Author: "Christian Thalmann" / Topic: astrophysics::earth and planetary astrophysics - Searchworks@Jio Institute Digital Library Search Results

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1. Subaru/HiCIAO HK s Imaging of LKHa 330: Multi-band Detection of the Gap and Spiral-like Structures

Author: Tomoyuki Kudo, Thomas Henning, Mickael Bonnefoy, Michael W. McElwain, Makoto Watanabe, Yutaka Hayano, Timothy D. Brandt, Sebastian Egner, Amaya Moro-Martin, Christian Thalmann, Takayuki Muto, Eugene Serabyn, Edwin L. Turner, Ryuji Suzuki, Carol A. Grady, Itsuki Sakon, Satoshi Mayama, Yasuhiro H. Takahashi, Markus Janson, Shoken M. Miyama, Klaus W. Hodapp, Hideki Takami, Tetsuo Nishimura, Toru Yamada, Thayne Currie, Masahiko Hayashi, John P. Wisniewski, Miki Ishii, Naruhisa Takato, Taro Matsuo, Saeko S. Hayashi, Tae-Soo Pyo, Nobuhiko Kusakabe, Takuya Suenaga, Jeffrey Fung, Yang Yang, Olivier Guyon, Michihiro Takami, Lyu Abe, Markus Feldt, Miwa Goto, Taichi Uyama, Tomonori Usuda, Jun-Ichi Morino, Eiji Akiyama, Ryo Kandori, Jun Hashimoto, Jungmi Kwon, Wolfgang Brandner, Masanori Iye, Joseph C. Carson, Motohide Tamura, Hiroshi Terada, Jerome de Leon, Hiroshi Suto, Ruobing Dong, Michael L. Sitko, Masayuki Kuzuhara, and Gillian R. Knapp
Subjects: Physics, planet-disk interactions, polarization, 010308 nuclear & particles physics, protoplanetary disks, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Azimuth, Wavelength, Multi band, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Spiral, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: 著者人数: 59名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 權, 靜美), Accepted: 2018-06-08, 資料番号: SA1180097000
Published: 2018

2. High-contrast Polarimetry Observation of T Tau Circumstellar Environment

Author: Eugene Serabyn, Wolfgang Brandner, Edwin L. Turner, Toru Yamada, Gillian R. Knapp, Thomas Henning, Satoshi Mayama, Shoken Miyama, Hideki Takami, Yi Yang, Jungmi Kwon, Eiji Akiyama, Michihiro Takami, Hiroshi Terada, Miwa Goto, Ryuji Suzuki, Takuya Suenaga, Naruhisa Takato, Lyu Abe, Yutaka Hayano, Tomoyuki Kudo, Michael W. McElwain, T. Currie, Tomonori Usuda, Ryo Kandori, Markus Janson, Takao Nakagawa, Nobuhiko Kusakabe, Klaus W. Hodapp, Yasuhiro H. Takahashi, Jun-Ichi Morino, Jun Hashimoto, Masayuki Kuzuhara, Tetsuo Nishimura, Roman R. Rafikov, Makoto Watanabe, Masanori Iye, Daehyeon Oh, Joseph C. Carson, Hiroshi Suto, Taro Matsuo, Munetake Momose, Timothy D. Brandt, Motohide Tamura, Tae-Soo Pyo, Christian Thalmann, Olivier Guyon, Amaya Moro-Martin, Miki Ishii, Carol A. Grady, Masahiko Hayashi, Sebastian Egner, Saeko S. Hayashi, Markus Feldt, John P. Wisniewski, Yang, Y [0000-0002-9024-4150], Mayama, S [0000-0002-3424-6266], Akiyama, E [0000-0002-5082-8880], Currie, T [0000-0002-7405-3119], Janson, M [0000-0001-8345-593X], Momose, M [0000-0002-3001-0897], Nakagawa, T [0000-0002-6660-9375], Oh, D [0000-0003-2691-804X], Kudo, T [0000-0002-9294-1793], Brandt, TD [0000-0003-2630-8073], Guyon, O [0000-0002-1097-9908], Hayano, Y [0000-0003-4937-4233], Hodapp, KW [0000-0003-0786-2140], Kandori, R [0000-0003-2610-6367], Knapp, GR [0000-0002-9259-1164], Kwon, J [0000-0003-2815-7774], Miyama, S [0000-0001-5017-180X], Moro-Martin, A [0000-0001-9504-8426], Pyo, TS [0000-0002-3273-0804], Takami, M [0000-0001-9248-7546], Terada, H [0000-0002-7914-6779], Thalmann, C [0000-0002-1664-2177], Watanabe, M [0000-0002-3656-4081], Wisniewski, J [0000-0001-9209-1808], Usuda, T [0000-0001-9855-0163], Tamura, M [0000-0002-6510-0681], and Apollo - University of Cambridge Repository
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, FOS: Physical sciences, Astrophysics, stars: pre-main sequence, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 010309 optics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Adaptive optics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, binaries: general (T Tau), protoplanetary disks, Astronomy and Astrophysics, Polarization (waves), Position angle, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, stars: variables: T Tauri, Herbig Ae/Be, Outflow, Astrophysics::Earth and Planetary Astrophysics, Circumbinary planet, Subaru Telescope, Astrophysics - Earth and Planetary Astrophysics
Abstract: 著者人数: 55名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 中川, 貴雄; 權, 靜美), Accepted: 2018-05-18, 資料番号: SA1180099000
Published: 2018

3. Results of the NaCo Large Program: probing the occurrence of exoplanets and brown dwarfs at wide orbit

Author: Maddalena Reggiani, Silvano Desidera, Arthur Vigan, C. Mordasini, G. Montagnier, Damien Ségransan, Mariangela Bonavita, Janis Hagelberg, Gael Chauvin, A-M. Lagrange, Laurent M. Mugnier, David Mouillet, Alice Zurlo, Beth Biller, M. Bonnefoy, Joseph C. Carson, Sergio Messina, Anthony Boccaletti, A. C. Lanzafame, C. Moutou, Esther Buenzli, Sascha P. Quanz, Christian Thalmann, Elvira Covino, Michael Meyer, M. Feldt, Francois Menard, P. Delorme, Dino Mesa, Jean-Charles Augereau, E. Brugaletta, J. L. Beuzit, Th. Henning, A. Eggenberger, Rens Waters, 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), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Erosion torrentielle neige et avalanches (UR ETGR (ETNA)), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Department of Biochemistry and Molecular Biology, Mayo Clinic, 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Catania (OACT), Recherche Nutrition Humaine, Hôpital de l'Hôtel-Dieu de Clermont-Ferrand, European Southern Observatory (ESO), Physikalisches Institut [Bern], Universität Bern [Bern], DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Dipartimento di Biochimica G. Moruzzi Sez di Chimica e Propedeutica Biochimica Bologna 40126, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Low Energy Astrophysics (API, FNWI), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), 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), Unité de Nutrition Humaine (UNH), Université d'Auvergne - Clermont-Ferrand I (UdA)-Clermont Université-Institut National de la Recherche Agronomique (INRA), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), 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 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), Institut National de la Recherche Agronomique (INRA)-Université d'Auvergne - Clermont-Ferrand I (UdA)-Clermont Université, Universität Bern [Bern] (UNIBE), and Université de Genève = University of Geneva (UNIGE)
Subjects: 010504 meteorology & atmospheric sciences, Stellar mass, Population, Brown dwarf, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, instrumentation: adaptive optics, 01 natural sciences, Planet, instrumentation: high angular resolution, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, education.field_of_study, methods: statistical, Astronomy, Astronomy and Astrophysics, Exoplanet, stars: imaging, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Planetary mass
Abstract: Over the past decade, a growing number of deep imaging surveys have started to provide meaningful constraints on the population of extrasolar giant planets at large orbital separation. Primary targets for these surveys have been carefully selected based on their age, distance and spectral type, and often on their membership to young nearby associations where all stars share common kinematics, photometric and spectroscopic properties. The next step is a wider statistical analysis of the frequency and properties of low mass companions as a function of stellar mass and orbital separation. In late 2009, we initiated a coordinated European Large Program using angular differential imaging in the H band (1.66 μm) with NaCo at the VLT. Our aim is to provide a comprehensive and statistically significant study of the occurrence of extrasolar giant planets and brown dwarfs at large (5-500 AU) orbital separation around ~150 young, nearby stars, a large fraction of which have never been observed at very deep contrast. The survey has now been completed and we present the data analysis and detection limits for the observed sample, for which we reach the planetary-mass domain at separations of ≳50 AU on average. We also present the results of the statistical analysis that has been performed over the 75 targets newly observed at high-contrast. We discuss the details of the statistical analysis and the physical constraints that our survey provides for the frequency and formation scenario of planetary mass companions at large separation.
Published: 2017

4. 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

5. RESOLVING THE PLANET-HOSTING INNER REGIONS OF THE LkCa 15 DISK

Author: Gael Chauvin, Johan Olofsson, Alice Zurlo, Dino Mesa, Thomas Henning, Carsten Dominik, Anthony Boccaletti, Mickael Bonnefoy, J. Lannier, François Ménard, Antonio Garufi, Sebastian Daemgen, Markus Feldt, E. Sissa, Raffaele Gratton, Christian Thalmann, N. Engler, Markus Janson, Anne-Marie Lagrange, H. M. Schmid, H. Le Coroller, Myriam Benisty, Silvano Desidera, Gijs D. Mulders, Michael R. Meyer, Christophe Pinte, Graeme Salter, Maud Langlois, Sascha P. Quanz, R. Ligi, Arthur Vigan, 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), 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), 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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), 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), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 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, 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), GDFSuez, 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, 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), 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), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), 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)-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], 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), 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), 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), 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)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), 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), Low Energy Astrophysics (API, FNWI), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Universidad de Chile-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Brightness, Scattering, Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, 010309 optics, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Substructure, Surface brightness, Astrophysics::Earth and Planetary Astrophysics, Protoplanet, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: LkCa 15 hosts a pre-transitional disk as well as at least one accreting protoplanet orbiting in its gap. Previous disk observations have focused mainly on the outer disk, which is cleared inward of ~50 au. The planet candidates, on the other hand, reside at orbital radii around 15 au, where disk observations have been unreliable until recently. Here we present new J-band imaging polarimetry of LkCa 15 with SPHERE IRDIS, yielding the most accurate and detailed scattered-light images of the disk to date down to the planet-hosting inner regions. We find what appear to be persistent asymmetric structures in the scattering material at the location of the planet candidates, which could be responsible at least for parts of the signals measured with sparse-aperture masking. These images further allow us to trace the gap edge in scattered light at all position angles and search the inner and outer disks for morphological substructure. The outer disk appears smooth with slight azimuthal variations in polarized surface brightness, which may be due to shadowing from the inner disk or a two-peaked polarized phase function. We find that the near-side gap edge revealed by polarimetry matches the sharp crescent seen in previous ADI imaging very well. Finally, the ratio of polarized disk to stellar flux is more than six times larger in J-band than in the RI bands., 6 pages, 4 figures, 1 table; accepted for publication in ApJ Letters
Published: 2016

6. Near-infrared imaging polarimetry of LkCa 15: A possible warped inner disk()

Author: Masahiko Hayashi, Carol A. Grady, T. Currie, Markus Feldt, Christian Thalmann, Jun-Ichi Morino, Ryo Kandori, Tomonori Usuda, Michael W. McElwain, Sebastian Egner, Edwin L. Turner, Miwa Goto, Eiji Akiyama, Masanori Iye, Eugene Serabyn, Motohide Tamura, Yasuhiro H. Takahashi, Miki Ishii, Hideki Takami, Gillian R. Knapp, Tetsuo Nishimura, Hiroshi Terada, Thomas Henning, Saeko S. Hayashi, Naruhisa Takato, Lyu Abe, Joseph C. Carson, Tae-Soo Pyo, Masayuki Kuzuhara, Takuya Suenaga, Olivier Guyon, John P. Wisniewski, Toru Yamada, Yutaka Hayano, Daehyeon Oh, Timothy D. Brandt, Wolfgang Brandner, Satoshi Mayama, Tomoyuki Kudo, Michihiro Takami, Shoken Miyama, Markus Janson, Jungmi Kwon, Hiroshi Suto, Makoto Watanabe, Klaus W. Hodapp, Nobuhiko Kusakabe, Ryuji Suzuki, Taro Matsuo, Amaya Moro-Martin, and Jun Hashimoto
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Planetary system, Position angle, 01 natural sciences, Article, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, Near infrared imaging, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Intensity (heat transfer), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present high-contrast H-band polarized intensity images of the transitional disk around the young solar-like star LkCa 15. By utilizing Subaru/HiCIAO for polarimetric differential imaging, both the angular resolution and the inner working angle reach 0.07" and r=0.1", respectively. We obtained a clearly resolved gap (width, Comment: 6 pages, 3 figures, accepted in PASJ on December 14, 2015
Published: 2016

7. The SEEDS High Contrast Imaging Survey of Exoplanets around Young Stellar Objects

Author: Jungmi Kwon, Hiroshi Suto, Ryo Kandori, Joseph C. Carson, Michael W. McElwain, Tomonori Usuda, Tomoyuki Kudo, Toru Yamada, Michihiro Takami, Thayne Currie, Nobuhiko Kusakabe, Thomas Henning, Klaus W. Hodapp, Taro Matsuo, Miwa Goto, Miki Ishii, Eugene Serabyn, Masayuki Kuzuhara, Satoshi Mayama, Christian Thalmann, Hideki Takami, Timothy D. Brandt, Eiji Akiyama, Yutaka Hayano, Makoto Watanabe, Tetsuo Nishimura, Saeko S. Hayashi, Tae-Soo Pyo, Shoken Miyama, Markus Janson, Olivier Guyon, Gillian R. Knapp, Jun Hashimoto, John H. Livingston, Amaya Moro-Martin, Sebastian Egner, Wolfgang Brandner, Takuya Suenaga, Taichi Uyama, Masanori Iye, John P. Wisniewski, Markus Feldt, Edwin L. Turner, Motohide Tamura, Masahiko Hayashi, Jun-Ichi Morino, Carol A. Grady, Ryuji Suzuki, Yasuhiro H. Takahashi, Hiroshi Terada, Naruhisa Takato, and Lyu Abe
Subjects: Proper motion, 010504 meteorology & atmospheric sciences, Young stellar object, Population, Brown dwarf, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, Giant planet, Astronomy, Astronomy and Astrophysics, Planetary system, Exoplanet, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present high-contrast observations of 68 young stellar objects (YSOs) explored as part of the SEEDS survey on the Subaru telescope. Our targets are very young ($, Comment: 31pages, 13 figures, accepted to AJ
Published: 2016
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8. SPOTS: The Search for Planets Orbiting Two Stars: II. First constraints on the frequency of sub-stellar companions on wide circumbinary orbits

Author: Silvano Desidera, Mariangela Bonavita, J. Lannier, Markus Janson, Arthur Vigan, Christian Thalmann, Gael Chauvin, 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), and 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)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Planetary system, 01 natural sciences, Exoplanet, Radial velocity, Orbit, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Circumbinary planet, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences, Eclipse
Abstract: A large number of direct imaging surveys for exoplanets have been performed in recent years, yielding the first directly imaged planets and providing constraints on the prevalence and distribution of wide planetary systems. However, like most of the radial velocity ones, these surveys generally focus on single stars, hence binaries and higher-order multiples have not been studied to the same level of scrutiny. This motivated the SPOTS (Search for Planets Orbiting Two Stars) survey, which is an ongoing direct imaging study of a large sample of close binaries, started with VLT/NACO and now continuing with VLT/SPHERE. To complement this survey, we have identified the close binary targets in 24 published direct imaging surveys. Here we present our statistical analysis of this combined body of data. We analysed a sample of 117 tight binary systems, using a combined Monte Carlo and Bayesian approach to derive the expected values of the frequency of companions, for different values of the companion's semi-major axis. Our analysis suggest that the frequency of sub-stellar companions in wide orbit is moderately low ($\lesssim $13% with a best value of 6% at 95% confidence level) and not significantly different between single stars and tight binaries. One implication of this result is that the very high frequency of circumbinary planets in wide orbits around post-common envelope binaries, implied by eclipse timing (up to 90% according to Zorotovic & Schreiber 2013), can not be uniquely due to planets formed before the common-envelope phase (first generation planets), supporting instead the second generation planet formation or a non-Keplerian origin of the timing variations., 21 pages, 3 figures
Published: 2016
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9. A Dual-Mask Coronagraph for Observing Faint Companions to Binary Stars

Author: Christian Thalmann, Michael W. McElwain, Eric Cady, N. Jeremy Kasdin, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Image plane, 01 natural sciences, law.invention, Stars, Apodization, Space and Planetary Science, law, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Scattered light, Astrophysics - Instrumentation and Methods for Astrophysics, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Coronagraph, Astrophysics::Galaxy Astrophysics
Abstract: Observations of binary stars for faint companions with conventional coronagraphic methods are challenging, as both targets will be bright enough to obscure any nearby faint companions if their scattered light is not suppressed. We propose coronagraphic examination of binary stars using an apodized pupil Lyot coronagraph and a pair of actively-controlled image plane masks to suppress both stars simultaneously. The performance is compared to imaging with a band-limited mask, a dual-mask Lyot coronagraph and with no coronagraph at all. An imaging procedure and control system for the masks are also described., Comment: 17 pages, 6 figures
Published: 2011

10. Search for outer massive bodies around transiting planetary systems: Candidates of faint stellar companions around HAT-P-7

Author: Jun Hashimoto, Amaya Moro-Martin, Masayuki Kuzuhara, Naruhisa Takato, Lyu Abe, Edwin L. Turner, Michihiro Takami, Yasuhiro H. Takahashi, Tetsuo Nishimura, Yutaka Hayano, Shoken Miyama, Takuya Suenaga, Ryuji Suzuki, Markus Janson, Tomonori Usuda, Tae-Soo Pyo, Michael W. McElwain, Joseph C. Carson, Olivier Guyon, Motohide Tamura, Toru Yamada, Hiroshi Terada, Christian Thalmann, Miki Ishii, C. Bergfors, Hiroshi Suto, Wolfgang Brandner, Hideki Takami, Bun'ei Sato, Tomoyuki Kudo, Taro Matsuo, Jun-Ichi Morino, Masahiko Hayashi, Ryo Kandori, Norio Narita, Eugene Serabyn, Thomas Henning, Taras Golota, Makiko Nagasawa, Miwa Goto, Klaus W. Hodapp, Shigeru Ida, Saeko S. Hayashi, Sebastian Egner, Makoto Watanabe, Markus Feldt, Gillian R. Knapp, Daigo Tomono, and Nobuhiko Kusakabe
Subjects: Third body, 010504 meteorology & atmospheric sciences, Brown dwarf, FOS: Physical sciences, Direct imaging, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy, Astronomy and Astrophysics, Planetary system, Orbit, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present results of direct imaging observations for HAT-P-7 taken with the Subaru HiCIAO and the Calar Alto AstraLux. Since the close-in transiting planet HAT-P-7b was reported to have a highly tilted orbit, massive bodies such as giant planets, brown dwarfs, or a binary star are expected to exist in the outer region of this system. We show that there are indeed two candidates for distant faint stellar companions around HAT-P-7. We discuss possible roles played by such companions on the orbital evolution of HAT-P-7b. We conclude that as there is a third body in the system as reported by Winn et al. (2009, ApJL, 763, L99), the Kozai migration is less likely while planet-planet scattering is possible., Comment: 8 pages, 3 figures, 2 tables, PASJ in press
Published: 2010

11. Fast-moving features in the debris disk around AU Microscopii

Author: Johan Olofsson, Thierry Fusco, Markus Feldt, Arthur Vigan, Thomas Henning, Anne-Lise Maire, Dean C. Hines, Carol A. Grady, Christian Ginski, Anne-Marie Lagrange, Christian Thalmann, Joshua E. Schlieder, Dimitri Mawet, John P. Wisniewski, John H. Debes, Massimo Turatto, Maud Langlois, Julien Girard, Kjetil Dohlen, Glenn Schneider, Stéphane Udry, Farrokh Vakili, Michael Meyer, Julien Milli, Markus Janson, N. Engler, Francois Menard, Anthony Boccaletti, Jean-Luc Beuzit, C. Moutou, Zahed Wahhaj, Hans Martin Schmid, Joseph C. Carson, Jean-François Sauvage, Carsten Dominik, David Mouillet, Jean-Charles Augereau, Markus Kasper, Timothy J. Rodigas, 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), Low Energy Astrophysics (API, FNWI), and ITA
Subjects: Physics, Brightness, Debris disk, Multidisciplinary, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomical unit, Brown dwarf, Astronomy, Astrophysics, 01 natural sciences, Exoplanet, Stars, Planet, 0103 physical sciences, Beta Pictoris, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: International audience; In the 1980s, excess infrared emission was discovered around main-sequence stars; subsequent direct-imaging observations revealed orbiting disks of cold dust to be the source(1). These `debris disks' were thought to be by-products of planet formation because they often exhibited morphological and brightness asymmetries that may result from gravitational perturbation by planets. This was proved to be true for the beta Pictoris system, in which the known planet generates an observable warp in the disk(2-5). The nearby, young, unusually active late-type star AU Microscopii hosts a well-studied edge-on debris disk; earlier observations in the visible and near-infrared found asymmetric localized structures in the form of intensity variations along the midplane of the disk beyond a distance of 20 astronomical units(6-9). Here we report high-contrast imaging that reveals a series of five large-scale features in the southeast side of the disk, at projected separations of 10-60 astronomical units, persisting over intervals of 1-4 years. All these features appear to move away from the star at projected speeds of 4-10 kilometres per second, suggesting highly eccentric or unbound trajectories if they are associated with physical entities. The origin, localization, morphology and rapid evolution of these features are difficult to reconcile with current theories.
Published: 2015

12. Near-IR Polarized Scattered Light Imagery of the DoAr 28 Transitional Disk

Author: Timothy D. Brandt, Tomonori Usuda, Joseph C. Carson, Nobuhiko Kusakabe, Christian Thalmann, Makoto Watanabe, Evan A. Rich, Daigo Tomono, Miki Ishii, Katherine B. Follette, Naruhisa Takato, Sebastian Egner, Lyu Abe, Chunhua Qi, Gillian R. Knapp, Michihiro Takami, Carol A. Grady, Amaya Moro-Martin, Thayne Currie, Takuya Suenaga, Miwa Goto, Yasuhiro H. Takahashi, Eiji Akiyama, Hiroshi Terada, Masayuki Kuzuhara, Michael W. McElwain, Jungmi Kwon, John P. Wisniewski, Tetsuo Nishimura, Thomas Henning, Eugene Serabyn, Tomoyuki Kudo, Jun-Ichi Morino, Catherine Espaillat, Ryuji Suzuki, Ryo Kandori, Shoken Miyama, Markus Feldt, Klaus W. Hodapp, Masanori Iye, Hideki Takami, Hiroshi Suto, Jun Hashimoto, Tae-Soo Pyo, Olivier Guyon, Edwin L. Turner, Motohide Tamura, Toru Yamada, Masahiko Hayashi, Saeko S. Hayashi, Wolfgang Brandner, Markus Janson, Yutaka Hayano, Satoshi Mayama, and Taro Matsuo
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Point source, Spatially resolved, Monte Carlo method, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Space and Planetary Science, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Sublimation (phase transition), Astrophysics::Earth and Planetary Astrophysics, Scattered light, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the first spatially resolved polarized scattered light H-band detection of the DoAr 28 transitional disk. Our two epochs of imagery detect the scattered light disk from our effective inner working angle of 0.10" (13 AU) out to 0.50" (65 AU). This inner working angle is interior to the location of the system's gap inferred by previous studies using SED modeling (15 AU). We detected a candidate point source companion 1.08" northwest of the system; however, our second epoch of imagery strongly suggests that this object is a background star. We constructed a grid of Monte Carlo Radiative Transfer models of the system, and our best fit models utilize a modestly inclined (50 deg), 0.01 Msun disk that has a partially depleted inner gap from the dust sublimation radius out to ~8 AU. Subtracting this best fit, axi-symmetric model from our polarized intensity data reveals evidence for two small asymmetries in the disk, which could be attributable to variety of mechanisms., 9 pages, 8 figures, 2 tables
Published: 2015

13. Near-Infrared Polarimetry of the GG Tauri A Binary System

Author: Ryo Kandori, Yasuhiro H. Takahashi, Hiroshi Terada, Klaus W. Hodapp, Hideki Takami, Thayne Currie, Ryuji Suzuki, Timothy D. Brandt, Wolfgang Brandner, Nobuhiko Kusakabe, Shoken Miyama, Takuya Suenaga, Eugene Serabyn, Markus Janson, Tomoyuki Kudo, Yoichi Itoh, Masayuki Kuzuhara, Yutaka Hayano, Michael W. McElwain, Jungmi Kwon, Naruhisa Takato, Hiroshi Suto, Gillian R. Knapp, Tetsuo Nishimura, Carol A. Grady, Satoshi Mayama, Taro Matsuo, Joseph C. Carson, Thomas Henning, Masahiko Hayashi, Sebastian Egner, Makoto Watanabe, Miki Ishii, Lyu Abe, Yumiko Oasa, Daigo Tomono, Edwin L. Turner, Markus Feldt, Motohide Tamura, Toru Yamada, Christian Thalmann, Tae-Soo Pyo, Olivier Guyon, Jun Hashimoto, Amaya Moro-Martin, Saeko S. Hayashi, Masanori Iye, Jun-Ichi Morino, Tomonori Usuda, and John P. Wisniewski
Subjects: Physics, 010504 meteorology & atmospheric sciences, Scattering, Polarimetry, Binary number, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, symbols.namesake, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Orbit (dynamics), symbols, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, Binary system, Astrophysics::Earth and Planetary Astrophysics, Rayleigh scattering, Circumbinary planet, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences
Abstract: A high angular resolution near-infrared polarized-intensity image of the GG Tau A binary system was obtained with the Subaru Telescope. The image shows the circumbinary disk scattering the light from the central binary. The azimuthal profile of the polarized intensity of the circumbinary disk is roughly reproduced by a simple disk model with the Henyey-Greenstein function and the Rayleigh function, indicating small dust grains at the surface of the disk. Combined with a previous observation of the circumbinary disk, our image indicates that the gap structure in the circumbinary disk orbits anti-clockwise, while material in the disk orbit clockwise. We propose a shadow of material located between the central binary and the circumbinary disk. The separations and position angles of the stellar components of the binary in the past 20 years are consistent with the binary orbit with a = 33.4 AU and e = 0.34., Comment: 10 pages, 3 figures
Published: 2015
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14. The Structure of Pre-transitional Protoplanetary Disks. II. Azimuthal Asymmetries, Different Radial Distributions of Large and Small Dust Grains in PDS 70

Author: Masayuki Kuzuhara, Joseph C. Carson, Thomas Henning, Miki Ishii, Shoken Miyama, D. Tomono, Sebastian Egner, Nagayoshi Ohashi, Tae-Soo Pyo, Satoshi Mayama, Carol A. Grady, Olivier Guyon, Ruobing Dong, Yasuhiro H. Takahashi, Markus Janson, Taro Matsuo, Edwin L. Turner, Thayne Currie, Nobuhiko Kusakabe, Makoto Watanabe, Motohide Tamura, Ryo Kandori, Toru Yamada, Masahiko Hayashi, Klaus W. Hodapp, Zhaohuan Zhu, Takayuki Muto, Michihiro Takami, Ryuji Suzuki, Hideki Takami, Christian Thalmann, Saeko S. Hayashi, Kyle Mede, Joanna M. Brown, Jungmi Kwon, Wolfgang Brandner, Yutaka Hayano, Jun-Ichi Morino, Hiroshi Terada, Timothy D. Brandt, Masanori Iye, Tomoyuki Kudo, Gene Serabyn, Naruhisa Takato, Lyu Abe, Tomonori Usuda, Tetsuro Nishimura, Eiji Akiyama, Gillian R. Knapp, Hiroshi Suto, Markus Feldt, John P. Wisniewski, Amaya Moro-Martin, Takashi Tsukagoshi, Jun Hashimoto, Takuya Suenaga, Michael W. McElwain, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Brightness, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Protoplanetary disk, Photoevaporation, Vortex, Wavelength, T Tauri star, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Planet, Astrophysics::Solar and Stellar Astrophysics, Millimeter, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The formation scenario of a gapped disk, i.e., transitional disk, and its asymmetry is still under debate. Proposed scenarios such as disk-planet interaction, photoevaporation, grain growth, anticyclonic vortex, eccentricity, and their combinations would result in different radial distributions of the gas and the small (sub-$\mu$m size) and large (millimeter size) dust grains as well as asymmetric structures in a disk. Optical/near-infrared (NIR) imaging observations and (sub-)millimeter interferometry can trace small and large dust grains, respectively; therefore multi-wavelength observations could help elucidate the origin of complicated structures of a disk. Here we report SMA observations of the dust continuum at 1.3~mm and $^{12}$CO~$J=2\rightarrow1$ line emission of the pre-transitional protoplanetary disk around the solar-mass star PDS~70. PDS~70, a weak-lined T Tauri star, exhibits a gap in the scattered light from its disk with a radius of $\sim$65~AU at NIR wavelengths. However, we found a larger gap in the disk with a radius of $\sim$80~AU at 1.3~mm. Emission from all three disk components (the gas and the small and large dust grains) in images exhibits a deficit in brightness in the central region of the disk, in particular, the dust-disk in small and large dust grains has asymmetric brightness. The contrast ratio of the flux density in the dust continuum between the peak position to the opposite side of the disk reaches 1.4. We suggest the asymmetries and different gap-radii of the disk around PDS~70 are potentially formed by several (unseen) accreting planets inducing dust filtration., Comment: Accepted by ApJ
Published: 2015

15. Near-IR High-Resolution Imaging Polarimetry of the SU Aur Disk: Clues for Tidal Tails?

Author: Masanori Iye, Carol A. Grady, Makoto Watanabe, Miwa Goto, Eiji Akiyama, Masayuki Kuzuhara, Tomoyuki Kudo, Jun-Ichi Morino, Thayne Currie, Ryo Kandori, Markus Feldt, Daigo Tomono, Katherine B. Follette, Naruhisa Takato, Lyu Abe, Michael L. Sitko, Michael W. McElwain, Jungmi Kwon, Klaus W. Hodapp, Hiroshi Suto, Tetsuo Nishimura, N. Kusakabe, Gillian R. Knapp, Jerome de Leon, Satoshi Mayama, Masahiko Hayashi, Yutaka Hayano, Michihiro Takami, Christian Thalmann, Saeko S. Hayashi, Ryuji Suzuki, Taro Matsuo, Tae-Soo Pyo, Olivier Guyon, Yasuhiro H. Takahashi, Timothy D. Brandt, Hiroshi Terada, Joseph C. Carson, Takuya Suenaga, John P. Wisniewski, Thomas Henning, Hideki Takami, Hauyu Baobab Liu, Wolfgang Brandner, Miki Ishii, Sebastian Egner, Tomonori Usuda, Edwin L. Turner, Shoken Miyama, Motohide Tamura, Markus Janson, Toru Yamada, Jennifer L. Karr, Eugene Serabyn, Jun Hashimoto, and Amaya Moro-Martin
Subjects: Brightness, 010504 meteorology & atmospheric sciences, Reflection nebula, media_common.quotation_subject, Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Asymmetry, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Image (category theory), Astronomy and Astrophysics, T Tauri star, Wavelength, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Sky, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present new high-resolution ($\sim$0\farcs09) $H$-band imaging observations of the circumstellar disk around the T Tauri star SU Aur. Our observations with Subaru-HiCIAO have revealed the presence of scattered light as close as 0\farcs15 ($\sim$20 AU) to the star. Within our image, we identify bright emission associated with a disk with a minimum radius of $\sim$90 AU, an inclination of $\sim$35\degr from the plane of the sky, and an approximate P.A. of 15\degr for the major axis. We find a brightness asymmetry between the northern and southern sides of the disk due to a non-axisymmetric disk structure. We also identify a pair of asymmetric tail structures extending east and west from the disk. The western tail extends at least 2\farcs5 (350 AU) from the star, and is probably associated with a reflection nebula previously observed at optical and near-IR wavelengths. The eastern tail extends at least 1\arcsec (140 AU) at the present signal-to-noise. These tails are likely due to an encounter with an unseen brown dwarf, but our results do not exclude the explanation that these tails are outflow cavities or jets., Comment: 12 pages, 3 figures, accepted by ApJ
Published: 2015
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16. Detection of Sharp Symmetric Features in the Circumbinary Disk Around AK Sco

Author: Jean-Charles Augereau, Antonio Garufi, Francesco Marzari, Ruben Asensio-Torres, Anne-Lise Maire, Alice Zurlo, Silvano Desidera, Adriana Pohl, Joseph C. Carson, Michael R. Meyer, Markus Janson, Thomas Henning, Christian Thalmann, Anthony Boccaletti, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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), 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), 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), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), Institut de sciences exactes et appliquées (ISEA), Université de la Nouvelle-Calédonie (UNC), 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), 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), 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), Universita degli Studi di Padova, Institut des Sciences Exactes et Appliquées, Université de la Nouvelle Calédonie (UNC), 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: FOS: Physical sciences, Double star, Astrophysics, Planet, planetdisk interactions, Binary star, Astrophysics::Solar and Stellar Astrophysics, planetary syst, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, [PHYS]Physics [physics], Earth and Planetary Astrophysics (astro-ph.EP), Spiral galaxy, Astronomy and Astrophysics, Planetary system, Stars, binaries: general, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Circumbinary planet, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: The Search for Planets Orbiting Two Stars (SPOTS) survey aims to study the formation and distribution of planets in binary systems by detecting and characterizing circumbinary planets and their formation environments through direct imaging. With the SPHERE Extreme Adaptive Optics instrument, a good contrast can be achieved even at small (, 10 pages, 3 figures, accepted for publication in ApJ Letters. Minor (proof-level) corrections implemented in this version
Published: 2015
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17. A narrow, edge-on disk resolved around HD 106906 with SPHERE

Author: Matthias Samland, Thomas Henning, Lyu Abe, S. Peretti, Anne-Lise Maire, Hervé Beust, H. Le Coroller, F. Madec, Clément Perrot, Raphael Galicher, Johan Olofsson, Gael Chauvin, Mickael Bonnefoy, Christian Thalmann, Cyril Petit, A-M. Lagrange, Maud Langlois, Markus Janson, Dino Mesa, Graeme Salter, E. Sissa, Julien Girard, J. L. Beuzit, L. Weber, Wolfgang Brandner, Raffaele Gratton, Matthew A. Kenworthy, Julien Milli, J. Lannier, Silvano Desidera, François Ménard, Markus Feldt, D. Perret, C. Soenke, Anthony Boccaletti, P. Rabou, David Mouillet, Esther Buenzli, Vanessa P. Bailey, Anthony Cheetham, Arthur Vigan, Zahed Wahhaj, Surace, Christian, 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 - 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), 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), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Steward Observatory, University of Arizona, 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), Centre scientifique et Technique Jean Feger (CSTJF), TOTAL FINA ELF, Sterrewacht Leiden, Universiteit Leiden [Leiden], Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Department of Astronomy, Stockholm University, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), 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), 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), ESO, Physics Department [Garching], Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM)-Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), 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)-Hospices Civils de Lyon (HCL)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble [2011-2019] (IPAG [2011-2019]), Observatoire des Sciences de l'Univers de Grenoble [1985-2015] (OSUG [1985-2015]), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-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 [2007-2019] (Grenoble INP [2007-2019])-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)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Instituto de Fisica y Astronomia, ICM nucleus on protoplanetary disks, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), 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), 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)-Centre National de la Recherche Scientifique (CNRS), ONERA - The French Aerospace Lab [Châtillon], Université Paris Saclay (COmUE)-ONERA, Université Joseph Fourier - Grenoble 1 (UJF), 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), TOTAL-Scientific and Technical Center Jean Féger (CSTJF), University of Geneva [Switzerland], 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 Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Technical University of Munich (TUM)-Technical University of Munich (TUM), 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 Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble [1985-2015] (OSUG [1985-2015]), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-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)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-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)-Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Universidad de Chile-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Universiteit Leiden, 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 de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - 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), 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 Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA), ONERA, and université J.Fourier
Subjects: Brightness, 010504 meteorology & atmospheric sciences, HD 106906, FOS: Physical sciences, Astrophysics, 01 natural sciences, [SDU] Sciences of the Universe [physics], Planet, 0103 physical sciences, PLANETARY SYSTEMS, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Debris disk, Spectrometer, Plane (geometry), HIGH ANGULAR RESOLUTION, Astronomy and Astrophysics, Planetary system, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Orbit, Astrophysics - Solar and Stellar Astrophysics, Radiation pressure, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: HD~106906AB is so far the only young binary system around which a planet has been imaged and a debris disk evidenced thanks to a strong IR excess. As such, it represents a unique opportunity to study the dynamics of young planetary systems. We aim at further investigating the close (tens of au scales) environment of the HD~106906AB system. We used the extreme AO fed, high contrast imager SPHERE recently installed on the VLT to observe HD~106906. Both the IRDIS imager and the Integral Field Spectrometer were used. We discovered a very inclined, ring-like disk at a distance of 65~au from the star. The disk shows a strong brightness asymmetry with respect to its semi-major axis. It shows a smooth outer edge, compatible with ejection of small grains by the stellar radiation pressure. We show furthermore that the planet's projected position is significantly above the disk's PA. Given the determined disk inclination, it is not excluded though that the planet could still orbit within the disk plane if at a large separation (2000--3000 au). We identified several additional point sources in the SPHERE/IRDIS field-of-view, that appear to be background objects. We compare this system with other debris disks sharing similarities, and we briefly discuss the present results in the framework of dynamical evolution., Comment: 7 pages, 6 figures, accepted by Astronomy & Astrophysics
Published: 2015
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18. A Statistical Analysis of SEEDS and Other High-Contrast Exoplanet Surveys: Massive Planets or Low-Mass Brown Dwarfs?

Author: Gillian R. Knapp, Christian Thalmann, Tomonori Usuda, Lyu Abe, Masayuki Kuzuhara, Edwin L. Turner, Miwa Goto, Motohide Tamura, Toru Yamada, Amaya Moro-Martin, Tomoyuki Kudo, Ryo Kandori, Joshua E. Schlieder, Jun-Ichi Morino, Hiroshi Suto, Kyle Mede, John P. Wisniewski, Masahiko Hayashi, Jungmi Kwon, David S. Spiegel, Yutaka Hayano, Masanori Iye, Markus Feldt, Thayne Currie, Tetsuro Nishimura, Jun Hashimoto, Shu-ichiro Inutsuka, Shoken Miyama, Michael W. McElwain, Naruhisa Takato, Beth Biller, Eugene Serabyn, Wolfgang Brandner, Nobuhiko Kusakabe, Taras Golota, Thomas Henning, Joseph C. Carson, Saeko S. Hayashi, Miki Ishii, D. Tomono, Tae-Soo Pyo, Olivier Guyon, Carol A. Grady, Hideki Takami, Markus Janson, Taro Matsuo, Makoto Watanabe, Sebastian Egner, Ryuji Suzuki, Hiroshi Terada, Michihiro Takami, Klaus W. Hodapp, and Timothy D. Brandt
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Planetary system, Stellar classification, 01 natural sciences, Exoplanet, Radial velocity, Distribution function, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Pleiades, 010303 astronomy & astrophysics, Main sequence, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We conduct a statistical analysis of a combined sample of direct imaging data, totalling nearly 250 stars. The stars cover a wide range of ages and spectral types, and include five detections ($\kappa$ And b, two $\sim$60 M$_{\rm J}$ brown dwarf companions in the Pleiades, PZ Tel B, and CD$-$35 2722B). For some analyses we add a currently unpublished set of SEEDS observations, including the detections GJ 504b and GJ 758B. We conduct a uniform, Bayesian analysis of all stellar ages using both membership in a kinematic moving group and activity/rotation age indicators. We then present a new statistical method for computing the likelihood of a substellar distribution function. By performing most of the integrals analytically, we achieve an enormous speedup over brute-force Monte Carlo. We use this method to place upper limits on the maximum semimajor axis of the distribution function derived from radial-velocity planets, finding model-dependent values of $\sim$30--100 AU. Finally, we model the entire substellar sample, from massive brown dwarfs to a theoretically motivated cutoff at $\sim$5 M$_{\rm Jup}$, with a single power law distribution. We find that $p(M, a) \propto M^{-0.65\pm0.60} a^{-0.85\pm0.39}$ (1$\sigma$ errors) provides an adequate fit to our data, with 1.0--3.1\% (68\% confidence) of stars hosting 5--70 $M_{\rm Jup}$ companions between 10 and 100 AU. This suggests that many of the directly imaged exoplanets known, including most (if not all) of the low-mass companions in our sample, formed by fragmentation in a cloud or disk, and represent the low-mass tail of the brown dwarfs., Comment: ApJ in press, replaced with accepted version. Methodology clarified, conclusions mostly unchanged
Published: 2014

19. High-contrast Imaging with Spitzer: Deep Observations of Vega, Fomalhaut, and epsilon Eridani

Author: Christian Thalmann, Joseph C. Carson, Markus Janson, Sascha P. Quanz, Adam Amara, and David Lafrenière
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Debris disk, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Planetary system, Exoplanet, Stars, Spitzer Space Telescope, Fomalhaut, Space and Planetary Science, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Jupiter mass, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Stars with debris disks are intriguing targets for direct imaging exoplanet searches, both due to previous detections of wide planets in debris disk systems, as well as commonly existing morphological features in the disks themselves that may be indicative of a planetary influence. Here we present observations of three of the most nearby young stars, that are also known to host massive debris disks: Vega, Fomalhaut, and eps Eri. The Spitzer Space Telescope is used at a range of orientation angles for each star, in order to supply a deep contrast through angular differential imaging combined with high-contrast algorithms. The observations provide the opportunity to probe substantially colder bound planets (120--330 K) than is possible with any other technique or instrument. For Vega, some apparently very red candidate point sources detected in the 4.5 micron image remain to be tested for common proper motion. The images are sensitive to ~2 Mjup companions at 150 AU in this system. The observations presented here represent the first search for planets around Vega using Spitzer. The upper 4.5 micron flux limit on Fomalhaut b could be further constrained relative to previous data. In the case of eps Eri, planets below both the effective temperature and the mass of Jupiter could be probed from 80 AU and outwards, although no such planets were found. The data sensitively probe the regions around the edges of the debris rings in the systems where planets can be expected to reside. These observations validate previous results showing that more than an order of magnitude improvement in performance in the contrast-limited regime can be acquired with respect to conventional methods by applying sophisticated high-contrast techniques to space-based telescopes, thanks to the high degree of PSF stability provided in this environment., Comment: 11 pages, 12 figures, accepted for publication in A&A
Published: 2014
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20. SPOTS: The Search for Planets Orbiting Two Stars. I. Survey description and first observations

Author: Miwa Goto, Mariangela Bonavita, Hubert Klahr, Rainer Köhler, Christian Thalmann, C. Bergfors, Christoph Mordasini, Wolfgang Brandner, Francesco Marzari, Markus Feldt, Anthony Boccaletti, Markus Janson, Silvano Desidera, Joseph C. Carson, Tomonori Usuda, and Thomas Henning
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Proper motion, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrometry, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Exoplanet, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Circumbinary planet, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: Direct imaging surveys for exoplanets commonly exclude binary stars from their target lists, leaving a large part of the overall planet demography unexplored. To address this gap in our understanding of planet formation and evolution, we have launched the first direct imaging survey dedicated to circumbinary planets: SPOTS, the Search for Planets Orbiting Two Stars. In this paper, we discuss the theoretical context, scientific merit, and technical feasibility of such observations, describe the target sample and observational strategy of our survey, and report on the first results from our pilot survey of 26 targets with the VLT NaCo facility. While we have not found any confirmed substellar companions to date, a number of promising candidate companions remain to be tested for common proper motion in upcoming follow-up observations. We also report on the astrometry of the three resolved binaries in our target sample. This pilot survey constitutes a successful proof of concept for our survey strategy and paves the way for a second stage of exploratory observations with VLT SPHERE., Comment: 12 pages, 4 figures, 3 tables. Accepted for publication in A&A
Published: 2014
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21. Indications of M-dwarf Deficits in the Halo and Thick Disk of the Galaxy

Author: Nobuhiko Kusakabe, Amaya Moro-Martin, Takuya Suenaga, Motohide Tamura, Jungmi Kwon, Tetsuo Nishimura, Jun-Ichi Morino, Jun Hashimoto, Christian Thalmann, Masahiko Hayashi, Takahiro Sumi, Thomas Henning, Tomoyuki Kudo, Tae-Soo Pyo, Masaru Kajisawa, Yutaka Hayano, Thayne Currie, Jun Sudo, Tomonori Usuda, Olivier Guyon, Hiroshi Shibai, Hideki Takami, Klaus W. Hodapp, Naruhisa Takato, Masayuki Kuzuhara, Lyu Abe, Wolfgang Brandner, Ryo Kandori, Miki Ishii, Nobuo Arimoto, Gillian R. Knapp, Timothy D. Brandt, Edwin L. Turner, Eugene Serabyn, Shoken M. Miyama, Carol A. Grady, Markus Janson, Michael W. McElwain, John P. Wisniewski, Sebastian Egner, Yasuhiro H. Takahashi, Yoichi Itoh, Saeko S. Hayashi, Makoto Watanabe, Masanori Iye, M. Samland, Joseph C. Carson, Markus Feldt, Miwa Goto, Daigo Tomono, Hiroshi Suto, Kodai Yamamoto, Ryuji Suzuki, Toru Yamada, Misato Fukagawa, Hiroshi Terada, Mihoko Konishi, and Taro Matsuo
Subjects: Physics, education.field_of_study, Population, FOS: Physical sciences, Astronomy and Astrophysics, Scale height, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Galaxy, Exoplanet, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Thick disk, Astrophysics::Solar and Stellar Astrophysics, Halo, Astrophysics::Earth and Planetary Astrophysics, education, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We compared the number of faint stars detected in deep survey fields with the current stellar distribution model of the Galaxy and found that the detected number in the H band is significantly smaller than the predicted number. This indicates that M-dwarfs, the major component, are fewer in the halo and the thick disk. We used archived data of several surveys in both the north and south field of GOODS (Great Observatories Origins Deep Survey), MODS in GOODS-N, and ERS and CANDELS in GOODS-S. The number density of M-dwarfs in the halo has to be 20+/-13% relative to that in the solar vicinity, in order for the detected number of stars fainter than 20.5 mag in the H band to match with the predicted value from the model. In the thick disk, the number density of M-dwarfs must be reduced (52+/-13%) or the scale height must be decreased (~600 pc). Alternatively, overall fractions of the halo and thick disks can be significantly reduced to achieve the same effect, because our sample mainly consists of faint M-dwarfs. Our results imply that the M-dwarf population in regions distant from the Galactic plane is significantly smaller than previously thought. We then discussed the implications this has on the suitability of the model predictions for the prediction of non-companion faint stars in direct imaging extrasolar planet surveys by using the best-fit number densities., Comment: 22 pages, 9 figures, accepted for Publications of the Astronomical Society of Japan
Published: 2014
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22. Surface Geometry of Protoplanetary Disks Inferred From Near-Infrared Imaging Polarimetry

Author: Makoto Watanabe, Tomoyuki Kudo, Masayuki Kuzuhara, Yutaka Hayano, Markus Feldt, Daigo Tomono, Ruobing Dong, John P. Wisniewski, Timothy D. Brandt, Mitsuhiko Honda, Michael W. McElwain, Jungmi Kwon, Ryuji Suzuki, Tomonori Usuda, Jun-Ichi Morino, Thomas Henning, Michael L. Sitko, Satoshi Mayama, Pin-Gao Gu, Sebastian Egner, Thayne Currie, Katherine B. Follette, Edwige Chapillon, Tetsuo Nishimura, Youchi Itoh, Eugene Serabyn, Gillian R. Knapp, Jennifer L. Karr, Markus Janson, Taro Matsuo, Joseph C. Carson, Ryo Kandori, Hideki Takami, Christian Thalmann, Klaus W. Hodapp, Miki Ishii, Eiji Akiyama, Naruhisa Takato, Masanori Iye, Saeko S. Hayashi, Carol A. Grady, Tae-Soo Pyo, Olivier Guyon, Wolfgang Brandner, N. Kusakabe, Ya-Wen Tang, Hiroshi Suto, Takayuki Muto, Edwin L. Turner, Motohide Tamura, Toru Yamada, Lyu Abe, Masahiko Hayashi, Yasuhiro Hasegawa, Shoken Miyama, Michihiro Takami, Yasuhiro H. Takahashi, Hiroshi Terada, Amaya Moro-Martin, Takuya Suenaga, and Jun Hashimoto
Subjects: Physics, Spiral galaxy, 010308 nuclear & particles physics, Scattering, Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Polarization (waves), Position angle, 01 natural sciences, Electromagnetic radiation, Computational physics, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Protoplanet, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present a new method of analysis for determining the surface geometry of five protoplanetary disks observed with near-infrared imaging polarimetry using Subaru-HiCIAO. Using as inputs the observed distribution of polarized intensity (PI), disk inclination, assumed properties for dust scattering, and other reasonable approximations, we calculate a differential equation to derive the surface geometry. This equation is numerically integrated along the distance from the star at a given position angle. We show that, using these approximations, the local maxima in the PI distribution of spiral arms (SAO 206462, MWC 758) and rings (2MASS J16042165-2130284, PDS 70) are associated with local concave-up structures on the disk surface. We also show that the observed presence of an inner gap in scattered light still allows the possibility of a disk surface that is parallel to the light path from the star, or a disk that is shadowed by structures in the inner radii. Our analysis for rings does not show the presence of a vertical inner wall as often assumed in studies of disks with an inner gap. Finally, we summarize the implications of spiral and ring structures as potential signatures of ongoing planet formation., Comment: 35 pages, 13 figures, 7 tables, accepted by ApJ
Published: 2014
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23. High-Contrast Near-Infrared Imaging Polarimetry of the Protoplanetary Disk around RY Tau

Author: John Wisnewski, Nobuhiko Kusakabe, Timothy D. Brandt, Hiroshi Terada, Jun-Ichi Morino, Jun Hashimoto, Thomas Henning, Katherine B. Follette, Toru Yamada, Gillian R. Knapp, Sebastian Egner, Jungmi Kwon, Taro Matsuo, Amaya Moro-Martin, Yutaka Hayano, Miki Ishii, Michihiro Takami, Markus Janson, Ryuji Suzuki, Tetsuo Nishimura, Munetake Momose, Eugene Serabyn, Wolfgang Brandner, Makoto Watanabe, Motohide Tamura, Mei-Yin Chou, Carol A. Grady, Tomoyuki Kudo, Daigo Tomono, Lyu Abe, Tae-Soo Pyo, Olivier Guyon, Shoken M. Miyama, Tomonori Usuda, Hyosun Kim, Ryo Kandori, Masahiko Hayashi, Masayuki Kuzuhara, Klaus W. Hodapp, Jennifer L. Karr, Masanori Iye, Joseph C. Carson, Saeko S. Hayashi, Hideki Takami, Hiroshi Suto, Michael W. McElwain, Edwin L. Turner, Markus Feldt, Yoichi Itoh, Christian Thalmann, Satoshi Mayama, Thayne Currie, Naruhisa Takato, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, 010308 nuclear & particles physics, Infrared, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Viewing angle, Protoplanetary disk, 01 natural sciences, Wavelength, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Thermal radiation, 0103 physical sciences, Thick disk, Radiative transfer, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present near-infrared coronagraphic imaging polarimetry of RY Tau. The scattered light in the circumstellar environment was imaged at H-band at a high resolution (~0".05) for the first time, using Subaru-HiCIAO. The observed polarized intensity (PI) distribution shows a butterfly-like distribution of bright emission with an angular scale similar to the disk observed at millimeter wavelengths. This distribution is offset toward the blueshifted jet, indicating the presence of a geometrically thick disk or a remnant envelope, and therefore the earliest stage of the Class II evolutionary phase. We perform comparisons between the observed PI distribution and disk models with: (1) full radiative transfer code, using the spectral energy distribution (SED) to constrain the disk parameters; and (2) monochromatic simulations of scattered light which explore a wide range of parameters space to constrain the disk and dust parameters. We show that these models cannot consistently explain the observed PI distribution, SED, and the viewing angle inferred by millimeter interferometry. We suggest that the scattered light in the near-infrared is associated with an optically thin and geometrically thick layer above the disk surface, with the surface responsible for the infrared SED. Half of the scattered light and thermal radiation in this layer illuminates the disk surface, and this process may significantly affect the thermal structure of the disk., Comment: 35 pages, 14 figures, 7 tables, accepted for publication in Astrophysical Journal
Published: 2013
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24. Direct Imaging of a Cold Jovian Exoplanet in Orbit around the Sun-like Star GJ 504

Author: Thomas Henning, Joseph C. Carson, Miki Ishii, D. Tomono, Masahiko Hayashi, Tae-Soo Pyo, Hiroshi Suto, Jungmi Kwon, Olivier Guyon, Yutaka Hayano, Miwa Goto, Michael W. McElwain, Yasuhiro H. Takahashi, Edwin L. Turner, Taro Matsuo, Motohide Tamura, Beth Biller, Eugene Serabyn, Naruhisa Takato, Masanori Iye, David S. Spiegel, Philip W. Lucas, Lyu Abe, Toru Yamada, Tetsuro Nishimura, Hideki Takami, Nobuhiko Kusakabe, Hiroshi Terada, Masayuki Kuzuhara, Satoshi Mayama, Michihiro Takami, Markus Feldt, Tomoyuki Kudo, Klaus W. Hodapp, Jun Hashimoto, Adam Burrows, Carol A. Grady, Shoken Miyama, Takayuki Kotani, H. Fujiwara, Christian Thalmann, Timothy D. Brandt, Ryo Kandori, Wolfgang Brandner, Tomonori Usuda, Jun-Ichi Morino, Saeko S. Hayashi, Gillian R. Knapp, Amaya Moro-Martin, Jun Nishikawa, Markus Janson, Yasunori Hori, John P. Wisniewski, Takuya Suenaga, Sebastian Egner, Ryuji Suzuki, Makoto Watanabe, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, 01 natural sciences, Jovian, Jupiter, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Exoplanet, Accretion (astrophysics), Orbit, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: Several exoplanets have recently been imaged at wide separations of >10 AU from their parent stars. These span a limited range of ages ( 0.5 mag), implying thick cloud covers. Furthermore, substantial model uncertainties exist at these young ages due to the unknown initial conditions at formation, which can lead to an order of magnitude of uncertainty in the modeled planet mass. Here, we report the direct imaging discovery of a Jovian exoplanet around the Sun-like star GJ 504, detected as part of the SEEDS survey. The system is older than all other known directly-imaged planets; as a result, its estimated mass remains in the planetary regime independent of uncertainties related to choices of initial conditions in the exoplanet modeling. Using the most common exoplanet cooling model, and given the system age of 160 [+350, -60] Myr, GJ 504 b has an estimated mass of 4 [+4.5, -1.0] Jupiter masses, among the lowest of directly imaged planets. Its projected separation of 43.5 AU exceeds the typical outer boundary of ~30 AU predicted for the core accretion mechanism. GJ 504 b is also significantly cooler (510 [+30, -20] K) and has a bluer color (J-H = -0.23 mag) than previously imaged exoplanets, suggesting a largely cloud-free atmosphere accessible to spectroscopic characterization. Thus, it has the potential of providing novel insights into the origins of giant planets, as well as their atmospheric properties., 20 pages, 12 figures, Accepted for publication in ApJ. Minor updates from the version 1
Published: 2013
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25. Mapping H-band Scattered Light Emission in the Mysterious SR21 Transitional Disk

Author: Masayuki Kuzuhara, Tae-Soo Pyo, Masanori Iye, Michael W. McElwain, Katherine B. Follette, Jungmi Kwon, Olivier Guyon, Gillian R. Knapp, Ryuji Suzuki, Laird M. Close, Sean M. Andrews, Jun Hashimoto, Masahiko Hayashi, Amaya Moro-Martin, Thayne Currie, Carol A. Grady, Tomoyuki Kudo, Miwa Goto, Jun-Ichi Morino, Markus Feldt, Tetsuo Nishimura, Edwin L. Turner, Saeko S. Hayashi, Joseph C. Carson, Michihiro Takami, Naruhisa Takato, Lyu Abe, Hideki Takami, Motohide Tamura, Eugene Serabyn, Miki Ishii, Toru Yamada, Satoshi Mayama, Hiroshi Terada, Shoken Miyama, Taro Matsuo, Yutaka Hayano, Tomonori Usuda, Hiroshi Suto, Barbara A. Whitney, John P. Wisniewski, Wolfgang Brandner, Ryo Kandori, Klaus W. Hodapp, Timothy D. Brandt, Markus Janson, Nobuhiko Kusakabe, Makoto Watanabe, Ruobing Dong, Daigo Tomono, Thomas Henning, Sebastian Egner, Christian Thalmann, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Scattering, Near-infrared spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, H band, Astrophysics, Submillimeter Array, Thin disk, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Computer Science::Computer Vision and Pattern Recognition, Radiative transfer, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, Cavity wall, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present the first near infrared (NIR) spatially resolved images of the circumstellar transitional disk around SR21. These images were obtained with the Subaru HiCIAO camera, adaptive optics, and the polarized differential imaging technique. We resolve the disk in scattered light at H-band for stellocentric 0.''1 ≤ r ≤ 0.''6 (12 lsim r lsim 75 AU). We compare our results with previously published spatially resolved 880 μm continuum Submillimeter Array images that show an inner r lsim 36 AU cavity in SR21. Radiative transfer models reveal that the large disk depletion factor invoked to explain SR21's sub-mm cavity cannot be "universal" for all grain sizes. Even significantly more moderate depletions (δ = 0.1, 0.01 relative to an undepleted disk) than those that reproduce the sub-mm cavity (δ ~ 10-6) are inconsistent with our H-band images when they are assumed to carry over to small grains, suggesting that surface grains scattering in the NIR either survive or are generated by whatever mechanism is clearing the disk midplane. In fact, the radial polarized intensity profile of our H-band observations is smooth and steeply inwardly-increasing (r -3), with no evidence of a break at the 36 AU sub-mm cavity wall. We hypothesize that this profile is dominated by an optically thin disk envelope or atmosphere component. We also discuss the compatibility of our data with the previously postulated existence of a sub-stellar companion to SR21 at r ~ 10-20 AU, and find that we can neither exclude nor verify this scenario. This study demonstrates the power of multiwavelength imaging of transitional disks to inform modeling efforts, including the debate over precisely what physical mechanism is responsible for clearing these disks of their large midplane grains.
Published: 2013

26. Spiral Arms in the Asymmetrically Illuminated Disk of MWC 758 and Constraints on Giant Planets

Author: Carol A. Grady, Tetsuro Nishimura, Edwin L. Turner, Lyu Abe, Motohide Tamura, Jeremy Hornbeck, Toru Yamada, Th. Henning, Sebastian Egner, Ruobing Dong, Jordy Bouwman, Nobuhiko Kusakabe, Klaus W. Hodapp, Satoshi Mayama, M. Bonnefoy, Jungmi Kwon, Michael L. Sitko, M. Hayashi, J.-U. Pott, G. Serabyn, Wolfgang Brandner, John P. Wisniewski, Sylvestre Lacour, Michihiro Takami, Saeko S. Hayashi, Timothy D. Brandt, Takayuki Muto, Hannah Jang-Condell, Masanori Iye, Markus Janson, Masayuki Kuzuhara, Miwa Goto, A. Crida, David J. Wilner, Tomoyuki Kudo, Jun-Ichi Morino, Jun Hashimoto, Katherine B. Follette, Joseph C. Carson, G. R. Knapp, Christian Thalmann, Miki Ishii, Ryo Kandori, Amaya Moro-Martin, Tomonori Usuda, Michael W. McElwain, Sean M. Andrews, Yutaka Hayano, Glenn Schneider, S. Sai, T. Currie, Adam L. Kraus, Makoto Watanabe, Hiroshi Suto, Gael Chauvin, Naruhisa Takato, Beth Biller, Thomas P. Robitaille, Dean C. Hines, Taro Matsuo, Daigo Tomono, Tae-Soo Pyo, Ray W. Russell, Olivier Guyon, Markus Feldt, Attila Juhasz, Scott Dahm, Ryuji Suzuki, A. Mueller, Hideki Takami, Hiroshi Terada, Misato Fukagawa, Shoken Miyama, Eiji Akiyama, 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), 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), Low Energy Astrophysics (API, FNWI), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Density wave theory, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [PHYS]Physics [physics], Spiral galaxy, Astronomy and Astrophysics, Planetary system, Exoplanet, Accretion (astrophysics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the first near-IR scattered light detection of the transitional disk associated with the Herbig Ae star MWC 758 using data obtained as part of the Strategic Exploration of Exoplanets and Disks with Subaru, and 1.1 micron HST/NICMOS data. While sub-millimeter studies suggested there is a dust-depleted cavity with r=0.35, we find scattered light as close as 0.1 (20-28 AU) from the star, with no visible cavity at H, K', or Ks. We find two small-scaled spiral structures which asymmetrically shadow the outer disk. We model one of the spirals using spiral density wave theory, and derive a disk aspect ratio of h ~ 0.18, indicating a dynamically warm disk. If the spiral pattern is excited by a perturber, we estimate its mass to be 5+3,-4 Mj, in the range where planet filtration models predict accretion continuing onto the star. Using a combination of non-redundant aperture masking data at L' and angular differential imaging with Locally Optimized Combination of Images at K' and Ks, we exclude stellar or massive brown dwarf companions within 300 mas of the Herbig Ae star, and all but planetary mass companions exterior to 0.5. We reach 5-sigma contrasts limiting companions to planetary masses, 3-4 MJ at 1.0 and 2 MJ at 1.55 using the COND models. Collectively, these data strengthen the case for MWC 758 already being a young planetary system., 45 pages, 9 figures; ApJ in press
Published: 2013

27. Sub-0.1′′ optical imaging of the Z CMa jets with SPHERE/ZIMPOL

Author: Andreas Bazzon, E. Lagadec, Massimo Turatto, Catherine Dougados, E. Sissa, Francesca Bacciotti, Simone Antoniucci, Christian Thalmann, T. Giannini, Linda Podio, H. M. Schmid, Mickael Bonnefoy, Gael Chauvin, Raffaele Gratton, A. La Camera, Brunella Nisini, Maud Langlois, Silvano Desidera, ITA, FRA, CHE, 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 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), 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: Be star, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Binary number, stars: pre-main sequence, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, circumstellar matter, 01 natural sciences, outflows, Collimated light, stars: individual: Z CMa, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, stars: variables: T Tauri, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Herbig Ae/Be, techniques: high angular resolution, Astronomy and Astrophysics, Accretion (astrophysics), 3. Good health, Stars, T Tauri star, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, stars: winds, Orbital motion, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Deconvolution
Abstract: Crucial information on the mass accretion-ejection in young stars can be obtained from high spatial resolution images of jets in sources with recurrent accretion outbursts. Using the SPHERE/ZIMPOL instrument, we observed the young binary Z CMa that is composed of a Herbig Be star and a FUor object, both driving a jet. We analyse the structure of the two jets in relation with previous accretion events observed in this target. We obtained optical images in the Halpha and OI 6300A lines at the unprecedented angular resolution of ~0.03 arcsec, on which we have performed both continuum subtraction and deconvolution, thereby deriving results that are consistent with each other. Our images reveal extended emission from both sources: a fairly compact and poorly collimated emission SW of the Herbig component and an extended collimated and precessing jet from the FUor component. The compact emission from the Herbig star is compatible with a wide-angle wind and is possibly connected to the recent outburst events shown by this component. The FUor jet is traced down to 70 mas (80 AU) from the source and is highly collimated with a width of 26-48 AU at distances 100-200 AU, which is similar to the width of jets from T Tauri stars. This strongly suggests that the same magneto-centrifugal jet-launching mechanism also operates in FUors. The observed jet wiggle can be modelled as originating from an orbital motion with a period of 4.2 yr around an unseen companion with mass between 0.48 and 1 Msun. The jet mass loss rate Mloss was derived from the OI luminosity and is in the range 1E-8 and 1E-6 Msun/yr. This is the first direct Mloss measurement from a jet in a FUor. If we assume previous Macc estimates obtained through modelling of the accretion disk, the derived range of Mloss would imply a very low mass-ejection efficiency (Mloss/Macc < 0.02), which is lower than that typical of T Tauri stars., Letter to Astronomy and Astrophysics
Published: 2016

28. CONSTRAINING THE MOVEMENT OF THE SPIRAL FEATURES AND THE LOCATIONS OF PLANETARY BODIES WITHIN THE AB AUR SYSTEM

Author: Eugene Serabyn, Yoshiko K. Okamoto, Naruhisa Takato, Lyu Abe, Wolfgang Brandner, Shoken Miyama, Markus Janson, Thomas Henning, Masahiko Hayashi, Carol A. Grady, Michihiro Takami, Yutaka Hayano, Jun-Ichi Morino, Toru Yamada, Jamie R. Lomax, Joseph C. Carson, Masanori Iye, Saeko S. Hayashi, Munetake Momose, Miwa Goto, Tae-Soo Pyo, Taro Matsuo, John P. Wisniewski, Olivier Guyon, Thayne Currie, Takuya Suenaga, Tomonori Usuda, Ryuji Suzuki, Jungmi Kwon, Hideki Takami, Hiroshi Suto, Edwin L. Turner, Tetsuo Nishimura, Glenn Schneider, Miki Ishii, Akio Inoue, Masayuki Kuzuhara, Gillian R. Knapp, Motohide Tamura, Misato Fukagawa, Tomoyuki Kudo, Jun Hashimoto, Ryo Kandori, Satoshi Mayama, Klaus W. Hodapp, Markus Feldt, Michael W. McElwain, Yasuhiro H. Takahashi, Hiroshi Terada, Timothy D. Brandt, Nobuhiko Kusakabe, Sebastian Egner, Michael L. Sitko, Christian Thalmann, Makoto Watanabe, Daigo Tomono, and Amaya Moro-Martin
Subjects: 010504 meteorology & atmospheric sciences, Monte Carlo method, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Rotation, 01 natural sciences, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Spiral, 0105 earth and related environmental sciences, Envelope (waves), Earth and Planetary Astrophysics (astro-ph.EP), Physics, Movement (music), Astronomy and Astrophysics, Intensity (physics), Orbit, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We used a Monte Carlo, radiative transfer code to simultaneously model the system's SED and H-band polarized intensity imagery. We find that a disk-dominated model, as opposed to one that is envelope dominated, can plausibly reproduce AB Aur's SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aur's spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and polarized intensity imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8 year baseline. If such structures are caused by disk-planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be >47 AU., 8 pages, 3 figures, 1 table, Accepted to ApJ
Published: 2016

29. Extreme asymmetry in the polarized disk of V1247 Orionis

Author: Olivier Guyon, Hiroshi Shibai, Miwa Goto, Jungmi Kwon, Makoto Watanabe, Hiroshi Suto, Takayuki Kotani, Michihiro Takami, Taro Matsuo, Nobuhiko Kusakabe, Joseph C. Carson, Stefan Kraus, Markus Feldt, Wolfgang Brandner, Satoshi Mayama, Yutaka Hayano, Michael L. Sitko, Thayne Currie, Takuya Suenaga, Masanori Iye, Daigo Tomono, Ryo Kandori, Jun Hashimoto, Eugene Serabyn, Michael W. McElwain, Saeko S. Hayashi, Masayuki Kuzuhara, Munetake Momose, Amaya Moro-Martin, Katherine B. Follette, Thomas Henning, Gillian R. Knapp, Tomoyuki Kudo, Takahiro Sumi, Christian Thalmann, Edwin L. Turner, Jun-Ichi Morino, Klaus W. Hodapp, John P. Wisniewski, Motohide Tamura, Tomonori Usuda, Sebastian Egner, Jeremy R. Swearingen, Timothy D. Brandt, Shoken Miyama, Markus Janson, Masahiko Hayashi, Miki Ishii, Hideki Takami, Carol A. Grady, Takayuki Muto, Misato Fukagawa, Ryuji Suzuki, Y. Ohta, Yoshiko K. Okamoto, Naruhisa Takato, Lyu Abe, Yasuhiro H. Takahashi, Hiroshi Terada, Eiji Akiyama, Tetsuo Nishimura, Toru Yamada, and Tae-Soo Pyo
Subjects: Physics, Brightness, Spiral galaxy, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, Astrophysics, Planetary system, 01 natural sciences, Asymmetry, Azimuth, Arc (geometry), Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Pitch angle, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common
Abstract: We present the first near-infrared scattered-light detection of the transitional disk around V1247 Ori, which was obtained using high-resolution polarimetric differential imaging observations with Subaru/HiCIAO. Our imaging in the H band reveals the disk morphology at separations of approx.0.14-0.86 (54-330 au) from the central star. The polarized intensity image shows a remarkable arc-like structure toward the southeast of the star, whereas the fainter northwest region does not exhibit any notable features. The shape of the arm is consistent with an arc of 0.28 +/- 0.09 in radius (108 au from the star), although the possibility of a spiral arm with a small pitch angle cannot be excluded. V1247 Ori features an exceptionally large azimuthal contrast in scattered, polarized light; the radial peak of the southeastern arc is about three times brighter than the northwestern disk measured at the same distance from the star. Combined with the previous indication of an inhomogeneous density distribution in the gap at 46 au, the notable asymmetry in the outer disk suggests the presence of unseen companions and/or planet-forming processes ongoing in the arc.
Published: 2016

30. 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

31. Polarimetric imaging of large cavity structures in the pre-transitional protoplanetary disk around PDS 70: observations of the disk

Author: Michael W. McElwain, Tomonori Usuda, Mitsuhiko Honda, Zhaohuan Zhu, Melissa McClure, Carol A. Grady, Markus Janson, Lyu Abe, Miki Ishii, Yutaka Hayano, Masao Hayashi, Ryuji Suzuki, Takuya Suenaga, Naruhisa Takato, John P. Wisniewski, Edwin L. Turner, Jungmi Kwon, Christian Thalmann, Klaus W. Hodapp, Yasuhiro H. Takahashi, Taro Matsuo, Michihiro Takami, Tomoyuki Kudo, Gene Serabyn, Timothy D. Brandt, Misato Fukagawa, Shoken Miyama, Masanori Iye, Masayuki Kuzuhara, Hiroshi Terada, Tetsuro Nishimura, Saeko S. Hayashi, Satoshi Mayama, Joseph C. Carson, Ryo Kandori, Makoto Watanabe, Miwa Goto, Markus Feldt, Hideki Takami, Tae-Soo Pyo, Olivier Guyon, Hiroshi Suto, Motohide Tamura, Toru Yamada, G. R. Knapp, Nobuhiko Kusakabe, Jun-Ichi Morino, Jun Hashimoto, Daigo Tomono, Takayuki Muto, Thomas Henning, Sebastian Egner, Amaya Moro-Martin, Wolfgang Brandner, Ruobing Dong, and Low Energy Astrophysics (API, FNWI)
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, Astrophysics, Radius, Protoplanetary disk, 01 natural sciences, T Tauri star, Full width at half maximum, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present high resolution H-band polarized intensity (PI; FWHM = 0."1: 14 AU) and L'-band imaging data (FWHM = 0."11: 15 AU) of the circumstellar disk around the weak-lined T Tauri star PDS 70 in Centaurus at a radial distance of 28 AU (0."2) up to 210 AU (1."5). In both images, a giant inner gap is clearly resolved for the first time, and the radius of the gap is ~70 AU. Our data show that the geometric center of the disk shifts by ~6 AU toward the minor axis. We confirm that the brown dwarf companion candidate to the north of PDS 70 is a background star based on its proper motion. As a result of SED fitting by Monte Carlo radiative transfer modeling, we infer the existence of an optically thick inner disk at a few AU. Combining our observations and modeling, we classify the disk of PDS 70 as a pre-transitional disk. Furthermore, based on the analysis of L'-band imaging data, we put an upper limit mass of companions at ~30 to ~50MJ within the gap. Taking account of the presence of the large and sharp gap, we suggest that the gap could be formed by dynamical interactions of sub-stellar companions or multiple unseen giant planets in the gap., accepted by APJL
Published: 2012

32. A Common Proper Motion Stellar Companion to HAT-P-7

Author: Christian Thalmann, Michihiro Takami, Ryuji Suzuki, Tae-Soo Pyo, Klaus W. Hodapp, Olivier Guyon, Masanori Iye, Saeko S. Hayashi, Carol A. Grady, Markus Feldt, Miwa Goto, Joseph C. Carson, Thomas Henning, Shoken M. Miyama, Yutaka Hayano, Bun'ei Sato, John P. Wisniewski, Nobuhiko Kusakabe, Lyu Abe, Tetsuo Nishimura, Daigo Tomono, Hiroshi Suto, Ryo Kandori, Toru Yamada, Jun-Ichi Morino, Jun Hashimoto, Markus Janson, Makiko Nagasawa, Sebastian Egner, Tomonori Usuda, Teruyuki Hirano, Takuya Suenaga, Yasuhiro H. Takahashi, Masahiko Hayashi, Hiroshi Terada, Motohide Tamara, Miki Ishii, Tomoyuki Kudo, Jungmi Kwon, Timothy D. Brandt, Norio Narita, Michael W. McElwain, Naruhisa Takato, Edwin L. Turner, Satoshi Mayama, Gillian R. Knapp, Makoto Watanab, Hideki Takami, Masayuki Kuzuhara, Taro Matsuo, Amaya Moro-Martin, Eugene Serabyn, Wolfgang Brandner, and Shigeru Ida
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Proper motion, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Outlier, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 10. No inequality, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report that HAT-P-7 has a common proper motion stellar companion. The companion is located at $\sim3.9$ arcsec to the east and estimated as an M5.5V dwarf based on its colors. We also confirm the presence of the third companion, which was first reported by Winn et al. (2009), based on long-term radial velocity measurements. We revisit the migration mechanism of HAT-P-7b given the presence of those companions, and propose sequential Kozai migration as a likely scenario in this system. This scenario may explain the reason for an outlier in the discussion of the spin-orbit alignment timescale for HAT-P-7b by Albrecht et al. (2012)., 5 pages, 4 figures, 2 tables, PASJ Letters in press
Published: 2012

33. Subaru Imaging of Asymmetric Features in a Transitional Disk in Upper Scorpius

Author: G. R. Knapp, Michael W. McElwain, Ruobing Dong, Eugene Serabyn, Ryuji Suzuki, Timothy D. Brandt, Christian Thalmann, Makoto Watanabe, Takayuki Muto, Daigo Tomono, Katherine B. Follette, Hiroshi Terada, Amaya Moro-Martin, Tomonori Usuda, Thomas Henning, Miki Ishii, Sebastian Egner, Nobuhiko Kusakabe, Hideki Takami, Carol A. Grady, Jungmi Kwon, Markus Janson, Wolfgang Brandner, John P. Wisniewski, Tetsuro Nishimura, Saeko S. Hayashi, Masahiko Hayashi, Miwa Goto, Takashi Tsukagoshi, Lyu Abe, Jun-Ichi Morino, Misato Fukagawa, Masayuki Kuzuhara, Shoken Miyama, Klaus W. Hodapp, Jun Hashimoto, Eiji Akiyama, Motohide Tamura, Toru Yamada, Naruhisa Takato, Tomoyuki Kudo, Edwin L. Turner, Ryo Kandori, Markus Feldt, Satoshi Mayama, Yasuhiro H. Takahashi, Taro Matsuo, Michihiro Takami, Masanori Iye, Joseph C. Carson, Hiroshi Suto, Yutaka Hayano, Munetake Momose, Tae-Soo Pyo, Olivier Guyon, and Low Energy Astrophysics (API, FNWI)
Subjects: 010504 meteorology & atmospheric sciences, Infrared, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Edge (geometry), 01 natural sciences, Submillimeter Array, law.invention, Telescope, Physics - Space Physics, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Position angle, Polarization (waves), Space Physics (physics.space-ph), Wavelength, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Scattered light, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report high-resolution (0.07 arcsec) near-infrared polarized intensity images of the circumstellar disk around the star 2MASS J16042165-2130284 obtained with HiCIAO mounted on the Subaru 8.2 m telescope. We present our $H$-band data, which clearly exhibits a resolved, face-on disk with a large inner hole for the first time at infrared wavelengths. We detect the centrosymmetric polarization pattern in the circumstellar material as has been observed in other disks. Elliptical fitting gives the semimajor axis, semiminor axis, and position angle (P.A.) of the disk as 63 AU, 62 AU, and -14 $^{\circ}$, respectively. The disk is asymmetric, with one dip located at P.A.s of $\sim85^{\circ}$. Our observed disk size agrees well with a previous study of dust and CO emission at submillimeter wavelength with Submillimeter Array. Hence, the near-infrared light is interpreted as scattered light reflected from the inner edge of the disk. Our observations also detect an elongated arc (50 AU) extending over the disk inner hole. It emanates at the inner edge of the western side of the disk, extending inward first, then curving to the northeast. We discuss the possibility that the inner hole, the dip, and the arc that we have observed may be related to the existence of unseen bodies within the disk., Comment: 21 pages, 3 figures, published 2012 November 7 by ApJL, typo corrected
Published: 2012
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34. The missing cavities in the SEEDS polarized scattered light images of transitional protoplanetary disks: A generic disk model

Author: Carol A. Grady, Tetsuro Nishimura, Masanori Iye, Joseph C. Carson, Tomonori Usuda, Masahiko Hayashi, Michihiro Takami, Takayuki Muto, Edwin L. Turner, Wolfgang Brandner, Barbara A. Whitney, Hiroshi Suto, Ryoko Tanii, Klaus W. Hodapp, Taro Matsuo, Ryuji Suzuki, Thomas Henning, Amaya Moro-Martin, Shoken Miyama, Sebastian Egner, Zhaohuan Zhu, Yutaka Hayano, Roman R. Rafikov, Miki Ishii, Makoto Watanabe, Markus Janson, Lyu Abe, G. R. Knapp, Naruhisa Takato, Daigo Tomono, Motohide Tamura, Toru Yamada, Hiroshi Terada, Masayuki Kuzuhara, Mitsuhiko Honda, Katherine B. Follette, Nobuhiko Kusakabe, Ruobing Dong, Lee Hartmann, Satoshi Mayama, Jun-Ichi Morino, Jun Hashimoto, Shu-ichiro Inutsuka, Tomoyuki Kudo, Ryo Kandori, Markus Feldt, Saeko S. Hayashi, Miwa Goto, Michael W. McElwain, Christian Thalmann, Tae-Soo Pyo, Yoichi Itoh, Olivier Guyon, Hideki Takami, John P. Wisniewski, Timothy D. Brandt, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Infrared, Young stellar object, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spatial distribution, 01 natural sciences, Submillimeter Array, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Scattered light, Subaru Telescope, 010303 astronomy & astrophysics, Spectrograph, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Transitional circumstellar disks around young stellar objects have a distinctive infrared deficit around 10 microns in their Spectral Energy Distributions (SED), recently measured by the Spitzer Infrared Spectrograph (IRS), suggesting dust depletion in the inner regions. These disks have been confirmed to have giant central cavities by imaging of the submillimeter (sub-mm) continuum emission using the Submillimeter Array (SMA). However, the polarized near-infrared scattered light images for most objects in a systematic IRS/SMA cross sample, obtained by HiCIAO on the Subaru telescope, show no evidence for the cavity, in clear contrast with SMA and Spitzer observations. Radiative transfer modeling indicates that many of these scattered light images are consistent with a smooth spatial distribution for micron-sized grains, with little discontinuity in the surface density of the micron-sized grains at the cavity edge. Here we present a generic disk model that can simultaneously account for the general features in IRS, SMA, and Subaru observations. Particularly, the scattered light images for this model are computed, which agree with the general trend seen in Subaru data. Decoupling between the spatial distributions of the micron-sized dust and mm-sized dust inside the cavity is suggested by the model, which, if confirmed, necessitates a mechanism, such as dust filtration, for differentiating the small and big dust in the cavity clearing process. Our model also suggests an inwardly increasing gas-to-dust-ratio in the inner disk, and different spatial distributions for the small dust inside and outside the cavity, echoing the predictions in grain coagulation and growth models., 41 pages (single column), 1 table, 10 figures, ApJ accepted
Published: 2012

35. A 5 Micron Image of beta Pictoris b at a Sub-Jupiter Projected Separation: Evidence for a Misalignment Between the Planet and the Inner, Warped Disk

Author: Adam Burrows, Marc J. Kuchner, Soko Matsumura, Nikku Madhusudhan, Christian Thalmann, Thayne Currie, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Debris disk, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Omega, Exoplanet, Jupiter, Orbit, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, Beta Pictoris, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Orbital analysis, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present and analyze a new M' detection of the young exoplanet beta Pictoris b from 2008 VLT/NaCo data at a separation of ~ 4 AU and a high signal-to-noise rereduction of L' data taken in December 2009. Based on our orbital analysis, the planet's orbit is viewed almost perfectly edge-on (i ~ 89 degrees) and has a Saturn-like semimajor axis of 9.50 (+3.93, -1.7) AU. Intriguingly, the planet's orbit is aligned with the major axis of the outer disk (Omega ~ 31 degrees) but probably misaligned with the warp/inclined disk at 80 AU often cited as a signpost for the planet's existence. Our results motivate new studies to clarify how $\beta$ Pic b sculpts debris disk structures and whether a second planet is required to explain the warp/inclined disk., Comment: 6 pages, 4 figures, 1 table; accepted for publication in The Astrophysical Journal Letters
Published: 2011

36. Imaging of a Transitional Disk Gap in Reflected Light: Indications of Planet Formation Around the Young Solar Analog LkCa 15

Author: Thomas Henning, Makoto Watanabe, Tae-Soo Pyo, Masahiko Hayashi, T. Fukue, Gillian R. Knapp, Tetsuro Nishimura, Olivier Guyon, Michiel Min, Hiroshi Shibai, Edwin L. Turner, Motohide Tamura, Toru Yamada, Markus Janson, Klaus W. Hodapp, Nobuhiko Kusakabe, Taro Matsuo, Hiroshi Suto, Hiroshi Terada, Masayuki Kuzuhara, Michihiro Takami, Jun Hashimoto, Carol A. Grady, Saeko S. Hayashi, Jun-Ichi Morino, Mitsuhiko Honda, Hideki Takami, Yutaka Hayano, Amaya Moro-Martin, Naruhisa Takato, Lyu Abe, Tomoyuki Kudo, Ryo Kandori, Sebastian Egner, Michael W. McElwain, Taras Golota, Eugene Serabyn, Joseph C. Carson, Misato Fukagawa, Shoken Miyama, Miki Ishii, D. Tomono, Tomonori Usuda, John P. Wisniewski, Gijs D. Mulders, Ryuji Suzuki, Markus Feldt, Miwa Goto, Christian Thalmann, Wolfgang Brandner, Low Energy Astrophysics (API, FNWI), and Kapteyn Astronomical Institute
Subjects: Offset (computer science), 010504 meteorology & atmospheric sciences, MWC-480, FOS: Physical sciences, Astrophysics, stars: pre-main sequence, 01 natural sciences, circumstellar matter, PHOTOEVAPORATION, Jupiter, Planet, Orientation (geometry), 0103 physical sciences, 010303 astronomy & astrophysics, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Solar analog, STAR, techniques: high angular resolution, Astronomy and Astrophysics, Radius, Planetary system, Starlight, stars: individual (LkCa 15), EVOLUTIONARY MODELS, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, PROTOPLANETARY DISCS, X-RAY, RADIATION, GROWTH, Astrophysics::Earth and Planetary Astrophysics, DM-TAU, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present H- and Ks-band imaging data resolving the gap in the transitional disk around LkCa 15, revealing the surrounding nebulosity. We detect sharp elliptical contours delimiting the nebulosity on the inside as well as the outside, consistent with the shape, size, ellipticity, and orientation of starlight reflected from the far-side disk wall, whereas the near-side wall is shielded from view by the disk's optically thick bulk. We note that forward-scattering of starlight on the near-side disk surface could provide an alternate interpretation of the nebulosity. In either case, this discovery provides confirmation of the disk geometry that has been proposed to explain the spectral energy distributions (SED) of such systems, comprising an optically thick outer disk with an inner truncation radius of ~46 AU enclosing a largely evacuated gap. Our data show an offset of the nebulosity contours along the major axis, likely corresponding to a physical pericenter offset of the disk gap. This reinforces the leading theory that dynamical clearing by at least one orbiting body is the cause of the gap. Based on evolutionary models, our high-contrast imagery imposes an upper limit of 21 Jupiter masses on companions at separations outside of 0.1" and of 13 Jupiter masses outside of 0.2". Thus, we find that a planetary system around LkCa 15 is the most likely explanation for the disk architecture., Comment: 5 pages, 4 figures, accepted for publication in ApJ Letters. Minor change to Figure 4
Published: 2010

37. Performance characterization of the HiCIAO instrument for the Subaru Telescope

Author: Shane Jacobson, Richard Shelton, Masayuki Hattori, Masayuki Kuzuhara, Miwa Goto, Vern Stahlberger, Christian Thalmann, Nobuhiko Kusakabe, Yutaka Hayano, Hubert Yamada, Yoshihiko Saito, Masanori Iye, Hideki Takami, Jun-Ichi Morino, Tomoyuki Kudo, Joseph C. Carson, Ryo Kandori, Taro Matsuo, Meguro Ito, Hiroshi Suto, Makoto Watanabe, Michael W. McElwain, Jun Hashimoto, Shin Oya, Motohide Tamura, Sebastian Egner, Ryuji Suzuki, Klaus W. Hodapp, McLean, Ian S., Ramsay, Suzanne K., and Takami, Hideki
Subjects: Physics, medicine.medical_specialty, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Strehl ratio, Optical polarization, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Exoplanet, law.invention, Spectral imaging, Telescope, Optics, law, medicine, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, Subaru Telescope, business, Coronagraph, Astrophysics::Galaxy Astrophysics
Abstract: HiCIAO is a near-infrared, high contrast instrument which is specifically designed for searches and studies for extrasolar planets and proto-planetary/debris disks on the Subaru 8.2 m telescope. A coronagraph technique and three differential observing modes, i.e., a dual-beam simultaneous polarimetric differential imaging mode, quad-beam simultaneous spectral differential imaging mode, and angular differential imaging mode, are used to extract faint objects from the sea of speckle around bright stars. We describe the instrument performances verified in the laboratory and during the commissioning period. Readout noise with a correlated double sampling method is 15 e- using the Sidecar ASIC controller with the HAWAII-2RG detector array, and it is as low as 5 e- with a multiple sampling method. Strehl ratio obtained by HiCIAO on the sky combined with the 188-actuator adaptive optics system (AO188) is 0.4 and 0.7 in the H and K-band, respectively, with natural guide stars that have R ~ 5 and under median seeing conditions. Image distortion is correctable to 7 milli-arcsec level using the ACS data as a reference image. Examples of contrast performances in the observing modes are presented from data obtained during the commissioning period. An observation for HR 8799 in the angular differential imaging mode shows a clear detection of three known planets, demonstrating the high contrast capability of AO188+HiCIAO.
Published: 2010

38. Discovery of the Coldest Imaged Companion of a Sun-Like Star

Author: Michael W. McElwain, Christoph Mordasini, Thomas Henning, Klaus W. Hodapp, Yutaka Hayano, Tomoyuki Kudo, Ryo Kandori, Joseph C. Carson, Nobuhiko Kusakabe, Hiroshi Suto, Markus Janson, Hubert Klahr, Ryuji Suzuki, Sebastian Egner, Motohide Tamura, Jun Hashimoto, Jun-Ichi Morino, Markus Feldt, Miwa Goto, and Christian Thalmann
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Brown dwarf, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Planetary system, 01 natural sciences, Accretion (astrophysics), Pluto, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Gravitational collapse, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Jupiter mass, Main sequence, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: We present the discovery of a brown dwarf or possible planet at a projected separation of 1.9" = 29 AU around the star GJ 758, placing it between the separations at which substellar companions are expected to form by core accretion (~5 AU) or direct gravitational collapse (typically >100 AU). The object was detected by direct imaging of its thermal glow with Subaru/HiCIAO. At 10-40 times the mass of Jupiter and a temperature of 550-640 K, GJ 758 B constitutes one of the few known T-type companions, and the coldest ever to be imaged in thermal light around a Sun-like star. Its orbit is likely eccentric and of a size comparable to Pluto's orbit, possibly as a result of gravitational scattering or outward migration. A candidate second companion is detected at 1.2" at one epoch., 5 pages, 3 figures, 2 tables. Accepted for publication in ApJ Letters
Published: 2009
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39. SPOTS: Search for Planets Of Two Stars—A Direct Imaging Survey for Exoplanets in Binary Systems

Author: Christian Thalmann, Miwa Goto, Joseph Carson, Markus Feldt, Thomas Henning, Yoichi Itoh, Markus Janson, Ryo Kandori, Gillian R. Knapp, Satoshi Mayama, Michael McElwain, Amaya Moro-Martín, Ryuji Suzuki, Motohide Tamura, Edwin L. Turner, Tomonori Usuda, John Wisniewski, and Miki Ishii
Subjects: Physics, education.field_of_study, Population, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Exoplanet, Kepler-47, Stars, Planet, Binary star, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Circumbinary planet, education, Planetary mass, Astrophysics::Galaxy Astrophysics
Abstract: The Subaru High‐contrast Coronagraphic Imager for Adaptive Optics (HiCIAO) instrument is participating in the planet hunt with its direct imaging survey, the Subaru Strategic Exploration of Exoplanets and Disks (SEEDS), from which binary stars are excluded. However, these systems are expected to harbor a population of planets comparable in number to that of single stars, but differing in many aspects, such as the distribution of planet mass, orbital separation, and eccentricity. Measuring these deviations would unlock a wealth of information on the processes by which planets form and evolve, providing much‐needed constraints to theory. The logical next step is therefore to complement SEEDS with a sister project focusing on binary stars: SPOTS, a “Search for Planets Of Two Stars.” We propose a direct imaging survey for circumbinary planets of very tight binaries and circumstellar planets of wide binaries.
Published: 2009

40. DIRECT IMAGING AND SPECTROSCOPY OF A YOUNG EXTRASOLAR KUIPER BELT IN THE NEAREST OB ASSOCIATION

Author: Thayne Currie, Joseph C. Carson, Nikku Madhusudhan, John H. Debes, Scott J. Kenyon, Carey M. Lisse, Marc J. Kuchner, and Christian Thalmann
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Solar System, Debris disk, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Planetary system, Debris, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Gemini Planet Imager, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Spectroscopy, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: We describe the discovery of a bright, young Kuiper belt-like debris disk around HD 115600, a $\sim$ 1.4--1.5 M$_\mathrm{\odot}$, $\sim$ 15 Myr old member of the Sco-Cen OB Association. Our H-band coronagraphy/integral field spectroscopy from the \textit{Gemini Planet Imager} shows the ring has a (luminosity scaled) semi major axis of ($\sim$ 22 AU) $\sim$ 48 AU, similar to the current Kuiper belt. The disk appears to have neutral scattering dust, is eccentric (e $\sim$ 0.1--0.2), and could be sculpted by analogues to the outer solar system planets. Spectroscopy of the disk ansae reveal a slightly blue to gray disk color, consistent with major Kuiper belt chemical constituents, where water-ice is a very plausible dominant constituent. Besides being the first object discovered with the next generation of extreme adaptive optics systems (i.e. SCExAO, GPI, SPHERE), HD 115600's debris ring and planetary system provides a key reference point for the early evolution of the solar system, the structure and composition of the Kuiper belt, and the interaction between debris disks and planets., Comment: 7 pages, 3 figures, 1 table; ApJ Letters, in press
Published: 2015

41. The EPICS project for the European Extremely Large Telescope: outcome of the Planet Finder concept study for OWL

Author: Pierre Baudoz, C. Correia da Silva, Massimo Turatto, J. L. Beuzit, Norbert Hubin, David Mouillet, Enrico Fedrigo, Kjetil Dohlen, Rainer Lenzen, Daphne Stam, E. Le Coarer, F. Selsis, Jacopo Antichi, M. Kasper, Christophe Verinaud, J. Paillet, N. Yaitskova, Florian Kerber, Achim Gandorfer, Christian Thalmann, Patrick Rabou, R. G. Gratton, Patrice Martinez, Ramón Navarro, Andy Longmore, Hans Martin Schmid, Anthony Boccaletti, F. Rahoui, Thierry Fusco, Markus Feldt, Rémi Soummer, J. Tinbergen, Harald Kuntschner, A. Chalabaev, 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, 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: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Active optics, Astrophysics::Cosmology and Extragalactic Astrophysics, High contrast imaging, Exoplanet, law.invention, Telescope, Planet, law, Extremely Large Telescope, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Adaptive optics, Spectrograph, Remote sensing
Abstract: The Exo-Planets Imaging Camera and Spectrograph (EPICS), is the Planet Finder Instrument concept for the European Extremely Large Telescope (ELT). The study made in the frame of the OWL 100-m telescope concept is being up-dated in direct relation with the re-baselining activities of the European Extremely Large Telescope.
Published: 2006

42. The different faces of transitional discs

Author: Michiel Min, Christian Thalmann, M. de Juan Ovelar, Til Birnstiel, Myriam Benisty, Paola Pinilla, Carsten Dominik, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Research Programm of Institute for Mathematics, Astrophysics and Particle Physics, Astronomy, Near-infrared spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimetry, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Wavelength, Space and Planetary Science, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Small particles, Astrophysics::Galaxy Astrophysics
Abstract: Recent imaging observations of transitional discs have revealed discrepancies between the structure observed at different wavelengths. In some targets, the gap measured using sub-mm observations disappears when observed using near infrared polarimetry, suggesting that the empty region is actually filled with small particles of dust (Dong et al., 2012). Assuming the gapped structure observed in transitional discs is caused by the presence of a planet, we try to explain such discrepancies simulating observations of physical models of disc/planet systems with VLT/SPHERE-ZIMPOL, Subaru/HiCIAO, VLT/VISIR and ALMA.
Published: 2013

43. The architecture of the LkCa 15 transitional disk revealed by high-contrast imaging

Author: Jarron Leisenring, Thomas Henning, Gijs D. Mulders, M. de Juan Ovelar, Carsten Dominik, Timothy D. Brandt, Christian Thalmann, Joseph C. Carson, Motohide Tamura, Michael W. McElwain, Klaus W. Hodapp, Mickael Bonnefoy, Michiel Min, Carol A. Grady, Markus Janson, and Low Energy Astrophysics (API, FNWI)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Offset (computer science), Forward scatter, media_common.quotation_subject, Orbital node, FOS: Physical sciences, Astronomy and Astrophysics, High contrast imaging, Astrophysics, Asymmetry, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, Perpendicular, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, media_common
Abstract: We present four new epochs of Ks-band images of the young pre-transitional disk around LkCa 15, and perform extensive forward modeling to derive the physical parameters of the disk. We find indications of strongly anisotropic scattering (Henyey-Greenstein g = 0.67 [-0.11,+0.18]) and a significantly tapered gap edge ('round wall'), but see no evidence that the inner disk, whose existence is predicted by the spectral energy distribution, shadows the outer regions of the disk visible in our images. We marginally confirm the existence of an offset between the disk center and the star along the line of nodes; however, the magnitude of this offset (x = 27 [-20,+19] mas) is notably lower than that found in our earlier H-band images (Thalmann et al. 2010). Intriguingly, we also find, at high significance, an offset of y = 69 [-25, +49] mas perpendicular to the line of nodes. If confirmed by future observations, this would imply a highly elliptical -- or otherwise asymmetric -- disk gap with an effective eccentricity of e = ~0.3. Such asymmetry would most likely be the result of dynamical sculpting by one or more unseen planets in the system. Finally, we find that the bright arc of scattered light we see in direct imaging observations originates from the near side of the disk, and appears brighter than the far side because of strong forward scattering., 24 pages, 25 figures, accepted for publication in A&A
Published: 2014

44. High-resolution Submillimeter and Near-infrared Studies of the Transition Disk around Sz 91

Author: Tomonori Usuda, Masayuki Kuzuhara, Hiroshi Suto, David J. Wilner, Joseph C. Carson, Carol A. Grady, Miki Ishii, Ryo Kandori, Klaus W. Hodapp, Miwa Goto, Yutaka Hayano, Saeko S. Hayashi, Munetake Momose, M. W. McElwain, Yasuhiro H. Takahashi, Masanori Iye, Ryuji Suzuki, Tae-Soo Pyo, Timothy D. Brandt, Ryohei Kawabe, Hiroshi Terada, Olivier Guyon, Edwin L. Turner, Hideki Takami, Naruhisa Takato, Tetsuro Nishimura, Taro Matsuo, Takashi Tsukagoshi, Motohide Tamura, Takuya Suenaga, Markus Janson, Toru Yamada, Yoshimi Kitamura, Eugene Serabyn, Masahiko Hayashi, Tomoyuki Kudo, Eiji Akiyama, Gillian R. Knapp, Jun-Ichi Morino, Nobuhiko Kusakabe, Jun Hashimoto, Amaya Moro-Martin, Michihiro Takami, Wolfgang Brandner, John P. Wisniewski, Sean M. Andrews, Satoshi Mayama, Masao Saito, Jungmi Kwon, Lyu Abe, Thayne Currie, Shoken Miyama, Thomas Henning, Sebastian Egner, Nagayoshi Ohashi, Christian Thalmann, Makoto Watanabe, Daigo Tomono, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Velocity gradient, Young stellar object, Aperture synthesis, protoplanetary disks, Near-infrared spectroscopy, FOS: Physical sciences, Astronomy and Astrophysics, stars: pre-main sequence, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radius, circumstellar matter, Submillimeter Array, stars: individual (Sz 91), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Protoplanet, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract: 著者人数: 58名, Accepted: 2014-01-16, 資料番号: SA1004554000
Published: 2014

45. Imaging diagnostics for transitional discs

Author: M. de Juan Ovelar, Carsten Dominik, Paola Pinilla, Myriam Benisty, Michiel Min, Til Birnstiel, Christian Thalmann, and Low Energy Astrophysics (API, FNWI)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Research Programm of Institute for Mathematics, Astrophysics and Particle Physics, 010308 nuclear & particles physics, Astronomy, Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Wavelength, Spatial differentiation, Space and Planetary Science, Position (vector), Planet, 0103 physical sciences, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics::Earth and Planetary Astrophysics, Scattered light, 010303 astronomy & astrophysics, Planetary mass, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Transitional discs are a special type of protoplanetary discs where planet formation is thought to be taking place. These objects feature characteristic inner cavities and/or gaps of a few tens of AUs in the sub-millimitre images of the disc. This signature suggests a localised depletion of matter in the disc that could be caused by planet formation processes. However, recent observations have revealed differences in the structures imaged at different wavelengths in some of these discs. In this paper, we aim to explain these observational differences using self-consistent physical 2-D hydrodynamical and dust evolution models of such objects, assuming their morphology is indeed generated by the presence of a planet. We use these models to derive the distribution of gas and dust in a theoretical planet-hosting disc, for various planet masses and orbital separations. We then simulate observations of the emitted and scattered light from these models with VLT/SPHERE ZIMPOL, Subaru/HiCIAO, VLT/VISIR and ALMA. We do this by first computing the full resolution images of the models at different wavelengths, and then simulating the observations accounting for the characteristics of each particular instrument. The presence of the planet generates pressure bumps in the gas distribution of the disc whose characteristics strongly depend on the planet mass and position. These bumps cause large grains to accumulate while small grains are allowed into inner regions. This spatial differentiation of the grain sizes explains the differences in the observations since different wavelengths and observing techniques trace different parts of the dust size distribution. Based on this effect, we conclude that the combination of visible/near-infrared polarimetric and sub-mm images is the best strategy to constrain the properties of the unseen planet responsible for the disc structure., Accepted for publication on the 31st of August 2013, A&A
Published: 2013

46. THE SEEDS DIRECT IMAGING SURVEY FOR PLANETS AND SCATTERED DUST EMISSION IN DEBRIS DISK SYSTEMS

Author: Tae-Soo Pyo, Olivier Guyon, Joseph C. Carson, Ryo Kandori, Yasuhiro H. Takahashi, Carol A. Grady, Miki Ishii, Miwa Goto, Hiroshi Terada, Misato Fukagawa, Shoken Miyama, Klaus W. Hodapp, Takuya Suenaga, Masanori Iye, Tetsuro Nishimura, Masayuki Kuzuhara, Ryuji Suzuki, Makoto Watanabe, John P. Wisniewski, Tomonori Usuda, Justin R. Crepp, Michihiro Takami, Hideki Takami, Tomoyuki Kudo, Jun Hashimoto, Edwin L. Turner, Motohide Tamura, Naruhisa Takato, Lyu Abe, Amaya Moro-Martin, Toru Yamada, Wolfgang Brandner, Jun-Ichi Morino, Nobuhiko Kusakabe, Yutaka Hayano, Saeko S. Hayashi, Masahiro Hayashi, Michael W. McElwain, Markus Janson, D. Tomono, Eugene Serabyn, Yoichi Itoh, Taro Matsuo, Thomas Henning, Timothy D. Brandt, Sebastian Egner, Thayne Currie, Christian Thalmann, Markus Feldt, Jungmi Kwon, Hiroshi Suto, Gillian R. Knapp, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Debris disk, education.field_of_study, Proper motion, 010308 nuclear & particles physics, Population, Giant planet, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Direct imaging, 01 natural sciences, Debris, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Debris disks around young main-sequence stars often have gaps and cavities which for a long time have been interpreted as possibly being caused by planets. In recent years, several giant planet discoveries have been made in systems hosting disks of precisely this nature, further implying that interactions with planets could be a common cause of such disk structures. As part of the SEEDS high-contrast imaging survey, we are surveying a population of debris disk-hosting stars with gaps and cavities implied by their spectral energy distributions, in order to attempt to spatially resolve the disk as well as to detect any planets that may be responsible for the disk structure. Here we report on intermediate results from this survey. Five debris disks have been spatially resolved, and a number of faint point sources have been discovered, most of which have been tested for common proper motion, which in each case has excluded physical companionship with the target stars. From the detection limits of the 50 targets that have been observed, we find that beta Pic b-like planets (~10 Mjup planets around G--A-type stars) near the gap edges are less frequent than 15--30%, implying that if giant planets are the dominant cause of these wide (27 AU on average) gaps, they are generally less massive than beta Pic b., 17 pages, 9 figures, accepted for publication in ApJ
Published: 2013

47. IMAGING DISCOVERY OF THE DEBRIS DISK AROUND HIP 79977

Author: Sebastian Egner, Markus Janson, Satoshi Mayama, Makoto Watanabe, John P. Wisniewski, Masayuki Kuzuhara, Tomonori Usuda, Amaya Moro-Martin, Ryo Kandori, Hiroshi Suto, Naruhisa Takato, Edwin L. Turner, Markus Feldt, Joseph C. Carson, Klaus W. Hodapp, Taro Matsuo, Masanori Iye, Ryuji Suzuki, Motohide Tamura, Shoken Miyama, Yutaka Hayano, Toru Yamada, Christian Thalmann, Timothy D. Brandt, Gillian R. Knapp, Masahiko Hayashi, Miki Ishii, D. Tomono, Wolfgang Brandner, Lyu Abe, Esther Buenzli, Michael W. McElwain, Nobuhiko Kusakabe, Carsten Dominik, Taras Golota, Michihiro Takami, Eugene Serabyn, Hideki Takami, Jun-Ichi Morino, Hiroshi Terada, Jun Hashimoto, Jungmi Kwon, Tomoyuki Kudo, Thayne Currie, Miwa Goto, Tetsuro Nishimura, Tae-Soo Pyo, Olivier Guyon, Saeko S. Hayashi, Thomas Henning, and Low Energy Astrophysics (API, FNWI)
Subjects: 010504 meteorology & atmospheric sciences, Astronomy, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 0103 physical sciences, Surface brightness, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Debris disk, Infrared excess, Research Programm of Institute for Mathematics, Astrophysics and Particle Physics, Linear polarization, Astronomy and Astrophysics, Radius, Polarization (waves), Astrophysics - Solar and Stellar Astrophysics, Radiation pressure, Space and Planetary Science, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics::Earth and Planetary Astrophysics, Halo, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present Subaru/HiCIAO H-band high-contrast images of the debris disk around HIP 79977, whose pres- ence was recently inferred from an infrared excess. Our images resolve the disk for the first time, allowing characterization of its shape, size, and dust grain properties. We use angular differential imaging (ADI) to reveal the disk geometry in unpolarized light out to a radius of ~2", as well as polarized differential imaging (PDI) to measure the degree of scattering polarization out to ~1.5". In order to strike a favorable balance between suppression of the stellar halo and conservation of disk flux, we explore the application of principal component analysis (PCA) to both ADI and reference star subtraction. This allows accurate forward modeling of the effects of data reduction on simulated disk images, and thus direct comparison with the imaged disk. The resulting best-fit values and well-fitting intervals for the model parameters are a surface brightness power-law slope of S_out = -3.2 [-3.6,-2.9], an inclination of i = 84{\deg} [81{\deg},86{\deg}], a high Henyey-Greenstein forward-scattering parameter of g = 0.45 [0.35, 0.60], and a non-significant disk-star offset of u = 3.0 [-1.5, 7.5] AU = 24 [-13, 61] mas along the line of nodes. Furthermore, the tangential linear polarization along the disk rises from ~10% at 0.5" to ~45% at 1.5". These measurements paint a consistent picture of a disk of dust grains produced by collisional cascades and blown out to larger radii by stellar radiation pressure., Comment: 6 pages, 4 figures, 1 table. Accepted for publication in ApJ Letters
Published: 2013

48. Discovery of Small-scale Spiral Structures in the Disk of SAO 206462 (HD 135344B): Implications for the Physical State of the Disk from Spiral Density Wave Theory

Author: Tae-Soo Pyo, Masanori Iye, Olivier Guyon, Amaya Moro-Martin, Ray W. Russell, Hiroshi Terada, Miwa Goto, Thomas Henning, Markus Feldt, Yutaka Hayano, Tomoyuki Kudo, Tetsuro Nishimura, C. Werren, Christian Thalmann, Taro Matsuo, Jun-Ichi Morino, Ryo Kandori, Gillian R. Knapp, Michael W. McElwain, Timothy D. Brandt, Jun Hashimoto, Michel Curé, Masahiko Hayashi, T. Fukue, Misato Fukagawa, Shoken Miyama, Mitsuhiko Honda, Markus Janson, Thayne Currie, Eugene Serabyn, Satoshi Mayama, Joseph C. Carson, Masayuki Kuzuhara, Saeko S. Hayashi, Munetake Momose, John P. Wisniewski, Carol A. Grady, Edwin L. Turner, Motohide Tamura, Klaus W. Hodapp, Sebastian Egner, Toru Yamada, Naruhisa Takato, Miki Ishii, D. Tomono, Jeremy Hornbeck, Tomonori Usuda, Taku Takeuchi, Shu-ichiro Inutsuka, Michihiro Takami, Nobuhiko Kusakabe, Ruobing Dong, Michael L. Sitko, Wolfgang Brandner, Hideki Takami, Takayuki Muto, Hiroshi Suto, Yoshiko K. Okamoto, Lyu Abe, Ryuji Suzuki, Makoto Watanabe, Nagayoshi Ohashi, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Aspect ratio, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Observable, Scale (descriptive set theory), Astrophysics, Star (graph theory), Rotation, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Density wave theory, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Spiral, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present high-resolution, H-band, imaging observations, collected with Subaru/HiCIAO, of the scattered light from the transitional disk around SAO 206462 (HD 135344B). Although previous sub-mm imagery suggested the existence of the dust-depleted cavity at r~46AU, our observations reveal the presence of scattered light components as close as 0.2" (~28AU) from the star. Moreover, we have discovered two small-scale spiral structures lying within 0.5" (~70AU). We present models for the spiral structures using the spiral density wave theory, and derive a disk aspect ratio of h~0.1, which is consistent with previous sub-mm observations. This model can potentially give estimates of the temperature and rotation profiles of the disk based on dynamical processes, independently from sub-mm observations. It also predicts the evolution of the spiral structures, which can be observable on timescales of 10-20 years, providing conclusive tests of the model. While we cannot uniquely identify the origin of these spirals, planets embedded in the disk may be capable of exciting the observed morphology. Assuming that this is the case, we can make predictions on the locations and, possibly, the masses of the unseen planets. Such planets may be detected by future multi-wavelengths observations., Comment: 8 pages, 5 figures, ApJL in press, typo corrected
Published: 2012

49. IMAGES OF THE EXTENDED OUTER REGIONS OF THE DEBRIS RING AROUND HR 4796 A

Author: Thomas Henning, Timothy D. Brandt, Markus Janson, Taro Matsuo, Shoken Miyama, Carsten Dominik, Taras Golota, Tetsuro Nishimura, Carol A. Grady, Jun-Ichi Morino, Naruhisa Takato, Lyu Abe, Joseph C. Carson, Hiroshi Terada, Michael W. McElwain, Miki Ishii, D. Tomono, Hideki Takami, Masayuki Kuzuhara, Glenn Schneider, Tomonori Usuda, Yasuhiro H. Takahashi, Tomoyuki Kudo, Saeko S. Hayashi, Tae-Soo Pyo, Olivier Guyon, Eugene Serabyn, Wolfgang Brandner, Ryo Kandori, Klaus W. Hodapp, Edwin L. Turner, Michihiro Takami, Motohide Tamura, Toru Yamada, Markus Feldt, Miwa Goto, Masahiko Hayashi, T. Fukue, Gillian R. Knapp, Amaya Moro-Martin, John P. Wisniewski, Esther Buenzli, Jun Hashimoto, Nobuhiko Kusakabe, Masanori Iye, Christian Thalmann, Makoto Watanabe, Yutaka Hayano, Sebastian Egner, Hiroshi Suto, Ryuji Suzuki, and Low Energy Astrophysics (API, FNWI)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Debris disk, Planetesimal, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radiation, 01 natural sciences, Debris, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, Cascade, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Surface brightness, 010303 astronomy & astrophysics, Planetary mass, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: We present high-contrast images of HR 4796 A taken with Subaru/HiCIAO in H-band, resolving the debris disk in scattered light. The application of specialized angular differential imaging methods (ADI) allows us to trace the inner edge of the disk with high precision, and reveals a pair of "streamers" extending radially outwards from the ansae. Using a simple disk model with a power-law surface brightness profile, we demonstrate that the observed streamers can be understood as part of the smoothly tapered outer boundary of the debris disk, which is most visible at the ansae. Our observations are consistent with the expected result of a narrow planetesimal ring being ground up in a collisional cascade, yielding dust with a wide range of grain sizes. Radiation forces leave large grains in the ring and push smaller grains onto elliptical, or even hyperbolic trajectories. We measure and characterize the disk's surface brightness profile, and confirm the previously suspected offset of the disk's center from the star's position along the ring's major axis. Furthermore, we present first evidence for an offset along the minor axis. Such offsets are commonly viewed as signposts for the presence of unseen planets within a disk's cavity. Our images also offer new constraints on the presence of companions down to the planetary mass regime (~9 Jupiter masses at 0.5", ~3 Jupiter masses at 1")., Comment: 6 pages, 4 figures, 1 table; accepted for publication in ApJ Letters
Published: 2011

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