, 196140, Russia, Bjorkman, K. S., Krugov, V. D., Usenko, I. A., Miroshnichenko, A. S.; Ritter Observatory, University of Toledo, Toledo, Ohio, 43606, USA; Pulkovo Observatory, Saint-Petersburg, 196140, Russia, Bjorkman, K. S., Krugov, V. D., and Usenko, I. A.

Abstract

We summarize results of the 25 year period of observations of Be-stars. We suggest that Be stars with moderate and strong Hα emission are good candidates to search for binary systems.

Published
2017

15. The simultaneous low state spectral energy distribution of 1ES 2344+514 from radio to very high energies

Author

MAGIC Collaboration, J. Aleksić(IFAE, Edifici Cn., Campus UAB, Spain), L. A. Antonelli(INAF National Institute for Astrophysics, Rome, Italy), P. Antoranz(Università di Siena, and INFN Pisa, Italy), M. Asensio(Universidad Complutense, Spain), M. Backes(Technische Universität Dortmund, Germany), U. Barres de Almeida(Max-Planck-Institut für Physik, München, Germany), J. A. Barrio(Universidad Complutense, Spain), W. Bednarek(University of Łódź, Poland), K. Berger(Inst. de Astrofísica de Canarias, Tenerife, Spain), E. Bernardini(Deutsches Elektronen-Synchrotron), A. Biland(ETH Zurich, Switzerland), O. Blanch(IFAE, Edifici Cn., Campus UAB, Spain), R. K. Bock(Max-Planck-Institut für Physik, München, Germany), A. Boller(ETH Zurich, Switzerland), S. Bonnefoy(Universidad Complutense, Spain), G. Bonnoli(INAF National Institute for Astrophysics, Rome, Italy), D. Borla Tridon(Max-Planck-Institut für Physik, München, Germany), T. Bretz(Universität Würzburg, Germany), E. Carmona(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Spain), A. Carosi(INAF National Institute for Astrophysics, Rome, Italy), D. Carreto Fidalgo(Universität Würzburg, Germany), P. Colin(Max-Planck-Institut für Physik, München, Germany), E. Colombo(Inst. de Astrofísica de Canarias, Tenerife, Spain), J. L. Contreras(Universidad Complutense, Spain), J. Cortina(IFAE, Edifici Cn., Campus UAB, Spain), L. Cossio(Università di Udine, and INFN Trieste, Italy), S. Covino(INAF National Institute for Astrophysics, Rome, Italy), P. Da Vela(Università di Siena, and INFN Pisa, Italy), F. Dazzi(Università di Udine, and INFN Trieste, Italy), A. De Angelis(Università di Udine, and INFN Trieste, Italy), G. De Caneva(Deutsches Elektronen-Synchrotron), B. De Lotto(Università di Udine, and INFN Trieste, Italy), C. Delgado Mendez(Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Spain), M. Doert(Technische Universität Dortmund, Germany), A. Domínguez(Inst. de Astrofísica de Andalucía), D. Dominis Prester(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Dorner(Universität Würzburg, Germany), M. Doro(Universitat Autònoma de Barcelona, Spain), D. Eisenacher(Universität Würzburg, Germany), D. Elsaesser(Universität Würzburg, Germany), D. Ferenc(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), M. V. Fonseca(Universidad Complutense, Spain), L. Font(Universitat Autònoma de Barcelona, Spain), C. Fruck(Max-Planck-Institut für Physik, München, Germany), R. J. García López(Inst. de Astrofísica de Canarias, Tenerife, Spain), M. Garczarczyk(Inst. de Astrofísica de Canarias, Tenerife, Spain), D. Garrido Terrats(Universitat Autònoma de Barcelona, Spain), M. Gaug(Universitat Autònoma de Barcelona, Spain), G. Giavitto(IFAE, Edifici Cn., Campus UAB, Spain), N. Godinović(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), A. González Muñoz(IFAE, Edifici Cn., Campus UAB, Spain), S. R. Gozzini(Deutsches Elektronen-Synchrotron), A. Hadamek(Technische Universität Dortmund, Germany), D. Hadasch(Institut de Ciències de l'Espai), A. Herrero(Inst. de Astrofísica de Canarias, Tenerife, Spain), J. Hose(Max-Planck-Institut für Physik, München, Germany), D. Hrupec(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), F. Jankowski(Deutsches Elektronen-Synchrotron), V. Kadenius(Tuorla Observatory, University of Turku, Finland), S. Klepser(IFAE, Edifici Cn., Campus UAB, Spain), M. L. Knoetig(Max-Planck-Institut für Physik, München, Germany), T. Krähenbühl(ETH Zurich, Switzerland), J. Krause(Max-Planck-Institut für Physik, München, Germany), J. Kushida(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), A. La Barbera(INAF National Institute for Astrophysics, Rome, Italy), D. Lelas(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), E. Leonardo(Università di Siena, and INFN Pisa, Italy), N. Lewandowska(Universität Würzburg, Germany), E. Lindfors(Tuorla Observatory, University of Turku, Finland), S. Lombardi(INAF National Institute for Astrophysics, Rome, Italy), M. López(Universidad Complutense, Spain), R. López-Coto(IFAE, Edifici Cn., Campus UAB, Spain), A. López-Oramas(IFAE, Edifici Cn., Campus UAB, Spain), E. Lorenz(Max-Planck-Institut für Physik, München, Germany), I. Lozano(Universidad Complutense, Spain), M. Makariev(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), K. Mallot(Deutsches Elektronen-Synchrotron), G. Maneva(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), N. Mankuzhiyil(Università di Udine, and INFN Trieste, Italy), K. Mannheim(Universität Würzburg, Germany), L. Maraschi(INAF National Institute for Astrophysics, Rome, Italy), B. Marcote(Universitat de Barcelona), M. Mariotti(Università di Padova and INFN Padova, Italy), M. Martínez(IFAE, Edifici Cn., Campus UAB, Spain), J. Masbou(Università di Padova and INFN Padova, Italy), D. Mazin(Max-Planck-Institut für Physik, München, Germany), M. Meucci(Università di Siena, and INFN Pisa, Italy), J. M. Miranda(Università di Siena, and INFN Pisa, Italy), R. Mirzoyan(Max-Planck-Institut für Physik, München, Germany), J. Moldón(Universitat de Barcelona), A. Moralejo(IFAE, Edifici Cn., Campus UAB, Spain), P. Munar-Adrover(Universitat de Barcelona), D. Nakajima(Max-Planck-Institut für Physik, München, Germany), A. Niedzwiecki(University of Łódź, Poland), D. Nieto(Universidad Complutense, Spain), K. Nilsson(Tuorla Observatory, University of Turku, Finland), N. Nowak(Max-Planck-Institut für Physik, München, Germany), R. Orito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), S. Paiano(Università di Padova and INFN Padova, Italy), M. Palatiello(Università di Udine, and INFN Trieste, Italy), D. Paneque(Max-Planck-Institut für Physik, München, Germany), R. Paoletti(Università di Siena, and INFN Pisa, Italy), J. M. Paredes(Universitat de Barcelona), S. Partini(Università di Siena, and INFN Pisa, Italy), M. Persic(Università di Udine, and INFN Trieste, Italy), M. Pilia(Università dell'Insubria, Como, Italy), F. Prada(Inst. de Astrofísica de Andalucía), P. G. Prada Moroni(Università di Pisa, and INFN Pisa, Italy), E. Prandini(Università di Padova and INFN Padova, Italy), I. Puljak(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), I. Reichardt(IFAE, Edifici Cn., Campus UAB, Spain), R. Reinthal(Tuorla Observatory, University of Turku, Finland), W. Rhode(Technische Universität Dortmund, Germany), M. Ribó(Universitat de Barcelona), J. Rico(ICREA, Barcelona, Spain), S. Rügamer(Universität Würzburg, Germany), A. Saggion(Università di Padova and INFN Padova, Italy), K. Saito(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), T. Y. Saito(Max-Planck-Institut für Physik, München, Germany), M. Salvati(INAF National Institute for Astrophysics, Rome, Italy), K. Satalecka(Universidad Complutense, Spain), V. Scalzotto(Università di Padova and INFN Padova, Italy), V. Scapin(Universidad Complutense, Spain), C. Schultz(Università di Padova and INFN Padova, Italy), T. Schweizer(Max-Planck-Institut für Physik, München, Germany), S. N. Shore(Università di Pisa, and INFN Pisa, Italy), A. Sillanpää(Tuorla Observatory, University of Turku, Finland), J. Sitarek(IFAE, Edifici Cn., Campus UAB, Spain), I. Snidaric(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Sobczynska(University of Łódź, Poland), F. Spanier(Universität Würzburg, Germany), S. Spiro(INAF National Institute for Astrophysics, Rome, Italy), V. Stamatescu(IFAE, Edifici Cn., Campus UAB, Spain), A. Stamerra(Università di Siena, and INFN Pisa, Italy), B. Steinke(Max-Planck-Institut für Physik, München, Germany), J. Storz(Universität Würzburg, Germany), S. Sun(Max-Planck-Institut für Physik, München, Germany), T. Surić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), L. Takalo(Tuorla Observatory, University of Turku, Finland), H. Takami(Japanese MAGIC Consortium, Division of Physics and Astronomy, Kyoto University, Japan), F. Tavecchio(INAF National Institute for Astrophysics, Rome, Italy), P. Temnikov(Inst. for Nucl. Research and Nucl. Energy, Sofia, Bulgaria), T. Terzić(Croatian MAGIC Consortium, Rudjer Boskovic Institute, University of Rijeka and University of Split, Croatia), D. Tescaro(Inst. de Astrofísica de Canarias, Tenerife, Spain), M. Teshima(Max-Planck-Institut für Physik, München, Germany), O. Tibolla(Universität Würzburg, Germany), D. F. Torres(ICREA, Barcelona, Spain), T. Toyama(Max-Planck-Institut für Physik, München, Germany), A. Treves(Università dell'Insubria, Como, Italy), M. Uellenbeck(Technische Universität Dortmund, Germany), P. Vogler(ETH Zurich, Switzerland), R. M. Wagner(Max-Planck-Institut für Physik, München, Germany), Q. Weitzel(ETH Zurich, Switzerland), F. Zandanel(Inst. de Astrofísica de Andalucía), R. Zanin(Universitat de Barcelona), The MAGIC Collaboration(Università di Trieste, and INFN Trieste, Italy), F. Longo(Università di Trieste, and INFN Trieste, Italy), F. Lucarelli(Agenzia Spaziale Italiana), C. Pittori(Agenzia Spaziale Italiana), S. Vercellone(INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Italy), for the AGILE team(Università di Padova and INFN Padova, Italy), D. Bastieri(Università di Padova and INFN Padova, Italy), C. Sbarra(INFN Padova, Italy), for the Fermi-LAT Collaboration(Max-Planck-Institut für Radioastronomie, Germany), E. Angelakis(Max-Planck-Institut für Radioastronomie, Germany), L. Fuhrmann(Max-Planck-Institut für Radioastronomie, Germany), I. Nestoras(Max-Planck-Institut für Radioastronomie, Germany), T. P. Krichbaum(Max-Planck-Institut für Radioastronomie, Germany), A. Sievers(Instituto de Radio Astronoma Milimétrica, Spain), J. A. Zensus(Max-Planck-Institut für Radioastronomie, Germany), for the F-GAMMA program(Crimean Astrophysical Observatory, Ukraine), K. A. Antonyuk(Crimean Astrophysical Observatory, Ukraine), W. Baumgartner(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), A. Berduygin(Tuorla Observatory, University of Turku, Finland), M. Carini(Department of Physics and Astronomy, Western Kentucky University, USA), K. Cook(Department of Physics and Astronomy, Western Kentucky University, USA), N. Gehrels(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), M. Kadler(Universität Würzburg, Germany), Yu. A. Kovalev(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), Y. Y. Kovalev(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), F. Krauss(Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany), H. A. Krimm(Universities Space Research Association, Columbia, MD 21044, USA), A. Lähteenmäki(Aalto University Metsähovi Radio Observatory, Finland), M. L. Lister(Department of Physics, Purdue University, USA), W. Max-Moerbeck(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, USA), M. Pasanen(Tuorla Observatory, University of Turku, Finland), A. B. Pushkarev(Pulkovo Observatory, St. Petersburg, Russia), A. C. S. Readhead(Cahill Center for Astronomy and Astrophysics, California Institute of Technology, USA), J. L. Richards(Department of Physics, Purdue University, USA), J. Sainio(Tuorla Observatory, University of Turku, Finland), D. N. Shakhovskoy(Crimean Astrophysical Observatory, Ukraine), K. V. Sokolovsky(Astro Space Center of Lebedev Physical Institute, 117997 Moscow, Russia), M. Tornikoski(Aalto University Metsähovi Radio Observatory, Finland), J. Tueller(Astrophysics Science Division, NASA Goddard Space Flight Center, USA), M. Weidinger(Theoretische Physik IV, Ruhr-Universität Bochum, Germany), J. Wilms(Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany), Anne Lähteenmäki Group, Aalto-yliopisto, Aalto University, Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Politecnico di Milano [Milan] (POLIMI), Universitá degli Studi dell’Insubria, Technische Universität Dortmund [Dortmund] (TU), IEEC-CSIC, Departamento de Ecología e Hidrología, Universidad de Murcia, Deutsches Elektronen-Synchrotron [Zeuthen] (DESY), Helmholtz-Gemeinschaft = Helmholtz Association, Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire d'études dynamiques et structurales de la sélectivité (LEDSS), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Departament d'Astronomia i Meteorologia [Barcelona] (DAM), Universitat de Barcelona (UB), Universita degli Studi di Padova, Universidad de Cantabria [Santander], Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) (MPI-P), Instituto de Biotecnología, Departamento de Biología Molecular de Plantas, UNAM, Institute for Physical Research (IPR), National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA), Netherlands Institute for Radio Astronomy (ASTRON), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), INAF-Cagliari Astronomical Observatory, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dept. of Physics, Institut de Ciencies del Cosmos (ICCUB), Kao Group, Centre de Recherches sur les Macromolécules Végétales (CERMAV), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Optoelectronic Research Centre, University of Southampton, Department of Chemistry, Oulu, INAF - Osservatorio Astronomico di Brera (OAB), Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Università degli Studi di Udine - University of Udine [Italie], Universita degli studi di Napoli 'Parthenope' [Napoli], Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Vecteurs - Infections tropicales et méditerranéennes (VITROME), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut de Recherche Biomédicale des Armées (IRBA), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), DAAA, ONERA, Université Paris Saclay (COmUE) [Meudon], ONERA-Université Paris-Saclay, University of Bath [Bath], Waves and Solitons LLC, 918 W. Windsong Dr., Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), J., Aleksić, L. A., Antonelli, P., Antoranz, M., Asensio, M., Backe, U., Barres de Almeida, J. A., Barrio, W., Bednarek, K., Berger, E., Bernardini, A., Biland, O., Blanch, R. K., Bock, A., Boller, S., Bonnefoy, G., Bonnoli, D., Borla Tridon, T., Bretz, E., Carmona, A., Carosi, D., Carreto Fidalgo, P., Colin, E., Colombo, J. L., Contrera, J., Cortina, L., Cossio, S., Covino, P., Da Vela, F., Dazzi, A., De Angeli, G., De Caneva, B., De Lotto, C., Delgado Mendez, M., Doert, A., Domínguez, D., Dominis Prester, D., Dorner, M., Doro, D., Eisenacher, D., Elsaesser, D., Ferenc, M. V., Fonseca, L., Font, C., Fruck, R. J., García López, M., Garczarczyk, D., Garrido Terrat, M., Gaug, G., Giavitto, N., Godinović, A., González Muñoz, S. R., Gozzini, A., Hadamek, D., Hadasch, A., Herrero, J., Hose, D., Hrupec, F., Jankowski, V., Kadeniu, S., Klepser, M. L., Knoetig, T., Krähenbühl, J., Krause, J., Kushida, A., La Barbera, D., Lela, E., Leonardo, N., Lewandowska, E., Lindfor, S., Lombardi, M., López, R., López Coto, A., López Orama, E., Lorenz, I., Lozano, M., Makariev, K., Mallot, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, B., Marcote, M., Mariotti, M., Martínez, J., Masbou, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, J., Moldón, A., Moralejo, P., Munar Adrover, D., Nakajima, A., Niedzwiecki, D., Nieto, K., Nilsson, N., Nowak, R., Orito, S., Paiano, M., Palatiello, D., Paneque, R., Paoletti, J. M., Parede, S., Partini, M., Persic, M., Pilia, F., Prada, P. G., Prada Moroni, E., Prandini, I., Puljak, I., Reichardt, R., Reinthal, W., Rhode, M., Ribó, J., Rico, S., Rügamer, A., Saggion, K., Saito, T. Y., Saito, M., Salvati, K., Satalecka, V., Scalzotto, V., Scapin, C., Schultz, T., Schweizer, S. N., Shore, A., Sillanpää, J., Sitarek, I., Snidaric, D., Sobczynska, F., Spanier, S., Spiro, V., Stamatescu, A., Stamerra, B., Steinke, J., Storz, S., Sun, T., Surić, L., Takalo, H., Takami, F., Tavecchio, P., Temnikov, T., Terzić, D., Tescaro, M., Teshima, O., Tibolla, D. F., Torre, T., Toyama, A., Treve, M., Uellenbeck, P., Vogler, R. M., Wagner, Q., Weitzel, F., Zandanel, R., Zanin, Longo, Francesco, F., Lucarelli, C., Pittori, S., Vercellone, D., Bastieri, C., Sbarra, E., Angelaki, L., Fuhrmann, I., Nestora, T. P., Krichbaum, A., Siever, J. A., Zensu, K. A., Antonyuk, W., Baumgartner, A., Berduygin, M., Carini, K., Cook, N., Gehrel, M., Kadler, Kovalev, Y. u. A., Y. Y., Kovalev, F., Krau, H. A., Krimm, A., Lähteenmäki, M. L., Lister, W., Max Moerbeck, M., Pasanen, A. B., Pushkarev, A. C. S., Readhead, J. L., Richard, J., Sainio, D. N., Shakhovskoy, K. V., Sokolovsky, M., Tornikoski, J., Tueller, M., Weidinger, J., Wilms, UAM. Departamento de Física Teórica, Universitá degli Studi dell’Insubria = University of Insubria [Varese] (Uninsubria), 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 Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Università degli Studi di Padova = University of Padua (Unipd), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), Université Joseph Fourier - Grenoble 1 (UJF)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Napoli 'Parthenope' = University of Naples (PARTHENOPE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut de Recherche Biomédicale des Armées [Brétigny-sur-Orge] (IRBA), Universitat Autònoma de Barcelona [Barcelona] (UAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universitat de València (UV), Helmholtz-Gemeinschaft, National Institute for Nuclear Physics (INFN), National Academy of Sciences of Armenia, The Netherlands Institute for Radio Astronomy (ASTRON), 7990-AA Dwingeloo, Netherlands, Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), INAF-OAB, and DAAA, ONERA, Université Paris Saclay [Meudon]

Subjects
galaxies [Gamma rays], Radiation mechanisms: non-thermal, Flux, Astrophysics, 01 natural sciences, LARGE-AREA TELESCOPE, law.invention, law, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], BL Lacertae objects: individual: 1ES 2344+514, MAGIC (telescope), 010303 astronomy & astrophysics, galaxies: active, BL Lacerae objects: individual: 1ES 2344+514, gamma rays: galaxies, X-rays: individuals: 1ES 2344+514, radiation mechanisms: non-thermal, ComputingMilieux_MISCELLANEOUS, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, ACTIVE GALACTIC NUCLEI, BL-LACERTAE OBJECTS, GAMMA-RAY EMISSION, SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS, SELF-COMPTON MODEL, X-RAY, LAC OBJECTS, RELATIVISTIC JETS, MARKARIAN 501, Gamma ray, non-thermal [radiation mechanisms], active [galaxies], astro-ph.CO, Spectral energy distribution, Electrónica, Física nuclear, Electricidad, Astrophysics - High Energy Astrophysical Phenomena, Flare, Astrophysics - Cosmology and Nongalactic Astrophysics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, galaxie [gamma rays], 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, Light curve, individual: 1ES 2344+514 [BL Lacertae objects], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], galaxies [gamma-rays], Space and Planetary Science, ddc:520, individuals: 1ES 2344+514 [X-rays], Fermi Gamma-ray Space Telescope
Abstract

Astronomy and Astrophysics 556 (2013): A67 reproduced with permission from Astronomy and Astrophysics, Context. BL Lacertae objects are variable at all energy bands on time scales down to minutes. To construct and interpret their spectral energy distribution (SED), simultaneous broad-band observations are mandatory. Up to now, the number of objects studied during such campaigns is very limited and biased towards high flux states. Aims.We present the results of a dedicated multi-wavelength study of the high-frequency peaked BL Lacertae (HBL) object and known TeV emitter 1ES 2344+514 by means of a pre-organised campaign. Methods.The observations were conducted during simultaneous visibility windows of MAGIC and AGILE in late 2008. The measurements were complemented by Metsähovi, RATAN-600, KVA+Tuorla, Swift and VLBA pointings. Additional coverage was provided by the ongoing long-term F-GAMMA and MOJAVE programs, the OVRO 40-m and CrAO telescopes as well as the Fermi satellite. The obtained SEDs are modelled using a one-zone as well as a self-consistent two-zone synchrotron self-Compton model. Results. 1ES 2344+514 was found at very low flux states in both X-rays and very high energy gamma rays. Variability was detected in the low frequency radio and X-ray bands only, where for the latter a small flare was observed. The X-ray flare was possibly caused by shock acceleration characterised by similar cooling and acceleration time scales. MOJAVE VLBA monitoring reveals a static jet whose components are stable over time scales of eleven years, contrary to previous findings. There appears to be no significant correlation between the 15 GHz and R-band monitoring light curves. The observations presented here constitute the first multi-wavelength campaign on 1ES 2344+514 from radio to VHE energies and one of the few simultaneous SEDs during low activity states. The quasi-simultaneous Fermi-LAT data poses some challenges for SED modelling, but in general the SEDs are described well by both applied models. The resulting parameters are typical for TeV emitting HBLs. Consequently it remains unclear whether a so-called quiescent state was found in this campaign, The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence “Origin and Structure of the Universe”, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The AGILE Mission is funded by the Italian Space Agency (ASI), with scientific and programmatic participation by the Italian Institute of Astrophysics (INAF) and the Italian Institute of Nuclear Physics (INFN). Research partially supported through the ASI grants no. I/089/06/2 and I/042/10/0. The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A.Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged

Published
2013
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16. SPECTRAL VARIABILITY OF THE UNUSUAL SOUTHERN Be STAR HD 152478

Author

Pogodin, M. A.; Pulkovo Observatory, St. Petersburg 196140, Russia, Drake, N. A., Jilinski, E. G., Ortega, V. G., de la Reza, R., Pogodin, M. A.; Pulkovo Observatory, St. Petersburg 196140, Russia, Drake, N. A., Jilinski, E. G., Ortega, V. G., and de la Reza, R.

Abstract

We present results of the spectroscopic investigationof the unusual southern Be star HD 152478. Fiveechelle high-resolution spectra of the object wereobtained in 2007 - 2009 with the FEROS spectrographmounted at the 2.2 m telescope of the European Southern Observatory (La Silla, Chile). The star exhibitsa specific remarkable variability of the numerous lineprofilesofsuchelementsasHi,Hei,Feii,etc. Theanalysis of the spectral behaviour of the object hasshown that the assumption of global oscillations inthe rotating equatorial gaseous disk is not confirmedby the observations. The alternative hypothesis of avariable magnetized stellar wind of flattened geometryflowing close to the equatorial disk can qualitativelyexplain the observed profile variations.

Published
2010

19. Massive evaluation and analysis of Poincar�� recurrences on grids of initial data: a tool to map chaotic diffusion

Author

Guillaume Rollin, A. V. Melnikov, Ivan I. Shevchenko, José Lages, Pulkovo Observatory, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), and Lehrstuhl für Angewandte Festkörperphysik

Subjects
Dynamical systems theory, Computer science, Chaotic, General Physics and Astronomy, FOS: Physical sciences, Lyapunov exponent, 01 natural sciences, 010305 fluids & plasmas, Hamiltonian system, symbols.namesake, Simple (abstract algebra), 0103 physical sciences, Applied mathematics, Diffusion (business), 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), ComputingMilieux_MISCELLANEOUS, Earth and Planetary Astrophysics (astro-ph.EP), Numerical analysis, Nonlinear Sciences - Chaotic Dynamics, Hardware and Architecture, Bounded function, symbols, Chaotic Dynamics (nlin.CD), Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a novel numerical method aimed to characterize global behaviour, in particular chaotic diffusion, in dynamical systems. It is based on an analysis of the Poincar\'e recurrence statistics on massive grids of initial data or values of parameters. We concentrate on Hamiltonian systems, featuring the method separately for the cases of bounded and non-bounded phase spaces. The embodiments of the method in each of the cases are specific. We compare the performances of the proposed Poincar\'e recurrence method (PRM) and the custom Lyapunov exponent (LE) methods and show that they expose the global dynamics almost identically. However, a major advantage of the new method over the known global numerical tools, such as LE, FLI, MEGNO, and FA, is that it allows one to construct, in some approximation, charts of local diffusion timescales. Moreover, it is algorithmically simple and straightforward to apply., Comment: 26 pages, 4 figures. Accepted for publication in Computer Physics Communications

Published
2019
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20. Kepler map

Author

Ivan Shevchenko, Dima Shepelyansky, José Lages, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Laboratoire de Physique Théorique (LPT), Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Pulkovo Observatory, Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3)

Subjects
Marketing, Pharmacology, [PHYS]Physics [physics], Organizational Behavior and Human Resource Management, Strategy and Management, 0103 physical sciences, Drug Discovery, Pharmaceutical Science, 010306 general physics, 010303 astronomy & astrophysics, 01 natural sciences, ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2018
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21. Chaotic zones around rotating small bodies

Author

Ivan I. Shevchenko, José Lages, Dima L. Shepelyansky, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Information et Chaos Quantiques (LPT), Laboratoire de Physique Théorique (LPT), Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Pulkovo Observatory, Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées, Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse)

Subjects
Solar System, 010504 meteorology & atmospheric sciences, Chaotic, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, Orbital mechanics, Rotation, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Nonlinear Sciences - Chaotic Dynamics, Breakup, Celestial mechanics, Swell, Space and Planetary Science, Asteroid, [NLIN.NLIN-CD]Nonlinear Sciences [physics]/Chaotic Dynamics [nlin.CD], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Chaotic Dynamics (nlin.CD), Astrophysics - Earth and Planetary Astrophysics
Abstract

Small bodies of the Solar system, like asteroids, trans-Neptunian objects, cometary nuclei, planetary satellites, with diameters smaller than one thousand kilometers usually have irregular shapes, often resembling dumb-bells, or contact binaries. The spinning of such a gravitating dumb-bell creates around it a zone of chaotic orbits. We determine its extent analytically and numerically. We find that the chaotic zone swells significantly if the rotation rate is decreased, in particular, the zone swells more than twice if the rotation rate is decreased ten times with respect to the "centrifugal breakup" threshold. We illustrate the properties of the chaotic orbital zones in examples of the global orbital dynamics about asteroid 243 Ida (which has a moon, Dactyl, orbiting near the edge of the chaotic zone) and asteroid 25143 Itokawa., Comment: 14 pages, 7 figures, accepted for publication in The Astronomical Journal

Published
2017
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22. The WEBT campaign on the BL Lac object PG 1553+113 in 2013. An analysis of the enigmatic synchrotron emission

Author

Sh. A. Ehgamberdiev, A. Strigachev, Merja Tornikoski, V. T. Doroshenko, Sofia O. Kurtanidze, Joni Tammi, N. V. Efimova, J. A. Acosta-Pulido, Paolo Leto, P. A. González-Morales, Lorand A. Sigua, Antonio Stamerra, Sergio Velasco, V. Ramakrishnan, O. M. Kurtanidze, Valeri M. Larionov, Goran Damljanović, J. M. Ohlert, Evgeni Semkov, D. O. Mirzaqulov, A. A. Mokrushina, V. Bozhilov, M. I. Carnerero, Erika Benítez, S. A. Klimanov, Ivan S. Troitsky, M. J. Arévalo, C. M. Raiteri, T. S. Grishina, Evgeni Ovcharov, Yu. V. Troitskaya, D. Carosati, Anne Lähteenmäki, Carla Buemi, Arkady A. Arkharov, A. C. Sadun, Marcello Giroletti, Sunay Ibryamov, Elena G. Larionova, R. Bachev, O. Vince, David Hiriart, G. Markovic, Alexander Kurtenkov, G. A. Borman, E. N. Kopatskaya, Corrado Trigilio, E. Prandini, G. Umana, A. B. Grinon-Marin, D. A. Morozova, R. A. Chigladze, M. G. Nikolashvili, P. Calcidese, A. Pastor Yabar, S. V. Nazarov, Raúl Mújica, C. Lázaro, S. Paiano, M. Villata, A. Di Paola, L. V. Larionova, INAF - Osservatorio Astrofisico di Torino, INFN, Isaac Newton Institute of Chile, St Petersburg Branch, University of La Laguna, Pulkovo Observatory, Bulgarian Academy of Sciences, Universidad Nacional Autónoma de México, University of Sofia 'St. Kliment Ohridski', Crimean Astrophysical Observatory, INAF, Osservatorio Astrofisico di Catania, Osservatorio Astronomico della Regione Autonoma Valle d'Aosta, Fundación Galileo Galilei - INAF, Abastumani Observatory, Astronomical Observatory, INAF - Osservatorio Astronomico di Roma, Lomonosov Moscow State University, Ulugh Beg Astronomical Institute, Maidanak Observatory, INAF Istituto di Radioastronomia, St. Petersburg State University, Engelhardt Astronomical Observatory, Kazan Federal University, Department of Radio Science and Engineering, University of Belgrade, Instituto Nacional de Astrofísica, Óptica y Electrónica, Michael Adrian Observatory, INAF, Osservatorio Astronomico di Padova, ISDC, Science Data Center for Astrophysics, Metsähovi Radio Observatory, University of Colorado Denver, Aalto-yliopisto, and Aalto University

Subjects
Brightness, Cosmic Origins Spectrograph, Astrophysics::High Energy Astrophysical Phenomena, ta221, ta1171, FOS: Physical sciences, active, BL Lacertae objects: general, BL Lacertae objects: individual: PG 1553+113 [Galaxies], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, BL Lacertae objects: individual: PG 1553+113, BL Lacertae objects: individual:PG 1553+113, Spectral line, law.invention, Radio telescope, Telescope, law, ta216, Blazar, Astrophysics::Galaxy Astrophysics, individual: PG 1553+113 [BL Lacertae objects], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), ta115, ta213, ta114, general [BL Lacertae objects], Astronomy, Astronomy and Astrophysics, Galaxies: active, Space and Planetary Science, Astrophysics - Astrophysics of Galaxies, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena, BL Lac object
Abstract

Monthly Notices of the Royal Astronomical Society, 454 (1), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711

Published
2015

23. The ICRF-3: Status, plans, and progress on the next generation International Celestial Reference Frame

Author

Malkin, Z., Jacobs, Carolyn, Arias, F., Boboltz, D., Böhm, J., Bolotin, S., Bourda, G., Charlot, P., de Witt, A., Fey, A., Gaume, R., Gordon, D., Heinkelmann, R., Lambert, S., Ma, C., Nothnagel, A., Seitz, M., Skurikhina, E., Souchay, J., Titov, O., Pulkovo Observatory, Laboratoire Génie électrique et électronique de Paris (GeePs), Centre National de la Recherche Scientifique (CNRS)-CentraleSupélec-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université Paris-Sud - Paris 11 (UP11), Atominstitut [Wien], Technische Universität Wien (TU Wien), M2A 2015, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Chimie Appliquée de l'État Solide (LCAES), Ecole Nationale Supérieure de Chimie de Paris- Chimie ParisTech-PSL (ENSCP)-Centre National de la Recherche Scientifique (CNRS), Paris-Jourdan Sciences Economiques (PSE), École normale supérieure - Paris (ENS Paris)-Institut National de la Recherche Agronomique (INRA)-École des hautes études en sciences sociales (EHESS)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS), Paris School of Economics (PSE), Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS), Vienna University of Technology (TU Wien), Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut National de la Recherche Agronomique (INRA)-École des hautes études en sciences sociales (EHESS)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS), École des Ponts ParisTech (ENPC)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris 1 Panthéon-Sorbonne (UP1)-Centre National de la Recherche Scientifique (CNRS)-École des hautes études en sciences sociales (EHESS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), École normale supérieure - Paris (ENS-PSL), Université Paris 1 Panthéon-Sorbonne (UP1)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École des hautes études en sciences sociales (EHESS)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), relativity, geopotential, Earth rotation, FOS: Physical sciences, astrometry, reference systems, ephemerides, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), time, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

International audience; The goal of this presentation is to report the latest progress in creation of the next generation of VLBI-based International Celestial Reference Frame, ICRF3. Two main directions of ICRF3 development are improvement of the S/X-band frame and extension of the ICRF to higher frequencies. Another important task of this work is the preparation for comparison of ICRF3 with the new generation optical frame GCRF expected by the end of the decade as a result of the Gaia mission.

Published
2015

24. The ICRF-3: Status, Plans, and Progress on the next generation Celestial Reference Frame

Author

Jacobs, Christopher S., Arias, F., Boboltz, D., Boehm, J., Bolotin, S., Bourda, G., Charlot, P., de Witt, A., Fey, A., Gaume, R., Gordon, D., Heinkelmann, R., Kudobov, S., Lambert, S., Ma, C., Malkin, Z., Nothnagel, A., Seitz, M., Skurikhina, E., Souchay, J., Titov, O., Supélec Sciences des Systèmes [Gif-sur-Yvette] (E3S), SUPELEC, M2A 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Laboratoire de Chimie Appliquée de l'État Solide (LCAES), Ecole Nationale Supérieure de Chimie de Paris- Chimie ParisTech-PSL (ENSCP)-Centre National de la Recherche Scientifique (CNRS), Flinders Medical Centre, Paris-Jourdan Sciences Economiques (PSE), École normale supérieure - Paris (ENS Paris)-Institut National de la Recherche Agronomique (INRA)-École des hautes études en sciences sociales (EHESS)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS), Paris School of Economics (PSE), Laboratoire de synthèse organique (DCSO), École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Pulkovo Observatory, Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Supélec Sciences des Systèmes (E3S), Ecole Supérieure d'Electricité - SUPELEC (FRANCE), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), 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)-Institut National de la Recherche Agronomique (INRA)-École des hautes études en sciences sociales (EHESS)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS), Université Paris 1 Panthéon-Sorbonne (UP1)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École des hautes études en sciences sociales (EHESS)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), École polytechnique (X)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), École des Ponts ParisTech (ENPC)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris 1 Panthéon-Sorbonne (UP1)-Centre National de la Recherche Scientifique (CNRS)-École des hautes études en sciences sociales (EHESS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)

Subjects
ICRF-3, ICRF, S/X-band, Gaia, astrometry, quasar, Celestial Reference Frame, K-band, interferometry, AGN, VLBI, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], X/Ka-band
Abstract

International audience; ICRF-3 seeks to improve upon the highly successful ICRF-2. Our goals are to improve the precision, spatial and frequency coverage relative to the ICRF-2 by 2018. This date is driven by the desire to create radio frames that are ready for comparison with the Gaia optical frame. Several specific actions are underway. A collaboration has started to improve at S/X-band precision of the VLBA Calibrator Survey's 2000+ sources which are typically 5 times less precise than the rest of the ICRF-2. S/X-band southern precision improvements are planned from observations with southern antennas such as the AuScope and HartRAO, S. Africa. We seek to improve radio frequency coverage with X/Ka and K-band work. An X/Ka frame of 631 sources now has full sky coverage from the addition of a 2nd southern station in Argentina which should strengthen the southern hemisphere in general. A K-band collaboration has formed with similar coverage and southern precision goals. On the analysis front, special attention will be given to combination techniques both of VLBI catalogs and of multiple data types. Consistency of the CRF with the TRF and EOP is another area of concern. Finally, work is underway to identify and pinpoint sources bright enough in both radio and optical to allow for a robust frame tie between VLBI and Gaia optical frames.

Published
2014

25. The ICRF3 Roadmap to the next generation International Celestial Reference Frame

Author

Jacobs, Christopher S., Arias, F., Boboltz, D., Boehm, J., Bolotin, S., Bourda, G., Charlot, P., de Witt, A., Fey, A., Gaume, R., Gordon, D., Heinkelmann, R., Lambert, S., Ma, C., Malkin, Z., Nothnagel, A., Seitz, M., Skurikhina, E., Souchay, J., Titov, O., Supélec Sciences des Systèmes (E3S), Ecole Supérieure d'Electricité - SUPELEC (FRANCE), M2A 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Laboratoire de Chimie Appliquée de l'État Solide (LCAES), Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Flinders Medical Centre, Erosion torrentielle neige et avalanches (UR ETGR (ETNA)), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Pulkovo Observatory, Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Supélec Sciences des Systèmes [Gif-sur-Yvette] (E3S), SUPELEC, Ecole Nationale Supérieure de Chimie de Paris- Chimie ParisTech-PSL (ENSCP)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB)

Subjects
ICRF-3, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], S/X-band, astrometry, quasar, Active Galactic Nuclei, Celestial Reference Frame, K-band, VLBI, X/Ka-band, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; We propose a 3rd generation radio-based International Celestial Reference Frame (ICRF-3) to improve upon the highly successful ICRF-2. Our goals are to improve the precision, spatial and frequency coverages relative to the ICRF-2 by 2018. This date is driven by the desire to create radio frames early enough to test the Gaia optical frame during its construction. Several specific actions are underway. A collaboration has been started to improve S/X-band precision of the 2000+ VLBA Calibrator Survey sources which are typically 5 times less precise than the rest of the ICRF-2. S/X-band southern precision improvements are planned from observations with southern antennas such as the AuScope and HartRAO, S. Africa. We seek to improve radio frequency coverage with X/Ka and K- band work. An X/Ka frame of 631 sources now has full sky coverage from the addition of a 2nd southern station in Argentina which should strengthen the southern hemisphere in general. A K-band collaboration has formed with similar coverage and southern precision goals. On the analysis front, special attention will be given to combination techniques both of VLBI catalogs and of multiple data types (e.g. VLBI+GPS). Finally, work is underway to identify and pinpoint sources bright enough in both radio and optical to allow for a robust frame tie between VLBI and Gaia optical frames.

Published
2014

26. Results of reduction of photographic plates taken with 26-inch refractor in Pulkovo observatory

Author

Kiselev, Aleksej Alekseevich, Kiyaeva, Olga V., Romanenko, Ludmila G., Shakht, Natalia A., Kalinichenko, Olga A., Vasilkova, Olga O., Vasileva, T. A., Poliakow, Eugene V., Institut De Mécanique Céleste Et De Calcul Des Éphémérides, Observatoire De Paris, IMCCE, Pulkovo Observatory, and Russian Academy of Sciences [Moscow] (RAS)

Subjects
[PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

Program available at: http://www.imcce.fr/hosted_sites/naroo/program.html; Photographic observations with 26-inch Zeiss refractor in Pulkovo were carried out since 1956 year. Though the production of photo plates was terminated in 90-s, the reserve of old plates was used to continue photographic observations till 2007 year along with CCD observations (started in 1995). Having about 8000 photographic plates measured with three type devices, we made an attempt to compare the accuracies of the measurements. The plates contain the images of more than 300 double and multiple stars from Pulkovo double star catalog. It should be noted that the analysis of measurement precision for different machines is more reliable in the case of double stars, where we measure the relative positions of double star components. Then the measurement system is determined only by the direction of diurnal trail and scale of the instrument, and the errors of measurements refl ect only the peculiarities of astroclimate, precision of measuring machine and the methods of measurement and processing. The errors of positions and movements of the reference stars are excluded, otherwise they could absorb the fi ne effects of comparison, especially when deal with long-term series of observations.

Published
2013

27. The ICRF-3: Proposed Roadmap to the Next Generation International Celestial Reference Frame

Author

Jacobs, Christopher S., Arias, F., Boehm, J., Bolotin, S., Bourda, G., Charlot, P., de Witt, A., Fey, A., Gaume, R., Gordon, D., Heinkelmann, R., Kurdubov, S., Lambert, S., Ma, C., Malkin, Z., Nothnagel, A., Seitz, M., Skurikhina, E., Souchay, J., Titov, O., M2A 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Laboratoire de Chimie Appliquée de l'État Solide (LCAES), Ecole Nationale Supérieure de Chimie de Paris- Chimie ParisTech-PSL (ENSCP)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Institute of Geodesy and Geophysics (IGG), Technische Universität Wien (TU Wien), Erosion torrentielle neige et avalanches (UR ETGR (ETNA)), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Pulkovo Observatory, Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Vienna University of Technology (TU Wien), Supélec Sciences des Systèmes [Gif-sur-Yvette] (E3S), SUPELEC, M2A 2014, Flinders Medical Centre, Paris-Jourdan Sciences Economiques (PSE), École normale supérieure - Paris (ENS Paris)-Institut National de la Recherche Agronomique (INRA)-École des hautes études en sciences sociales (EHESS)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS), Paris School of Economics (PSE), Laboratoire de synthèse organique (DCSO), École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Supélec Sciences des Systèmes (E3S), Ecole Supérieure d'Electricité - SUPELEC (FRANCE), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut National de la Recherche Agronomique (INRA)-École des hautes études en sciences sociales (EHESS)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS), École des Ponts ParisTech (ENPC)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris 1 Panthéon-Sorbonne (UP1)-Centre National de la Recherche Scientifique (CNRS)-École des hautes études en sciences sociales (EHESS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), École polytechnique (X)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), École normale supérieure - Paris (ENS-PSL), Université Paris 1 Panthéon-Sorbonne (UP1)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École des hautes études en sciences sociales (EHESS)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)

Subjects
ICRF-3, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], ICRF, S/X-band, Gaia, Active Galactic Nuclei, Celestial Reference Frame, frame tie, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], astrometry, quasar, K-band, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], VLBI, X/Ka-band
Abstract

International audience; ICRF-3 seeks to improve upon the highly successful ICRF-2. Our goals are to improve the precision, spatial and frequency coverage relative to the ICRF-2 by 2018. This date is driven by the desire to create radio frames that are ready for comparison with the Gaia optical frame.Several specific actions are underway. A collaboration has started to improve at S/X-band precision of the VLBA Calibrator Survey's ~2200 sources which are typically 5 times less precise than the rest of the ICRF-2. S/X-band southern precision improvements are underway with observations using southern antennas such as the AuScope and HartRAO, S. Africa.We also seek to improve radio frequency coverage with X/Ka and K-band work. An X/Ka frame of 654 sources now has full sky coverage from the addition of a 2nd southern station in Argentina which should strengthen the southern hemisphere in general. A K-band collaboration has formed with similar coverage and southern precision goals.On the analysis front, special attention is being given to combination techniques both of VLBI frames and of multiple data types. Consistency of the CRF with the TRF and EOP is another area of concern. Comparison of celestial frame solutions from various groups is underway in order to identify and correct systematic errors.Finally, work is underway to identify and pinpoint sources bright enough in both radio and optical to allow for a robust frame tie between VLBI and Gaia optical frames.

Published
2013

28. The ICRF-3: A Proposed Roadmap to the Next Generation International Celestial Reference Frame

Author

Heinkelmann, Robert, Jacobs, Christopher S., Arias, F., Boboltz, D., Boehm, J., Bolotin, S., Bourda, G., Charlot, P., De Witt, A., Fey, A., Gaume, R., Gordon, D., Lambert, S., Ma, C., Malkin, Z., Nothnagel, A., Seitz, M., Skuikhina, E., Souchay, J., Titov, O., M2A 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Laboratoire de Chimie Appliquée de l'État Solide (LCAES), Ecole Nationale Supérieure de Chimie de Paris- Chimie ParisTech-PSL (ENSCP)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Erosion torrentielle neige et avalanches (UR ETGR (ETNA)), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Pulkovo Observatory, Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB)

Subjects
ICRF-3, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], ICRF, S/X-band, astrometry, quasar, Active Galactic Nuclei, Celestial Reference Frame, K-band, VLBI, X/Ka-band, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; The International Celestial Reference Frame's current realization, the ICRF-2 (Ma et al, 2009), has the potential to be improved in several ways. In order to achieve this potential in time for comparisons with ESA's optical Gaia mission, the IAU has formed the ICRF-3 working group with the goal of producing the next generation ICRF by its 2018 General Assembly. With Gaia aiming for sub-100 μas precision for quasars in its frame, our goal for the ICRF-3 is to achieve sub-100 μas precision in the radio for as many sources at as many observing bands as possible. This talk will review the intiatives underway which collectively form our roadmap for achieving these goals. VCS-II: Noting that ~2/3 of the ICRF-2's 3414 sources have been observed in only 1 or 2 sessions (mostly the VLBA Calibrator Survey (VCS)) which produced median precisions of 620/ 1120 μas in RAcosDec/ Dec, respectively, we have instigated a collaboration to re-observe the VCS sources using modern systems which are 5 times more sensitive than the original VCS system. This will allow the VCS sources to have precision more nearly comparable to the other ICRF sources. High Frequency radio: Noting that comparison of radio frame to the Gaia optical frame will require an accurate undersanding of frequency dependent changes in source morphology (source structure) and frequency dependent opacity effects (core shift), we are encouraging the construction of 100 μas precision radio frames at multple radio frequencies such as X/Ka (8.4/32 Ghz), K-band (~24 GHz) and Q-band (43 GHz). Southern coverage: Noting that all current radio frames have poorer spatial covereage and precision in the southern hemisphere, we are encouraging increased astrometric observations from the southern hemisphere. Observations using stations from Australia, South Africa, and Argentina are currently being organized. Frame consistency: Noting that Celestial Reference Frames are often used in combination with other frames such as the planetary emphemeris, the Earth Orientation Parameters (EOP), and the International Terrestrial Reference Frame (ITRF) which are of keen interest to geodesists and planetary scientists, a key ICRF-3 goal is to maintain and improve consistency with these other frames. This component of the work will study various combination techniques such as multi-technique data combinations for EOPs and TRFs, combined radio frames, and various modelling improvements such as galactic abberration.

Published
2013

29. Challenges and Perspectives for TRF and CRF Determination

Author

Böhm, J., Malkin, Z., Lambert, Sébastien, Ma, C., Department of Geodesy and Geoinformation, Research Group Remote Sensing, Vienna University of Technology, Pulkovo Observatory, Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Systèmes de référence célestes, Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, Behrend, D., Baver, and K. D.

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; The improved and consistent determination of terrestrial and celestial reference frames has been the subject of many studies in the past and --- due to technological innovations and new planned missions --- is a topic of immediate interest today. We present and discuss challenges and perspectives which are tackled within three working groups of Sub-Commission 1.4 on the Interaction of Celestial and Terrestrial Reference Frames within the International Association of Geodesy (IAG), covering improved geophysical and astronomical models, rigorous combination strategies of space geodetic observations, new observation scenarios with radio telescopes to satellites, or the implication of the GAIA mission for the celestial reference frame.

Published
2012

30. The Connection between the Radio Jet and the γ-ray Emission in the Radio Galaxy 3C 120 and the Blazar CTA 102

Author

Andrea Di Paola, Alan P. Marscher, Vladimir A. Hagen-Thorn, Ivan S. Troitsky, Ivan Agudo, Vishal Bala, Ryosuke Itoh, Clemens Thum, Tuomas Savolainen, Sergey G. Sergeev, Paul S. Smith, Sol N. Molina, Evgenia N. Kopatskaya, Svetlana G. Jorstad, Paola Grandi, Merja Tornikoski, G. A. Borman, L. V. Larionova, José L. Gómez, Elena G. Larionova, Arkady A. Arkharov, Brian W. Taylor, T. S. Grishina, Carolina Casadio, Anne Lähteenmäki, Helmut Wiesemeyer, Matthew L. Lister, Elizaveta Rastorgueva-Foi, Mark Gurwell, Yuri Y. Kovalev, Valeri M. Larionov, Alexander B. Pushkarev, Dmitry A. Blinov, Karen E. Williamson, Manasvita Joshi, Daria A. Morozova, Max-Planck-Institut für Radioastronomie, CSIC, Boston University, Istituto Nazionale Astrofisica, St. Petersburg State University, Purdue University, University of Arizona, Harvard-Smithsonian Center for Astrophysics, Metsähovi Radio Observatory, Pulkovo Observatory, Crimean Astrophysical Observatory, INAF, Osservatorio Astronomico di Roma, Hiroshima University, Instituto de Radio Astronomia Milimétrica, Department of Radio Science and Engineering, Aalto-yliopisto, and Aalto University

Subjects
galaxies: active, galaxies: radio continuum, galaxies: jets, lcsh:Astronomy, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, lcsh:QB1-991, X-shaped radio galaxy, 0103 physical sciences, Very-long-baseline interferometry, Blazar, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, ta115, Line-of-sight, Superluminal motion, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, CTA-102
Abstract

We present multi-wavelength studies of the radio galaxy 3C 120 and the blazar CTA 102 during unprecedented γ-ray flares for both sources. In both studies the analysis of γ-ray data has been compared with a series of 43 GHz VLBA images from the VLBA-BU-BLAZAR program, providing the necessary spatial resolution to probe the parsec scale jet evolution during the high energy events. To extend the radio dataset for 3C 120 we also used 15 GHz VLBA data from the MOJAVE sample. These two objects which represent very different classes of AGN, have similar properties during the γ-ray events. The γ-ray flares are associated with the passage of a new superluminal component through the mm VLBI core, but not all ejections of new components lead to γ-ray events. In both sources γ-ray events occurred only when the new components are moving in a direction closer to our line of sight. We locate the γ-ray dissipation zone a short distance from the radio core but outside of the broad line region, suggesting synchrotron self-Compton scattering as the probable mechanism for the γ-ray production.

Published
2016
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31. Astrometric results of observations of mutual occultations and eclipses of the Saturnian satellites in 2009

Author

D. L. Gorshanov, O. Dechambre, Ricard Casas, A. Sergeev, A. Murphy, Brian Loader, G. Dourneau, F. Colas, A. Kurenya, A. Farmakopoulos, Marcelo Assafin, V. Kozlov, Julio Camargo, J. F. Le Campion, A. Dias-Oliveira, P. Valdes Sada, D. N. da Silva Neto, V. Tsamis, X. Zhang, D. Gault, J. Lecacheux, N. V. Emelyanov, Dave Herald, Apostolos A. Christou, Felipe Braga-Ribas, A. Massalle, R. Vieira-Martins, Jean-Eudes Arlot, T. George, N. Parakhin, Maksim V. Andreev, C. Schnabel, Valery Lainey, Alexandre Roman-Lopes, M. Mc Brien, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatório do Valongo/UFRJ [Rio de Janeiro], Universidade Federal do Rio de Janeiro (UFRJ), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatorio Nacional/MCT, Observatório Nacional/MCT, Observatório do Valongo, Universidade Federal do Rio de Janeiro Ladeira do Pedro Antônio, Universidade Estadual da Zona Oeste (UEZO), Universidade Estadual da Zona Oeste, M2A 2012, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), International Occulting and Timing Association (IOTA), International Occulting and Timing Association, Pulkovo Observatory, Russian Academy of Sciences [Moscow] (RAS), Canberra Astronomical Society, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB)

Subjects
010504 meteorology & atmospheric sciences, planets and satellites: dynamical evolution and stability, Context (language use), Ephemeris, 01 natural sciences, Geocentric coordinates, Photometry (optics), 0103 physical sciences, occultations, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrometry, Position angle, Light curve, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, astrometry, Astrophysics::Earth and Planetary Astrophysics, Right ascension, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs
Abstract

Context. The photometry of mutual occultations and eclipses of natural planetary satellites can be used to infer very accurate astrometric data. This can be achieved by processing the light curves of the satellites observed during international campaigns of photometric observations of these mutual events. Aims. This work focuses on processing the complete database of photometric observations of the mutual occultations and eclipses of the Uranian satellites made during the international campaign in 2007. The final goal is to derive new accurate astrometric data. Methods. We used an accurate photometric model of mutual events that explicitly depends on parameters that these accurate observations should be sensitive to, including the albedos of the satellites. Our original method is applied to derive astrometric data in relative positions from photometric observations of mutual occultations and eclipses of the Uranian satellites. Results. We process the 41 light-curves obtained during the international campaign of photometric observations of the Uranian satellites in 2007. The root-mean-square (rms) of the residuals “observations minus calculations” (O‐C) with respect to theory for the best 34 observations are equal to 10.3 and 17.7 mas in right ascension and declination, respectively. For five observations only the position angle was derived. Topocentric or heliocentric angular differences for satellites pairs were obtained from 25 central instant offsets between observation and theory during the time period from May 4, 2007 to January 4, 2008. Conclusions. The rms of the residuals is from 10 to 20 mas that corresponds in situ to 10 to 20 km. These mutual event observations appear to be the most accurate astrometric ground-based observations of the major Uranian satellites to-date and should be used for dynamical purposes.

Published
2012
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32. Observations of Asteroids in International Scientific Optical Network

Author

Krugly, Yurij, Molotov, Igor, Agapov, Vladimir, Elenin, L., Gaftonyuk, Ninel, Kouprianov, Vladimir, Minikulov, Nasredin, Gulyamov, Makhmud, Abdulloev, Safarali, Donchev, Z., Ivanova, Violeta, Sergeev, A. V., Burkhonov, O. A., Ehgamberdiev, Sh. A., Rumyantsev, V. V., Inasaridze, R. Ya., Ivashchenko, Yuri, Satovskiy, B., Сappelletti, Chantal, Baransky, A., Dorokhov, N.I., Institute of Astronomy [Kharkiv], V.N. Karazin Kharkiv National University (KhNU), Keldysh Institute of Applied Mathematics, Russian Academy of Sciences [Moscow] (RAS), Crimean Astrophysical Observatory (CrAO), Pulkovo Observatory, Institute of Astrophysics [Tadjikistan], Academy of Sciences of the Republic of Tajikistan, Institute of Astronomy, Bulgarian Academy of Sciences (BAS), Ulugh Beg Astronomical Institute, Uzbekistan Academy of Sciences, Abastumani Astrophysical Observatory, Ilia State University [Tbilisi], Andrushivka Astronomical Observatory, Astrotel Observatory, Kazan State University (KPFU), Gruppo di Astrodinamica, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Astronomical Observatory of Kiev, Taras Shevchenko National University of Kyiv, Astronomical observatory of Odessa National University [Odessa], Odessa National I.I.Mechnikov University, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), and Gaia Fun-SSO

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
Abstract

4 p.; International audience; The International Scientific Optical Network (ISON) was established in 2004 to carry out regular monitoring of the population of artificial objects at high altitude orbits (mainly GEO). Now the network joins 23 observatories in 10 countries, which are located at different longitudes and latitudes of the globe (Molotov et al., 2009). Since 2006 the photometric observations of asteroids has been started in frame of ISON to increase the network scientific output. The main targets of these observations are near-Earth asteroids (NEAs) as hazardous objects pose a threat for the Earth civilization. The observations are aimed to investigate physical properties of the asteroids and astrometric positions. The network is also involved into projects on searching binary asteroids, support of asteroid radar research and investigation of the YORP effect. In last two years the project was also directed to be involved in follow-up and discovery asteroids and comets, especially NEAs in frame of the Asteroid Hazard problem. Capabilities of our network to obtain astrometry and photometric data can be used in frame of the project GAIA for doing observations of newly discovered asteroids and comets.

Published
2010

33. Modern Observations of Solar Systems Bodies on 65 cm Pulkovo's Refractor

Author

Shakht, N. A., Kiselev, A. A., Bykov, O. P., Grosheva, E. A., Izmailov, I. S., Kiyaeva, O. V., L'Vov, V. N., Romanenko, L. G., Tsekmejster, S. D., Pulkovo Observatory, Russian Academy of Sciences [Moscow] (RAS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Gaia Fun-SSO, and Institut De Mécanique Céleste Et De Calcul Des Éphémérides, Observatoire De Paris

Subjects
[PHYS.ASTR.SR] Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]
Abstract

4 p.; International audience; Photographic observations of Solar system bodies started at Pulkovo since the end of XIX century. CCD-observations have been carried out with 65cm Zeiss refractor at Pulkovo since 1995. In 2007 the telescope was equipped with the CCD camera FLI Pro Line 09000 (field of view is 12×12 arcmin). In this paper we report about CCD observations of Solar system bodies with a 65-cm refractor at present. The accuracy estimations of observed positions and the used methods of detrmination of preliminary orbits are presented.

Published
2010

34. The PHEMU03 catalogue of observations of the mutual phenomena of the Galilean satellites of Jupiter

Author

J. P. Coquerel, J. Gerbos, T. P. Kiseleva, G. Pizzetti, T. N. Dorokhova, J. Cuypers, M. Appakutty, M. Michelli, E. Lo Savio, F. Salvaggio, D. Fiel, P. Sarlin, D. Parrat, V. Turcu, C. Cremaschini, G. Selvakumar, J. Vidal-Sainz, S. Sorescu, A. V. Devyatkin, A. Dumitrescu, S. Foglia, R. Vasundhara, M. Harrington, V. G. Tejfel, M. Lou, I. S. Izmailov, N. Baron, P. Rapavy, G. Marino, B. Ramachandran, S. Montagnac, E. Lellouch, Michel Dennefeld, Ch. Ruatti, P. Anbazhagan, Apostolos A. Christou, A. Amossé, J. M. Nier, I. Stellmacher, D. Ferrara, A. Ahmad, P. Vingerhoets, Benoît Noyelles, J. Kieken, N. Emelianov, K. Kuppuswamy, A. Fienga, R. M. D. Goncalves, D. Gonzales, A. K. Venkataramana, W. Marinello, D. Buettner, T. Flatres, R. Casas, T. Noel, W. Vollman, David Asher, J.-J. Sacré, J. F. Le Campion, Valery Lainey, M. Berthe, C. Sciuto, Z. L. Li, S. Yu. Gorda, V. Moorthy, P. Vantyghem, P. Lazzarotti, V. Ivanova, R. Bogdanovski, E. Magny, M. Yu. Khovritchev, M. Andreyev, D. Crussaire, T. R. Irsmambetova, J. Garlitz, Pedro V. Sada, A. Antov, G. D. Chis, M. Buromsky, S. A. Spampinato, V. Tudose, S. Cammarata, Morten W. Hansen, A. Oksanen, N. Bassiere, Pascal Descamps, E. Bredner, Nicolas Rambaux, J. P. McAuliffe, C. Velu, M. Duenas, N. I. Dorokhov, M. Rapaport, E. M. Trunkovsky, Alain Vienne, Y. Ito, T. Pauwels, Jeremie Vaubaillon, J. Vilar, M. Sidorov, D. Moldovan, V. Priban, F. Bosq, Robin C. Gilbert, E. V. Khrutskaya, Dinko Dimitrov, S. Aubry, D. L. Gorshanov, R. Corlan, J. Manek, Jean-Eudes Arlot, O. Nickel, G. Rau, G. Dourneau, A. Sergeyev, M. Lavayssiére, William Thuillot, Q. Y. Peng, I. Ugarte, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université 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), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Association Jonckheere-Les Amis de l’Observatoire de Lille [Lille] (AJAOL), Indian Institute of Astrophysics (IIA), Armagh Observatory [Armagh], Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Lille, Instituto de Astrofisica de Canarias (IAC), Observatoire de Paris, Université Paris sciences et lettres (PSL), Royal Observatory of Belgium [Brussels] (ROB), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), The Central Astronomical Observatory of the Russian Academy of Sciences [Pulkovo], Russian Academy of Sciences [Moscow] (RAS), National Astronomical Observatory - Rozhen (NAO), Bulgarian Academy of Sciences (BAS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Ural Federal University [Ekaterinburg] (UrFU), Pulkovo Observatory, Observatoire de Dax, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Astronomical Observatory Cluj-Napoca, Romanian Academy, Microbiologie cellulaire et moléculaire et pathogénicité (MCMP), Université Bordeaux Segalen - Bordeaux 2-Centre National de la Recherche Scientifique (CNRS), Namur Center for Complex Systems [Namur] (NaXys), Université de Namur [Namur] (UNamur), Nyrölä Observatory (NYTT), Department of Computer Science [Jinan], JiNan University, Observatory and Planetarium Praha [Prague], Gruppo Astrofili Catanesi [Catania] (GAC), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Paediatric Department, University Hospital of Catania, Institute of Space Science [Bucharest-Măgurele] (ISS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Microbiologie Fondamentale et Pathogénicité (MFP)

Subjects
010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Context (language use), planets and satellites: individual: Jupiter, 01 natural sciences, eclipses, law.invention, Telescope, Jupiter, symbols.namesake, law, 0103 physical sciences, occultations, Rare events, 10. No inequality, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, Astronomy, Astronomy and Astrophysics, Astrometry, Light curve, Galilean moons, Space and Planetary Science, symbols, astrometry, Astrophysics::Earth and Planetary Astrophysics
Abstract

International audience; Context: In 2003, the Sun and the Earth passed through both the equatorial plane of Jupiter and therefore the orbital planes of its main satellites. Aims: During this period, mutual eclipses and occultations were observed and we present the data collected. Methods: Light curves of mutual eclipses and occultations were recorded by the observers of the international campaign PHEMU03 organized by the Institut de mécanique céleste, Paris, France. Results: We completed 377 observations of 118 mutual events from 42 sites and the corresponding data are presented in this paper. For each observation, information about the telescope, receptor, site, and observational conditions are provided. Conclusions: This paper gathers all data and indicates a first estimate of its precision. This catalogue of these rare events should constitute an improved basis for accurate astrometric data useful in the development of dynamical models.

Published
2009
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35. Recent Progress in the VLBI2010 Development

Author

Behrend, J., Boehm, J., Charlot, P., Clark, T., Corey, B., Gipson, J., Haas, R., Koyama, Y., MacMillan, D., Malkin, Z., Niell, A., Nilsson, T., Petrachenko, B., Rogers, A., Tuccari, G., Wresnik, J., Max-Planck-Institut für Radioastronomie (MPIFR), NVI, Inc., NASA Goddard Space Flight Center (GSFC), institut de geodesie et geophysique de Vienne (INSTITUT DE GEODESIE ET GEOPHYSIQUE), Institut de geodesie et geophysique, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), MIT Haystack Observatory, Massachusetts Institute of Technology (MIT), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], Kashima Space Technology Center, National Institute of Information and Communications Technology [Tokyo, Japan] (NICT), Pulkovo Observatory, Geodetic Survey Division, Istituto di Radioastronomia di Noto, and Istituto Nazionale di Astrofisica (INAF)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], next generation VLBI2010, IVS, geodetic VLBI, Monte Carlo simulations
Abstract

chapter in book series "International Association of Geodesy Symposia" book "Observing our Changing Earth" ISBN 978-3-540-85425-8; International audience; From October 2003 to September 2005, the International VLBI Service for Geodesy and Astrometry (IVS) examined current and future requirements for geodetic VLBI, including all components from antennas to analysis. IVS Working Group 3 ‘VLBI 2010', which was tasked with this effort, concluded with recommendations for a new generation of VLBI systems. These recommendations were based on the goals of achieving 1 mm measurement accuracy on global baselines, performing continuous measurements for time series of station positions and Earth orientation parameters, and reaching a turnaround time from measurement to initial geodetic results of less than 24 hours. To realize these recommendations and goals, along with the need for low cost of construction and operation, requires a complete examination of all aspects of geodetic VLBI including equipment, processes, and observational strategies. Hence, in October 2005, the IVS VLBI2010 Committee (V2C) commenced work on defining the VLBI2010 system specifications. In this paper we give a summary of the recent progress of the VLBI2010 project.

Published
2008
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36. Polarized blazar X-rays imply particle acceleration in shocks.

Author

Liodakis I, Marscher AP, Agudo I, Berdyugin AV, Bernardos MI, Bonnoli G, Borman GA, Casadio C, Casanova VC, Cavazzuti E, Rodriguez Cavero N, Di Gesu L, Di Lalla N, Donnarumma I, Ehlert SR, Errando M, Escudero J, Garcı A-Comas M, Agı S-González B, Husillos C, Jormanainen J, Jorstad SG, Kagitani M, Kopatskaya EN, Kravtsov V, Krawczynski H, Lindfors E, Larionova EG, Madejski GM, Marin F, Marchini A, Marshall HL, Morozova DA, Massaro F, Masiero JR, Mawet D, Middei R, Millar-Blanchaer MA, Myserlis I, Negro M, Nilsson K, O'Dell SL, Omodei N, Pacciani L, Paggi A, Panopoulou GV, Peirson AL, Perri M, Petrucci PO, Poutanen J, Puccetti S, Romani RW, Sakanoi T, Savchenko SS, Sota A, Tavecchio F, Tinyanont S, Vasilyev AA, Weaver ZR, Zhovtan AV, Antonelli LA, Bachetti M, Baldini L, Baumgartner WH, Bellazzini R, Bianchi S, Bongiorno SD, Bonino R, Brez A, Bucciantini N, Capitanio F, Castellano S, Ciprini S, Costa E, De Rosa A, Del Monte E, Di Marco A, Doroshenko V, Dovčiak M, Enoto T, Evangelista Y, Fabiani S, Ferrazzoli R, Garcia JA, Gunji S, Hayashida K, Heyl J, Iwakiri W, Karas V, Kitaguchi T, Kolodziejczak JJ, La Monaca F, Latronico L, Maldera S, Manfreda A, Marinucci A, Matt G, Mitsuishi I, Mizuno T, Muleri F, Ng SC, Oppedisano C, Papitto A, Pavlov GG, Pesce-Rollins M, Pilia M, Possenti A, Ramsey BD, Rankin J, Ratheesh A, Sgró C, Slane P, Soffitta P, Spandre G, Tamagawa T, Taverna R, Tawara Y, Tennant AF, Thomas NE, Tombesi F, Trois A, Tsygankov S, Turolla R, Vink J, Weisskopf MC, Wu K, Xie F, and Zane S

Abstract

Most of the light from blazars, active galactic nuclei with jets of magnetized plasma that point nearly along the line of sight, is produced by high-energy particles, up to around 1 TeV. Although the jets are known to be ultimately powered by a supermassive black hole, how the particles are accelerated to such high energies has been an unanswered question. The process must be related to the magnetic field, which can be probed by observations of the polarization of light from the jets. Measurements of the radio to optical polarization-the only range available until now-probe extended regions of the jet containing particles that left the acceleration site days to years earlier 1-3 , and hence do not directly explore the acceleration mechanism, as could X-ray measurements. Here we report the detection of X-ray polarization from the blazar Markarian 501 (Mrk 501). We measure an X-ray linear polarization degree Π X of around 10%, which is a factor of around 2 higher than the value at optical wavelengths, with a polarization angle parallel to the radio jet. This points to a shock front as the source of particle acceleration and also implies that the plasma becomes increasingly turbulent with distance from the shock., (© 2022. The Author(s).)

Published
2022
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37. Rapid quasi-periodic oscillations in the relativistic jet of BL Lacertae.

Author

Jorstad SG, Marscher AP, Raiteri CM, Villata M, Weaver ZR, Zhang H, Dong L, Gómez JL, Perel MV, Savchenko SS, Larionov VM, Carosati D, Chen WP, Kurtanidze OM, Marchini A, Matsumoto K, Mortari F, Aceti P, Acosta-Pulido JA, Andreeva T, Apolonio G, Arena C, Arkharov A, Bachev R, Banfi M, Bonnoli G, Borman GA, Bozhilov V, Carnerero MI, Damljanovic G, Ehgamberdiev SA, Elsässer D, Frasca A, Gabellini D, Grishina TS, Gupta AC, Hagen-Thorn VA, Hallum MK, Hart M, Hasuda K, Hemrich F, Hsiao HY, Ibryamov S, Irsmambetova TR, Ivanov DV, Joner MD, Kimeridze GN, Klimanov SA, Knött J, Kopatskaya EN, Kurtanidze SO, Kurtenkov A, Kuutma T, Larionova EG, Leonini S, Lin HC, Lorey C, Mannheim K, Marino G, Minev M, Mirzaqulov DO, Morozova DA, Nikiforova AA, Nikolashvili MG, Ovcharov E, Papini R, Pursimo T, Rahimov I, Reinhart D, Sakamoto T, Salvaggio F, Semkov E, Shakhovskoy DN, Sigua LA, Steineke R, Stojanovic M, Strigachev A, Troitskaya YV, Troitskiy IS, Tsai A, Valcheva A, Vasilyev AA, Vince O, Waller L, Zaharieva E, and Chatterjee R

Abstract

Blazars are active galactic nuclei (AGN) with relativistic jets whose non-thermal radiation is extremely variable on various timescales 1-3 . This variability seems mostly random, although some quasi-periodic oscillations (QPOs), implying systematic processes, have been reported in blazars and other AGN. QPOs with timescales of days or hours are especially rare 4 in AGN and their nature is highly debated, explained by emitting plasma moving helically inside the jet 5 , plasma instabilities 6,7 or orbital motion in an accretion disc 7,8 . Here we report results of intense optical and γ-ray flux monitoring of BL Lacertae (BL Lac) during a dramatic outburst in 2020 (ref.  9 ). BL Lac, the prototype of a subclass of blazars 10 , is powered by a 1.7 × 10 8  M Sun (ref.  11 ) black hole in an elliptical galaxy (distance = 313 megaparsecs (ref.  12 )). Our observations show QPOs of optical flux and linear polarization, and γ-ray flux, with cycles as short as approximately 13 h during the highest state of the outburst. The QPO properties match the expectations of current-driven kink instabilities 6 near a recollimation shock about 5 parsecs (pc) from the black hole in the wake of an apparent superluminal feature moving down the jet. Such a kink is apparent in a microwave Very Long Baseline Array (VLBA) image., (© 2022. The Author(s), under exclusive licence to Springer Nature Limited.)

Published
2022
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38. Detection of a New Large Free Core Nutation Phase Jump.

Author

Malkin Z, Belda S, and Modiri S

Subjects
Time Factors
Abstract

We announce the detection of a new large jump in the phase of the free core nutation (FCN). This is only the second such large FCN phase jump in more than thirty years of FCN monitoring by means of a very long baseline interferometry (VLBI) technique. The new event was revealed and confirmed by analyzing two FCN models derived from a long-time series of VLBI observations. The jump started in 2021 and is expected to last until the late fall of 2022. The amplitude of the phase jump is expected to be approximately 3 rad, which is as much as 1.5 times larger than the first phase jump in 1999-2000. A connection of the new FCN phase jump with the recent geomagnetic jerk started in 2020 is suggested.

Published
2022
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39. Blazar spectral variability as explained by a twisted inhomogeneous jet.

Author

Raiteri CM, Villata M, Acosta-Pulido JA, Agudo I, Arkharov AA, Bachev R, Baida GV, Benítez E, Borman GA, Boschin W, Bozhilov V, Butuzova MS, Calcidese P, Carnerero MI, Carosati D, Casadio C, Castro-Segura N, Chen WP, Damljanovic G, D'Ammando F, Di Paola A, Echevarría J, Efimova NV, Ehgamberdiev SA, Espinosa C, Fuentes A, Giunta A, Gómez JL, Grishina TS, Gurwell MA, Hiriart D, Jermak H, Jordan B, Jorstad SG, Joshi M, Kopatskaya EN, Kuratov K, Kurtanidze OM, Kurtanidze SO, Lähteenmäki A, Larionov VM, Larionova EG, Larionova LV, Lázaro C, Lin CS, Malmrose MP, Marscher AP, Matsumoto K, McBreen B, Michel R, Mihov B, Minev M, Mirzaqulov DO, Mokrushina AA, Molina SN, Moody JW, Morozova DA, Nazarov SV, Nikolashvili MG, Ohlert JM, Okhmat DN, Ovcharov E, Pinna F, Polakis TA, Protasio C, Pursimo T, Redondo-Lorenzo FJ, Rizzi N, Rodriguez-Coira G, Sadakane K, Sadun AC, Samal MR, Savchenko SS, Semkov E, Skiff BA, Slavcheva-Mihova L, Smith PS, Steele IA, Strigachev A, Tammi J, Thum C, Tornikoski M, Troitskaya YV, Troitsky IS, Vasilyev AA, and Vince O

Abstract

Blazars are active galactic nuclei, which are powerful sources of radiation whose central engine is located in the core of the host galaxy. Blazar emission is dominated by non-thermal radiation from a jet that moves relativistically towards us, and therefore undergoes Doppler beaming. This beaming causes flux enhancement and contraction of the variability timescales, so that most blazars appear as luminous sources characterized by noticeable and fast changes in brightness at all frequencies. The mechanism that produces this unpredictable variability is under debate, but proposed mechanisms include injection, acceleration and cooling of particles, with possible intervention of shock waves or turbulence. Changes in the viewing angle of the observed emitting knots or jet regions have also been suggested as an explanation of flaring events and can also explain specific properties of blazar emission, such as intra-day variability, quasi-periodicity and the delay of radio flux variations relative to optical changes. Such a geometric interpretation, however, is not universally accepted because alternative explanations based on changes in physical conditions-such as the size and speed of the emitting zone, the magnetic field, the number of emitting particles and their energy distribution-can explain snapshots of the spectral behaviour of blazars in many cases. Here we report the results of optical-to-radio-wavelength monitoring of the blazar CTA 102 and show that the observed long-term trends of the flux and spectral variability are best explained by an inhomogeneous, curved jet that undergoes changes in orientation over time. We propose that magnetohydrodynamic instabilities or rotation of the twisted jet cause different jet regions to change their orientation and hence their relative Doppler factors. In particular, the extreme optical outburst of 2016-2017 (brightness increase of six magnitudes) occurred when the corresponding emitting region had a small viewing angle. The agreement between observations and theoretical predictions can be seen as further validation of the relativistic beaming theory.

Published
2017
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40. Non-linear VLBI station motions and their impact on the celestial reference frame and Earth orientation parameters.

Author

Krásná H, Malkin Z, and Böhm J

Abstract

The increasing accuracy and growing time span of Very Long Baseline Interferometry (VLBI) observations allow the determination of seasonal signals in station positions which still remain unmodelled in conventional analysis approaches. In this study we focus on the impact of the neglected seasonal signals in the station displacement on the celestial reference frame and Earth orientation parameters. We estimate empirical harmonic models for selected stations within a global solution of all suitable VLBI sessions and create mean annual models by stacking yearly time series of station positions which are then entered a priori in the analysis of VLBI observations. Our results reveal that there is no systematic propagation of the seasonal signal into the orientation of celestial reference frame but position changes occur for radio sources observed non-evenly over the year. On the other hand, the omitted seasonal harmonic signal in horizontal station coordinates propagates directly into the Earth rotation parameters causing differences of several tens of microarcseconds.

Published
2015
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41. Suppression of cooling by strong magnetic fields in white dwarf stars.

Author

Valyavin G, Shulyak D, Wade GA, Antonyuk K, Zharikov SV, Galazutdinov GA, Plachinda S, Bagnulo S, Machado LF, Alvarez M, Clark DM, Lopez JM, Hiriart D, Han I, Jeon YB, Zurita C, Mujica R, Burlakova T, Szeifert T, and Burenkov A

Abstract

Isolated cool white dwarf stars more often have strong magnetic fields than young, hotter white dwarfs, which has been a puzzle because magnetic fields are expected to decay with time but a cool surface suggests that the star is old. In addition, some white dwarfs with strong fields vary in brightness as they rotate, which has been variously attributed to surface brightness inhomogeneities similar to sunspots, chemical inhomogeneities and other magneto-optical effects. Here we describe optical observations of the brightness and magnetic field of the cool white dwarf WD 1953-011 taken over about eight years, and the results of an analysis of its surface temperature and magnetic field distribution. We find that the magnetic field suppresses atmospheric convection, leading to dark spots in the most magnetized areas. We also find that strong fields are sufficient to suppress convection over the entire surface in cool magnetic white dwarfs, which inhibits their cooling evolution relative to weakly magnetic and non-magnetic white dwarfs, making them appear younger than they truly are. This explains the long-standing mystery of why magnetic fields are more common amongst cool white dwarfs, and implies that the currently accepted ages of strongly magnetic white dwarfs are systematically too young.

Published
2014
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42. Width of the chaotic layer: maxima due to marginal resonances.

Author

Shevchenko II

Subjects
Computer Simulation, Models, Theoretical, Nonlinear Dynamics, Oscillometry methods
Abstract

Modern theoretical methods for estimating the width of the chaotic layer in the presence of prominent marginal resonances are considered in the perturbed pendulum model of nonlinear resonance. The fields of applicability of these methods are explicitly and precisely formulated. The comparative accuracy is investigated in massive and long-run numerical experiments. It is shown that the methods are naturally subdivided in classes applicable for adiabatic and nonadiabatic cases of perturbation. It is explicitly shown that the pendulum approximation of marginal resonance works well in the nonadiabatic case. In this case, the role of marginal resonances in determining the total layer width is demonstrated to diminish with increasing main parameter λ (equal to the ratio of the perturbation frequency to the frequency of small-amplitude phase oscillations on the resonance). Solely the "bending effect" is important in determining the total amplitude of the energy deviations of the near-separatrix motion at λ≳7. In the adiabatic case, it is demonstrated that the geometrical form of the separatrix cell can be described analytically quite easily by means of using a specific representation of the separatrix map. It is shown that the nonadiabatic (and, to some extent, intermediary) case is most actual, in comparison with the adiabatic one, for the physical or technical applications that concern the energy jumps in the near-separatrix chaotic motion.

Published
2012
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43. Hamiltonian intermittency and Lévy flights in the three-body problem.

Author

Shevchenko II

Abstract

We consider statistics of the disruption and Lyapunov times in an hierarchical restricted three-body problem. We show that at the edge of disruption the orbital periods and the size of the orbit of the escaping body exhibit Lévy flights. Due to them, the time decay of the survival probability is heavy-tailed with the power-law index equal to -2/3, while the relation between the Lyapunov and disruption times is quasilinear. Applicability of these results in an "hierarchical resonant scattering" setting for a three-body interaction is discussed.

Published
2010
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