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1. ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations

Author

A. Kokori, A. Tsiaras, B. Edwards, A. Jones, G. Pantelidou, G. Tinetti, L. Bewersdorff, A. Iliadou, Y. Jongen, G. Lekkas, A. Nastasi, E. Poultourtzidis, C. Sidiropoulos, F. Walter, A. Wünsche, R. Abraham, V. K. Agnihotri, R. Albanesi, E. Arce-Mansego, D. Arnot, M. Audejean, C. Aumasson, M. Bachschmidt, G. Baj, P. R. Barroy, A. A. Belinski, D. Bennett, P. Benni, K. Bernacki, L. Betti, A. Biagini, P. Bosch, P. Brandebourg, L. Brát, M. Bretton, S. M. Brincat, S. Brouillard, A. Bruzas, A. Bruzzone, R. A. Buckland, M. Caló, F. Campos, A. Carreño, J. A. Carrion Rodrigo, R. Casali, G. Casalnuovo, M. Cataneo, C.-M. Chang, L. Changeat, V. Chowdhury, R. Ciantini, M. Cilluffo, J.-F. Coliac, G. Conzo, M. Correa, G. Coulon, N. Crouzet, M. V. Crow, I. A. Curtis, D. Daniel, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, G. Dransfield, R. Dymock, T. Eenmäe, N. Esseiva, P. Evans, C. Falco, R. G. Farfán, E. Fernández-Lajús, S. Ferratfiat, S. L. Ferreira, A. Ferretti, J. Fiołka, M. Fowler, S. R. Futcher, D. Gabellini, T. Gainey, J. Gaitan, P. Gajdoš, A. García-Sánchez, J. Garlitz, C. Gillier, C. Gison, J. Gonzales, D. Gorshanov, F. Grau Horta, G. Grivas, P. Guerra, T. Guillot, C. A. Haswell, T. Haymes, V.-P. Hentunen, K. Hills, K. Hose, T. Humbert, F. Hurter, T. Hynek, M. Irzyk, J. Jacobsen, A. L. Jannetta, K. Johnson, P. Jóźwik-Wabik, A. E. Kaeouach, W. Kang, H. Kiiskinen, T. Kim, Ü. Kivila, B. Koch, U. Kolb, H. Kučáková, S.-P. Lai, D. Laloum, S. Lasota, L. A. Lewis, G.-I. Liakos, F. Libotte, F. Lomoz, C. Lopresti, R. Majewski, A. Malcher, M. Mallonn, M. Mannucci, A. Marchini, J.-M. Mari, A. Marino, G. Marino, J.-C. Mario, J.-B. Marquette, F. A. Martínez-Bravo, M. Mašek, P. Matassa, P. Michel, J. Michelet, M. Miller, E. Miny, D. Molina, T. Mollier, B. Monteleone, N. Montigiani, M. Morales-Aimar, F. Mortari, M. Morvan, L. V. Mugnai, G. Murawski, L. Naponiello, J.-L. Naudin, R. Naves, D. Néel, R. Neito, S. Neveu, A. Noschese, Y. Öğmen, O. Ohshima, Z. Orbanic, E. P. Pace, C. Pantacchini, N. I. Paschalis, C. Pereira, I. Peretto, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, J. Plazas, A. J. Poelarends, A. Popowicz, J. Purcell, N. Quinn, M. Raetz, D. Rees, F. Regembal, M. Rocchetto, P.-F. Rocci, M. Rockenbauer, R. Roth, L. Rousselot, X. Rubia, N. Ruocco, E. Russo, M. Salisbury, F. Salvaggio, A. Santos, J. Savage, F. Scaggiante, D. Sedita, S. Shadick, A. F. Silva, N. Sioulas, V. Školník, M. Smith, M. Smolka, A. Solmaz, N. Stanbury, D. Stouraitis, T.-G. Tan, M. Theusner, G. Thurston, F. P. Tifner, A. Tomacelli, A. Tomatis, J. Trnka, M. Tylšar, P. Valeau, J.-P. Vignes, A. Villa, A. Vives Sureda, K. Vora, M. Vrašt’ák, D. Walliang, B. Wenzel, D. E. Wright, R. Zambelli, M. Zhang, and M. Zíbar

Subjects
Ephemerides, Transits, Amateur astronomers, Photometry, Open source software, Astrophysics, QB460-466
Abstract

The ExoClock project has been created to increase the efficiency of the Ariel mission. It will achieve this by continuously monitoring and updating the ephemerides of Ariel candidates, in order to produce a consistent catalog of reliable and precise ephemerides. This work presents a homogenous catalog of updated ephemerides for 450 planets, generated by the integration of ∼18,000 data points from multiple sources. These sources include observations from ground-based telescopes (the ExoClock network and the Exoplanet Transit Database), midtime values from the literature, and light curves from space telescopes (Kepler, K2, and TESS). With all the above, we manage to collect observations for half of the postdiscovery years (median), with data that have a median uncertainty less than 1 minute. In comparison with the literature, the ephemerides generated by the project are more precise and less biased. More than 40% of the initial literature ephemerides had to be updated to reach the goals of the project, as they were either of low precision or drifting. Moreover, the integrated approach of the project enables both the monitoring of the majority of the Ariel candidates (95%), and also the identification of missing data. These results highlight the need for continuous monitoring to increase the observing coverage of the candidate planets. Finally, the extended observing coverage of planets allows us to detect trends (transit-timing variations) for a sample of 19 planets. All the products, data, and codes used in this work are open and accessible to the wider scientific community.

Published
2023
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2. ExoClock project II: A large-scale integrated study with 180 updated exoplanet ephemerides

Author

A. Kokori, A. Tsiaras, B. Edwards, M. Rocchetto, G. Tinetti, L. Bewersdorff, Y. Jongen, G. Lekkas, G. Pantelidou, E. Poultourtzidis, A. Wünsche, C. Aggelis, V. K. Agnihotri, C. Arena, M. Bachschmidt, D. Bennett, P. Benni, K. Bernacki, E. Besson, L. Betti, A. Biagini, P. Brandebourg, M. Bretton, S. M. Brincat, M. Caló, F. Campos, R. Casali, R. Ciantini, M. V. Crow, B. Dauchet, S. Dawes, M. Deldem, D. Deligeorgopoulos, R. Dymock, T. Eenmäe, P. Evans, N. Esseiva, C. Falco, S. Ferratfiat, M. Fowler, S. R. Futcher, J. Gaitan, F. Grau Horta, P. Guerra, F. Hurter, A. Jones, W. Kang, H. Kiiskinen, T. Kim, D. Laloum, R. Lee, F. Lomoz, C. Lopresti, M. Mallonn, M. Mannucci, A. Marino, J.-C. Mario, J.-B. Marquette, J. Michelet, M. Miller, T. Mollier, D. Molina, N. Montigiani, F. Mortari, M. Morvan, L. V. Mugnai, L. Naponiello, A. Nastasi, R. Neito, E. Pace, P. Papadeas, N. Paschalis, C. Pereira, V. Perroud, M. Phillips, P. Pintr, J.-B. Pioppa, A. Popowicz, M. Raetz, F. Regembal, K. Rickard, M. Roberts, L. Rousselot, X. Rubia, J. Savage, D. Sedita, D. Shave-Wall, N. Sioulas, V. Školník, M. Smith, D. St-Gelais, D. Stouraitis, I. Strikis, G. Thurston, A. Tomacelli, A. Tomatis, B. Trevan, P. Valeau, J.-P. Vignes, K. Vora, M. Vrašťák, F. Walter, B. Wenzel, D. E. Wright, M. Zíbar, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Société Astronomique de France (SAF), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Amateur astronomy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], Space and Planetary Science, Exoplanets, FOS: Physical sciences, Astronomy and Astrophysics, Transit photometry, Ephemerides, Transit photometry, Ephemerides, Exoplanets, Amateur astronomy, Astrophysics - Earth and Planetary Astrophysics
Abstract

The ExoClock project is an inclusive, integrated, and interactive platform that was developed to monitor the ephemerides of the Ariel targets to increase the mission efficiency. The project makes the best use of all available resources, i.e., observations from ground telescopes, mid-time values from the literature and finally, observations from space instruments. Currently, the ExoClock network includes 280 participants with telescopes capable of observing 85\% of the currently known Ariel candidate targets. This work includes the results of $\sim$1600 observations obtained up to the 31st of December 2020 from the ExoClock network. These data in combination with $\sim$2350 mid-time values collected from the literature are used to update the ephemerides of 180 planets. The analysis shows that 40\% of the updated ephemerides will have an impact on future scheduling as either they have a significantly improved precision, or they have revealed biases in the old ephemerides. With the new observations, the observing coverage and rate for half of the planets in the sample has been doubled or more. Finally, from a population perspective, we identify that the differences in the 2028 predictions between the old and the new ephemerides have an STD that is double what is expected from gaussian uncertainties. These findings have implications for planning future observations, where we will need to account for drifts potentially greater than the prediction uncertainties. The updated ephemerides are open and accessible to the wider exoplanet community both from our Open Science Framework (OSF) repository and our website., Comment: 9 pages (47 with appendices and references), 8 figures, 2 tables. Submitted to ApJS. Revised based on the reviewer's comments

Published
2022
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3. Spin states of asteroids in the Eos collisional family

Author

Josef Hanus, Luc Arnold, Maria J. Esteban, E. Morelle, H. Gully, P. Antonini, Peter Kusnirak, Silvano Casulli, Marco Delbo, F. Manzini, P. Pravec, H. Cibulková, Bryce Bolin, Victor Ali-Lagoa, J. Michelet, Josef Ďurech, M. Lehký, H. de Groot, R. Dymock, L. Bernasconi, M. Bachschmidt, M. Audejean, Julian Oey, P. A. Salom, Robert Jedicke, N. Esseiva, Brian D. Warner, L. Brunetto, Raoul Behrend, F. Marchis, Rupak Roy, Frederick Pilcher, Hiroko Hamanowa, F. Reignier, P. Krafft, Hiromi Hamanowa, O. Gerteis, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, media_common.quotation_subject, Population, Inverse transform sampling, FOS: Physical sciences, 01 natural sciences, law.invention, Telescope, Photometry (optics), law, 0103 physical sciences, education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, Collisional family, Astronomy, Astronomy and Astrophysics, Collision, Space and Planetary Science, Sky, Asteroid, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

Eos family was created during a catastrophic impact about 1.3 Gyr ago. Rotation states of individual family members contain information about the history of the whole population. We aim to increase the number of asteroid shape models and rotation states within the Eos collision family, as well as to revise previously published shape models from the literature. Such results can be used to constrain theoretical collisional and evolution models of the family, or to estimate other physical parameters by a thermophysical modeling of the thermal infrared data. We use all available disk-integrated optical data (i.e., classical dense-in-time photometry obtained from public databases and through a large collaboration network as well as sparse-in-time individual measurements from a few sky surveys) as input for the convex inversion method, and derive 3D shape models of asteroids together with their rotation periods and orientations of rotation axes. We present updated shape models for 15 asteroids and new shape model determinations for 16 asteroids. Together with the already published models from the publicly available DAMIT database, we compiled a sample of 56 Eos family members with known shape models that we used in our analysis of physical properties within the family. Rotation states of asteroids smaller than ~20 km are heavily influenced by the YORP effect, whilst the large objects more or less retained their rotation state properties since the family creation. Moreover, we also present a shape model and bulk density of asteroid (423) Diotima, an interloper in the Eos family, based on the disk-resolved data obtained by the Near InfraRed Camera (Nirc2) mounted on the W.M. Keck II telescope., Comment: Accepted for publication in ICARUS Special Issue - Asteroids: Origin, Evolution & Characterization

Published
2018
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4. Witches and Witchcraft: Five Classic Books

Author

J. Michelet and J. Michelet

Subjects
Witchcraft, Witches
Abstract

Collection of five classic books on witches and witchcraft: The Witch Mania by Charles Mackay, The History of the Devil by Daniel Defoe, The Witch in the Middle Ages by Michelet, Wonders of the Invisible World by Cotton Mather, and Letters on Demonology and Witchcraft by Sir Walter Scott.

Published
2018

5. The Witch of the Middle Ages

Author

J. Michelet and J. Michelet

Subjects
Civilization, Medieval, Demonomania, Witchcraft
Abstract

History of witchcraft in the Middle Ages. According to Wikipedia:'Jules Michelet (21 August 1798 – 9 February 1874) was a French historian. He was born in Paris to a family with Huguenot traditions.'The Preface begins:'In this translation of a work rich in the raciest beauties and defects of an author long since made known to the British public, the present writer has striven to recast the trenchant humour, the scornful eloquence, the epigrammatic dash of Mr. Michelet, in language not all unworthy of such a word-master. How far he has succeeded others may be left to judge. In one point only is he aware of having been less true to his original than in theory he was bound to be.'

Published
2018

6. An outbreak of diarrhoeic shellfish poisoning in Antwerp, Belgium

Author

K De Schrijver, I Maes, L De Man, and J Michelet

Subjects
Adult, Diarrhea, Veterinary medicine, Abdominal pain, animal structures, Adolescent, Epidemiology, Nausea, Comorbidity, Disease Outbreaks, Microbiology, Foodborne Diseases, Feces, chemistry.chemical_compound, Age Distribution, Belgium, Virology, Okadaic Acid, medicine, Humans, Shellfish Poisoning, Child, Aged, Shellfish, Aged, 80 and over, Protozoan Infections, business.industry, Public Health, Environmental and Occupational Health, Outbreak, Okadaic acid, Middle Aged, Diarrhoeic shellfish poisoning, chemistry, Child, Preschool, Vomiting, medicine.symptom, business
Abstract

In Antwerp, Belgium, 403 cases of diarrhoeic shellfish poisoning were reported after consumption of blue mussels. Symptoms included diarrhoea, vomiting, abdominal pain, and nausea. The analysis of faecal specimens from patients allowed diagnosis exclusions for bacteria and viruses. Mouse-assays revealed the presence of biotoxins specific of dinoflagellates, which were identified and quantified by LC-MS. The mussels were imported from Denmark, and were part of a batch presenting high concentrations of okadaic acid above the regulatory limits.

Published
2002
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7. SOPHIE velocimetry of Kepler transit candidates XII. KOI-1257 b: a highly eccentric three-month period transiting exoplanet

Author

D. Verilhac, Isabelle Boisse, L. Bernasconi, J. Michelet, D. Gravallon, G. Bruno, Olga Suarez, Jean-Pierre Rivet, Ph. Bendjoya, Cilia Damiani, François Bouchy, Tristan Guillot, M. Audejean, P. Martinez, C. Moutou, Luc Arnold, S. C. C. Barros, R. Montaigut, Alexandre C. M. Correia, Magali Deleuil, Lyu Abe, M. Havel, C. Rinner, Guillaume Montagnier, J. Gregorio, G. Rousseau, O. Labrevoir, Roi Alonso, Rodrigo F. Díaz, C. Gillier, Nuno C. Santos, Alexandre Santerne, J. M. Almenara, R. Roy, Aldo S. Bonomo, Raoul Behrend, R. Poncy, Guillaume Hébrard, M. Vanhuysse, Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, 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), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), Centro de Biología Molecular Severo Ochoa [Madrid] (CBMSO), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Geneva Observatory, University of Geneva [Switzerland], CdR & CdL group, Observatoire des Engarouines, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Laboratoire de Mathématiques Nicolas Oresme (LMNO), Centre National de la Recherche Scientifique (CNRS)-Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Association des Utilisateurs de Détecteurs Electroniques (AUDE), Association des Utilisateurs de Détecteurs Electroniques, Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto-Universidade do Porto, Observatoire de Chinon, UMR 5805 Environnements et Paléoenvironnements Océaniques et Continentaux (EPOC), 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)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Club d'Astronomie Lyon Ampéré [Vaulx-en-Velin] (CALA), Chercheur indépendant, Laboratoire SUBATECH Nantes (SUBATECH), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Nantes (UN)-Mines Nantes (Mines Nantes), Simulation et Traitement de l'information pour l'Exploitation des systèmes de Production (EDF R&D STEP), EDF R&D (EDF R&D), EDF (EDF)-EDF (EDF), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidade do Porto [Porto], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Centro de Biología Molecular Severo Ochoa (CBMSO), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Université de Caen Normandie (UNICAEN), Normandie Université (NU)-Normandie Université (NU)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Departamento de Física e Astronomia [Porto], 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)-École pratique des hautes études (EPHE)-Centre National de la Recherche Scientifique (CNRS), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Universidade do Porto = University of Porto, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Université de Genève = University of Geneva (UNIGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Environnements et Paléoenvironnements OCéaniques (EPOC), and 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)-École Pratique des Hautes Études (EPHE)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Population, Giant planet, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Light curve, Exoplanet, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Primary (astronomy), Planet, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), Astrophysics::Earth and Planetary Astrophysics, education, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

In this paper we report a new transiting warm giant planet: KOI-1257 b. It was first detected in photometry as a planet-candidate by the ${\it Kepler}$ space telescope and then validated thanks to a radial velocity follow-up with the SOPHIE spectrograph. It orbits its host star with a period of 86.647661 d $\pm$ 3 s and a high eccentricity of 0.772 $\pm$ 0.045. The planet transits the main star of a metal-rich, relatively old binary system with stars of mass of 0.99 $\pm$ 0.05 Msun and 0.70 $ \pm $ 0.07 Msun for the primary and secondary, respectively. This binary system is constrained thanks to a self-consistent modelling of the ${\it Kepler}$ transit light curve, the SOPHIE radial velocities, line bisector and full-width half maximum (FWHM) variations, and the spectral energy distribution. However, future observations are needed to confirm it. The PASTIS fully-Bayesian software was used to validate the nature of the planet and to determine which star of the binary system is the transit host. By accounting for the dilution from the binary both in photometry and in radial velocity, we find that the planet has a mass of 1.45 $ \pm $ 0.35 Mjup, and a radius of 0.94 $ \pm $ 0.12 Rjup, and thus a bulk density of 2.1 $ \pm $ 1.2 g.cm$^{-3}$. The planet has an equilibrium temperature of 511 $\pm$ 50 K, making it one of the few known members of the warm-jupiter population. The HARPS-N spectrograph was also used to observe a transit of KOI-1257 b, simultaneously with a joint amateur and professional photometric follow-up, with the aim of constraining the orbital obliquity of the planet. However, the Rossiter-McLaughlin effect was not clearly detected, resulting in poor constraints on the orbital obliquity of the planet., 39 pages, 17 figures, accepted for publication in Astronomy & Astrophysics

Published
2014
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8. Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution

Author

J. Hanuš, J. Ďurech, M. Brož, A. Marciniak, B. D. Warner, F. Pilcher, R. Stephens, R. Behrend, B. Carry, D. Čapek, P. Antonini, M. Audejean, K. Augustesen, E. Barbotin, P. Baudouin, A. Bayol, L. Bernasconi, W. Borczyk, J.-G. Bosch, E. Brochard, L. Brunetto, S. Casulli, A. Cazenave, S. Charbonnel, B. Christophe, F. Colas, J. Coloma, M. Conjat, W. Cooney, H. Correira, V. Cotrez, A. Coupier, R. Crippa, M. Cristofanelli, Ch. Dalmas, C. Danavaro, C. Demeautis, T. Droege, R. Durkee, N. Esseiva, M. Esteban, M. Fagas, G. Farroni, M. Fauvaud, S. Fauvaud, F. Del Freo, L. Garcia, S. Geier, C. Godon, K. Grangeon, H. Hamanowa, N. Heck, S. Hellmich, D. Higgins, R. Hirsch, M. Husarik, T. Itkonen, O. Jade, K. Kamiński, P. Kankiewicz, A. Klotz, R. A. Koff, A. Kryszczyńska, T. Kwiatkowski, A. Laffont, A. Leroy, J. Lecacheux, Y. Leonie, C. Leyrat, F. Manzini, A. Martin, G. Masi, D. Matter, J. Michałowski, M. J. Michałowski, T. Michałowski, J. Michelet, R. Michelsen, E. Morelle, S. Mottola, R. Naves, J. Nomen, J. Oey, W. Ogłoza, A. Oksanen, D. Oszkiewicz, P. Pääkkönen, M. Paiella, H. Pallares, J. Paulo, M. Pavic, B. Payet, M. Polińska, D. Polishook, R. Poncy, Y. Revaz, C. Rinner, M. Rocca, A. Roche, D. Romeuf, R. Roy, H. Saguin, P. A. Salom, S. Sanchez, G. Santacana, T. Santana-Ros, J.-P. Sareyan, K. Sobkowiak, S. Sposetti, D. Starkey, R. Stoss, J. Strajnic, J.-P. Teng, B. Trégon, A. Vagnozzi, F. P. Velichko, N. Waelchli, K. Wagrez, H. Wücher, Astronomical Institute of Charles University, Charles University [Prague] (CU), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Palmer Divide Observatory, Organ Mesa Observatory, Goat Mountain Astronomical Research Station, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Observatoire de Bédoin, Observatoire de Chinon, Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), CdR & CdL group, Association T60, Observatoire Midi-Pyrénées, Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, Harfleur Observatory, Observatoire des Engarouines, Collonges Observatory, Chercheur indépendant, Observatoire N°139 d'Antibes, Osservatorio Colleverde di Guidonia, Observatoire de Saint-Sulpice N°947, DPHY, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatorio de San Gervasi, Observatoire de Cabris, Blackberry Observatory, Centre d'Astronomie de Saint-Michel l'Observatoire, Observatoire de Sainte-Hélène, Observatorio Astronómico de Tradate, 138 Village-Neuf, The Amateur Sky Survey (TASS), The Amateur Sky Survey, Shed of Science Observatory, Association AstroQueyras, Association des Utilisateurs de Détecteurs Electroniques (AUDE), Association des Utilisateurs de Détecteurs Electroniques, Observatoire du Bois de Bardon, Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Nordic Optical Telescope (NOT), Instituto de Astrofisica de Canarias (IAC), Hamanowa Astronomical Observatory, DLR Institute of Planetary Research, German Aerospace Center (DLR), Hunters Hill Observatory, Skalnaté Pleso Observatory, A83 Jakokoski Observatory, Institute of Physics [Kielce], Jan Kochanowski University, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Antelope Hills Observatory, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Stazione Astronomica di Sozzago, Forte Software, Scottish Universities Physics Alliance, Institute for Astronomy (SUPA), University of Edinburgh, Club d'Astronomie Lyon Ampéré [Vaulx-en-Velin] (CALA), Nyrölä Observatory (NYTT), Observatorio Montcabre, Observatorio Astronómico de Mallorca (OAM), Observatorio Astronómico de Mallorca, Kingsgrove Observatory, Mt. Suhora Observatory, Pedagogical University, Astronomy Department, Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), François-Xavier Bagnoud Observatory, Blauvac Obsevatory, Blauvac Observatory, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Gnosca Observatory, DeKalb Observatory, Observatoire astronomique des Makes, Laboratoire Kastler Brossel (LKB (Lhomond)), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institute of Astronomy [Kharkiv], V.N. Karazin Kharkiv National University (KhNU), University of Geneva [Switzerland], European Space Agency (ESA), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Helsinki-University of Helsinki, Université Pierre et Marie Curie - Paris 6 (UPMC)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, photometry, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], media_common.quotation_subject, Population, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Inverse transform sampling, Astrophysics, 01 natural sciences, Photometry (optics), models, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Physical model, Minor planets, Astronomy and Astrophysics, Asteroids: general, 13. Climate action, Space and Planetary Science, Sky, Asteroid, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The larger number of models of asteroid shapes and their rotational states derived by the lightcurve inversion give us better insight into both the nature of individual objects and the whole asteroid population. With a larger statistical sample we can study the physical properties of asteroid populations, such as main-belt asteroids or individual asteroid families, in more detail. Shape models can also be used in combination with other types of observational data (IR, adaptive optics images, stellar occultations), e.g., to determine sizes and thermal properties. We use all available photometric data of asteroids to derive their physical models by the lightcurve inversion method and compare the observed pole latitude distributions of all asteroids with known convex shape models with the simulated pole latitude distributions. We used classical dense photometric lightcurves from several sources and sparse-in-time photometry from the U.S. Naval Observatory in Flagstaff, Catalina Sky Survey, and La Palma surveys (IAU codes 689, 703, 950) in the lightcurve inversion method to determine asteroid convex models and their rotational states. We also extended a simple dynamical model for the spin evolution of asteroids used in our previous paper. We present 119 new asteroid models derived from combined dense and sparse-in-time photometry. We discuss the reliability of asteroid shape models derived only from Catalina Sky Survey data (IAU code 703) and present 20 such models. By using different values for a scaling parameter cYORP (corresponds to the magnitude of the YORP momentum) in the dynamical model for the spin evolution and by comparing synthetics and observed pole-latitude distributions, we were able to constrain the typical values of the cYORP parameter as between 0.05 and 0.6., Accepted for publication in A&A, January 15, 2013

Published
2013
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10. The field high-amplitude SX Phe variable BL Cam: Results from a multisite photometric campaign: II. Evidence of a binary - Possibly triple - System

Author

M. Helvaci, M. Blauzek, V. Casanova, J. Michelet, G. Santacana, J. P. Sareyan, L. Kotková, A.-Y. Zhou, Hana Kučáková, S. Fauvaud, I. Scheggia, A. Avdibegovic, J. J. Rives, Petr Zasche, A. Nava-Vega, F. Fumagalli, M. Alvarez, C. Ulusoy, K. Truparová, J. Kliner, P. van Cauteren, B. Yasarsoy, Eric G. Hintz, Raoul Behrend, B. H. Granslo, L. Král, Cahit Yeşilyaprak, J. A. Farrell, S. Bartošíková, M. J. López-González, Patricia Lampens, M. Vilášek, Marek Wolf, F. Van Den Abbeel, G. Klingenberg, K. A. Graham, R. Kocián, I. Ribas, H. Wücher, Raul Michel, M. Fauvaud, John H. Simonetti, F. J. Aceituno, M. P. Nicholson, E. Rodriguez, J.-M. Vugnon, O. Trondal, L. Fox-Machado, Ege Üniversitesi, Observatoire du Bois de Bardon, Groupe européen d’observation stellaire (GEOS), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai (ICE), Instituto de Astrofisica de Andalucia, CSIC (IAA), Koninklijke Sterrenwacht van België, Variable Star Section, Norwegian Astronomical Society, Sulphur Flats Observatory, Martin Observatory, Physics Dep., Virginia Polytechnic Institute & State University, Blacksburg, Astronomical Institute, Charles University, National Astronomical Observatoires-CAS, Observatorio Astronómico Nacional, Instituto de Astronomía, Universidad Nacional Autónoma de México, Facultad de Ciencias Químicas e Ingeniería, Universidad Autónoma de Baja California, Societá Astronomica Le pleiadi, Observatoire des Trois Korrigans, Department of Physics and Astronomy, Brigham Young University, Beersel Hills Observatory, Department of Physics, Akdeniz University, Department of Physics, Ataturk University, American Association of Variable Star Observers (AAVSO), Project Eridanus, Observatory and Planetarium of Johann Palisa, Club d'Astronomie Lyon Ampéré [Vaulx-en-Velin] (CALA), Club Eclipse : Club d'Etudes du Ciel, de la Lune, des Instruments, des Planètes, du Soleil et des Etoiles..., Astronomical Institute, Academy of Sciences, Ege University Observatory, Vesqueville Observatory, and Observatoire Astronomique de l'Université de Genève

Subjects
Physics, Stars: individual: BL Camelopardalis, Stars: variables: ? Scuti, education.field_of_study, Cepheid variable, Population, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Stars, Orbit, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Stars: oscillations, Binaries: general, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Maxima, Instability strip, education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Stellar evolution, Solar and Stellar Astrophysics (astro-ph.SR), Techniques: photometric
Abstract

Short-period high-amplitude pulsating stars of Population I ($\delta$ Sct stars) and II (SX Phe variables) exist in the lower part of the classical (Cepheid) instability strip. Most of them have very simple pulsational behaviours, only one or two radial modes being excited. Nevertheless, BL Cam is a unique object among them, being an extreme metal-deficient field high-amplitude SX Phe variable with a large number of frequencies. Based on a frequency analysis, a pulsational interpretation was previously given. aims heading (mandatory) We attempt to interpret the long-term behaviour of the residuals that were not taken into account in the previous Observed-Calculated (O-C) short-term analyses. methods heading (mandatory) An investigation of the O-C times has been carried out, using a data set based on the previous published times of light maxima, largely enriched by those obtained during an intensive multisite photometric campaign of BL Cam lasting several months. results heading (mandatory) In addition to a positive (161 $\pm$ 3) x 10$^{-9}$ yr$^{-1}$ secular relative increase in the main pulsation period of BL Cam, we detected in the O-C data short- (144.2 d) and long-term ($\sim$ 3400 d) variations, both incompatible with a scenario of stellar evolution. conclusions heading (mandatory) Interpreted as a light travel-time effect, the short-term O-C variation is indicative of a massive stellar component (0.46 to 1 M$_{\sun}$) with a short period orbit (144.2 d), within a distance of 0.7 AU from the primary. More observations are needed to confirm the long-term O-C variations: if they were also to be caused by a light travel-time effect, they could be interpreted in terms of a third component, in this case probably a brown dwarf star ($\geq$ 0.03 \ M$_{\sun}$), orbiting in $\sim$ 3400 d at a distance of 4.5 AU from the primary., Comment: 7 pages, 5 figures, accepted for publication in A&A

Published
2010
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11. A comprehensive study of the SX Phoenicis star BL Camelopardalis

Author

J. A. Farrell, G. Klingenberg, J. J. Rives, J. Michelet, S. E. Robinson, J. P. Sareyan, A. Y. Zhou, S. Fauvaud, Michael D. Reed, G. Santacana, Elizandro Rodriguez, Ignasi Ribas, Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Frequency analysis, Photosphere, 010308 nuclear & particles physics, Cepheid variable, Metallicity, Astronomy, Astronomy and Astrophysics, Orbital eccentricity, Astrophysics, Light curve, 01 natural sciences, law.invention, Amplitude, Space and Planetary Science, law, 0103 physical sciences, Variable star, 010303 astronomy & astrophysics
Abstract

Context. BL Cam is an extreme field multiperiodic short-period low-metallicity high-amplitude SX Phe-type variable where its probably complex pulsational content is subject of controversies. Aims. A comprehensive study has been carried out to investigate the nature and pulsational properties of this object. Methods. The analysis is based on new photometric data collected during the last few years at different sites, as well as on all available previously published data. Frequency analyses have been performed on a number of reliable data sets to analyse the pulsational content. In addition, the classical O−C method was used to study the behaviour of the main period. Results. Our frequency analysis confirms some aspects on the multiperiodicity of BL Cam, previously found by other authors, showing a number of secondary modes close to the main frequency f0 = 25.5769 cd −1 . The secondary modes present eventual amplitude variations. However, the main frequency exhibits no significant changes in its amplitude and seems to correspond to the fundamental mode of radial pulsation. Abrupt changes sometimes observed in the light curves could be due to spurious activity on or close to the star’s photosphere. We confirm the existence of a secondary frequency at 31.6 or 32.6 cd −1 , with variable amplitude, and with the possibility of both frequencies being intrinsic to the star. More than one hundred of new times of light maxima have been determined in the present work. These together with those available in the literature allow us a more discriminating analysis of the O–C diagram. This shows that the observed variations of the main period can be described by two terms: (i) a secular increase of the main period at a rate of dP/Pdt = 117(±3) × 10 −9 yr −1 ; and (ii) a perturbation from a companion star in a rather eccentric orbit with a period of 10.5(±0.2) yr causing a light time semi-amplitude of 148(±12) s.

Published
2006
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12. Programación de Matemáticas: CP, curso 1993/94

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 6-7 años extraídas del informe anual de la Escuela J. Michelet.

Published
1994

14. Actividades de Matemáticas: CM2, curso 1990/91

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas extraídas de la memoria anual de la Escuela J. Michelet.

Published
1990

15. Programación de Matemáticas: CE2, curso 1989/90

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, mathematics education
Abstract

Actividades matemáticas de alumnos de 8- 9 años extraídas del informe anual de la Escuela J. Michelet

Published
1990

16. Actividades de Matemáticas: Maternal Gs, curso 1989/90

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas extraídas de la memoria anual de la Escuela J. Michelet. Nivel Maternal Sección Grande 4.

Published
1990

22. Programación de Matemáticas: Maternal Ms3, curso 1986/87

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 4-5 años extraídas del informe anual de la Escuela J. Michelet.

Published
1987

23. Programación de Matemáticas: Maternal Ps1, curso 1980/81

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 3-4 años extraídas del informe anual (BILAN) de la escuela J. Michelet.

Published
1981

24. Programación de Matemáticas: CM1, curso 1985/86

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 9-10 años extraidas del informe anual de la Escuela J. Michelet

Published
1986

26. Programación de Matemáticas: Maternal Gs4, curso 1981/82

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 5-6 años extraídas del informe anual (BILAN) de la Escuela Maternal J. Michelet.

Published
1982

28. Programación de Matemáticas: CM1, curso 1981/82

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 9-10 años extraídas del informe anual de la Escuela J. Michelet.

Published
1982

29. Programación de Matemáticas: CM2, curso 1984/85

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 10-11 años extraídas del informe anual de la Escuela J. Michelet.

Published
1985

30. Programación de Matemáticas: CM2, curso 1979/80

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de10-11 años extraídas del informe anual de la Escuela J. Michelet.

Published
1980

31. Programación de Matemáticas: CE1, curso 1974/75

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las Matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 7-8 años extraídas del informe anual de la Escuela J. Michelet.

Published
1975

32. Programación de Matemáticas: Maternal Ps1, curso 1978/79

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las Matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 3-4 años, extraídas del informe anual de la Escuela J. Michelet.

Published
1979

35. Programación de Matemáticas: CM1, curso 1975/76

Author

Escuela J. Michelet

Subjects
Didáctica de las matemáticas, mathematics education
Abstract

Actividades matemáticas de alumnos de 9-10 años extraídas del informe anual de la Escuela J. Michelet

Published
1976

36. Programación de Matemáticas: CE1, curso 1983/84

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 7-8 años extraídas de la memoria anual de la Escuela J. Michelet.

Published
1984

37. Programación de Matemáticas: CM1, curso 1982/83

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas extraídas de la memoria anual de la Escuela J. Michelet. Nivel Curso Medio 1.

Published
1983

39. Programación de Matemáticas: Maternal Ps1, curso 1987/88

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 3-4 años extraídas del informe anual de la Escuela J. Michelet.

Published
1988

40. Programación de Matemáticas: Maternal Ms3, curso 1981/82

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas extraídas de la memoria anual de la Escuela J. Michelet. Nivel Maternal Sección 3.

Published
1982

42. Programación de Matemáticas: CE1, curso 1987/88

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 7-8 años extraídas del informe anual de la Escuela J. Michelet.

Published
1988

43. Programación de Matemáticas: CP, curso 1976/77

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 6-7 años extraídas del informe anual de la Escuela J. Michelet.

Published
1977

44. Programación de Matemáticas: CP, curso 1978/79

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 6-7 años extraídas del informe anual de la Escuela J. Michelet.

Published
1979

46. Programación de Matemáticas: Maternal Gs, curso 1986/87

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 5-6 extraídas de la memoria anual de la Escuel J. Michelet.

Published
1986

47. Programación de Matemáticas: Maternal Gs4, curso 1984/85

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 5-6 años extraídas del informe anual de la Escuela J. Michelet.

Published
1985

48. Programación de Matemáticas: Maternal Gs4, curso 1983/84

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 5-6 años extraídas del informe anual de la Escuela J. Michelet.

Published
1984

50. Programación de Matemáticas: Maternal Ps1, curso 1979/80

Author

Escuela J. Michelet and COREM

Subjects
Didáctica de las matemáticas, Mathematics education
Abstract

Actividades matemáticas de alumnos de 3- 4 años extraídas del informe anual de la Escuela J. Michelet.

Published
1980

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