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1. Post-conjunction detection of β Pictoris b with VLT/SPHERE

Author: A.-M. Lagrange, A. Boccaletti, M. Langlois, G. Chauvin, R. Gratton, H. Beust, S. Desidera, J. Milli, M. Bonnefoy, A. Cheetham, M. Feldt, M. Meyer, A. Vigan, B. Biller, M. Bonavita, J.-L. Baudino, F. Cantalloube, M. Cudel, S. Daemgen, P. Delorme, V. D’Orazi, J. Girard, C. Fontanive, J. Hagelberg, M. Janson, M. Keppler, T. Koypitova, R. Galicher, J. Lannier, H. Le Coroller, R. Ligi, A.-L. Maire, D. Mesa, S. Messina, A. Müeller, S. Peretti, C. Perrot, D. Rouan, G. Salter, M. Samland, T. Schmidt, E. Sissa, A. Zurlo, J.-L. Beuzit, D. Mouillet, C. Dominik, T. Henning, E. Lagadec, F. Ménard, H.-M. Schmid, M. Turatto, S. Udry, A. J. Bohn, B. Charnay, C. A. Gomez Gonzales, C. Gry, M. Kenworthy, Q. Kral, C. Mordasini, C. Moutou, G. van der Plas, J. E. Schlieder, L. Abe, J. Antichi, A. Baruffolo, P. Baudoz, J. Baudrand, P. Blanchard, A. Bazzon, T. Buey, M. Carbillet, M. Carle, J. Charton, E. Cascone, R. Claudi, A. Costille, A. Deboulbe, V. De Caprio, K. Dohlen, D. Fantinel, P. Feautrier, T. Fusco, P. Gigan, E. Giro, D. Gisler, L. Gluck, N. Hubin, E. Hugot, M. Jaquet, M. Kasper, F. Madec, Y. Magnard, P. Martinez, D. Maurel, D. Le Mignant, O. Möller-Nilsson, M. Llored, T. Moulin, A. Origné, A. Pavlov, D. Perret, C. Petit, J. Pragt, J. Szulagyi, and F. Wildi
Subjects: Astronomy, Astrophysics
Abstract: Context. With an orbital distance comparable to that of Saturn in the solar system, β Pictoris b is the closest (semi-major axis ≃9 au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to β Pictoris have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet’s orbital parameters. Aims. We aimed at further constraining β Pictoris b orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. Methods. We used SPHERE at the VLT to precisely monitor the orbital motion of beta β Pictoris b since first light of the instrument in 2014. Results. We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6 au) and prevented further detection. We redetected β Pictoris b on the northeast side of the disk at a separation of 139 mas and a PA of 30° in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of a = 9.0 ± 0.5 au (1σ), it definitely excludes previously reported possible long orbital periods, and excludes β Pictoris b as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away.
Published: 2019
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2. The SPHERE infrared survey for exoplanets (SHINE). I. Sample definition and target characterization

Author: E. L. Rickman, Julien Charton, Stéphane Udry, A. Roux, S. Rochat, Alice Zurlo, O. Möller-Nilsson, Riccardo Claudi, D. Fantinel, A. Pavlov, E. Covino, Christian Soenke, M. Kasper, Valentina D'Orazi, Anne-Lise Maire, Joshua E. Schlieder, J. Pragt, Enrico Cascone, Markus Janson, Mariangela Bonavita, T. Kopytova, C. Petit, P. Martinez, Mickael Bonnefoy, A. Deboulbe, Joany Andreina Manjarres Ramos, Franz-Josef Hambsch, L. Weber, Francois Menard, Thibaut Moulin, A. Bazzon, Yves Magnard, Norbert Hubin, F. Rigal, Thiam-Guan Tan, Eric Stadler, J.-F. Sauvage, T. O. B. Schmidt, Emmanuel Hugot, L. Gluck, Th. Henning, S. Benatti, Michael Meyer, Raphaël Galicher, Anne-Marie Lagrange, M. Feldt, M. Carle, Carsten Dominik, G. Rousset, Matthias Samland, Tristan Buey, Janis Hagelberg, H. M. Schmid, Philippe Feautrier, D. Le Mignant, Arnaud Sevin, H. LeCoroller, Pierre Baudoz, J. Antichi, Arthur Vigan, Wolfgang Brandner, Massimo Turatto, Gael Chauvin, Alain Origne, R. Ligi, P. Gigan, Bernardo Salasnich, C. Lazzoni, V. De Caprio, M. Jaquet, D. Gisler, Pascal Puget, Philippe Delorme, D. Perret, T. Fusco, Dino Mesa, E. Sissa, Francois Wildi, Silvano Desidera, D. Maurel, F. Madec, Joseph C. Carson, J. M. Alcalá, E. Rigliaco, S. Messina, J. Baudrand, Anne Costille, R. G. Gratton, M. Millward, André Müller, Beth Biller, Enrico Giro, Andrea Baruffolo, Faustine Cantalloube, Jean-Luc Beuzit, Ronald Roelfsema, Marcel Carbillet, Eric Lagadec, Kjetil Dohlen, R. Asensio-Torres, Anthony Cheetham, P. Rabou, M. Llored, Maud Langlois, P. Blanchard, Anthony Boccaletti, C. Fontanive, Marcos Suarez, L. Abe, and Low Energy Astrophysics (API, FNWI)
Subjects: PRE-MAIN SEQUENCE [STARS], HIGH CONTRAST IMAGING, STATISTICAL CONSTRAINTS, PLANET DETECTION, FOS: Physical sciences, Sample (statistics), Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ROTATION [STARS], ROTATION PERIOD, 01 natural sciences, 7. Clean energy, FUNDAMENTAL PARAMETERS [STARS], Planet, 0103 physical sciences, GENERAL [PLANETS AND SATELLITES], DETECTION LIMITS, Astrophysics::Solar and Stellar Astrophysics, KINEMATICS AND DYNAMICS [STARS], ACTIVITY [STARS], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astronomy and Astrophysics, TARGET CHARACTERIZATION, Light curve, Exoplanet, Characterization (materials science), SPHERES, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, ORIGINAL SAMPLE, STATISTICAL SAMPLES, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Rotation (mathematics), SURVEYS, STARS, EXTRASOLAR PLANETS, Astrophysics - Earth and Planetary Astrophysics
Abstract: Large surveys with new-generation high-contrast imaging instruments are needed to derive the frequency and properties of exoplanet populations with separations from ~5 to 300 au. A careful assessment of the stellar properties is crucial for a proper understanding of when, where, and how frequently planets form, and how they evolve. The sensitivity of detection limits to stellar age makes this a key parameter for direct imaging surveys. Aims. We describe the SpHere INfrared survey for Exoplanets (SHINE), the largest direct imaging planet-search campaign initiated at the VLT in 2015 in the context of the SPHERE Guaranteed Time Observations of the SPHERE consortium. In this first paper we present the selection and the properties of the complete sample of stars surveyed with SHINE, focusing on the targets observed during the first phase of the survey (from February 2015 to February 2017). This early sample composed of 150 stars is used to perform a preliminary statistical analysis of the SHINE data, deferred to two companion papers presenting the survey performance, main discoveries, and the preliminary statistical constraints set by SHINE. Methods. Based on a large database collecting the stellar properties of all young nearby stars in the solar vicinity (including kinematics, membership to moving groups, isochrones, lithium abundance, rotation, and activity), we selected the original sample of 800 stars that were ranked in order of priority according to their sensitivity for planet detection in direct imaging with SPHERE. The properties of the stars that are part of the early statistical sample wererevisited, including for instance measurements from the Gaia Data Release 2. Rotation periods were derived for the vast majority of the late-type objects exploiting TESS light curves and dedicated photometric observations. Results. The properties of individual targets and of the sample as a whole are presented. © ESO 2021. SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF – Osservatorio di Padova (Italy), Observatoire de Genève (Switzerland), ETH Zürich (Switzerland), NOVA (Netherlands), ONERA (France) and ASTRON (Netherlands) in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland) and NOVA (Netherlands). SPHERE also received funding from the European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004–2008), grant number 226 604 for FP7 (2009–2012) and grant number 312430 for FP7 (2013–2016). This research has made use of the SIMBAD database and Vizier services, operated at CDS, Strasbourg, France and of the Washington Double Star Catalog maintained at the US Naval Observatory. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. This paper has made use of data products available in ESO archive. Program ID: 60.A-9036(A); 072.C-0488(E) (PI Mayor), 074.C-0364(A) (PI Robichon), 074.C-0037(A) (PI Gunther), 075.C-0202(A) (PI Gunther), 075.C-0689(A) (PI Galland), 076.C-0010(A) (PI Gunther), 077.C-0012(A) (PI Gunther), 077.C-0295(D) (PI Galland), 078.D-0245(C) (PI Dall), 079.C-0046(A) (PI Gunther), 080.D-0151(A) (PI Hatzes), 080.C-0712(A) (PI Desort), 180.C-0886(A) (PI Bonfils), 082.C-0718(B) (PI Bonfils), 082.C-0427(A) (PI Doellinger), 082.C-0390(A) (PI Weise), 183.C-0437(A) (PI Bonfils), 083.C-0794(A) (PI Chauvin), 084.C-1039(A) (PI Chauvin), 184.C-0815(B) (PI Desort), 089.C-0732(A) (PI Lo Curto), 191.C-0873(D) (PI Bonfils), 192.C-0224(A) (PI Lagrange), 097.C-0864(B) (PI Lannier), 098.C-0739(A) (PI Lagrange), 099.C-0205(A) (PI Lagrange), 099.C-0458(A) (PI Lo Curto), 1101.C-0557(A) (PI Lagrange). We have used data from the WASP public archive in this research. The WASP consortium comprises of the University of Cambridge, Keele University, University of Leicester, The Open University, The Queen’s University Belfast, St. Andrews University and the Isaac Newton Group. Funding for WASP comes from the consortium universities and from the UK’s Science and Technology Facilities Council. Based on data retrieved from the SOPHIE archive at Observatoire de Haute-Provence (OHP), available at http://atlas.obs-hp.fr/sophie/. We thank the anonymous referee for useful comments. S.D., V.D., D.M. and R.G. acknowledge the support by INAF/Frontiera through the “Progetti Premiali” funding scheme of the Italian Ministry of Education, University, and Research, the PRIN-INAF 2019 “Planetary systems at young ages” (PLATEA) and the ASI-INAF agreement n.2018-16-HH.0. AV acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 757561). A.M.L. acknowledges funding from Agence Nationale de la Recherche (France) under contract number ANR-14-CE33-0018. J.C. was supported by SC Space Grant and Fulbright Colombia. M.B. acknowledges funding by the UK Science and Technology Facilities Council (STFC) grant no. ST/M001229.
Published: 2021

3. K-Stacker: an algorithm to hack the orbital parameters of planets hidden in high-contrast imaging: First applications to VLT/SPHERE multi-epoch observations

Author: Jean-Luc Beuzit, Arthur Vigan, Markus Feldt, Kjetil Dohlen, H. Le Coroller, E. Sissa, A. L. Maire, Pierre Vernazza, A. Schneeberger, Anthony Cheetham, S. Rochat, Michael R. Meyer, Thierry Fusco, Mariangela Bonavita, D. Estevez, D. Le Mignant, François Ménard, Joany Andreina Manjarres Ramos, Matthias Samland, Mathias Nowak, Mickael Bonnefoy, J. C. Lambert, Alice Zurlo, Valentina D'Orazi, Dino Mesa, Philippe Delorme, A. Boccaletti, Hervé Beust, R. Galicher, Roxanne Ligi, Gael Chauvin, A-M. Lagrange, Markus Janson, T. Fenouillet, Raffaele Gratton, David Mouillet, L. Arnold, M. Devinat, Silvano Desidera, Maud Langlois, J. Bec-Canet, C. Desgrange, Jean-François Sauvage, 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 d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Astronomy, Stockholm University, Department of Biochemistry and Molecular Biology, Mayo Clinic, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, University of Copenhagen = Københavns Universitet (KU), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), and University of Copenhagen = Københavns Universitet (UCPH)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], planets and satellites: dynamical evolution and stability, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Context (language use), Astrophysics, instrumentation: adaptive optics, 01 natural sciences, stars: individual: HD 95086, 03 medical and health sciences, Planet, instrumentation: high angular resolution, 0103 physical sciences, Gemini Planet Imager, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 030304 developmental biology, Orbital elements, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 0303 health sciences, stars: individual: β Pictoris, Astronomy and Astrophysics, Astrometry, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], methods: data analysis, Exoplanet, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Orbital motion, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Algorithm, Astrophysics - Earth and Planetary Astrophysics
Abstract: Recent high-contrast imaging surveys, looking for planets in young, nearby systems showed evidence of a small number of giant planets at relatively large separation beyond typically 20 au where those surveys are the most sensitive. Access to smaller physical separations between 5 and 20 au is the next step for future planet imagers on 10 m telescopes and ELTs in order to bridge the gap with indirect techniques (radial velocity, transit, astrometry with Gaia). In that context, we recently proposed a new algorithm, Keplerian-Stacker, combining multiple observations acquired at different epochs and taking into account the orbital motion of a potential planet present in the images to boost the ultimate detection limit. We showed that this algorithm is able to find planets in time series of simulated images of SPHERE even when a planet remains undetected at one epoch. Here, we validate the K-Stacker algorithm performances on real SPHERE datasets, to demonstrate its resilience to instrumental speckles and the gain offered in terms of true detection. This will motivate future dedicated multi-epoch observation campaigns in high-contrast imaging to search for planets in emitted and reflected light. Results. We show that K-Stacker achieves high success rate when the SNR of the planet in the stacked image reaches 7. The improvement of the SNR ratio goes as the square root of the total exposure time. During the blind test and the redetection of HD 95086 b, and betaPic b, we highlight the ability of K-Stacker to find orbital solutions consistent with the ones derived by the state of the art MCMC orbital fitting techniques, confirming that in addition to the detection gain, K-Stacker offers the opportunity to characterize the most probable orbital solutions of the exoplanets recovered at low signal to noise., Comment: Astronomy & Astrophysics accepted, 13 Pages, 11 Figures
Published: 2020
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4. The SPHERE infrared survey for exoplanets (SHINE)

Author: Kjetil Dohlen, André Müller, C. Petit, A. Pavlov, Valentina D'Orazi, Alexandre Emsenhuber, Alice Zurlo, E. Sissa, Ronald Roelfsema, Norbert Hubin, Marc Jaquet, Gabriel-Dominique Marleau, Gérard Rousset, Anthony Cheetham, H. Le Coroller, Alain Roux, S. Brown Sevilla, Enrico Giro, Faustine Cantalloube, Anne Costille, Janis Hagelberg, Jean-Luc Beuzit, Thierry Fusco, P. Gigan, Julien Charton, Markus Feldt, A. Bazzon, Ruben Asensio-Torres, C. Fontanive, Zahed Wahhaj, Anne-Lise Maire, Th. Henning, M. Carle, Marcel Carbillet, J. Ramos, Matthias Samland, Alain Origne, Raffaele Gratton, Arthur Vigan, Stéphane Udry, H. M. Schmid, Pierre Baudoz, Patrice Martinez, Markus Janson, O. Möller-Nilsson, L. Weber, Marcos Suarez, Cecile Gry, Michael Meyer, Sergio Messina, N. Engler, Emmanuel Hugot, Arnaud Sevin, A. Boccaletti, Alexander J. Bohn, P. Rabou, Julien Girard, T. Moulin, Jacopo Antichi, Beth Biller, F. Rigal, David Mouillet, C. Soenke, F. Madec, Riccardo Claudi, Silvano Desidera, M. Llored, E. Cascone, Daniela Fantinel, D. Gisler, R. Galicher, J. Baudrand, T. O. B. Schmidt, J. Pragt, Mickael Bonnefoy, D. Le Mignant, Mariangela Bonavita, Philippe Delorme, Jean-François Sauvage, Francois Wildi, Duncan Forgan, C. Mordasini, L. Gluck, Denis Perret, E. L. Rickman, Carsten Dominik, C. Lazzoni, E. Lagadec, Roxanne Ligi, Andrea Baruffolo, Lyu Abe, Gael Chauvin, A-M. Lagrange, Massimo Turatto, Pascal Puget, Philippe Feautrier, Yves Magnard, Bernardo Salasnich, Maud Langlois, V. De Caprio, D. Maurel, M. Kasper, Ken Rice, Dino Mesa, S. Rochat, C. Moutou, C. Perrot, Alain Delboulbé, P. Blanchard, François Ménard, Eric Stadler, Low Energy Astrophysics (API, FNWI), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Center for Space and Habitability (CSH), University of Bern, University of Edinburgh, Max Planck Institute for Radio Astronomy, Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Scottish Universities Physics Alliance (SUPA), Max Planck Institute for Astronomy (MPIA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Department of Biochemistry and Molecular Biology, Mayo Clinic, INAF - Osservatorio Astrofisico di Catania (OACT), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 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), Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), CHU Tenon [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), CHU Pitié-Salpêtrière [AP-HP], Laboratoire des biomolécules (LBM UMR 7203), Chimie Moléculaire de Paris Centre (FR 2769), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Hippolyte Fizeau (FIZEAU), INAF - Osservatorio Astronomico di Capodimonte (OAC), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen], European Southern Observatory (ESO), Environnements et Paléoenvironnements OCéaniques (EPOC), 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)-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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Institut de Recherche pour le Développement (IRD), Centre Hospitalier Henri Duffaut (Avignon), ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016), University of Michigan [Ann Arbor], University of Michigan System, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre for Exoplanet Science, Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Laboratoire Franco-Chilien d'Astronomie (LFCA), Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Chile, University of Geneva [Switzerland], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Anton Pannekoek Institute for Astronomy, University of Amsterdam [Amsterdam] (UvA), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), 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), Universidad Diego Portales [Santiago] (UDP), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Radboud university [Nijmegen], DAAA, ONERA, Université Paris Saclay [Meudon], Eberhard Karls Universität Tübingen, Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Lagrange, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS., Laboratoire de Biomécanique et Mécanique des Chocs (LBMC UMR T9406 ), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Université Gustave Eiffel, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université 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)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), CHU Tenon [APHP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université, Département Médico-Universitaire APPROCHES, Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université-Sorbonne Université (SU), Sorbonne Université-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Institut National de la Santé et de la Recherche Médicale (INSERM)-Chimie Moléculaire de Paris Centre (FR 2769), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), 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)-Centre National de la Recherche Scientifique (CNRS)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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, ARCHEORIENT - Environnements et sociétés de l'Orient ancien (Archéorient), Université Lumière - Lyon 2 (UL2)-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)-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), Institut des sciences analytiques et de physico-chimie pour l'environnement et les materiaux (IPREM), Université de Pau et des Pays de l'Adour (UPPA)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidad de Chile = University of Chile [Santiago] (UCHILE)-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción - University of Concepcion [Chile], Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Chimie Moléculaire de Paris Centre (FR 2769), Institut de Chimie du CNRS (INC)-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)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM), and Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: astro-ph.SR, astro-ph.GA, Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, planets and satellites: formation, 10. No inequality, infrared: planetary systems, 010303 astronomy & astrophysics, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Very Large Telescope, methods: statistical, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, techniques: high angular resolution, Astronomy and Astrophysics, Planetary system, Astrophysics - Astrophysics of Galaxies, Exoplanet, Accretion (astrophysics), Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: The SHINE project is a 500-star survey performed with SPHERE on the VLT for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. Here we present an initial statistical analysis for a subsample of 150 stars that are representative of the full SHINE sample. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 MJup and semimajor axes between 5 and 300 au. We adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Based on the results obtained for each star and on the 13 detections in the sample, we use a MCMC tool to compare our observations to two different types of models. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are $23.0_{-9.7}^{+13.5}\%$, $5.8_{-2.8}^{+4.7}\%$, and $12.6_{-7.1}^{+12.9}\%$ for BA, FGK, and M stars, respectively. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1-75 MJup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using our population model and restricting our sample to FGK stars, we derive a frequency of $5.7_{-2.8}^{+3.8}\%$, consistent with predictions from the parametric model. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies., Comment: 24 pages, 14 figures, 3 tables. Accepted for publication in A&A
Published: 2020
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5. Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70

Author: Jean-Loup Baudino, Janis Hagelberg, Christophe Pinte, Cyril Petit, Quentin Kral, A. Delboulbe, A. Pohl, Pierre Baudoz, Anne-Lise Maire, Eric Stadler, T. O. B. Schmidt, Alain Origne, F. Madec, Laura M. Pérez, N. Hubin, Enrico Giro, Marcos Suarez, Andrea Baruffolo, Anne-Marie Lagrange, Mario Flock, A. Pavlov, Jonathan Williams, P. Martinez, L. Abe, L. Gluck, Raffaele Gratton, G. Rousset, Jean-Luc Beuzit, Zahed Wahhaj, Esther Buenzli, Paul Mollière, S. S. Brems, Michael Meyer, P. Pinilla, Markus Janson, Tomas Stolker, M. Feldt, Pascal Puget, Christian Ginski, R. van Boekel, Myriam Benisty, Christoph Mordasini, D. Perret, Christian Soenke, R. G. van Holstein, D. Le Mignant, Francois Menard, F. Rigal, Patrick Rabou, Thierry Fusco, Massimo Turatto, Raphaël Galicher, J. de Boer, Th. Henning, N. Pawellek, J. Antichi, André Müller, Julien Milli, J. Lannier, Kjetil Dohlen, Ronald Roelfsema, Attila Juhasz, Yves Magnard, J. Pragt, Jean-Charles Augereau, M. Carle, Emmanuel Hugot, Miriam Keppler, Marcel Carbillet, Anthony Cheetham, Alice Zurlo, P. Blanchard, Andrea Isella, Tilman Birnstiel, S. Peretti, G. Salter, M. Bonnefoy, Juan-Luis Ramos, M. Llored, Laurent M. Mugnier, G.-D. Marleau, L. Weber, Anthony Boccaletti, Tristan Buey, Philippe Feautrier, Julien Girard, M. Kasper, Carsten Dominik, Faustine Cantalloube, Alexis Matter, Dino Mesa, Silvano Desidera, Stéphane Udry, Enrico Cascone, Arthur Vigan, Gael Chauvin, David Mouillet, C. Lazzoni, Andreas Bazzon, Riccardo Claudi, Jean-François Sauvage, Thibaut Moulin, E. Sissa, M. Cudel, Wolfgang Brandner, D. Gisler, Sascha P. Quanz, O. Moeller-Nilsson, Ralf Launhardt, Francois Wildi, M. Samland, Henning Avenhaus, Sylvain Rochat, Arnaud Sevin, Bernardo Salasnich, Maud Langlois, V. De Caprio, M. Jaquet, D. Maurel, Anne Costille, J. Kemmer, A. Roux, C. Perrot, D. Fantinel, Johan Olofsson, Cecile Gry, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), DOTA, ONERA, Université Paris Saclay (COmUE) [Palaiseau], ONERA-Université Paris Saclay (COmUE), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Oxford [Oxford], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Physikalisches Institut [Bern], Universität Bern [Bern], Hungarian Academy of Sciences (MTA), Ludwig-Maximilians-Universität München (LMU), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Kavli Institute for Theoretical Physics [Santa Barbara] (KITP), University of California [Santa Barbara] (UCSB), University of California-University of California, INAF - Osservatorio Astrofisico di Arcetri (OAA), Stockholm University, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), 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, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Department of Physical Geography and Ecosystem Science [Lund], Lund University [Lund], Universidad de Chile, University of Arizona, Monash Centre for Astrophysics (MoCA), Monash University [Clayton], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institute for Astronomy (IfA), University of Hawai‘i [Mānoa] (UHM), Geneva Observatory, University of Geneva [Switzerland], Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], INAF - Osservatorio Astronomico di Capodimonte (OAC), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], Department of Mathematics - University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, NOVA Optical Infrared Instrumentation Group, Universidade de Lisboa (ULISBOA), Anton Pannekoek Institute for Astronomy, Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Eberhard Karls Universität Tübingen, 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), DOTA, ONERA, Université Paris Saclay [Châtillon], Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Universiteit Leiden, University of Oxford, Universität Bern [Bern] (UNIBE), University of California [Santa Barbara] (UC Santa Barbara), University of California (UC)-University of California (UC), 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), Universidad de Chile = University of Chile [Santiago] (UCHILE), Université de Genève = University of Geneva (UNIGE), Universität Heidelberg [Heidelberg] = Heidelberg University, Universidade de Lisboa = University of Lisbon (ULISBOA), ANR-10-LABX-0056,OSUG@2020,Innovative strategies for observing and modelling natural systems(2010), European Project: 226604,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2008-1,OPTICON(2009), European Project: 312430,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2012-1-RTD,OPTICON(2013), and Low Energy Astrophysics (API, FNWI)
Subjects: Brightness, planets and satellites: detection, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Point source, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, symbols.namesake, stars: individual: PDS 70, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Rayleigh scattering, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, scattering, protoplanetary disks, techniques: high angular resolution, Astronomy and Astrophysics, Radius, Astrometry, Space and Planetary Science, radiative transfer, symbols, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: Young circumstellar disks are of prime interest to understand the physical and chemical conditions under which planet formation takes place. Only very few detections of planet candidates within these disks exist, and most of them are currently suspected to be disk features. In this context, the transition disk around the young star PDS 70 is of particular interest, due to its large gap identified in previous observations, indicative of ongoing planet formation. We aim to search for the presence of planets and search for disk structures indicative for disk-planet interactions and other evolutionary processes. We analyse new and archival near-infrared (NIR) images of the transition disk PDS 70 obtained with the VLT/SPHERE, VLT/NaCo and Gemini/NICI instruments in polarimetric differential imaging (PDI) and angular differential imaging (ADI) modes. We detect a point source within the gap of the disk at about 195 mas (about 22 au) projected separation. The detection is confirmed at five different epochs, in three filter bands and using different instruments. The astrometry results in an object of bound nature, with high significance. The comparison of the measured magnitudes and colours to evolutionary tracks suggests that the detection is a companion of planetary mass. We confirm the detection of a large gap of about 54 au in size within the disk in our scattered light images, and detect a signal from an inner disk component. We find that its spatial extent is very likely smaller than about 17 au in radius. The images of the outer disk show evidence of a complex azimuthal brightness distribution which may in part be explained by Rayleigh scattering from very small grains. Future observations of this system at different wavelengths and continuing astrometry will allow us to test theoretical predictions regarding planet-disk interactions, planetary atmospheres and evolutionary models., Comment: 23 pages, accepted by A&A
Published: 2018
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6. SUBARU prime focus spectrograph integration and performance at LAM

Author: A. Le Fur, Naoyuki Tamura, M. Belhadi, Stephen A. Smee, Rudy Barette, F. Roman, Kjetil Dohlen, Murdock Hart, F. Madec, M. Golebiowski, Ligia Souza de Oliveira, Philippe Balard, J. F. Gabriel, V. Lapere, Atsushi Shimono, Sandrine Pascal, James E. Gunn, D. Le Mignant, Décio Ferreira, M. Jaquet, P. Blanchard, M. Llored, Craig P. Loomis, Antonio Cesar de Oliveira, and J. Le Merrer
Subjects: Cryostat, Physics, business.industry, Near-infrared spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Collimated light, 010309 optics, Optics, Software, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, Focus (optics), Subaru Telescope, 010303 astronomy & astrophysics, Spectrograph, Astrophysics::Galaxy Astrophysics
Abstract: The Prime Focus Spectrograph (PFS) of the Subaru Measurement of Images and Redshifts (SuMIRe) project for Subaru telescope includes four identical spectrograph modules fed by 600 fibers each. This paper presents the integration, alignment and test procedures for the first spectrograph module composed by an optical entrance unit that creates a collimated beam and distributes the light to three channels, two visible and one near infrared. In particular, we present the performance of the single Red channel module. Firstly, we report on the measured optical performance: optical quality and ghost analysis. We also report on the thermal performance of the visible camera cryostat. Finally, we describe the software used to control and monitor the instrument.
Published: 2018
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7. Discovery of a brown dwarf companion to the star HIP 64892

Author: Jacopo Antichi, L. Weber, E. Sissa, Johan Olofsson, H. Le Coroller, Markus Kasper, Damien Ségransan, Alain Roux, T. Buey, Alice Zurlo, Cyril Petit, Alain Delboulbé, Andrea Baruffolo, Thomas Henning, Arnaud Sevin, P. Blanchard, Ronald Roelfsema, Daniela Fantinel, Alain Origne, R. Ligi, Anne Costille, M. Carle, Kjetil Dohlen, François Ménard, Bernardo Salasnich, Maud Langlois, Pierre Baudoz, V. De Caprio, Enrico Giro, D. Maurel, Lyu Abe, Markus Janson, O. Möller-Nilsson, Raffaele Gratton, Jean-Luc Beuzit, Riccardo Claudi, Beth Biller, Eric Stadler, Valentina D'Orazi, Massimo Turatto, Marc Jaquet, Joshua E. Schlieder, Pascal Puget, Taisiya Kopytova, Yves Magnard, Arthur Vigan, C. Soenke, Anthony Cheetham, Anne-Lise Maire, Patrice Martinez, D. Le Mignant, Gérard Rousset, A. Pavlov, Norbert Hubin, M. Keppler, Anne-Marie Lagrange, Emmanuel Hugot, Eric Lagadec, Hubert Klahr, Daniel Rouan, Dino Mesa, Michael Meyer, Thierry Fusco, Janis Hagelberg, Markus Feldt, Philippe Feautrier, Joany Andreina Manjarres Ramos, Quentin Kral, M. Llored, E. Cascone, Marcel Carbillet, S. Rochat, T. O. B. Schmidt, Mickael Bonnefoy, T. Moulin, S. Peretti, P. Rabou, David Mouillet, L. Gluck, J. Pragt, Gael Chauvin, F. Madec, Jean-François Sauvage, Francois Wildi, C. Mordasini, Denis Perret, Carsten Dominik, Anthony Boccaletti, F. Rigal, Marcos Suarez, Stéphane Udry, Silvano Desidera, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Universidad de Chile, Universidad de Valparaiso [Chile], Stockholm University, University of Edinburgh, Instituto de Astronomia y ciencias Planetarias de Atacama (INCT), Universidad de Atacama, University of Cambridge [UK] (CAM), NASA Goddard Space Flight Center (GSFC), University of Bern, Universidad Diego Portales [Santiago] (UDP), Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Mathematics - University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Arizona State University [Tempe] (ASU), Ural Federal University [Ekaterinburg] (UrFU), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), 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, 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), INAF - Osservatorio Astrofisico di Arcetri (OAA), INAF - Osservatorio Astronomico di Capodimonte (OAC), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), European Southern Observatory (ESO), NOVA Optical Infrared Instrumentation Group, European Southern Observatory [Santiago] (ESO), Université de Genève = University of Geneva (UNIGE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidad de Chile = University of Chile [Santiago] (UCHILE), 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), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), 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), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, 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), Low Energy Astrophysics (API, FNWI), Department of Physical Geography and Ecosystem Science [Lund], Lund University [Lund], Institute for Astronomy [Edinburgh] (IfA), Geneva Observatory, Department of Biochemistry and Molecular Biology, Mayo Clinic, Observatoire de Paris, Université Paris sciences et lettres (PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], INDIVIDUAL: HIP 64892 [STARS], HIGH ANGULAR RESOLUTIONS [TECHNIQUES], 530 Physics, Astrophysics::High Energy Astrophysical Phenomena, BROWN DWARFS, FOS: Physical sciences, Library science, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, DETECTIONS [PLANETS AND SATELLITES], OPTIQUE ADAPTATIVE, 01 natural sciences, Techniques: high angular resolution, VLT, 0103 physical sciences, DETECTION [PLANETS AND SATELLITES], Astrophysics::Solar and Stellar Astrophysics, European commission, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Stars: brown dwarfs individual: HIP 64892, HIGH ANGULAR RESOLUTION [TECHNIQUES], Earth and Planetary Astrophysics (astro-ph.EP), Physics, ASTRONOMIE, INDIVIDUAL [STARS], 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 520 Astronomy, EFFECTIVE TEMPERATURE, Astronomy and Astrophysics, Planets and satellites: detection, 500 Science, 620 Engineering, EVOLUTIONARY MODELS, Astrophysics - Solar and Stellar Astrophysics, FORMATION AND EVOLUTIONS, Space and Planetary Science, ATMOSPHERES [SATELLITES], SPECTRAL ENERGY DISTRIBUTION, Christian ministry, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SATELLITES, STARS, Astrophysics - Earth and Planetary Astrophysics, PLANETS
Abstract: We report the discovery of a bright, brown dwarf companion to the star HIP 64892, imaged with VLT/SPHERE during the SHINE exoplanet survey. The host is a B9.5V member of the Lower-Centaurus-Crux subgroup of the Scorpius Centaurus OB association. The measured angular separation of the companion ($1.2705\pm0.0023$") corresponds to a projected distance of $159\pm12$ AU. We observed the target with the dual-band imaging and long-slit spectroscopy modes of the IRDIS imager to obtain its SED and astrometry. In addition, we reprocessed archival NACO L-band data, from which we also recover the companion. Its SED is consistent with a young (, Comment: 12 pages, 11 figures, accepted for publication in A&A
Published: 2018
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8. Assembly, integration, test, and verification scenarios for the ELT MOSAIC instrument

Author: D. Le Mignant, Francois Hammer, F. Madec, Marc Ferrari, Kjetil Dohlen, Ewan Fitzsimons, Thierry Fusco, P. Vola, Marc Dubbeldam, Jean-Gabriel Cuby, K. El Hadi, Tim Morris, Fanny Chemla, P. Jagourel, Benoit Neichel, 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), W.M. Keck Observatory, 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), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Durham University, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Compagnie industrielle des lasers [Orléans] (CILAS), Compagnie industrielle des lasers (CILAS), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, PSL Research University (PSL)-PSL Research University (PSL)-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), and 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)
Subjects: ADAPTIVE OPTICS, AIV, Computer science, Integration testing, business.industry, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], AIT, Mosaic (geodemography), Modular design, LAM, EXTREMELY LARGE TELESCOPES, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, ELT-MOS, MOSAIC, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010309 optics, MULTI-OBJECT SPECTROGRAPH, Identification (information), 0103 physical sciences, Systems engineering, business, 010303 astronomy & astrophysics
Abstract: International audience; Assembly, Integration, Test and Validation (AIT/V) phases for AO instruments, in laboratory as in the telescope, represent numerous technical challenges. The Laboratoire d’Astrophysique de Marseille (LAM) is in charge of the AIT/V preparation and planning for the MOSAIC (ELT-MOS) instrument, from identification of needs, challenges, risks, to defining the optimal AIT strategy for this highly modular and serialized instrument. In this paper, we present the status of this study and describe several AIT/V scenarios as well as a planning for AIT phases in Europe and in Chile. We also show our capabilities, experience and expertise to lead the instrument MOSAIC AIT/V activities.
Published: 2018
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9. Investigating the young solar system analog HD 95086. A combined HARPS and SPHERE exploration

Author: Eric Lagadec, C. Perrot, H. Le Coroller, R. van Boekel, Silvano Desidera, N. Meunier, D. Perret, P. Feautrier, Mickael Bonnefoy, Mariangela Bonavita, Christian Ginski, C. Lazzoni, Miriam Keppler, Joany Andreina Manjarres Ramos, C. Fontanive, Matthias Samland, S. Peretti, Johan Olofsson, P. Janin-Potiron, J. Hagelberg, H. Beust, Wolfgang Brandner, Markus Janson, S. Rochat, J.-L. Beuzit, Attila Moór, S. Borgniet, Th. Henning, M. Cudel, A. Boccaletti, Anthony Cheetham, G. Salter, L. Rodet, Anne-Lise Maire, G. Chauvin, Sergio Messina, Andreas Bazzon, J. Lannier, Sascha P. Quanz, Anne-Marie Lagrange, R. G. Gratton, P. Delorme, Raphaël Galicher, Maud Langlois, Francois Menard, Arthur Vigan, J. de Boer, David Mouillet, Henning Avenhaus, E. Sissa, T. Bhowmik, Dino Mesa, J. Milli, Q. Kral, D. Le Mignant, T. O. B. Schmidt, Michael Meyer, M. Feldt, and Alice Zurlo
Subjects: Physics, Debris disk, Solar System, Giant planet, Astronomy and Astrophysics, Astrophysics, Planetary system, 01 natural sciences, 010309 optics, Radial velocity, Orbit, Space and Planetary Science, Planet, 0103 physical sciences, Spectral energy distribution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Context. HD 95086 (A8V, 17 Myr) hosts a rare planetary system for which a multi-belt debris disk and a giant planet of 4–5 MJup have been directly imaged. Aims. Our study aims to characterize the global architecture of this young system using the combination of radial velocity and direct imaging observations. We want to characterize the physical and orbital properties of HD 95086 b, search for additional planets at short and wide orbits and image the cold outer debris belt in scattered light. Methods. We used HARPS at the ESO 3.6 m telescope to monitor the radial velocity of HD 95086 over two years and investigate the existence of giant planets at less than 3 au orbital distance. With the IRDIS dual-band imager and the IFS integral field spectrograph of SPHERE at VLT, we imaged the faint circumstellar environment beyond 10 au at six epochs between 2015 and 2017. Results. We do not detect additional giant planets around HD 95086. We identify the nature (bound companion or background contaminant) of all point-like sources detected in the IRDIS field of view. None of them correspond to the ones recently discovered near the edge of the cold outer belt by ALMA. HD 95086 b is resolved for the first time in J-band with IFS. Its near-infrared spectral energy distribution is well fitted by a few dusty and/or young L7–L9 dwarf spectral templates. The extremely red 1–4 μm spectral distribution is typical of low-gravity objects at the L/T spectral type transition. The planet’s orbital motion is resolved between January 2015 and May 2017. Together with past NaCo measurements properly re-calibrated, our orbital fitting solutions favor a retrograde low to moderate-eccentricity orbit e = 0.2+0.3−0.2, with a semi-major axis ~52 au corresponding to orbital periods of ~288 yr and an inclination that peaks at i = 141°, which is compatible with a planet-disk coplanar configuration. Finally, we report the detection in polarimetric differential imaging of the cold outer debris belt between 100 and 300 au, consistent in radial extent with recent ALMA 1.3 mm resolved observations.
Published: 2018

10. Testing giant planet formation in the transitional disk of SAO 206462 using deep VLT/SPHERE imaging

Author: Christian Thalmann, Gael Chauvin, Dino Mesa, M. Millward, J. Lannier, T. Buey, Alice Zurlo, C. Perrot, S. Messina, Arthur Vigan, Carsten Dominik, Anne-Lise Maire, Silvano Desidera, R. Galicher, Anne-Marie Lagrange, Adriana Pohl, Matthias Samland, Thayne Currie, Anthony Boccaletti, Enrico Giro, Mickael Bonnefoy, André Müller, E. Sissa, Norbert Hubin, Thierry Fusco, Markus Feldt, Michael Meyer, Maud Langlois, Tomas Stolker, Raffaele Gratton, Wolfgang Brandner, Jose Ramos, D. Le Mignant, Esther Buenzli, Stéphane Udry, Carol A. Grady, Christian Ginski, R. van Boekel, Graeme Salter, L. Weber, Beth Biller, Thomas Henning, S. Peretti, Eric Stadler, Sascha P. Quanz, Low Energy Astrophysics (API, FNWI), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, National Astronomical Observatory of Japan (NAOJ), GSFC Exoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center (GSFC), 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 Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), York Creek Observatory, Heidelberg University, International Max Planck Research School on Astrophysics (IMPRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Department of Astronomy University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Universidad Diego Portales [Santiago] (UDP), Universidad de Santiago de Chile [Santiago] (USACH), INAF - Osservatorio Astronomico di Padova (OAPD), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-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), Universiteit Leiden, Université de Genève = University of Geneva (UNIGE), Exoplanets and Stellar Astrophysics Lab, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), ONERA, Astronomical Institute Anton Pannekoek, University of Amsterdam, INAF-Osservatorio Astrofisico di Catania (INAF-OACt), Institute for Astronomy, The University of Edinburgh, Royal Observatory, Blackford Hill View, Edinburgh, EH9 3HJ, UK, National Astronomical Observatory of Japan, Subaru Telescope, Hilo, HI, 96720, USA, Exoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center, Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, York Creek Observatory, Georgetown, Tasmania, Australia, Department of Astronomy, University of Michigan, 1085 S. University Ave, Ann Arbor, MI, 48109-1107, USA, Institute for Astronomy, Department of Physics, ETH Zürich, Nucleo de Astronomia, Facultad de Ingenieria, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile, INAF-Osservatorio Astronomico di Padova, Leiden Observatory, and ISDC, Geneva Observatory, University of Geneva
Subjects: IMAGE PROCESSING, INDIVIDUAL, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, OPTIQUE ADAPTATIVE, 01 natural sciences, Density wave theory, Jupiter, VLT, DATA ANALYSIS, SPHERE, Planet, TECHNIQUES, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Spiral, Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, SAO 206462 (HD 135344B), Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Giant planet, HIGH ANGULAR RESOLUTION, Astronomy and Astrophysics, SPECTROSCOPIC, 13. Climate action, Space and Planetary Science, METHODS, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Protoplanet, STARS, Astrophysics - Earth and Planetary Astrophysics, PLANETARY DISKS
Abstract: Context. The SAO 206462 (HD 135344B) disk is one of the few known transitional disks showing asymmetric features in scattered light and thermal emission. Near-infrared scattered-light images revealed two bright outer spiral arms and an inner cavity depleted in dust. Giant protoplanets have been proposed to account for the disk morphology. Aims. We aim to search for giant planets responsible for the disk features and, in the case of non-detection, to constrain recent planet predictions using the data detection limits. Methods. We obtained new high-contrast and high-resolution total intensity images of the target spanning the Y to the K bands (0.95-2.3 mic) using the VLT/SPHERE near-infrared camera and integral field spectrometer. Results. The spiral arms and the outer cavity edge are revealed at high resolutions and sensitivities without the need for image post-processing techniques, which introduce photometric biases. We do not detect any close-in companions. For the derivation of the detection limits on putative giant planets embedded in the disk, we show that the knowledge of the disk aspect ratio and viscosity is critical for the estimation of the attenuation of a planet signal by the protoplanetary dust because of the gaps that these putative planets may open. Given assumptions on these parameters, the mass limits can vary from ~2-5 to ~4-7 Jupiter masses at separations beyond the disk spiral arms. The SPHERE detection limits are more stringent than those derived from archival NaCo/L' data and provide new constraints on a few recent predictions of massive planets (4-15 MJ) based on the spiral density wave theory. The SPHERE and ALMA data do not favor the hypotheses on massive giant planets in the outer disk (beyond 0.6). There could still be low-mass planets in the outer disk and/or planets inside the cavity., A&A, in press. 16 pages, 17 figures. Updated to match proofs
Published: 2017
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11. ZELDA, a Zernike sensor for accurate calibration of aberrations in coronagraphic instruments: validation in VLT/SPHERE and preliminary on-sky results

Author: P. Blanchard, J.-F. Sauvage, Julien Girard, Mamadou N'Diaye, Anne Costille, M. Kasper, J. Le Merrer, J. L. Beuzit, Gérard Zins, F. Madec, D. Le Mignant, A. Caillat, T. Fusco, David Mouillet, Kjetil Dohlen, and Arthur Vigan
Subjects: Physics, symbols.namesake, Sky, Calibration (statistics), Zernike polynomials, media_common.quotation_subject, symbols, media_common, Remote sensing
Published: 2017
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12. Calibration of quasi-static aberrations in exoplanet direct-imaging instruments with a Zernike phase-mask sensor II. Concept validation with ZELDA on VLT/SPHERE

Author: F. Madec, Kjetil Dohlen, Anne Costille, G. Zins, Jean-François Sauvage, J. Le Merrer, Pascal Puget, Gabriel Moreaux, Thierry Fusco, P. Blanchard, Arthur Vigan, J. L. Beuzit, Julien Girard, Mamadou N'Diaye, A. Caillat, D. Le Mignant, David Mouillet, Space Telescope Science Institute (STSci), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), ONERA, Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)
Subjects: TELESCOPE, Zernike polynomials, Brown dwarf, FOS: Physical sciences, METHODS: DATA ANALYSIS, Astrophysics, OPTIQUE ADAPTATIVE, 01 natural sciences, 7. Clean energy, Deformable mirror, HIGH ANGULAR RESOLLUTION, law.invention, 010309 optics, symbols.namesake, Optics, law, Planet, RESOLUTION ANGULAIRE ELEVEE, 0103 physical sciences, TECHNIQUES, ANALYSE DONNEES, INSTRUMENTATION, Adaptive optics, 010303 astronomy & astrophysics, Coronagraph, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), ADAPTIVE OPTICS, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, HIGH ANGULAR RESOLUTION, Astronomy and Astrophysics, Wavefront sensor, Exoplanet, 13. Climate action, Space and Planetary Science, symbols, TELESCOPES, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Warm or massive gas giant planets, brown dwarfs, and debris disks around nearby stars are now routinely observed by dedicated high-contrast imaging instruments on large, ground-based observatories. These facilities include extreme adaptive optics (ExAO) and state-of-the-art coronagraphy to achieve unprecedented sensitivities for exoplanet detection and spectral characterization. However, differential aberrations between the ExAO sensing path and the science path represent a critical limitation for the detection of giant planets with a contrast lower than a few $10^{-6}$ at very small separations (, 13 pages, 12 figures, A&A accepted on June 3rd, 2016. v2 after language editing
Published: 2016
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13. First light of the VLT planet finder SPHERE I. Detection and characterization of the substellar companion GJ 758 B

Author: A. Vigan, M. Bonnefoy, C. Ginski, H. Beust, R. Galicher, M. Janson, J.-L. Baudino, E. Buenzli, J. Hagelberg, V. D’Orazi, S. Desidera, A.-L. Maire, R. Gratton, J.-F. Sauvage, G. Chauvin, C. Thalmann, L. Malo, G. Salter, A. Zurlo, J. Antichi, A. Baruffolo, P. Baudoz, P. Blanchard, A. Boccaletti, J.-L. Beuzit, M. Carle, R. Claudi, A. Costille, A. Delboulbé, K. Dohlen, C. Dominik, M. Feldt, T. Fusco, L. Gluck, J. Girard, E. Giro, C. Gry, T. Henning, N. Hubin, E. Hugot, M. Jaquet, M. Kasper, A.-M. Lagrange, M. Langlois, D. Le Mignant, M. Llored, F. Madec, P. Martinez, D. Mawet, D. Mesa, J. Milli, D. Mouillet, T. Moulin, C. Moutou, A. Origné, A. Pavlov, D. Perret, C. Petit, J. Pragt, P. Puget, P. Rabou, S. Rochat, R. Roelfsema, B. Salasnich, H.-M. Schmid, A. Sevin, R. Siebenmorgen, A. Smette, E. Stadler, M. Suarez, M. Turatto, S. Udry, F. Vakili, Z. Wahhaj, L. Weber, F. Wildi, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Leiden Observatory [Leiden], Universiteit Leiden, 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), Stockholm University, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Macquarie University, Monash University [Melbourne], DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), CFHT, Universidad Diego Portales [Santiago] (UDP), Universidad de Santiago de Chile [Santiago] (USACH), INAF - Osservatorio Astrofisico di Arcetri (OAA), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Environnements et Paléoenvironnements OCéaniques (EPOC), 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)-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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), De la Molécule aux Nanos-objets : Réactivité, Interactions et Spectroscopies (MONARIS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), NOVA Optical Infrared Instrumentation Group, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), European Synchrotron Radiation Facility (ESRF), Centre de Recherche en Acquisition et Traitement de l'Image pour la Santé (CREATIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Low Energy Astrophysics (API, FNWI), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden [Leiden], Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Genève (UNIGE), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), UMR 5805 Environnements et Paléoenvironnements Océaniques et Continentaux (EPOC), 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), Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-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), Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Institut de Chimie du CNRS (INC)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Proper motion, 010308 nuclear & particles physics, Monte Carlo method, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Markov chain Monte Carlo, Astrophysics, Astrometry, First light, 01 natural sciences, Photometry (optics), symbols.namesake, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: GJ758 B is a brown dwarf companion to a nearby (15.76 pc) solar-type, metal-rich (M/H = +0.2 dex) main-sequence star (G9V) that was discovered with Subaru/HiCIAO in 2009. From previous studies, it has drawn attention as being the coldest (~600K) companion ever directly imaged around a neighboring star. We present new high-contrast data obtained during the commissioning of the SPHERE instrument at the VLT. The data was obtained in Y-, J-, H-, and Ks-bands with the dual-band imaging (DBI) mode of IRDIS, providing a broad coverage of the full near-infrared (near-IR) range at higher contrast and better spectral sampling than previously reported. In this new set of high-quality data, we report the re-detection of the companion, as well as the first detection of a new candidate closer-in to the star. We use the new 8 photometric points for an extended comparison of GJ758 B with empirical objects and 4 families of atmospheric models. From comparison to empirical object, we estimate a T8 spectral type, but none of the comparison object can accurately represent the observed near-IR fluxes of GJ758 B. From comparison to atmospheric models, we attribute a Teff = 600K $\pm$ 100K, but we find that no atmospheric model can adequately fit all the fluxes of GJ758 B. The photometry of the new candidate companion is broadly consistent with L-type objects, but a second epoch with improved photometry is necessary to clarify its status. The new astrometry of GJ758 B shows a significant proper motion since the last epoch. We use this result to improve the determination of the orbital characteristics using two fitting approaches, Least-Square Monte Carlo and Markov Chain Monte Carlo. Finally, we analyze the sensitivity of our data to additional closer-in companions and reject the possibility of other massive brown dwarf companions down to 4-5 AU. [abridged], 20 pages, 15 figures. Accepted for publication in A&A
Published: 2016
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14. Resolving faint structures in the debris disk around TWA 7

Author: Francois Menard, Maud Langlois, Markus Janson, R. G. van Holstein, R. G. Gratton, Philippe Feautrier, Claudio Caceres, Wolfgang Brandner, D. Mawet, Graeme Salter, Th. Henning, E. Sissa, Amelia Bayo, Dino Mesa, M. Feldt, A. Roux, A. Pavlov, C. A. Grady, Gael Chauvin, Silvano Desidera, C. Perrot, David Mouillet, J. Lannier, Ch. Ginski, Philippe Thébault, Johan Olofsson, Thibaut Moulin, A-L. Maire, D. Le Mignant, A-M. Lagrange, T. Schmidt, Matthias R. Schreiber, C. Lazzoni, R. Ligi, Julien Milli, N. Godoy, C. Thalmann, Stephen Durkan, P. Rabou, Janis Hagelberg, Christophe Pinte, Quentin Kral, Anthony Boccaletti, L. Abe, Esther Buenzli, N. Engler, Hector Canovas, Arthur Vigan, Gérard Rousset, J. C. Augereau, Joshua E. Schlieder, S. Peretti, Ruben Asensio-Torres, and Mickael Bonnefoy
Subjects: Physics, Debris disk, Spiral galaxy, 010504 meteorology & atmospheric sciences, instrumentation: polarimeters, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Position angle, circumstellar matter, 01 natural sciences, Stars, instrumentation: high angular resolution, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Low Mass, 010303 astronomy & astrophysics, Planetary mass, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: Context. Debris disks are the intrinsic by-products of the star and planet formation processes. Most likely due to instrumental limitations and their natural faintness, little is known about debris disks around low mass stars, especially when it comes to spatially resolved observations. Aims. We present new VLT/SPHERE IRDIS dual-polarization imaging (DPI) observations in which we detect the dust ring around the M2 spectral type star TWA 7. Combined with additional angular differential imaging observations we aim at a fine characterization of the debris disk and setting constraints on the presence of low-mass planets. Methods. We modeled the SPHERE DPI observations and constrain the location of the small dust grains, as well as the spectral energy distribution of the debris disk, using the results inferred from the observations, and performed simple N-body simulations. Results. We find that the dust density distribution peaks at ~0.72′′ (25 au), with a very shallow outer power-law slope, and that the disk has an inclination of ~13° with a position angle of ~91° east of north. We also report low signal-to-noise ratio detections of an outer belt at a distance of ~1.5′′ (~52 au) from the star, of a spiral arm in the southern side of the star, and of a possible dusty clump at 0.11′′. These findings seem to persist over timescales of at least a year. Using the intensity images, we do not detect any planets in the close vicinity of the star, but the sensitivity reaches Jovian planet mass upper limits. We find that the SED is best reproduced with an inner disk at ~0.2′′ (~7 au) and another belt at 0.72′′ (25 au). Conclusions. We report the detections of several unexpected features in the disk around TWA 7. A yet undetected 100M⊕ planet with a semi-major axis at 20−30 au could possibly explain the outer belt as well as the spiral arm. We conclude that stellar winds are unlikely to be responsible for the spiral arm.
Published: 2018
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15. First light of the VLT planet finder SPHERE. II. The physical properties and the architecture of the young systems PZ Telescopii and HD 1160 revisited

Author: Th. Henning, Emmanuel Hugot, Cyril Petit, Julien Milli, Massimo Turatto, Dimitri Mawet, Silvano Desidera, M. Kasper, O. Möller-Nilsson, Stéphane Udry, Alice Zurlo, A. Pavlov, Enrico Giro, Cecile Gry, M. Millward, Andrea Baruffolo, David Ehrenreich, Sergio Messina, Enrico Cascone, Jean-Luc Beuzit, M. Llored, T. Kopytova, Zahed Wahhaj, Andreas Bazzon, P. Martinez, Norbert Hubin, C. Moutou, Mickael Bonnefoy, Thibaut Moulin, Raffaele Gratton, Kjetil Dohlen, P. Blanchard, L. Weber, S. Rochat, Ch. Ginski, Riccardo Claudi, Pascal Puget, Anne Costille, Alain Origne, M. Carle, D. Le Mignant, Gael Chauvin, David Mouillet, H. M. Schmid, A. Delboulbe, M. Feldt, Anthony Boccaletti, Raphaël Galicher, Arthur Vigan, J. Pragt, D. Gisler, C. Thalmann, Jacopo Antichi, L. Gluck, Jose Ramos, J. de Boer, Anne-Marie Lagrange, Anne-Lise Maire, Ronald Roelfsema, Thierry Fusco, Julien Girard, Farrokh Vakili, Dino Mesa, Bernardo Salasnich, Maud Langlois, V. De Caprio, M. Jaquet, Carsten Dominik, Jean-François Sauvage, Francois Wildi, F. Madec, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), INAF - Osservatorio Astrofisico di Catania (OACT), 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, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Geneva Observatory, University of Geneva [Switzerland], Universidad Diego Portales [Santiago] (UDP), Departamento de Astronomia (DAS), Universidad de Santiago de Chile [Santiago] (USACH), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Euratom/UKAEA Fusion Assoc., Culham Science Centre [Abingdon], Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), ONERA - The French Aerospace Lab [Châtillon], ONERA, Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), ESO, Physics Department [Garching], Technical University of Munich (TUM)-Technical University of Munich (TUM), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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)-Centre National de la Recherche Scientifique (CNRS), Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Canada-France-Hawaii Telescope Corporation, NASA Goddard Space Flight Center (GSFC), De la Molécule aux Nanos-objets : Réactivité, Interactions et Spectroscopies (MONARIS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), European Synchrotron Radiation Facility (ESRF), Centre de Recherche en Acquisition et Traitement de l'Image pour la Santé (CREATIS), Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Universiteit Leiden, 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Université de Genève = University of Geneva (UNIGE), ONERA-Université Paris Saclay (COmUE), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM)-Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Environnements et Paléoenvironnements OCéaniques (EPOC), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), 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), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Institut de Chimie du CNRS (INC)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), and Low Energy Astrophysics (API, FNWI)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Very Large Telescope, 010308 nuclear & particles physics, Metallicity, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, 01 natural sciences, Exoplanet, Luminosity, Photometry (optics), Space and Planetary Science, 0103 physical sciences, Spectral energy distribution, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: [Abridged] Context. The young systems PZ Tel and HD 1160, hosting known low-mass companions, were observed during the commissioning of the new planet finder SPHERE with several imaging and spectroscopic modes. Aims. We aim to refine the physical properties and architecture of both systems. Methods. We use SPHERE commissioning data and REM observations, as well as literature and unpublished data from VLT/SINFONI, VLT/NaCo, Gemini/NICI, and Keck/NIRC2. Results. We derive new photometry and confirm the nearly daily photometric variability of PZ Tel A. Using literature data spanning 38 yr, we show that the star also exhibits a long-term variability trend. The 0.63-3.8 mic SED of PZ Tel B allows us to revise its properties: spectral type M7+/-1, Teff=2700+/-100 K, log(g)0.66) of PZ Tel B. For e4 MJ) outside 0.5" for the PZ Tel system. We also show that K1-K2 color can be used with YJH low-resolution spectra to identify young L-type companions, provided high photometric accuracy (, 25 pages, 23 figures, accepted for publication in A&A on Oct. 13th, 2015; version including language editing. Typo on co-author name on astroph page corrected, manuscript unchanged
Published: 2016
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16. Direct measurement of the size, shape, and pole of 511 Davida with Keck AO in a single night

Author: William J. Merline, Thierry Fusco, Jack D. Drummond, Randy Campbell, Christophe Dumas, Robert W. Goodrich, Frederic H. Chaffee, Shui Kwok, R. I. Knight, Al Conrad, and D. Le Mignant
Subjects: Physics, Solar System, Ecliptic coordinate system, business.industry, Astronomy and Astrophysics, Radius, Astrophysics, Light curve, Rotation, Ellipsoid, law.invention, Telescope, Optics, Space and Planetary Science, law, Asteroid, business
Abstract: Using the high-quality data set of 165 images taken at 11 epochs over the 5.13 h rotation of the large C-type Asteroid 511 Davida, we find the dimensions of its triaxial ellipsoid model to be 357 ± 2 × 294 ± 2 × 231 ± 50 km . The images were acquired with the adaptive optics system on the 10 m Keck II telescope on December 27, 2002. The a and b diameters are much better determined than previously estimated from speckle interferometry and indirect measurements, and our mean diameter, ( a b c ) 1 / 3 = 289 ± 21 km , is 19% below previous estimates. We find the pole to lie within 2° of [ RA = 295 ° ; Dec = 0 ° ] or in Ecliptic coordinates [ λ = 297 ° ; β = + 21 ° ], a significant improvement to the pole direction. Otherwise, previous determinations of the axial ratios agree with our new results. These observations illustrate that our technique of finding the dimensions and pole of an asteroid from its changing projected size and shape is very powerful because it can be done in essentially one night as opposed to decades of lightcurves. Average departures of 3% (5 km) of the asteroid's mean radius from a smooth outline are detected, with at least two local positive-relief features and at least one flat facet showing approximately 15 km deviations from the reference best-fit ellipsoid. The facet is reminiscent of large global-scale craters on Asteroid 253 Mathilde (also a C-type) when seen edge-on in close-up images from the NEAR mission flyby. We show that giant craters (up to 150 km diameter, the size of the largest facets seen on Davida) can be expected from the impactor size distribution, without likelihood of catastrophic disruption of Davida.
Published: 2007
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17. Adaptive Optics Imaging of IRAS 18276−1431: A Bipolar Preplanetary Nebula with Circumstellar 'Searchlight Beams' and 'Arcs'

Author: A. Gil de Paz, Raghvendra Sahai, D. Le Mignant, C. Sánchez Contreras, Mark Morris, European Commission, National Aeronautics and Space Administration (US), Ministerio de Ciencia y Tecnología (España), and National Science Foundation (US)
Subjects: Astrofísica, Stars: mass loss, Stars: imaging, 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, 0103 physical sciences, Thermal, Planetary nebulae: general, education, Adaptive optics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, education.field_of_study, Nebula, jets and outflows [ISM], Instrumentation: adaptive optics, Astrophysics (astro-ph), Stars: AGB and post-AGB, Astronomy and Astrophysics, AGB and post-AGB [Stars], Circumstellar matter, Planetary nebula, adaptive optics [Instrumentation], Infrared: stars, Astronomía, Interferometry, ISM: jets and outflows, Space and Planetary Science, imaging [Stars], stars [Infrared], Guide star, Halo, mass loss [Stars], general [Planetary nebulae]
Abstract: 17 pags., 14 figs., 3 tabs., We present high angular resolution images of the post-AGB nebula IRAS 18276-1431 (also known as OH 17.7-2.0) obtained with the Keck II adaptive optics (AO) system in its natural guide star (NGS) mode in the Kp, L p, and Ms near-infrared bands. We also present supporting optical F606W and F814W HST images as well as interferometric observations of the 12CO J = 1-0, 13CO J = 1-0, and 2.6 mm continuum emission with OVRO. The envelope of IRAS 18276-1431 displays a clear bipolar morphology in our optical and NIR images with two lobes separated by a dark waist and surrounded by a faint 4.5″ × 3.4″ halo. Our K p-band image reveals two pairs of radial >searchlight beams> emerging from the nebula center and several intersecting, arclike features. From our CO data we derive a mass of M > 0.38(D/3 kpc)2 M⊙ and an expansion velocity Vexp = 17 kms-1 for the molecular envelope. The density in the halo follows a radial power law ∝r-3, which is consistent with a mass-loss rate increasing with time. Analysis of the NIR colors indicates the presence of a compact central source of ∼300-500 K dust illuminating the nebula in addition to the central star. Modeling of the thermal IR suggests a two-shell structure in the dust envelope: (1) an outer shell with inner and outer radius Rin ∼ 1.6 × 1016 and Rout ≳ 1.25 × 10 17 cm, dust temperature Tdust ∼ 105-50 K, and a mean mass-loss rate of M ≈ 10-3 M⊙ yr-1; and (2) an inner shell with Rin ∼ 6.3 × 1014 cm, Tdust ∼ 500-105 K, and Ṁ ∼ 3 × 10-5 M⊙ yr-1. An additional population of big dust grains (radius a ≳; 0.4 mm) with Tdust 150-20 K and mass M dust = (0.16-1.6) × 10-3 (D/3 kpc)2 M⊙can account for the observed submillimeter and millimeter flux excess. The mass of the envelope enclosed within Aout = 1.25 × 1017 cm derived from SED modeling is ∼1 (D/ 3 kpc)2 Ṁ. © 2007. The American Astronomical Society. All rights reserved., This work has been partially performed at the California Institute of Technology and the Department of Molecular and Infrared Astrophysics of the Instituto de Estructura de la Materia, CSIC, and has been partially supported by National Science Foundation grant 9981546 to Owens Valley Radio Observatory and the Spanish MCyT under project DGES/AYA2003- 02785. R. S. is thankful for partial financial support for this work fromaNASA/ADP grant.A.G. d. P. is financed by theMAGPOP EU Marie Curie Research Training Network and par tially by the Spanish Programa Nacional de Astronomıa y Astrofisica under grant AYA2003-01676. M. M. and R. S. acknowledge financial support for this work from NASA LTSA and ADP awards RTOP 399-20-40-06 and RTOP 399-20-00-08, and HST/GO awardGO 09101.01-A. .
Published: 2007
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18. Keck Interferometer Observations of FU Orionis Objects

Author: Gautam Vasisht, Chas Beichman, M. Shao, R. Billmeier, Robert R. Thompson, Peter G. Tuthill, John D. Monnier, M. Hrynevych, D. Le Mignant, Bertrand Mennesson, M. Mark Colavita, Rafael Millan-Gabet, Marc J. Kuchner, G. van Belle, J.-P. Berger, Lynne A. Hillenbrand, Paola D'Alessio, Nuria Calvet, J. Gathright, S. Melnikov, Anneila I. Sargent, Stephen C. Unwin, A. Booth, A. Tannirkulam, Chris Neyman, Mark R. Swain, Peter Wizinowich, C. Koresko, Rachel Akeson, Michelle Creech-Eakman, Lee Hartmann, Wesley A. Traub, R. Ligon, A. F. Boden, Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 010504 meteorology & atmospheric sciences, Infrared, Scattering, Astrophysics::High Energy Astrophysical Phenomena, Young stellar object, Astrophysics (astro-ph), FOS: Physical sciences, Spectral density, Astronomy and Astrophysics, Field of view, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Interferometry, Amplitude, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Visibility, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We present new K-band long baseline interferometer observations of three young stellar objects of the FU Orionis class, V1057 Cyg, V1515 Cyg and Z CMa-SE, obtained at the Keck Interferometer during its commissioning science period. The interferometer clearly resolves the source of near-infrared emission in all three objects. Using simple geometrical models we derive size scales (0.5-4.5 AU) for this emission. All three objects appear significantly more resolved than expected from simple models of accretion disks tuned to fit the broadband optical and infrared spectro-photometry. We explore variations in the key parameters that are able to lower the predicted visibility amplitudes to the measured levels, and conclude that accretion disks alone do not reproduce the spectral energy distributions and K-band visibilities simultaneously. We conclude that either disk models are inadequate to describe the near-infrared emission, or additional source components are needed. We hypothesize that large scale emission (10s of AU) in the interferometer field of view is responsible for the surprisingly low visibilities. This emission may arise in scattering by large envelopes believed to surround these objects., Accepted by The Astrophysical Journal, in press
Published: 2006
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19. Long Baseline Nulling Interferometry with the Keck Telescopes: a Progress Report

Author: T. Panteleeva, C. Tyau, K. Tsubota, J. Herstein, Bertrand Mennesson, Andy C. Rudeen, Michelle Creech-Eakman, Rafael Millan-Gabet, Eugene Serabyn, J. Gathright, Erik M. Johansson, Mark R. Swain, S. Crawford, Gautam Vasisht, Christopher D. Koresko, T. Saloga, M. Hrynevych, E. Hovland, A. J. Booth, M. Shao, Rachel Akeson, L. Reder, Peter Wizinowich, D. Le Mignant, M. Mark Colavita, J. Bell, J. Garcia, E. Appleby, S. Ragland, K. Summers, Dean L. Palmer, R. Smythe, Christopher G. Paine, James L. Fanson, C. Felizardo, Julien Woillez, Christopher R. Neyman, R. Ligon, W. Dahl, and James G. Moore
Subjects: Physics, Astronomical optical interferometry, business.industry, media_common.quotation_subject, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Terrestrial Planet Finder, Interferometry, Optical path, Optics, Space and Planetary Science, Sky, Astronomical interferometer, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics::Galaxy Astrophysics, Nuller, media_common
Abstract: The Keck Interferometer Nuller (KIN) is one of the major scientific and technical precursors to the Terrestrial Planet Finder Interferometer (TPF-I) mission. KIN's primary objective is to measure the level of exo-zodiacal mid-infrared emission around nearby main sequence stars, which requires deep broad-band nulling of astronomical sources of a few Janskys at 10 microns. A number of new capabilities are needed in order to reach that goal with the Keck telescopes: mid-infrared coherent recombination, interferometric operation in 'split pupil' mode, N-band optical path stabilization using K-band fringe tracking and internal metrology, and eventually, active atmospheric dispersion correction. We report here on the progress made implementing these new functionalities, and discuss the initial levels of extinction achieved on the sky.
Published: 2005
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20. Keck AO survey of Io global volcanic activity between 2 and 5 μm

Author: I. de Pater, Ashley Davies, R. Prange, Paola Amico, Al Conrad, Robert W. Goodrich, D. Le Mignant, T. Fusco, Franck Marchis, Randy Campbell, Shui Kwok, and Frederic H. Chaffee
Subjects: Physics, Brightness, Wavelength, Heat flux, Space and Planetary Science, Absorption band, Flux, Astronomy, Astronomy and Astrophysics, Angular resolution, Albedo, Image resolution
Abstract: We present in this Keck AO paper the first global high angular resolution observations of Io in three broadband near-infrared filters: Kc (2.3 mu m), Lp (3.8 mu m), and Ms (4.7 mu m). The Keck AO observations are composed of 13 data sets taken during short time intervals spanning 10 nights in December, 2001. The MISTRAL deconvolution process, which is specifically aimed for planetary images, was applied to each image. The spatial resolution achieved with those ground-based observations is 150, 240, and 300 km in the Kc, Lp, and Ms band, respectively, making them similar in quality to most of the distant observations of the Galileo/NIMS instrument. Eleven images per filter were selected and stitched together after being deprojected to build a cylindrical map of the entire surface of the satellite. In Kc-band, surface albedc, features, such as paterae (R > 60 km) are easily identifiable. The Babbar region is characterized by extremely low albedo at 2.2 mu m, and shows an absorption band at 0.9 mu m in Galileo/SSI data. These suggest that this region is covered by dark silicate deposits, possibly made of orthopyroxene. In the Lp-Ms (3-5 mu m) bands, the thermal emission from active centers is easily identified. We detected 26 hot spots in both broadband filters over the entire surface of the minor planet; two have never been seen active before, nine more are seen in the Ms band. We focused our study on the hot spots detected in both broadband filters. Using the measurements of their brightness, we derived the temperature and area covered by 100 brightness measurements. Loki displayed a relatively quiescent activity. Dazhbog, a new eruption detected by Galileo/NIMS in August 2001, is a major feature in our survey. We also point out the fading of Tvashtar volcanic activity after more than two years of energetic activity, and the presence of a hot, but small, active center at the location of Surt, possibly a remnant of its exceptional eruption detected in February 2001. Two new active centers, labeled F and V on our data, are detected. Using the best temperature and the surface area derived from the L and M band intensities, we calculated the thermal output of each active center. The most energetic hot spots are Loki and Dazhbog, representing respectively 36 and 19% of the total output calculated from a temperature fit of all hot spots (20.6 x 10(12) W). Based on the temperature derived from hot spots (similar to 400 K), our measurement can unambiguously identify the contribution to the heat flux from the silicate portion of the surface. Because the entire surface was observed, no extrapolation was required to calculate that flux. It is also important to note that we measured the brightness of the individual hot spots when they were located close to the Central Meridian. This minimizes the line-of-sight effect which does not follow strictly a classical cosine law. Finally, we argue that despite the widespread volcanic activity detected, Io was relatively quiescent in December 2001, with a minimum mean total output of 0.4-1.2 W m(-2). This output is at least a factor of two lower than those inferred from observations made at longer wavelengths and at different epochs. (c) 2005 Elsevier Inc. All rights reserved.
Published: 2005
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21. Sculpting a Pre-planetary Nebula with a Precessing Jet: IRAS 16342-3814

Author: Raghvendra Sahai, Frederic H. Chaffee, D. Le Mignant, C. Sánchez Contreras, and Randy Campbell
Subjects: Physics, Brightness, Nebula, Stellar mass, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Planetary nebula, Interstellar medium, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Asymptotic giant branch, Circumstellar dust, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We have imaged the bipolar pre-planetary nebula IRAS 16342-3814 with the Keck adaptive optics (AO) system in four near-infrared bands in the 1.6-4.7 (micro)m range. The lobes, which showed smoothly varying brightness distributions in previous optical images taken with the Hubble Space Telescope, have a limb-brightened appearance in the AO images, with a remarkable corkscrew structure inscribed on the lobe walls. A well-collimated, precessing jet with a diameter less than or approximately equal to 100 AU and a precession period less than or approximately equal to 50 yr, interacting with ambient circumstellar material, is most likely responsible for the corkscrew structure and the lobes, as indicated by a detailed comparison of our observations with published numerical simulations. The very red colors of the lobes in the near-infrared, coupled with their visibility at optical wavelengths, require that at least half, but not all, of the light of the central star be trapped by a compact circumstellar dust cloud heated to approximately 600-700 K and reradiated in the infrared. The lobes are thus illuminated both by the infrared light from this dust cloud as well as by the optical light from the central star.
Published: 2005
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22. High-Resolution Keck Adaptive Optics Imaging of Violent Volcanic Activity on Io

Author: Henry G. Roe, I. de Pater, Bruce Macintosh, R. Prange, Pascal Descamps, Franck Marchis, D. Le Mignant, Thierry Fusco, Ashley Davies, 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), Physique des plasmas, and 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Subjects: Basalt, Solar System, geography, geography.geographical_feature_category, Astronomy, Astronomy and Astrophysics, Volcanism, Galilean, law.invention, Jupiter, Telescope, Volcano, Space and Planetary Science, law, Satellite, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology
Abstract: Io, the innermost Galilean satellite of Jupiter, is a fascinating world. Data taken by Voyager and Galileo instruments have established that it is by far the most volcanic body in the Solar System and suggest that the nature of this volcanism could radically differ from volcanism on Earth. We report on near-IR observations taken in February 2001 from the Earth-based 10-m W. M. Keck II telescope using its adaptive optics system. After application of an appropriate deconvolution technique (MISTRAL), the resolution, ∼100 km on Io's disk, compares well with the best Galileo/NIMS resolution for global imaging and allows us for the first time to investigate the very nature of individual eruptions. On 19 February, we detected two volcanoes, Amirani and Tvashtar, with temperatures differing from the Galileo observations. On 20 February, we noticed a slight brightening near the Surt volcano. Two days later it had turned into an extremely bright volcanic outburst. The hot spot temperatures (>1400 K) are consistent with a basaltic eruption and, being lower limits, do not exclude an ultramafic eruption. These outburst data have been fitted with a silicate-cooling model, which indicates that this is a highly vigorous eruption with a highly dynamic emplacement mechanism, akin to fire-fountaining. Its integrated thermal output was close to the total estimated output of Io, making this the largest ionian thermal outburst yet witnessed.
Published: 2002
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23. Current status of the Spectrograph System for the SuMIRe/PFS

Author: Sandrine Pascal, S. Vives, F. Madec, Thomas Pegot-Ogier, M. Golebiowski, Murdock Hart, L. Souza de Oliveira, James E. Gunn, M. Vital de Arruda, Hajime Sugai, Didier Ferrand, Stephen A. Smee, Alexandre Bozier, Naoyuki Tamura, Robert H. Barkhouser, M. Jaquet, A. C. de Oliveira, D. Le Mignant, Michael A. Carr, Stephen C. Hope, 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), National Institute for Fusion Science (NIFS), Advanced Science Research Center and Nuclear Science Research Institute, Japan Atomic Energy Agency, Japan Atomic Energy Agency, and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Near-infrared spectroscopy, FOS: Physical sciences, Collimator, Ranging, 02 engineering and technology, 021001 nanoscience & nanotechnology, 01 natural sciences, law.invention, 010309 optics, Telescope, Optics, law, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Spectral resolution, Astrophysics - Instrumentation and Methods for Astrophysics, 0210 nano-technology, Focus (optics), business, Subaru Telescope, Spectrograph, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The Prime Focus Spectrograph (PFS) is a new facility instrument for Subaru Telescope which will be installed in around 2017. It is a multi-object spectrograph fed by about 2400 fibers placed at the prime focus covering a hexagonal field-of-view with 1.35 deg diagonals and capable of simultaneously obtaining data of spectra with wavelengths ranging from 0.38 um to 1.26 um. The spectrograph system is composed of four identical modules each receiving the light from 600 fibers. Each module incorporates three channels covering the wavelength ranges 0.38-0.65 mu ("Blue"), 0.63-0.97 mu ("Red"), and 0.94-1.26 mu ("NIR") respectively; with resolving power which progresses fairly smoothly from about 2000 in the blue to about 4000 in the infrared. An additional spectral mode allows reaching a spectral resolution of 5000 at 0.8mu (red). The proposed optical design is based on a Schmidt collimator facing three Schmidt cameras (one per spectral channel). This architecture is very robust, well known and documented. It allows for high image quality with only few simple elements (high throughput) at the expense of the central obscuration, which leads to larger optics. Each module has to be modular in its design to allow for integration and tests and for its safe transport up to the telescope: this is the main driver for the mechanical design. In particular, each module will be firstly fully integrated and validated at LAM (France) before it is shipped to Hawaii. All sub-assemblies will be indexed on the bench to allow for their accurate repositioning. This paper will give an overview of the spectrograph system which has successfully passed the Critical Design Review (CDR) in 2014 March and which is now in the construction phase., Comment: 9 pages, 7 figures, submitted to "Ground-based and Airborne Instrumentation for Astronomy V, Suzanne K. Ramsay, Ian S. McLean, Hideki Takami, Editors, Proc. SPIE 9147 (2014)"
Published: 2014
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24. The Keck Interferometer

Author: Michelle Creech-Eakman, Charles Beichman, R. R. Thompson, B. C. Berkey, A. Tumminello, E. Hovland, Richard L. Johnson, T. Panteleeva, G. Hardy, A. Niessner, James Wallace, W. Dahl, J. Chin, J. Beletic, Eugene Serabyn, G. Eychaner, Andrew F. Boden, A. I. Sargent, Andy C. Rudeen, B. Parvin, R. Kendrick, Mark R. Swain, Dean L. Palmer, James D. Moore, Michael Shao, M. Mark Colavita, D. McBride, Peter Wizinowich, Christopher R. Neyman, E. R. Ligon, Rachel Akeson, H. A. Lewis, Erik M. Johansson, D. Chan, F. Vescelus, Christopher G. Paine, L. Reder, William Lupton, Christopher D. Koresko, Andrew Cooper, Michael Hess, G. Vasisht, C. Felizardo, Richard Cohen, M. Abajian, R. Smythe, Samuel L. Crawford, Jean Garcia-Gathright, T. Saloga, K. Summers, G. T. van Belle, Drew Medeiros, E. Appleby, C. Tyau, P. Kurpis, J. Walker, Rafael Millan-Gabet, J. Gathright, R. Boutell, Craig E. Nance, H. Henderson, K. Tsubota, J. Vause, A. J. Booth, J. Herstein, P. Swanson, Julien Woillez, B. Smith, J. Berlin, M. Papin, E. Wetherell, J. Kelley, D. Le Mignant, D. S. Acton, J. Bell, S. Ragland, David Morrison, U. Wehmeier, Paul J. Stomski, Frederic H. Chaffee, Bertrand Mennesson, J. Chock, M. Hrynevych, and James L. Fanson
Subjects: Wavefront, Astronomical optical interferometry, business.industry, Computer science, Instrumentation, Detector, Astronomy and Astrophysics, Cophasing, Interferometry, Optics, Space and Planetary Science, Observatory, business, Adaptive optics, Remote sensing
Abstract: The Keck Interferometer (KI) combined the two 10 m W. M. Keck Observatory telescopes on Mauna Kea, Hawaii, as a long-baseline near- and mid-infrared interferometer. Funded by NASA, it operated from 2001 until 2012. KI used adaptive optics on the two Keck telescopes to correct the individual wavefronts, as well as active fringe tracking in all modes for path-length control, including the implementation of cophasing to provide long coherent integration times. KI implemented high sensitivity fringe-visibility measurements at H (1.6 μm), K (2.2 μm), and L (3.8 μm) bands, and nulling measurements at N band (10 μm), which were used to address a broad range of science topics. Supporting these capabilities was an extensive interferometer infrastructure and unique instrumentation, including some additional functionality added as part of the NSF-funded ASTRA program. This paper provides an overview of the instrument architecture and some of the key design and implementation decisions, as well as a description of all of the key elements and their configuration at the end of the project. The objective is to provide a view of KI as an integrated system, and to provide adequate technical detail to assess the implementation. Included is a discussion of the operational aspects of the system, as well as of the achieved system performance. Finally, details on V^2 calibration in the presence of detector nonlinearities as applied in the data pipeline are provided.
Published: 2013

25. IRDIS, the dual-band imager camera of SPHERE: testing the performances in laboratory

Author: Dino Mesa, F. Madec, Arthur Vigan, Jean-François Sauvage, Anne Costille, Silvano Desidera, David Mouillet, Maud Langlois, D. Le Mignant, Alice Zurlo, J. L. Beuzit, Raffaele Gratton, K. Dolhen, C. Moutou, Cecile Gry, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 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 Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, instrumentation, 010308 nuclear & particles physics, business.industry, Instrumentation, Pipeline (computing), FOS: Physical sciences, Astronomy and Astrophysics, Direct imaging, 01 natural sciences, Exoplanet, Optics, Integral field spectrograph, Space and Planetary Science, 0103 physical sciences, Multi-band device, business, Adaptive optics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Next year the second generation instrument SPHERE will begin science operations at the Very Large Telecope (ESO). This instrument will be dedicated to the search for exoplanets through the direct imaging techniques, with the new generation extreme adaptive optics. In this poster, we present the performances of one of the focal instruments, the Infra-Red Dual-beam Imaging and Spectroscopy (IRDIS). All the results have been obtained with tests in laboratory, simulating the observing conditions in Paranal. We tested several configurations using the sub-system Integral Field Spectrograph (IFS) in parallel and simulating long coronographic exposures on a star, calibrating instrumental ghosts, checking the performance of the adaptive optics system and reducing data with the consortium pipeline. The contrast one can reach with IRDIS is of the order of 2\times 10^{-6}$ at 0.5 arcsec separation from the central star., 2 pages, 1 figure, IAU Symposium n 299 proceedings
Published: 2013
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26. VLT/SPHERE deep insight of NGC 3603’s core: Segregation or confusion?

Author: Jean-François Sauvage, Cyril Petit, Wolfgang Brandner, D. Le Mignant, Kjetil Dohlen, Anthony Boccaletti, C. Perrot, Olivier Chesneau, T. Lanz, Anne Costille, H. M. Schmid, Eric Lagadec, Marcel Carbillet, David Mouillet, Zeinab Khorrami, Michael R. Meyer, Maud Langlois, Lyu Abe, A. Pavlov, Farrokh Vakili, Christian Thalmann, Jean-Luc Beuzit, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), GDFSuez, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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), NASA Goddard Space Flight Center (GSFC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), De la Molécule aux Nanos-objets : Réactivité, Interactions et Spectroscopies (MONARIS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut de Chimie du CNRS (INC)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), 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), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Field (physics), Extinction (astronomy), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 010309 optics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Adaptive optics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, Very Large Telescope, Astronomy and Astrophysics, Spectral bands, Astrophysics - Astrophysics of Galaxies, Core (optical fiber), Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Main sequence
Abstract: We present new near infrared photometric measurements of the core of the young massive cluster NGC 3603 obtained with extreme adaptive optics. The data were obtained with the SPHERE instrument mounted on ESO's Very Large Telescope and cover three fields in the core of this cluster. We applied a correction for the effect of extinction to our data obtained in the J and K broadband filters and estimated the mass of detected sources inside the field of view of SPHERE/IRDIS which is 13.5''×13.5''. We derived the mass function (MF) slope for each spectral band and field. The MF slope in the core is unusual compared to previous results based on HST and VLT observations. The average slope in the core is estimated as 1.06 ± 0.26 for the main sequence stars with 3.5 M? < M < 120M?. Thanks to the SPHERE extreme adaptive optics 814 low mass stars were detected to estimate the MF slope for the pre main sequence stars with 0.6 M? < M < 3.5M? G = 0.54 ± 0.11 in the K band images in two fields in the core of the cluster. For the first time we derive the MF of the very core of the NGC 3603 young cluster for masses in the range 0.6 120 M?. Previous studies were either limited by crowding lack of dynamic range or a combination of both. Based on data collected at the European Southern Observatory Chile (guaranteed time observation 095.D 0309(A) and 095.D 0309(E))
Published: 2016
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27. Apodization in high-contrast long-slit spectroscopy

Author: Alain Origne, Jean-François Sauvage, Pascal Puget, David Mouillet, Andrea Baruffolo, D. Le Mignant, Arthur Vigan, Marc Ferrari, Thierry Fusco, F. Madec, M. Llored, Kjetil Dohlen, Marc Jaquet, Anne Costille, M. Carle, L. Gluck, A. Caillat, Mamadou N'Diaye, J. L. Beuzit, Emmanuel Hugot, P. Blanchard, Bernardo Salasnich, Maud Langlois, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Space Telescope Science Institute (STSci), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ITA, USA, FRA, CHL, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), ONERA, Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)
Subjects: media_common.quotation_subject, Phase (waves), FOS: Physical sciences, OPTIQUE ADAPTATIVE, 01 natural sciences, law.invention, 010309 optics, DATA ANALYSIS, Optics, Apodization, law, RESOLUTION ANGULAIRE ELEVEE, 0103 physical sciences, PLANETARY SYSTEMS, NUMERIQUE, ANALYSE DONNEES, INSTRUMENTATION, NUMERICAL, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Coronagraph, Spectrograph, media_common, Long-slit spectroscopy, Earth and Planetary Astrophysics (astro-ph.EP), ADAPTIVE OPTICS, Physics, Lyot stop, business.industry, HIGH ANGULAR RESOLUTION, Astronomy and Astrophysics, Transmission (telecommunications), [SDU]Sciences of the Universe [physics], Space and Planetary Science, Sky, SPECTROGRAPHIE, SPECTROGRAPHS, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, METHODS, Astrophysics - Instrumentation and Methods for Astrophysics, SYSTEME PLANETAIRE, business, Astrophysics - Earth and Planetary Astrophysics
Abstract: Spectral characterization of young, giant exoplanets detected by direct imaging is one of the tasks of the new generation of high-contrast imagers. For this purpose, the VLT/SPHERE instrument includes a unique long-slit spectroscopy (LSS) mode coupled with Lyot coronagraphy in its infrared dual-band imager and spectrograph (IRDIS). The performance of this mode is intrinsically limited by the use of a non-optimal coronagraph, but in a previous work we demonstrated that it could be significantly improved at small inner-working angles using the stop-less Lyot coronagraph (SLLC). We now present the development, testing, and validation of the first SLLC prototype for VLT/SPHERE. Based on the transmission profile previously proposed, the prototype was manufactured using microdots technology and was installed inside the instrument in 2014. The transmission measurements agree well with the specifications, except in the very low transmissions (, 13 pages, 13 figures. Accepted for publication in A&A
Published: 2016
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28. New modelling of freeform surfaces for optical design of astronomical instruments

Author: Sandrine Pascal, D. Le Mignant, Marc Ferrari, S. Vives, M. Gray, Kjetil Dohlen, and Jean-Gabriel Cuby
Subjects: business.industry, Computer science, Mechanical engineering, Context (language use), Computer vision, Artificial intelligence, Degrees of freedom (mechanics), Instrument design, business, Focus (optics), Bernstein polynomial
Abstract: Freeform optics offer additional degrees of freedom that can lead to a simplification of instrument optical designs with compact solutions. In this context, we propose a new mathematical description of freeform surfaces. This new mathematical formalism, based on the "eigen-modes" of Bernstein polynomials was developed for off-axis highly aspherical surfaces modelling. It allows to take into account different kinds of deformations of the optical surface with local influence capabilities. We present the mathematical formalism developed and then we focus on the optical analysis of an innovative instrument design. The advantages provided by this new modelling are examined.
Published: 2012
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29. Modeling highly aspherical optical surfaces using a new polynomial formalism into Zemax

Author: M. Gray, Jean-Gabriel Cuby, Sandrine Pascal, Sébastien Vivès, D. Le Mignant, A. Secroun, and Marc Ferrari
Subjects: symbols.namesake, Formalism (philosophy of mathematics), Mathematical definition, Zernike polynomials, Optical surface, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, symbols, Calculus, High order, Zemax, Bernstein polynomial, Computational science, Mathematics
Abstract: We developed a new mathematical formalism to model highly aspherical optical surfaces opening the possibility to explore innovative optical designs. This formalism is based on Bernstein polynomials allowing to describe from low to high order deformations of the optical surface. It has been implemented into Zemax making use of the User-Defined Surface (UDS-DLL) Zemax capability. In this case, the mathematical definition of the surface is imported into Zemax then allowing to apply classical optimization and analysis functionalities. This paper presents the UDS-DLL tool based on Bernstein polynomials together with an initial optical analysis performed to evaluate the gain obtained in using such a new formalism.
Published: 2011
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30. A Dynamical Solution of the Triple Asteroid System (45) Eugenia

Author: I. de Pater, B. Macomber, Frédéric Vachier, Franck Marchis, Mark R. Showalter, Valery Lainey, M. Baek, Pascal Descamps, Heidi B. Hammel, M. van Dam, Jérôme Berthier, D. Le Mignant, 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), Department of Astronomy [Berkeley], University of California [Berkeley], University of California-University of California, SETI Institute, Flat Wavefronts, W.M. Keck Observatory, Space Science Institute [Boulder] (SSI), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)
Subjects: Solar System, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Equator, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Perturbation (astronomy), FOS: Physical sciences, Regular moon, 01 natural sciences, Gravitation, Asteroids Dynamics, 0103 physical sciences, Circular orbit, Satellites Dynamics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Infrared observations, Astronomy, Astronomy and Astrophysics, Asteroids, Secular resonance, Space and Planetary Science, Asteroid, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the first dynamical solution of the triple asteroid system (45) Eugenia and its two moons Petit-Prince (Diameter~7 km) and S/2004 (45) 1 (Diameter~5 km). The two moons orbit at 1165 and 610 km from the primary, describing an almost-circular orbit (e~6x10-3 and e~7x10-2 respectively). The system is quite different from the other known triple systems in the main belt since the inclinations of the moon orbits are sizeable (9 deg and 18 deg with respect to the equator of the primary respectively). No resonances, neither secular nor due to Lidov-Kozai mechanism, were detected in our dynamical solution, suggesting that these inclinations are not due to excitation modes between the primary and the moons. A 10-year evolution study shows that the orbits are slightly affected by perturbations from the Sun, and to a lesser extent by mutual interactions between the moons. The estimated J2 of the primary is three times lower than the theoretical one, calculated assuming the shape of the primary and an homogeneous interior, possibly suggesting the importance of other gravitational harmonics., 38 pages, 5 Tables, 5 Figures, revised for Icarus Journal
Published: 2010
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31. E-ELT Instrument study for first light: OPTIMOS-DIORAMAS: mechanical concept study for slit masks system

Author: D. Le Mignant, L. Hill, S. Paltani, V. De Caprio, O. Le Fevre, L. Chiappetti, Marc Jaquet, Laurent Martin, D. Maccagni, and B. Garilli
Subjects: Vignetting, business.industry, Computer science, Near-infrared spectroscopy, Field of view, First light, Curvature, Laser, law.invention, Telescope, Optics, Cardinal point, law, business, Spectroscopy, Spectrograph
Abstract: The Seeing-limited, large multiplex, optical/near-IR spectrograph, Optimos-Dioramas, currently under study by a Consortium of Institutes from France, Italy, and Switzerland, is one of the possible candidates for first light on the EELT Telescope. The spectograph is designed to maximize the field of view and cover in one-shot the spectral range (0.37micron - 1.6micron). This paper describes the studies performed to establish a base-line conceptual design of the Slit Masks System for the Optimos-Dioramas spectrograph. This unit has been designed in order to better satisfy the limits of the allowed volume on the Nasmyth E-ELT platform, and it is also able to guarantee all the optical specifications needed to cover the overall field of view (7x7arcmin). In order to take and position the masks in the focal plane, the performed system is fully robotic and able to load/unload the masks in the proper quadrant. A central cross structure, about 8.33arcsec wide, is needed. Each mask will necessarily be larger than 719x719mm, i.e. 780x780mm. The system based on four 0.6mm thick (black painted steel) masks is fully feasible and complies with all specifications. Vignetting due to the focal plane curvature is minimized and the slits (cut via a stencil-laser machine) can have all shapes and sizes.
Published: 2010
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32. EAGLE MOAO system conceptual design and related technologies

Author: M. Cohen, Philippe Laporte, Richard M. Myers, Damien Gratadour, William Taylor, Gérard Rousset, Simon L. Morris, Chris Evans, P. Parr-Burman, D. Le Mignant, F. Assemat, Eric Gendron, T. Fusco, H. Schnetler, Mathieu Puech, Nigel Dipper, Fabrice Vidal, Tim Morris, Jean-Gabriel Cuby, P. Jagourel, M. D. Lehnert, Clélia Robert, 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), Pôle Astronomie du 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Groupement d'Intérêt Scientifique du Partenariat Haute résolution Angulaire Sol-Espace (GIS PHASE ), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Duke University [Durham], ONERA, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, United Kingdom Astronomy Technology Ctr, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, business.industry, media_common.quotation_subject, Astronomy, Encircled energy, Deformable mirror, Stars, Optics, Apparent magnitude, Laser guide star, Sky, business, Adaptive optics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Spectrograph, media_common
Abstract: International audience; EAGLE is the multi-object spatially-resolved near-IR spectrograph instrument concept for the E-ELT, relying on a distributed Adaptive Optics, so-called Multi Object Adaptive Optics. This paper presents the results of a phase A study. Using 84×84 actuator deformable mirrors, the performed analysis demonstrates that 6 laser guide stars (on an outer ring of 7.2' diameter) and up to 5 natural guide stars of magnitude R < 17, picked-up in a 7.3' diameter patrol field of view, allow us to obtain an overall performance in terms of Ensquared Energy of 35% in a 75×75mas2 resolution element at H band whatever the target direction in the centred 5' science field for median seeing conditions. In terms of sky coverage, the probability to find the 5 natural guide stars is close to 90% at galactic latitudes |b| ~ 60 deg. Several MOAO demonstration activities are also on-going.
Published: 2010
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33. Active Laser Guide Star refocusing system for EAGLE instrument

Author: F. Madec, Marc Ferrari, D. Le Mignant, J. G. Cuby, Silvio P. Mazzanti, P. Vola, S. Vives, Emmanuel Hugot, Jean-Luc Gimenez, and Elodie Chardin
Subjects: Engineering, business.industry, Frame (networking), Sodium layer, Curvature, Encircled energy, Finite element method, law.invention, Metrology, Telescope, Laser guide star, Optics, law, business
Abstract: We detail the study of a laser guide star (LGS) refocusing system based on an variable curvature mirror (VCM) of high dynamic, in the frame of the EAGLE instrument for the E-ELT. From the top level require- ments, an on axis optical design based on an active component is optimised to ensure maximal performance in terms of encircled energy. The refocusing is operated by the VCM, which shape varies with the distance of the sodium layer to the telescope. The VCM system concept is based on an embedded metrology. We detail the finite element analysis (FEA) of the VCM, allowing an optimization of the thickness profile to get an optical quality better than /5 RMS at each curvature. Mechanical design and manufacturing of prototypes are also presented.
Published: 2010
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34. EAGLE multi-object AO concept study for the E-ELT

Author: M. D. Lehnert, D. Gratadour, Tim Morris, Fabrice Vidal, Richard M. Myers, D. Le Mignant, Eric Gendron, Philippe Laporte, M. Cohen, M. Brangier, Gérard Rousset, Clélia Robert, Thierry Fusco, F. Assemat, Nigel Dipper, Mathieu Puech, P. Parr-Burmann, Hermine Schnetler, J. G. Cuby, P. Jagourel, Simon L. Morris, Chris Evans, W. D. Taylor, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Durham University, Galaxies, Etoiles, Physique, Instrumentation (GEPI), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)
Subjects: media_common.quotation_subject, FOS: Physical sciences, Field of view, 02 engineering and technology, OPTICAL TELESCOPES, 01 natural sciences, Encircled energy, Optical telescope, Deformable mirror, 010309 optics, [SPI]Engineering Sciences [physics], Optics, 0103 physical sciences, Adaptive optics, Spectrograph, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Physics, [PHYS]Physics [physics], business.industry, LASER MIRRORS, 021001 nanoscience & nanotechnology, Stars, Sky, 0210 nano-technology, business, Astrophysics - Instrumentation and Methods for Astrophysics, STARS
Abstract: EAGLE is the multi-object, spatially-resolved, near-IR spectrograph instrument concept for the E-ELT, relying on a distributed Adaptive Optics, so-called Multi Object Adaptive Optics. This paper presents the results of a phase A study. Using 84x84 actuator deformable mirrors, the performed analysis demonstrates that 6 laser guide stars and up to 5 natural guide stars of magnitude R, 6 pages, to appear in the proceedings of the AO4ELT conference, held in Paris, 22-26 June 2009
Published: 2009
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35. GRB 071003: Broadband Follow-up Observations of a Very Bright Gamma-Ray Burst in a Galactic Halo

Author: D. B. Fox, M. A. van Dam, Erik M. Johansson, Nat Butler, Ryan Chornock, S. A. Yost, Wenxiong Li, J. S. Bloom, Jason X. Prochaska, D. Le Mignant, Matthew W. Auger, M. Modjaz, R. Russell, Timothy A. McKay, Alexei V. Filippenko, Dale A. Frail, Ian Smith, Daniel A. Perley, H. F. Swan, L. K. Pollack, Hsiao-Wen Chen, S. B. Cenko, Fang Yuan, Wiphu Rujopakarn, P. Chandra, M. Skinner, Carl W. Akerlof, G. H. Smith, and Christopher D. Fassnacht
Subjects: Physics, 010308 nuclear & particles physics, Star formation, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Galaxy, Redshift, Afterglow, Galactic halo, GRB 070125, Space and Planetary Science, 0103 physical sciences, QD, Gamma-ray burst, 010303 astronomy & astrophysics, QC, QB
Abstract: The optical afterglow of long-duration GRB 071003 is among the brightest yet to be detected from any GRB, with R ~ 12 mag in KAIT observations starting 42 s after the GRB trigger, including filtered detections during prompt emission. However, our high S/N ratio afterglow spectrum displays only extremely weak absorption lines at what we argue is the host redshift of z = 1.60435 - in contrast to the three other, much stronger Mg II absorption systems observed at lower redshifts. Together with Keck adaptive optics observations which fail to reveal a host galaxy coincident with the burst position, our observations suggest a halo progenitor and offer a cautionary tale about the use of Mg II for GRB redshift determination. We present early through late-time observations spanning the electromagnetic spectrum, constrain the connection between the prompt emission and early variations in the light curve (we observe no correlation), and discuss possible origins for an unusual, marked rebrightening that occurs a few hours after the burst: likely either a late-time refreshed shock or a wide-angle secondary jet. Analysis of the late-time afterglow is most consistent with a wind environment, suggesting a massive star progenitor. Together with GRB 070125, this may indicate that a small but significant portion of star formation in the early universe occurred far outside what we consider a normal galactic disk., 24 pages, 14 figures, 12 tables. Accepted for publication by ApJ. Contains minor revisions and additional authors
Published: 2008

36. W. M. Keck Observatory's next-generation adaptive optics facility

Author: P. Wizinowich, R. Dekany, D. Gavel, C. Max, S. Adkins, B. Bauman, J. Bell, A. Bouchez, M. Britton, J. Chin, R. Flicker, E. Johansson, R. Kupke, D. Le Mignant, C. Lockwood, D. Medeiros, E. McGrath, A. Moore, C. Neyman, M. Reinig, V. Velur, Hubin, Norbert, Max, Claire E., and Wizinowich, Peter L.
Abstract: W. M. Keck Observatory (WMKO) is currently engaged in the design of a powerful new Adaptive Optics (AO) science capability providing precision correction in the near-IR, good correction in the visible, and faint object multiplexed integral field spectroscopy. Improved sensitivity will result from significantly higher Strehl ratios over narrow fields (< 30" diameter) and from lower backgrounds. Quantitative astronomy will benefit from improved PSF stability and knowledge. Strehl ratios of 15 to 25% are expected at wavelengths as short as 750 nm. A multi-object AO approach will be taken for the correction of multiple science targets over modest fields of regard (< 2' diameter) and to achieve high sky coverage using AO compensated near-IR tip/tilt sensing. In this paper we present the conceptual design for this system including discussion of the requirements, system architecture, key design features, performance predictions and implementation plans.
Published: 2008

37. The science case for the Next Generation AO system at W. M. Keck Observatory

Author: Claire E. Max, Peter Wizinowich, D. Le Mignant, Donald T. Gavel, Elizabeth J. McGrath, Richard Dekany, Hubin, Norbert, Max, Claire E., and Wizinowich, Peter L.
Subjects: Physics, W. M. Keck Observatory, Active galactic nucleus, Galactic astronomy, Galactic Center, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Integral field spectrograph, Observatory, Planet, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The W. M. Keck Observatory is designing a new adaptive optics system providing precision AO correction in the near infrared, good correction at visible wavelengths, and multiplexed spatially resolved spectroscopy. We discuss science cases for this Next Generation AO (NGAO), and show how the system requirements were derived from these science cases. Key science drivers include asteroid companions, planets around low-mass stars, general relativistic effects around the Galactic Center black hole, nearby active galactic nuclei, and high-redshift galaxies (including galaxies lensed by intervening galaxies or clusters). The multi-object AO-corrected integral field spectrograph will be optimized for high-redshift galaxy science.
Published: 2008

38. Superresolving Distant Galaxies with Gravitational Telescopes: Keck Laser Guide Star Adaptive Optics and Hubble Space Telescope Imaging of the Lens System SDSS J0737+3216

Author: Leonidas A. Moustakas, Adam S. Bolton, C. E. Max, Kevin Bundy, Eric Steinbring, James E. Larkin, David C. Koo, Luitje Koopmans, Stephen Ammons, D. Le Mignant, Shelley A. Wright, J. Melbourne, Raphael Gavazzi, Philip J. Marshall, Scott Burles, Tommaso Treu, and Kapteyn Astronomical Institute
Subjects: Stellar mass, SIZE EVOLUTION, DEEP FIELD, gravitational lensing, methods : data analysis, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, HIGH-REDSHIFT GALAXIES, law.invention, Telescope, techniques : high angular resolution, law, galaxies : fundamental parameters, 0103 physical sciences, LARGE-SCALE STRUCTURE, Galaxy formation and evolution, DARK-MATTER, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, DISK GALAXIES, Galaxy, Redshift, Lens (optics), COMPACT BLUE GALAXIES, Laser guide star, Gravitational lens, Space and Planetary Science, FUNDAMENTAL PLANE, Astrophysics::Earth and Planetary Astrophysics, instrumentation : adaptive optics, ACS SURVEY, SURFACE-BRIGHTNESS
Abstract: We combine high-resolution images in four optical/infrared bands, obtained with the laser guide star adaptive optics ( LGSAO) system on the Keck telescope and with the Hubble Space Telescope ( HST), to study the gravitational lens system SDSS J0737 + 3216 ( lens redshift 0.3223, source redshift 0.5812). We show that ( under favorable observing conditions) ground-based images are comparable to those obtained with HST in terms of precision in the determination of the parameters of both the lens mass distribution and the background source. We also quantify the systematic errors associated with both the incomplete knowledge of the PSF and the uncertain process of lens galaxy light removal and find that similar accuracy can be achieved with Keck LGSAO as with HST. We then exploit this well-calibrated combination of optical and gravitational telescopes to perform a multiwavelength study of the source galaxy at 0.01 '' effective resolution. We find the Sersic index to be indicative of a disklike object, but the measured half-light radius (r(e) = 0.59 +/- 0.007 stat +/- 0.1 sys kpc) and stellar mass (M* = 2.0 +/- 1.0 stat +/- 0.8 sys x 10(9) M(circle dot)) place it more than 3 sigma away from the local disk size-mass relation. The SDSS J0737 + 3216 source has the characteristics of the most compact faint blue galaxies studied and comparable size and mass to dwarf early-type galaxies in the local universe. With the aid of gravitational telescopes to measure individual objects' brightness profiles to 10% accuracy, the study of the high-redshift size-mass relation may be extended by an order of magnitude or more beyond existing surveys at the low-mass end, thus providing a new observational test of galaxy formation models.
Published: 2007
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39. Shape, size and multiplicity of main-belt asteroids. I. Keck Adaptive Optics survey

Author: I. de Pater, Jérôme Berthier, Erik F. Y. Hom, D. Le Mignant, J. E. Enriquez, Franck Marchis, Daniel Hestroffer, Mikko Kaasalainen, Department of Astronomy, University of California, Department of Mathematics and Statistics, Rolf Nevanlinna Institute, University of Helsinki, Graduate Group in Biophysics, University of California, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Groupe Astrométrie et Planétologie (GAP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and W. M. Keck Observatory
Subjects: Physics, Solar System, 010504 meteorology & atmospheric sciences, Ecliptic, Astronomy, Astronomy and Astrophysics, Contact binary, Light curve, 01 natural sciences, Article, Space and Planetary Science, Asteroid, 0103 physical sciences, Hill sphere, Asteroid belt, Ejecta, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: This paper presents results from a high spatial resolution survey of 33 main-belt asteroids with diameters >40 km using the Keck II Adaptive Optics (AO) facility. Five of these (45 Eugenia, 87 Sylvia, 107 Camilla, 121 Hermione, 130 Elektra) were confirmed to have satellite. Assuming the same albedo as the primary, these moonlets are relatively small (∼5% of the primary size) suggesting that they are fragments captured after a disruptive collision of a parent body or captured ejecta due to an impact. For each asteroid, we have estimated the minimum size of a moonlet that can positively detected within the Hill sphere of the system by estimating and modeling a 2-σ detection profile: in average on the data set, a moonlet located at 2/100 × RHill (1/4 × RHill) with a diameter larger than 6 km (4 km) would have been unambiguously seen. The apparent size and shape of each asteroid was estimated after deconvolution using a new algorithm called AIDA. The mean diameter for the majority of asteroids is in good agreement with IRAS radiometric measurements, though for asteroids with a D < 200 km, it is underestimated on average by 6–8%. Most asteroids had a size ratio that was very close to those determined by lightcurve measurements. One observation of 104 Klymene suggests it has a bifurcated shape. The bi-lobed shape of 121 Hermione described in Marchis et al. [Marchis, F., Hestroffer, D., Descamps, P., Berthier, J., Laver, C., de Pater, I., 2005c. Icarus 178, 450–464] was confirmed after deconvolution. The ratio of contact binaries in our survey, which is limited to asteroids larger than 40 km, is surprisingly high (∼6%), suggesting that a non-single configuration is common in the main-belt. Several asteroids have been analyzed with lightcurve inversions. We compared lightcurve inversion models for plane-of-sky predictions with the observed images (9 Metis, 52 Europa, 87 Sylvia, 130 Elektra, 192 Nausikaa, and 423 Diotima, 511 Davida). The AO images allowed us to determine a unique photometric mirror pole solution, which is normally ambiguous for asteroids moving close to the plane of the ecliptic (e.g., 192 Nausikaa and 52 Europa). The photometric inversion models agree well with the AO images, thus confirming the validity of both the lightcurve inversion method and the AO image reduction technique.
Published: 2006
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40. The dusty AGB star RS CrB: first mid-infrared interferometric observations with the Keck Telescopes

Author: B. Mennesson, C. Koresko, M. J. Creech-Eakman, E. Serabyn, M. M. Colavita, R. Akeson, E. Appleby, J. Bell, A. Booth, S. Crawford, W. Dahl, J. Fanson, C. Felizardo, J. Garcia, J. Gathright, J. Herstein, E. Hovland, M. Hrynevych, E. Johansson, D. Le Mignant, R. Ligon, R. Millan-Gabet, J. Moore, C. Neyman, D. Palmer, T. Panteleeva, C. Paine, S. Ragland, L. Reder, A. Rudeen, T. Saloga, M. Shao, R. Smythe, K. Summers, M. Swain, K. Tsubota, C. Tyau, G. Vasisht, P. Wizinowich, and J. Woillez
Subjects: Physics, Photosphere, Spectrometer, Opacity, Red giant, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spectral line, Wavelength, Space and Planetary Science, Asymptotic giant branch, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Variable star, Astrophysics::Galaxy Astrophysics
Abstract: We report interferometric observations of the semi-regular variable star RS CrB, a red giant with strong silicate emission features. The data were among the first long baseline mid-infrared stellar fringes obtained between the Keck telescopes, using parts of the new nulling beam combiner. The light was dispersed by a low-resolution spectrometer, allowing simultaneous measurement of the source visibility and intensity spectra from 8 to 12 microns. The interferometric observations allow a non-ambiguous determination of the dust shell spatial scale and relative flux contribution. Using a simple spherically-symmetric model, in which a geometrically thin shell surrounds the stellar photosphere, we find that ~30% to ~70% of the overall mid-infrared flux - depending on the wavelength - originates from 7-8 stellar radii. The derived shell opacity profile shows a broad peak around 11 microns (tau ~ 0.06), characteristic of Mg-rich silicate dust particles., Accepted for publication in ApJ Letters
Published: 2005

41. Keck Observatory Laser Guide Star Adaptive Optics Discovery and Characterization of a Satellite to the Large Kuiper Belt Object 2003 EL_(61)

Author: Jason C. Y. Chin, Doug Summers, Paul J. Stomski, R. Lafon, Randy Campbell, Erik M. Johansson, D. Rabinowitz, Antonin Bouchez, Michael E. Brown, Ramazan Sari, D. Le Mignant, S. K. Hartman, Peter Wizinowich, C. A. Trujillo, and M. van Dam
Subjects: Physics, Pluto, Solar System, Laser guide star, Space and Planetary Science, Observatory, Planet, Haumea, Astronomy, Astronomy and Astrophysics, Satellite, Astrophysics, Orbital period
Abstract: The newly commissioned laser guide star adaptive optics system at Keck Observatory has been used to discover and characterize the orbit of a satellite to the bright Kuiper Belt object 2003 EL_(61). Observations over a 6 month period show that the satellite has a semimajor axis of 49,500 ± 400 km, an orbital period of 49.12 ± 0.03 days, and an eccentricity of 0.050 ± 0.003. The inferred mass of the system is (4.2 ± 0.1) × 10^(21) kg, or ~32% of the mass of Pluto and 28.6% ± 0.7% of the mass of the Pluto-Charon system. Mutual occultations occurred in 1999 and will not occur again until 2138. The orbit is fully consistent neither with one tidally evolved from an earlier closer configuration nor with one evolved inward by dynamical friction from an earlier more distant configuration.
Published: 2005

42. The First Laser Guide Star Adaptive Optics Observations of the Galactic Center: Sgr A*'s Infrared Color and the Extended Red Emission in its Vicinity

Author: R. Lafon, Douglas M. Summers, Seth D. Hornstein, M. A. van Dam, Andrea M. Ghez, Randy Campbell, D. Le Mignant, Jessica R. Lu, Antonin Bouchez, Keith Matthews, Erik M. Johansson, Eric E. Becklin, Paul J. Stomski, Mark Morris, Jason C. Y. Chin, Peter Wizinowich, and S. K. Hartman
Subjects: Physics, Spectral index, Supermassive black hole, Infrared, Galactic Center, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, law.invention, Black hole, Laser guide star, 13. Climate action, Space and Planetary Science, law, Flare
Abstract: (Abridged) We present the first Laser Guide Star Adaptive Optics (LGS-AO) observations of the Galactic center. LGS-AO has dramatically improved the quality, robustness, and versatility with which high angular resolution infrared images of the Galactic center can be obtained with the W. M. Keck II 10-meter telescope. Specifically, Strehl ratios of 0.7 and 0.3 at L'[3.8 micron] and K'[2.1 micron], respectively, are achieved in these LGS-AO images. During our observations, the infrared counterpart to the central supermassive black hole, Sgr A*-IR, showed significant infrared intensity variations, with observed L' magnitudes ranging from 12.6 to 14.5 mag. The faintest end of our L' detections, 1.3 mJy (dereddened), is the lowest level of emission yet observed for this source by a factor of 3. No significant variation in the location of SgrA*-IR is detected as a function of either wavelength or intensity. Near a peak in its intensity, we obtained the first measurement of SgrA*-IR's K'-L' color (3.0 +- 0.2 mag, observed), which corresponds to an intrinsic spectral index of -0.5 +- 0.3. This is significantly bluer than other recent infrared measurements. Because our measurement was taken at a time when Sgr A* was ~6 times brighter in the infrared than the other measurements, we posit that the spectral index of the emission arising from the vicinity of our Galaxy's central black hole may depend on the strength of the flare, with stronger flares giving rise to a higher fraction of high energy electrons in the emitting region., Accepted for publication in ApJ (to appear in 20 Dec 2005, vol. 635 issue), 9 pages and 5 figures
Published: 2005

43. Merging Galaxies in Goods-s: First Extragalactic Results from Keck Laser Adaptive Optics

Author: Claire E. Max, Douglas M. Summers, D. Le Mignant, Jennifer M. Lotz, M. A. van Dam, R. Lafon, Erik M. Johansson, Jason Melbourne, Paul J. Stomski, Shelley A. Wright, Deanna Marie Pennington, Matthew Barczys, Jason C. Y. Chin, Peter Wizinowich, David C. Koo, A. H. Bouchez, S. K. Hartman, and James E. Larkin
Subjects: Physics, Active galactic nucleus, Stellar population, Star formation, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Astrophysics, 01 natural sciences, Redshift, Galaxy, Laser guide star, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, Adaptive optics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The Center for Adaptive Optics Treasury Survey (CATS) aims to combine deep HST images in the optical with deep Keck adaptive optics (AO) data in the near-infrared (NIR) to study distant galaxies, AGN, and supernovae. We recently achieved an important new milestone by securing the first Keck laser guide star AO image of faint galaxies. Six galaxies with redshifts ranging from 0.3-1.0 were targeted in one pointing in the GOODS-S field. Two are Chandra Deep Field South sources, XID-56 and XID-536, with complex morphologies suggestive of recent merger activity. Substructures seen in the NIR AO image (FWHM ~ 0.1"), including multiple tight knots in XID-56 and a double nucleus in XID-536, are confirmed in the optical HST images. These structures are unresolved in the best seeing-limited (FWHM ~ 0.5") NIR images. Stellar population synthesis models of the substructures indicate that XID-56 is a gas rich merger with a recent burst of star formation and significant amounts of dust. XID-536 appears to be a merger of two evolved stellar populations., 6 pages, 4 figures, 1 table, accepted ApJL 2005
Published: 2005

44. The Near-Infrared Size-Luminosity Relations for Herbig Ae/Be Disks

Author: M. Shao, M. Hrynevych, G. T. van Belle, Paola D'Alessio, John D. Monnier, J. Beletic, Jean-Philippe Berger, M. Mark Colavita, Michelle Creech-Eakman, C. Beichman, Mark R. Swain, D. Wallace, Peter Wizinowich, R. R. Thompson, Marc J. Kuchner, A. Booth, Gautam Vasisht, William C. Danchi, Nuria Calvet, A. Sargent, Rachel Akeson, Lynne A. Hillenbrand, J. Gathright, Wesley A. Traub, A. Boden, C. Koresko, R. Billmeier, J. Rajagopal, Lee Hartmann, R. Ligon, Peter G. Tuthill, D. Le Mignant, Chris Neyman, Rafael Millan-Gabet, Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 010308 nuclear & particles physics, Near-infrared spectroscopy, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Effective temperature, 01 natural sciences, Stars, Interferometry, Disk size, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Sublimation (phase transition), Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We report the results of a sensitive K-band survey of Herbig Ae/Be disk sizes using the 85-m baseline Keck Interferometer. Targets were chosen to span the maximum range of stellar properties to probe the disk size dependence on luminosity and effective temperature. For most targets, the measured near-infrared sizes (ranging from 0.2 to 4 AU) support a simple disk model possessing a central optically-thin (dust-free) cavity, ringed by hot dust emitting at the expected sublimation temperatures (T_sub~1000-1500K). Furthermore, we find a tight correlation of disk size with source luminosity R propto L^(1/2) for Ae and late Be systems (valid over more than 2 decades in luminosity), confirming earlier suggestions based on lower-quality data. Interestingly, the inferred dust-free inner cavities of the highest luminosity sources (Herbig B0-B3 stars) are under-sized compared to predictions of the optically-thin cavity model, likely due to optically-thick gas within the inner AU., Accepted by Astrophysical Journal; 24 pages, 4 figures, 4 tables
Published: 2005
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45. Satellites of the largest Kuiper belt objects

Author: D. Le Mignant, M. A. van Dam, R. Lafon, Peter Wizinowich, Douglas M. Summers, Antonin Bouchez, Michael E. Brown, David Rabinowitz, Paul J. Stomski, Al Conrad, Chadwick A. Trujillo, Erik M. Johansson, S. K. Hartman, Randy Campbell, and Jason C. Y. Chin
Subjects: Physics, Brightness, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Pluto, Laser guide star, Space and Planetary Science, Primary (astronomy), Observatory, Satellite, Adaptive optics
Abstract: We have searched the four brightest objects in the Kuiper Belt for the presence of satellites using the newly commissioned Keck Observatory Laser Guide Star Adaptive Optics system. Satellites are seen around three of the four objects: Pluto (whose satellite Charon is well-known and whose recently discovered smaller satellites are too faint to be detected), 2003 EL61 (where a second satellite is seen in addition to the previously known satellite), and 2003 UB313 (where a satellite is seen for the first time). The object 2005 FY9, the brightest Kuiper Belt object (KBO) after Pluto, does not have a satellite detectable within 0".4 with a brightness of more than 1% of the primary. The presence of satellites around three of the four brightest KBOs is inconsistent with the fraction of satellites in the Kuiper Belt at large at the 99.2% confidence level, suggesting a different formation mechanism for these largest KBO satellites. The two satellites of 2003 EL61, and the one satellite of 2003 UB313, with fractional brightnesses of 5% and 1.5%, and 2%, of their primaries, respectively, are significantly fainter relative to their primaries than other known KBO satellites, again pointing to possible differences in their origin.
Published: 2005
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46. Variable Infrared Emission from the Supermassive Black Hole at the Center of the Milky Way

Author: Shelley A. Wright, Mark Morris, Eric E. Becklin, K. Matthews, Andrea M. Ghez, David R. Thompson, B. T. Soifer, Angelle Tanner, D. Le Mignant, and Seth D. Hornstein
Subjects: Physics, Supermassive black hole, Accretion (meteorology), 010308 nuclear & particles physics, Point source, Infrared, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Black hole, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Magnitude (astronomy), Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We report the detection of a variable point source, imaged at L'(3.8 microns) with the W. M. Keck II 10-meter telescope's adaptive optics system, that is coincident to within 18 mas of the Galaxy's central supermassive black hole and the unique radio source Sgr A*. While in 2002 this source (SgrA*-IR) was confused with the stellar source S0-2, in 2003 these two sources are separated by 87 mas allowing the new source's properties to be determined directly. On four separate nights, its observed L' magnitude ranges from 12.2 to 13.8, which corresponds to a flux density of 0.7 - 3 mJy, observed, and 4 - 17 mJy, dereddened; no other source in this region shows such large variations in flux density - a factor of 4 over a week and a factor of 2 over 40 min. In addition, it has a K-L' color greater than 2.1, which is at least 1 mag redder than any other source detected at L' in its vicinity. Based on this source's coincidence with the Galaxy's dynamical center, its lack of motion, its variability, and its red color, we conclude that it is associated with the central supermassive black hole. The short timescale for the 3.8 micron flux density variations implies that the emission arises in the accretion flow on physical size scales smaller than 5 AU, or 80 R_s for a 4x10^6 Mo black hole. We suggest that the 3.8 micron emission and the X-ray flares arise from the same underlying physical process, possibly the acceleration of a small populations of electrons to ultrarelativistic energies. In contrast to the X-ray flares which are only detectable 2% of the time, the 3.8 micron emission provides a new, constantly accessible, window into the physical conditions of the plasma in close proximity to the central black hole., published in Astrophysical Journal Letters
Published: 2003

47. Observations of DG Tauri with the Keck Interferometer

Author: M. Colavita, R. Akeson, P. Wizinowich, M. Shao, S. Acton, J. Beletic, J. Bell, J. Berlin, A. Boden, A. Booth, R. Boutell, F. Chaffee, D. Chan, J. Chock, R. Cohen, S. Crawford, M. Creech-Eakman, G. Eychaner, C. Felizardo, J. Gathright, G. Hardy, H. Henderson, J. Herstein, M. Hess, E. Hovland, M. Hrynevych, R. Johnson, J. Kelley, R. Kendrick, C. Koresko, P. Kurpis, D. Le Mignant, H. Lewis, E. Ligon, W. Lupton, D. McBride, B. Mennesson, R. Millan-Gabet, J. Monnier, J. Moore, C. Nance, C. Neyman, A. Niessner, D. Palmer, L. Reder, A. Rudeen, T. Saloga, A. Sargent, E. Serabyn, R. Smythe, P. Stomski, K. Summers, M. Swain, P. Swanson, R. Thompson, K. Tsubota, A. Tumminello, G. van Belle, G. Vasisht, J. Vause, J. Walker, K. Wallace, and U. Wehmeier
Subjects: Physics, Infrared, Component (thermodynamics), Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, T Tauri star, Interferometry, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present the first science results from the Keck Interferometer, a direct-detection infrared interferometer utilizing the two 10-meter Keck telescopes. The instrument and system components are briefly described. We then present observations of the T Tauri object DG Tau, which is resolved by the interferometer. The resolved component has a radius of 0.12 to 0.24 AU, depending on the assumed stellar and extended component fluxes and the model geometry used. Possible origins and implications of the resolved emission are discussed., 10 pages, 2 figures, to appear in ApJ Letters
Published: 2003

48. Interferometer Observations of Subparsec-scale Infrared Emission in the Nucleus of NGC 4151

Author: M. Shao, R. Ligon, Michelle Creech-Eakman, D. Le Mignant, Robert R. Thompson, Rafael Millan-Gabet, Mark R. Swain, Chris Neyman, A. F. Boden, M. Mark Colavita, J. Beletic, Peter Wizinowich, John D. Monnier, M. Hrynevych, G. T. van Belle, Chas Beichman, Bertrand Mennesson, Gautam Vasisht, Stephen C. Unwin, A. Booth, Rachel Akeson, J. Gathright, Eugene Serabyn, C. Koresko, and Anneila I. Sargent
Subjects: Physics, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Resolution (electron density), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Interferometry, medicine.anatomical_structure, Accretion disc, Space and Planetary Science, K band, medicine, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Nucleus, Astrophysics::Galaxy Astrophysics
Abstract: We report novel, high-angular resolution interferometric measurements that imply the near-infrared nuclear emission in NGC 4151 is unexpectedly compact. We have observed the nucleus of NGC 4151 at 2.2 microns using the two 10-meter Keck telescopes as an interferometer and find a marginally resolved source ~0.1 pc in diameter. Our measurements rule out models in which a majority of the K band nuclear emission is produced on scales larger than this size. The interpretation of our measurement most consistent with other observations is that the emission mainly originates directly in the central accretion disk. This implies that AGN unification models invoking hot, optically thick dust may not be applicable to NGC 4151., Comment: 9 pages, 1 figure, accepted for publication in the Astrophysical Journal, Letters
Published: 2003
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49. Search for low-mass PMS companions around X-ray selected late B stars

Author: Pierre North, J. Krautter, Swetlana Hubrig, and D. Le Mignant
Subjects: Physics, Stars, Space and Planetary Science, Observatory, Near-infrared spectroscopy, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Low Mass
Abstract: We have observed 49 X-ray detected bright late B-type dwarfs to search for close low-mass pre-main sequence (PMS) companions using the European Southern Observatory's ADONIS (Adaptive Optics Near Infrared System) instrument. We announce the discovery of 21 new companions in 9 binaries, 5 triple, 4 quadruple system and 1 system consisting of five stars. The detected new companions have K magnitudes between 6.5 mag and 17.3 mag. and angular separations ranging from 0.2 and 14.1 arcsec (18-2358 AU)., Accepted for publication in Astronomy and Astrophysics
Published: 2001

50. Adaptive Optics observations of LBQS 0108+0028: K-band detection of the host galaxy of a radio-quiet QSO at z=2

Author: D. Le Mignant, Roberto Terlevich, Itziar Aretxaga, B. J. Boyle, and Jorge Melnick
Subjects: Physics, QSOS, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift, Galaxy, Luminosity, Space and Planetary Science, K band, QUIET, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, Host (network), Astrophysics::Galaxy Astrophysics
Abstract: We report the first unambiguous detection of the host galaxy of a normal radio-quiet QSO at high-redshift in K-band. The luminosity of the host comprises about 35% of the total K-band luminosity. Assuming the average colour of QSOs at z=2, the host would be about 5 to 6 mag brighter than an unevolved L* galaxy placed at z=2, and 3 to 4 mag brighter than a passively evolved L* galaxy at the same redshift. The luminosity of the host galaxy of the QSO would thus overlap with the highest found in radio-loud QSOs and radio-galaxies at the same redshift., Accepted to be published in MNRAS. 4 pages, 2 postscript figures. Also available at http://www.mpa-garching.mpg.de/~itziar
Published: 1998

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