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1. High-resolution Near-infrared Polarimetry and Submillimeter Imaging of FS Tau A: Possible Streamers in Misaligned Circumbinary Disk System

Author: Yi Yang, Eiji Akiyama, Thayne Currie, Ruobing Dong, Jun Hashimoto, Saeko S Hayashi, Carol A Grady, Markus Janson, Nemanja Jovanovic, Taichi Uyama, Takao Nakagawa, Tomoyuki Kudo, Nobuhiko Kusakabe, Masayuki Kuzuhara, Lyu Abe, Wolfgang Brandner, Timothy D. Brandt, Michael Bonnefoy, Joseph C Carson, Jeffrey Chilcote, Evan A Rich, Markus Feldt, Miwa Goto, Tyler Dean Groff, Olivier Guyon, Yutaka Hayano, Masahiko Hayashi, Thomas Henning, Klaus W Hodapp, Miki Ishii, Masanori Iye, Ryo Kandori, Jeremy Kasdin, Gillian R. Knapp, Jungmi Kwon, Julien Lozi, Frantz Martinanche, Taro Matsuo, Satoshi Mayama, Michael William Mcelwain, Shoken Miyama, Jun-Ichi Morino, Amaya Moro-Martin, Tetsuo Nishimura, Tae-Soo Pyo, Eugene Serabyn, Hiroshi Suto, Ryuji Suzuki, Michihiro Takami, Naruhisa Takato, Hiroshi Terada, Christian Thalmann, Edwin L Turner, Makoto Watanabe, John P Wisniewski, Toru Yamada, Hideki Takami, Tomonori Usuda, and Motohide Tamura
Subjects: Astronomy
Abstract: We analyzed the young (2.8 Myr-old) binary system FS Tau A using near-infrared (H-band) high-contrast polarimetry data from Subaru/HiCIAO and submillimeter CO (J = 2–1) line emission data from Atacama Large Millimeter/submillimeter Array (ALMA). Both the near-infrared and submillimeter observations reveal several clear structures extending to ~240 au from the stars. Based on these observations at different wavelengths, we report the following discoveries. One arm-like structure detected in the near-infrared band initially extends from the south of the binary with a subsequent turn to the northeast, corresponding to two bar-like structures detected in ALMA observations with an local standard of rest kinematic (LSRK) velocity of 1.19–5.64 km s−1. Another feature detected in the near-infrared band extends initially from the north of the binary, relating to an arm-like structure detected in ALMA observations with an LSRK velocity of 8.17–16.43 km s−1. From their shapes and velocities, we suggest that these structures can mostly be explained by two streamers that connect the outer circumbinary disk and the central binary components. These discoveries will be helpful for understanding the evolution of streamers and circumstellar disks in young binary systems.
Published: 2020
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2. Subaru Near-Infrared Imaging Polarimetry of Misaligned Disks Around the SR 24 Hierachical Triple System

Author: Satoshi Mayama, Sebastian Perez, Nobuhiko Kusakabe, Takayuki Muto, Takashi Tsukagoshi, Michael L. Sitko, Michihiro Takami, Jun Hashimoto, Ruobing Dong, Jungmi Kwon, Saeko S. Hayashi, Tomoyuki Kudo, Masayuki Kuzuhara, Katherine Follette, Misato Fukagawa, Munetake Momose, Daehyeon Oh, Jerome de Leon, Eiji Akiyama, John P. Wisniewski, Yi Yang, Lyu Abe, Wolfgang Brandner, Timothy D. Brandt, Michael Bonnefoy, Joseph C. Carson, Jeffrey Chilcote, Thayne Currie, Markus Feldt, Miwa Goto, Carol A Grady, Tyler Groff, Olivier Guyon, Yutaka Hayano, Masahiko Hayashi, Thomas Henning, Klaus W. Hodapp, Miki Ishii, Masanori Iye, Markus Janson, Nemanja Jovanovic, Ryo Kandori, Jeremy Kasdin, Gillian R. Knapp, Julien Lozi, Frantz Martinache, Taro Matsuo, Michael W Mcelwain, Shoken Miyama, Jun-Ichi Morino, Amaya Moro-Martin, Takao Nakagawa, Tetsuo Nishimura, Tae-Soo Pyo, Evan A. Rich, Eugene Serabyn, Hiroshi Suto, Ryuji Suzuki, Naruhisa Takato, Hiroshi Terada, Christian Thalmann, Daigo Tomono, Edwin L. Turner, Makoto Watanabe, Toru Yamada, Hideki Takami, Tomonori Usuda, Taichi Uyama, and Motohide Tamura
Subjects: Astronomy
Abstract: The SR 24 multistar system hosts both circumprimary and circumsecondary disks, which are strongly misaligned with each other. The circumsecondary disk is circumbinary in nature. Interestingly, both disks are interacting, and they possibly rotate in opposite directions. To investigate the nature of this unique twin disk system, we present 0.″1 resolution near-infrared polarized intensity images of the circumstellar structures around SR 24, obtained with HiCIAO mounted on the Subaru 8.2 m telescope. Both the circumprimary disk and the circumsecondary disk are resolved and have elongated features. While the position angle of the major axis and radius of the near-IR (NIR) polarization disk around SR 24S are 55° and 137 au, respectively, those around SR 24N are 110° and 34 au, respectively. With regard to overall morphology, the circumprimary disk around SR 24S shows strong asymmetry, whereas the circumsecondary disk around SR 24N shows relatively strong symmetry. Our NIR observations confirm the previous claim that the circumprimary and circumsecondary disks are misaligned from each other. Both the circumprimary and circumsecondary disks show similar structures in 12CO observations in terms of its size and elongation direction. This consistency is because both NIR and 12CO are tracing surface layers of the flared disks. As the radius of the polarization disk around SR 24N is roughly consistent with the size of the outer Roche lobe, it is natural to interpret the polarization disk around SR 24N as a circumbinary disk surrounding the SR 24Nb─Nc system.
Published: 2019
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3. Multi-epoch Direct Imaging and Time-variable Scattered Light Morphology of the HD 163296 Protoplanetary Disk

Author: Evan A. Rich, John P. Wisniewski, Thayne Currie, Misato Fukagawa, Carol A. Grady, Michael L. Sitko, Monika Pikhartova, Jun Hashimoto, Lyu Abe, Wolfgang Brandner, Timothy D. Brandt, Joseph C. Carson, Jeffrey Chilcote, Ruobing Dong, Markus Feldt, Miwa Goto, Tyler Groff, Olivier Guyon, Yutaka Hayano, Masahiko Hayashi, Saeko S. Hayashi, Thomas Henning, Klaus W. Hodapp, Miki Ishii, Masanori Iye, Markus Janson, Nemanja Jovanovic, Ryo Kandori, Jeremy Kasdin, Gillian R. Knapp, Tomoyuki Kudo, Nobuhiko Kusakabe, Masayuki Kuzuhara, Jungmi Kwon, Julien Lozi, Frantz Martinache, Taro Matsuo, Satoshi Mayama, Michael W Mcelwain, Shoken Miyama, Jun-Ichi Morino, Amaya Moro-Martin, Takao Nakagawa, Tetsuo Nishimura, Tae-Soo Pyo, Eugene Serabyn, Hiroshi Suto, Ray W. Russel, Ryuji Suzuki, Michihiro Takami, Naruhisa Takato, Hiroshi Terada, Christian Thalmann, Edwin L. Turner, Taichi Uyama, Kevin R. Wagner, Makoto Watanabe, Toru Yamada, Hideki Takami, Tomonori Usuda, and Motohide Tamura
Subjects: Astrophysics
Abstract: We present H-band polarized scattered light imagery and JHK high-contrast spectroscopy of the protoplanetary disk around HD 163296 observed with the High-Contrast Coronographic Imager for Adaptive Optics (HiCIAO) and Subaru Coronagraphic Extreme Adaptive Optics (SCExAO)/Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS) instruments at Subaru Observatory. The polarimetric imagery resolve a broken ring structure surrounding HD 163296 that peaks at a distance along the major axis of 0 65 (66 au) and extends out to 0 98 (100 au) along the major axis. Our 2011 H-band data exhibit clear axisymmetry, with the NW and SE side of the disk exhibiting similar intensities. Our data are clearly different from 2016 epoch H-band observations of the Very Large Telescope (VLT)/Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE), which found a strong 2.7 x asymmetry between the NW and SE side of the disk. Collectively, these results indicate the presence of time-variable, non-azimuthally symmetric illumination of the outer disk. While our SCExAO/CHARIS data are sensitive enough to recover the planet candidate identiﬁed from NIRC2 in the thermal infrared (IR), we fail to detect an object with JHK brightness nominally consistent with this object. This suggests that the candidate is either fainter in JHK bands than model predictions, possibly due to extinction from the disk or atmospheric dust/ clouds, or that it is an artifact of the data set/data processing, such as a residual speckle or partially subtracted disk feature. Assuming standard hot-start evolutionary models and a system age of 5Myr, we set new, direct mass limits for the inner (outer) Atacama Large Millimeter/submillimeter Array (ALMA)-predicted protoplanet candidate along the major (minor) disk axis of of 1.5 (2) M(J).
Published: 2019
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4. A wide-orbit giant planet in the high-mass b Centauri binary system

Author: Markus Janson, Raffaele Gratton, Laetitia Rodet, Arthur Vigan, Mickaël Bonnefoy, Philippe Delorme, Eric E. Mamajek, Sabine Reffert, Lukas Stock, Gabriel-Dominique Marleau, Maud Langlois, Gaël Chauvin, Silvano Desidera, Simon Ringqvist, Lucio Mayer, Gayathri Viswanath, Vito Squicciarini, Michael R. Meyer, Matthias Samland, Simon Petrus, Ravit Helled, Matthew A. Kenworthy, Sascha P. Quanz, Beth Biller, Thomas Henning, Dino Mesa, Natalia Engler, Joseph C. Carson, University of Zurich, Janson, Markus, Stockholm University, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-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, 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), Landessternwarte Königstuhl [ZAH] (LSW), Universität Heidelberg [Heidelberg] = Heidelberg University, Institut für Astronomie und Astrophysik [Tübingen] (IAAT), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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 Franco-Chilien d'Astronomie (LFCA), 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], Universität Zürich [Zürich] = University of Zurich (UZH), Leiden Observatory [Leiden], Universiteit Leiden, SUPA School of Physics and Astronomy [Edinburgh], University of Edinburgh, and Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), 1000 Multidisciplinary, astro-ph.SR, Multidisciplinary, 530 Physics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Earth and planetary astrophysics, Astrophysics - solar and stellar astrophysics, [SDU]Sciences of the Universe [physics], 10231 Institute for Computational Science, astro-ph.EP, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Planet formation occurs around a wide range of stellar masses and stellar system architectures. An improved understanding of the formation process can be achieved by studying it across the full parameter space, particularly toward the extremes. Earlier studies of planets in close-in orbits around high-mass stars have revealed an increase in giant planet frequency with increasing stellar mass until a turnover point at 1.9 solar masses, above which the frequency rapidly decreases. This could potentially imply that planet formation is impeded around more massive stars, and that giant planets around stars exceeding 3 solar masses may be rare or non-existent. However, the methods used to detect planets in small orbits are insensitive to planets in wide orbits. Here we demonstrate the existence of a planet at 560 times the Sun-Earth distance from the 6-10 solar mass binary b Centauri through direct imaging. The planet-to-star mass ratio of 0.10-0.17% is similar to the Jupiter-Sun ratio, but the separation of the detected planet is ~100 times wider than that of Jupiter. Our results show that planets can reside in much more massive stellar systems than what would be expected from extrapolation of previous results. The planet is unlikely to have formed in-situ through the conventional core accretion mechanism, but might have formed elsewhere and arrived to its present location through dynamical interactions, or might have formed via gravitational instability., Comment: Manuscript version. Published in Nature 9 December 2021
Published: 2021

5. BEAST begins: sample characteristics and survey performance of the B-star Exoplanet Abundance Study

Author: Raffaele Gratton, Lucio Mayer, Simon C. Eriksson, Markus Janson, Thomas Henning, Arthur Vigan, Gabriel-Dominique Marleau, Philippe Delorme, Gael Chauvin, Eric E. Mamajek, Mickael Bonnefoy, N. Engler, Joseph C. Carson, Michael R. Meyer, Alexander J. Bohn, Sabine Reffert, Silvano Desidera, Sascha P. Quanz, Matthias Samland, Matthew A. Kenworthy, Valentina D'Orazi, Vito Squicciarini, Maud Langlois, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Landessternwarte Königstuhl [ZAH] (LSW), Universität Heidelberg [Heidelberg], 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), 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), 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, Universität Heidelberg [Heidelberg] = Heidelberg University, 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), and University of Zurich
Subjects: Stellar mass, 530 Physics, FOS: Physical sciences, Sample (statistics), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Earth and planetary astrophysics, 01 natural sciences, Astrophysics - solar and stellar astrophysics, Stars: early-type, 1912 Space and Planetary Science, Planet, Abundance (ecology), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Brown dwarfs, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Epoch (reference date), Astronomy, Astronomy and Astrophysics, Planets and satellites: detection, Outcome (probability), Exoplanet, Stars, Space and Planetary Science, 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Geology
Abstract: While the occurrence rate of wide giant planets appears to increase with stellar mass at least up through the A-type regime, B-type stars have not been systematically studied in large-scale surveys so far. It therefore remains unclear up to what stellar mass this occurrence trend continues. The B-star Exoplanet Abundance Study (BEAST) is a direct imaging survey with the extreme adaptive optics instrument SPHERE, targeting 85 B-type stars in the young Scorpius-Centaurus (Sco-Cen) region with the aim to detect giant planets at wide separations and constrain their occurrence rate and physical properties. The statistical outcome of the survey will help determine if and where an upper stellar mass limit for planet formation occurs. In this work, we describe the selection and characterization of the BEAST target sample. Particular emphasis is placed on the age of each system, which is a central parameter in interpreting direct imaging observations. We implement a novel scheme for age dating based on kinematic sub-structures within Sco-Cen, which complements and expands upon previous age determinations in the literature. We also present initial results from the first epoch observations, including the detections of ten stellar companions, of which six were previously unknown. All planetary candidates in the survey will need follow up in second epoch observations, which are part of the allocated observational programme and will be executed in the near future., Comment: 22 pages, 15 figures, accepted for publication in A&A
Published: 2021

6. The SPHERE infrared survey for exoplanets (SHINE). I. Sample definition and target characterization

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

7. High-resolution Near-infrared Polarimetry and Submillimeter Imaging of FS Tau A: Possible Streamers in Misaligned Circumbinary Disk System

Author: Tae-Soo Pyo, Tomoyuki Kudo, Julien Lozi, Olivier Guyon, Ryuji Suzuki, Jungmi Kwon, Masanori Iye, Joseph C. Carson, Hiroshi Suto, Jeffrey Chilcote, Masahiko Hayashi, Takao Nakagawa, Nemanja Jovanovic, Thomas Henning, Christian Thalmann, M. Bonnefoy, Yutaka Hayano, Tetsuo Nishimura, Eugene Serabyn, Miki Ishii, Klaus W. Hodapp, Yang Yang, Tomonori Usuda, Ryo Kandori, Michael W. McElwain, Makoto Watanabe, Eiji Akiyama, Toru Yamada, Taichi Uyama, Masayuki Kuzuhara, Gillian R. Knapp, Nobuhiko Kusakabe, Evan A. Rich, Shoken M. Miyama, Markus Janson, Carol A. Grady, Saeko S. Hayashi, Wolfgang Brandner, Lyu Abe, Jun-Ichi Morino, Jun Hashimoto, Michihiro Takami, Thayne Currie, Timothy D. Brandt, Motohide Tamura, Markus Feldt, Miwa Goto, Naruhisa Takato, Jeremy Kasdin, Tyler D. Groff, Hideki Takami, Edwin L. Turner, John P. Wisniewski, Frantz Martinache, Satoshi Mayama, Ruobing Dong, Hiroshi Terada, Amaya Moro-Martin, Taro Matsuo, 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), Signal Processing Laboratory (SPL), Wuhan University [China], Hokkaido University [Sapporo, Japan], National Astronomical Observatory of Japan (NAOJ), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, NASA Goddard Space Flight Center (GSFC), California Institute of Technology (CALTECH), The University of Tokyo (UTokyo), Institut méditerranéen de biodiversité et d'écologie marine et continentale (IMBE), Avignon Université (AU)-Aix Marseille Université (AMU)-Institut de recherche pour le développement [IRD] : UMR237-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556, and Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France
Subjects: 010504 meteorology & atmospheric sciences, Polarimetry, FOS: Physical sciences, Binary number, Astrophysics, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Line (formation), Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Near-infrared spectroscopy, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Wavelength, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Millimeter, Circumbinary planet, Astrophysics - Earth and Planetary Astrophysics
Abstract: We analyzed the young (2.8-Myr-old) binary system FS Tau A using near-infrared (H-band) high-contrast polarimetry data from Subaru/HiCIAO and sub-millimeter CO (J=2-1) line emission data from ALMA. Both the near-infrared and sub-millimeter observations reveal several clear structures extending to $\sim$240 AU from the stars. Based on these observations at different wavelengths, we report the following discoveries. One arm-like structure detected in the near-infrared band initially extends from the south of the binary with a subsequent turn to the northeast, corresponding to two bar-like structures detected in ALMA observations with an LSRK velocity of 1.19-5.64 km/s. Another feature detected in the near-infrared band extends initially from the north of the binary, relating to an arm-like structure detected in ALMA observations with an LSRK velocity of 8.17-16.43 km/s. From their shapes and velocities, we suggest that these structures can mostly be explained by two streamers that connect the outer circumbinary disk and the central binary components. These discoveries will be helpful for understanding the evolution of streamers and circumstellar disks in young binary systems., 20 pages, 11 figures, accepted for publication in The Astrophysical Journal
Published: 2020

8. SUBARU Near-Infrared Imaging Polarimetry of Misaligned Disks Around The SR24 Hierarchical Triple System

Author: Katherine B. Follette, Gillian R. Knapp, Hideki Takami, Markus Janson, Amaya Moro-Martin, Yutaka Hayano, Sebastián Pérez, Eiji Akiyama, Shoken Miyama, Naruhisa Takato, Michael W. McElwain, Wolfgang Brandner, Takao Nakagawa, Thomas Henning, Masayuki Kuzuhara, Jerome de Leon, Edwin L. Turner, Satoshi Mayama, Tetsuo Nishimura, Takashi Tsukagoshi, Nemanja Jovanovic, Tomonori Usuda, Jeremy Kasdin, Miki Ishii, Thayne Currie, Tyler D. Groff, Nobuhiko Kusakabe, Hiroshi Terada, Evan A. Rich, Misato Fukagawa, Ryo Kandori, Daehyeon Oh, Michihiro Takami, Taichi Uyama, Takayuki Muto, Jun-Ichi Morino, John P. Wisniewski, Frantz Martinache, Taro Matsuo, Munetake Momose, Christian Thalmann, Carol A. Grady, Tomoyuki Kudo, Julien Lozi, Jun Hashimoto, Saeko S. Hayashi, Makoto Watanabe, Eugene Serabyn, Motohide Tamura, Markus Feldt, Miwa Goto, Masanori Iye, Masahiko Hayashi, Joseph C. Carson, Daigo Tomono, Hiroshi Suto, M. Bonnefoy, Tae-Soo Pyo, Olivier Guyon, Timothy D. Brandt, Toru Yamada, Ruobing Dong, Michael L. Sitko, Lyu Abe, Jeffrey Chilcote, Yi Yang, Klaus W. Hodapp, Ryuji Suzuki, Jungmi Kwon, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France, Ibaraki University, Space Science Institute, Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, ISAS/JAXA, National Astronomical Observatory of Japan (NAOJ), Amherst College, and Hokkaido University [Sapporo, Japan]
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Triple system, business.industry, Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Optics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Near infrared imaging, business, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: The SR24 multi-star system hosts both circumprimary and circumsecondary disks, which are strongly misaligned from each other. The circumsecondary disk is circumbinary in nature. Interestingly, both disks are interacting, and they possibly rotate in opposite directions. To investigate the nature of this unique twin disk system, we present 0.''1 resolution near-infrared polarized intensity images of the circumstellar structures around SR24, obtained with HiCIAO mounted on the Subaru 8.2 m telescope. Both the circumprimary disk and the circumsecondary disk are resolved and have elongated features. While the position angle of the major axis and radius of the NIR polarization disk around SR24S are 55$^{\circ}$ and 137 au, respectively, those around SR24N are 110$^{\circ}$ and 34 au, respectively. With regard to overall morphology, the circumprimary disk around SR24S shows strong asymmetry, whereas the circumsecondary disk around SR24N shows relatively strong symmetry. Our NIR observations confirm the previous claim that the circumprimary and circumsecondary disks are misaligned from each other. Both the circumprimary and circumsecondary disks show similar structures in $^{12}$CO observations in terms of its size and elongation direction. This consistency is because both NIR and $^{12}$CO are tracing surface layers of the flared disks. As the radius of the polarization disk around SR24N is roughly consistent with the size of the outer Roche lobe, it is natural to interpret the polarization disk around SR24N as a circumbinary disk surrounding the SR24Nb-Nc system., Comment: 14 pages, 5 figures, accepted for publication in AJ
Published: 2019
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9. Hint of curvature in the orbital motion of the exoplanet 51 Eridani b using 3 years of VLT/SPHERE monitoring

Author: Riccardo Claudi, E. L. Rickman, T. Schmidt, Th. Henning, Michael Meyer, Henning Avenhaus, Wolfgang Brandner, M. Cudel, Mickael Bonnefoy, Janis Hagelberg, S. Daemgen, Mariangela Bonavita, A. Roux, C. Fontanive, A. Zurlo, Arthur Vigan, L. Rodet, Dino Mesa, L. Abe, Johan Olofsson, Hervé Beust, Gérard Rousset, Matthias Samland, Raphaël Galicher, L. Weber, Francois Menard, Faustine Cantalloube, Anthony Boccaletti, Daniel Rouan, Jean-Luc Beuzit, Markus Janson, Valentina D'Orazi, Zahed Wahhaj, Stéphane Udry, Sergio Messina, Silvano Desidera, Beth Biller, Anne-Marie Lagrange, Kjetil Dohlen, Anne-Lise Maire, Anthony Cheetham, R. G. Gratton, F. Rigal, C. Lazzoni, Joseph C. Carson, H. Le Coroller, D. Melnick, Gael Chauvin, C. Perrot, E. Sissa, Alain Origne, Maud Langlois, 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]), 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, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut für Geowissenschaften [Potsdam], Universität Potsdam, Royal Observatory Edinburgh (ROE), University of Edinburgh, European Southern Observatory (ESO), 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), Stockholm University, Department of Physical Geography and Ecosystem Science [Lund], Lund University [Lund], Université libre de Bruxelles (ULB), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), 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), Institute for Astronomy [Edinburgh] (IfA), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NOVA Optical Infrared Instrumentation Group, Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Université Libre de Bruxelles [Bruxelles] (ULB), 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)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), University of Potsdam = Universität Potsdam, College of Charleston, Observatoire de Paris, Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université de Genève = University of Geneva (UNIGE), 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, and 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)
Subjects: 010504 meteorology & atmospheric sciences, planets and satellites: dynamical evolution and stability, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, techniques: image processing, Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, planetary systems, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Orbital elements, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Giant planet, techniques: high angular resolution, Astronomy and Astrophysics, Planetary system, Orbital period, methods: data analysis, Exoplanet, stars: individual: 51 Eridani, Orbit, Space and Planetary Science, Orbital motion, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. The 51 Eridani system harbors a complex architecture with its primary star forming a hierarchical system with the binary GJ 3305AB at a projected separation of 2000 au, a giant planet orbiting the primary star at 13 au, and a low-mass debris disk around the primary star with possibly a cold component and a warm component inferred from the spectral energy distribution. Aims. We aim to better constrain the orbital parameters of the known giant planet. Methods. We monitored the system over three years from 2015 to 2018 with the VLT/SPHERE exoplanet imaging instrument. Results. We measure an orbital motion for the planet of ~130 mas with a slightly decreasing separation (~10 mas) and find a hint of curvature. This potential curvature is further supported at 3$\sigma$ significance when including literature GPI astrometry corrected for calibration systematics. Fits of the SPHERE and GPI data using three complementary approaches provide broadly similar results. The data suggest an orbital period of 32$^{+17}_{-9}$ yr (i.e. 12$^{+4}_{-2}$ au in semi-major axis), an inclination of 133$^{+14}_{-7}$ deg, an eccentricity of 0.45$^{+0.10}_{-0.15}$, and an argument of periastron passage of 87$^{+34}_{-30}$ deg [mod 180 deg]. The time at periastron passage and the longitude of node exhibit bimodal distributions because we do not detect yet if the planet is accelerating or decelerating along its orbit. Given the inclinations of the planet's orbit and of the stellar rotation axis (134-144 deg), we infer alignment or misalignment within 18 deg for the star-planet spin-orbit. Further astrometric monitoring in the next 3-4 years is required to confirm at a higher significance the curvature in the planet's motion, determine if the planet is accelerating or decelerating on its orbit, and further constrain its orbital parameters and the star-planet spin-orbit., Comment: Accepted for publication in A&A. 15 pages, 12 figures, 6 tables. Updated following language editing, added epoch labels in Fig. 2, and changed color of orbital predictions in Fig. 5
Published: 2019
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10. 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

11. 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

12. SCExAO/CHARIS Near-Infrared Direct Imaging, Spectroscopy, and Forward-Modeling of kappa And b: A Likely Young, Low-Gravity Superjovian Companion

Author: Jungmi Kwon, Eugene Serabyn, Timothy D. Brandt, Nour Skaf, Nemanja Jovanovic, Christian Marois, Jun Nishikawa, Markus Janson, Frantz Martinache, Taichi Uyama, Olivier Guyon, Eiji Akiyama, Sean Goebel, Daehyeon Oh, Kyle Mede, Klaus W. Hodapp, M. Hayashi, Motohide Tamura, Thayne Currie, Masayuki Kuzuhara, Joshua E. Schlieder, Jeffrey Chilcote, Julien Lozi, Eric L. Nielsen, Gillian R. Knapp, Ruben Asensio-Torres, N. Jeremy Kasdin, Joseph C. Carson, Carol A. Grady, Michael L. Sitko, Michael W. McElwain, Tyler D. Groff, Sarah Blunt, Département Sciences de la Fabrication et Logistique (SFL-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-CMP-GC, University of Victoria [Canada] (UVIC), ONERA - The French Aerospace Lab [Palaiseau], ONERA-Université Paris Saclay (COmUE), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Jet Propulsion Laboratory (JPL), and NASA-California Institute of Technology (CALTECH)
Subjects: FOS: Physical sciences, Direct imaging, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Low Gravity, 010309 optics, 0103 physical sciences, Field spectroscopy, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Solar and Stellar Astrophysics (astro-ph.SR), Physics, [PHYS]Physics [physics], Earth and Planetary Astrophysics (astro-ph.EP), Near-infrared spectroscopy, techniques: high angular resolution, Astronomy and Astrophysics, stars: early-type, Planetary system, planetary system, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, stars: individual: (HD 222439), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: 著者人数: 33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: 2018-10-17, 資料番号: SA1180200000
Published: 2018
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13. In-depth study of moderately young but extremely red, very dusty substellar companion HD 206893B

Author: Olivier Absil, Anne-Marie Lagrange, Alice Zurlo, Franz-Josef Hambsch, J. L. Beuzit, P. W. Lucas, C. Petit, Th. Henning, Anne-Lise Maire, Mickael Bonnefoy, Daniel Rouan, Norbert Hubin, T. Schmidt, Francois Wildi, Christian Ginski, L. Rodet, Julien Milli, Joshua E. Schlieder, Mariangela Bonavita, Johan Olofsson, A. Pavlov, Valentina D'Orazi, Joseph C. Carson, C. Mordasini, Anthony Cheetham, Elvira Covino, Janis Hagelberg, Raphaël Galicher, Julien Girard, Baptiste Lavie, Valentin Christiaens, M. Feldt, Anthony Boccaletti, Gael Chauvin, David Mouillet, C. Lazzoni, Federico Marocco, Stéphane Udry, Benjamin Charnay, Sergio Messina, Silvano Desidera, Arthur Vigan, Ronald Roelfsema, R. G. Gratton, A. Delboulbe, Beth Biller, Faustine Cantalloube, Maud Langlois, V. De Caprio, Philippe Delorme, 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 = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Leiden Observatory [Leiden], Universiteit Leiden, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Departamento de Astronomía, Universidad de Chile = University of Chile [Santiago] (UCHILE), Millenium Nucleus Protoplanetary Disks in ALMA Early Science, Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, INAF - Osservatorio Astrofisico di Catania (OACT), Monash University [Melbourne], European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, NASA ExoPlanet Science Institute (NExScI), California Institute of Technology (CALTECH), 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), SUPA, Institute for Astronomy, University of Edinburgh, Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Universidad Diego Portales [Santiago] (UDP), Instituto de Fisica y Astronomia [Valparaiso], Universidad de Valparaiso [Chile], DAAA, ONERA, Université Paris-Saclay [Châtillon], ONERA-Université Paris-Saclay, Remote Observatory Atacama Desert (ROAD), Arizona Materials Laboratory (AML), University of Arizona, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), College of Charleston, INAF - Osservatorio Astronomico di Capodimonte (OAC), NOVA Optical Infrared Instrumentation Group, ANR-14-CE33-0018,GIPSE,Exploration des planetes géantes extrasolaires(2014), ANR-10-LABX-0056,OSUG@2020,Innovative strategies for observing and modelling natural systems(2010), European Project: 226604,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2008-1,OPTICON(2009), European Project: 312430,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2012-1-RTD,OPTICON(2013), European Project: 337569,EC:FP7:ERC,ERC-2013-StG,VORTEX(2013), 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'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universiteit Leiden [Leiden], Universidad de Chile, Universität Bern [Bern], Université de Genève (UNIGE), Instituto de Fisica y Astronomia, ONERA - The French Aerospace Lab [Châtillon], ONERA, 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, 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 Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, INAF-Osservatorio Astronomico di Padova, Leiden Observatory, University of Liège, INAF-Osservatorio Astrofisico di Catania (INAF-OACt), European Southern Observatory, Institute for Astronomy, The University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK, ISDC, Geneva Observatory, University of Geneva, Nucleo de Astronomia, Facultad de Ingenieria, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile, Remote Observatory Atacama Desert (ROAD), Vereniging Voor Sterrenkunde (VVS), Oude Bleken 12, 2400, Mol, Belgium, 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), University of Bern (UBERN), Centre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Institute for Astronomy, Blackford Hill, INAF Napoli: INAF, Astrophysical Observatory of Capodimonte, Salita Moiariello 16, 80131, Napoli, Italy, Netherlands Institute for Radio Astronomy (ASTRON), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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: 010504 meteorology & atmospheric sciences, 530 Physics, Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, planets and satellites: atmospheres, planet-disk interactions, 520 Astronomy, techniques: high angular resolution, Astronomy and Astrophysics, 500 Science, 620 Engineering, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], brown dwarfs
Abstract: The substellar companion HD206893b has recently been discovered by direct imaging of its disc-bearing host star with the SPHERE instrument. We investigate the atypical properties of the companion, which has the reddest near-infrared colours among all known substellar objects, either orbiting a star or isolated, and we provide a comprehensive characterisation of the host star-disc-companion system. We conducted a follow-up of the companion with adaptive optics imaging and spectro-imaging with SPHERE, and a multiinstrument follow-up of its host star. We obtain a R=30 spectrum from 0.95 to 1.64 micron of the companion and additional photometry at 2.11 and 2.25 micron. We carried out extensive atmosphere model fitting for the companions and the host star in order to derive their age, mass, and metallicity. We found no additional companion in the system in spite of exquisite observing conditions resulting in sensitivity to 6MJup (2MJup) at 0.5" for an age of 300 Myr (50 Myr). We detect orbital motion over more than one year and characterise the possible Keplerian orbits. We constrain the age of the system to a minimum of 50 Myr and a maximum of 700 Myr, and determine that the host-star metallicity is nearly solar. The comparison of the companion spectrum and photometry to model atmospheres indicates that the companion is an extremely dusty late L dwarf, with an intermediate gravity (log g 4.5-5.0) which is compatible with the independent age estimate of the system. Though our best fit corresponds to a brown dwarf of 15-30 MJup aged 100-300 Myr, our analysis is also compatible with a range of masses and ages going from a 50 Myr 12MJup planetary-mass object to a 50 MJup Hyades-age brown dwarf..., Comment: Accepted to A&A
Published: 2017

14. The outer disks of Herbig stars from the UV to NIR

Author: Edwin L. Turner, M. W. McElwain, Th. Henning, Takuya Suenaga, Taro Matsuo, Toru Yamada, Makoto Watanabe, John P. Wisniewski, Takayuki Kotani, Tae-Soo Pyo, Olivier Guyon, Jennifer L. Karr, Masanori Iye, Y. Maruta, Yasuhiro H. Takahashi, Joseph C. Carson, Michihiro Takami, Takayuki Muto, Nobuhiko Kusakabe, Miwa Goto, M. Feldt, R. Suzuki, Naruhisa Takato, C. Thalmann, Yoshiko K. Okamoto, Mickael Bonnefoy, Hiroshi Suto, D. Tomono, Jun Hashimoto, Amaya Moro-Martin, Carol A. Grady, Hiroshi Terada, Timothy D. Brandt, Motohide Tamura, Markus Janson, Eugene Serabyn, R. Kandori, Masahiko Hayashi, Jun-Ichi Morino, Masayuki Kuzuhara, Misato Fukagawa, Shoken Miyama, Sebastian Egner, Saeko S. Hayashi, Munetake Momose, Jungmi Kwon, Tetsuo Nishimura, Miki Ishii, Tomoyuki Kudo, Katherine B. Follette, Lyu Abe, Hideki Takami, Gillian R. Knapp, T. Currie, Klaus W. Hodapp, Y. Ohta, Michael L. Sitko, Wolfgang Brandner, Yutaka Hayano, and Tomonori Usuda
Subjects: Physics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Herbig Ae/Be star, Cosmology, Exoplanet, Stars, T Tauri star, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Herbig–Haro object, Astrophysics::Galaxy Astrophysics, Cosmic dust
Abstract: Spatially-resolved imaging of Herbig stars and related objects began with HST, but intensified with commissioning of high-contrast imagers on 8-m class telescopes. The bulk of the data taken from the ground have been polarized intensity imagery at H-band, with the majority of the sources observed as part of the Strategic Exploration of Exoplanets and Disks with Subaru (SEEDS) survey. Sufficiently many systems have been imaged that we discuss disk properties in scattered, polarized light in terms of groups defined by the IR spectral energy distribution. We find novel phenomena in many of the disks, including spiral density waves, and discuss the disks in terms of clearing mechanisms. Some of the disks have sufficient data to map the dust and gas components, including water ice dissociation products.
Published: 2014

15. 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

16. The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits

Author: Ken Rice, Christian Thalmann, Thomas Henning, Damien Ségransan, H. Le Coroller, Maddalena Reggiani, Julien Girard, J. L. Beuzit, Raffaele Gratton, Markus Feldt, S. Messina, Joshua E. Schlieder, Mariangela Bonavita, David Mouillet, Gael Chauvin, Arthur Vigan, A-M. Lagrange, Sascha P. Quanz, Philippe Delorme, Silvano Desidera, Duncan Forgan, Markus Janson, C. Mordasini, Beth Biller, Joseph C. Carson, Anthony Boccaletti, Janis Hagelberg, Dino Mesa, Guillaume Montagnier, C. Moutou, Elvira Covino, Michael Meyer, Alice Zurlo, J.-C. Meunier, Esther Buenzli, Markus Kasper, Mickael Bonnefoy, 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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), Erosion torrentielle neige et avalanches (UR ETGR (ETNA)), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), 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'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), ESO, Physics Department [Garching], Technical University of Munich (TUM)-Technical University of Munich (TUM), 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), Department of Biochemistry and Molecular Biology, Mayo Clinic, 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], 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), SUPA, Institute for Astronomy, The University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK, SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, St. Andrews, KY16 9SS, UK, 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, NASA ExoPlanet Science Institute (NExScI), California Institute of Technology (CALTECH), Department of Physics and Astronomy, University of Missouri, Osservatorio Astronomico di Cagliari, Astrochemistry Group (INAF), Department of Astronomy, Stockholm University, AlbaNova University Center, 106 91, Stockholm, Sweden, Institute for Astronomy, Department of Physics, ETH Zürich, Nucleo de Astronomia, Facultad de Ingenieria, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile, 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), European Southern Observatory, INAF-Osservatorio Astrofisico di Catania (INAF-OACt), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), University of Bern (UBERN), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Observatoire Astronomique de l'Université de Genève, 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), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Max Planck Institute for Astronomy (MPIA), SUPA School of Physics and Astronomy [University of St Andrews], University of St Andrews [Scotland]-Scottish Universities Physics Alliance (SUPA), Centre for Exoplanet Science, 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]), Max Planck Society, College of Charleston, INAF - Osservatorio Astronomico di Capodimonte (OAC), Stockholm University, 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 Chile = University of Chile [Santiago] (UCHILE), 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), French National Research Agency (ANR) : ANR10-BLANC0504-01, French National Research Agency (ANR) : ANR-14-CE33-0018, ECOGAL - European Research Council under ERC-ADG : 291227, Istituto Nazionale Astrofisica (INAF)Ministry of Education, Universities and Research (MIUR)Research Projects of National Relevance (PRIN), Ministry of Education, Universities and Research (MIUR), UK Research & Innovation (UKRI) - Science & Technology Facilities Council (STFC) : ST/M001229/1, National Science Foundation (NSF) : 1009203, Swiss National Science Foundation (SNSF) - European Commission : BSSGI0_155816, and European Union Seventh Framework Programme (ETAEARTH) : 313014
Subjects: statistical [methods], Monte Carlo method, Brown dwarf, FOS: Physical sciences, Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, planets and satellites: formation, infrared: planetary systems, planetary systems [infrared], 10. No inequality, planetary systems, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [PHYS]Physics [physics], methods: statistical, Mass distribution, 010308 nuclear & particles physics, high angular resolution [techniques], techniques: high angular resolution, formation [planets and satellites], Astronomy and Astrophysics, Planetary system, Exoplanet, Accretion (astrophysics), Stars, 13. Climate action, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: Understanding the formation and evolution of giant planets ($\ge$1 $M_{Jup}$) at wide orbital separation ($\ge$5 AU) is one of the goals of direct imaging. Over the past 15 years, many surveys have placed strong constraints on the occurrence rate of wide-orbit giants, mostly based on non-detections, but very few have tried to make a direct link with planet formation theories. In the present work, we combine the results of our previously published VLT/NaCo large program with the results of 12 past imaging surveys to constitute a statistical sample of 199 FGK stars within 100 pc, including 3 stars with sub-stellar companions. Using Monte Carlo simulations and assuming linear flat distributions for the mass and semi-major axis of planets, we estimate the sub-stellar companion frequency to be within 0.75-5.7% at the 68% confidence level (CL) within 20-300 AU and 0.5-75 $M_{Jup}$, which is compatible with previously published results. We also compare our results with the predictions of state-of-the-art population synthesis models based on the gravitational instability (GI) formation scenario by Forgan & Rice (2013), with and without scattering. We estimate that in both the scattered and non-scattered populations, we would be able to detect more than 30% of companions in the 1-75 $M_{Jup}$ range (95% CL). With the 3 sub-stellar detections in our sample, we estimate the fraction of stars that host a planetary system formed by GI to be within 1.0-8.6% (95% CL). We also conclude that even though GI is not common, it predicts a mass distribution of wide-orbit massive companions that is much closer to what is observed than what the core accretion scenario predicts. Finally, we associate the present paper with the release of the Direct Imaging Virtual Archive (DIVA, http://cesam.lam.fr/diva/), a public database that aims at gathering the results of past, present, and future direct imaging surveys., 20 pages, 11 figures. Accepted for publication in A&A
Published: 2017

17. SEEDS direct imaging of the RV-detected companion to V450 Andromedae, and characterization of the system

Author: Ryuji Suzuki, Krzysztof G. Hełminiak, Markus Feldt, Saeko S. Hayashi, Tae-Soo Pyo, Olivier Guyon, Jun Hashimoto, Christian Thalmann, Jungmi Kwon, Tomonori Usuda, Yasuhiro H. Takahashi, Makoto Watanabe, Taro Matsuo, Timothy D. Brandt, Michael W. McElwain, Edwin L. Turner, Joseph C. Carson, Tomoyuki Kudo, Amaya Moro-Martin, Eiji Akiyama, Carol A. Grady, Tetsuro Nishimura, Motohide Tamura, Hiroshi Suto, Eugene Serabyn, Hiroshi Terada, Toru Yamada, Miki Ishii, Gillian R. Knapp, Takuya Suenaga, Thayne Currie, Shoken Miyama, John P. Wisniewski, Masahiko Hayashi, Ryo Kandori, Masayuki Kuzuhara, Klaus W. Hodapp, Hideki Takami, Nobuhiko Kusakabe, Tsuguru Ryu, Naruhisa Takato, Yutaka Hayano, Lyu Abe, Michihiro Takami, Kyle Mede, Norio Narita, Miwa Goto, Masanori Iye, Jun-Ichi Morino, Wolfgang Brandner, Markus Janson, and Thomas Henning
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, FOS: Physical sciences, High resolution, Library science, Astronomy and Astrophysics, Direct imaging, 01 natural sciences, 010309 optics, Science research, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Spectrum analysis, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the direct imaging detection of a low-mass companion to a young, moderately active star V450 And, that was previously identified with the radial velocity method. The companion was found in high-contrast images obtained with the Subaru Telescope equipped with the HiCIAO camera and AO188 adaptive optics system. From the public ELODIE and SOPHIE archives we extracted available high-resolution spectra and radial velocity (RV) measurements, along with RVs from the Lick planet search program. We combined our multi-epoch astrometry with these archival, partially unpublished RVs, and found that the companion is a low-mass star, not a brown dwarf, as previously suggested. We found the best-fitting dynamical masses to be $m_1=1.141_{-0.091}^{+0.037}$ and $m_2=0.279^{+0.023}_{-0.020}$ M$_\odot$. We also performed spectral analysis of the SOPHIE spectra with the iSpec code. The Hipparcos time-series photometry shows a periodicity of $P=5.743$ d, which is also seen in SOPHIE spectra as an RV modulation of the star A. We interpret it as being caused by spots on the stellar surface, and the star to be rotating with the given period. From the rotation and level of activity, we found that the system is $380^{+220}_{-100}$ Myr old, consistent with an isochrone analysis ($220^{+2120}_{-90}$ Myr). This work may serve as a test case for future studies of low-mass stars, brown dwarfs and exoplanets by combination of RV and direct imaging data., 15 pages, 9 figures, 7 tables, to appear in ApJ
Published: 2016

18. Spiral Structure and Differential Dust Size Distribution in the LkHa 330 Disk

Author: Saeko S. Hayashi, Takayuki Muto, M. Feldt, Miwa Goto, Jennifer I-Hsiu Li, Tetsuo Nishimura, Hideki Takami, Th. Henning, Motohide Tamura, Ryo Kandori, Takuya Suenaga, Yutaka Hayano, M. L. Sitko, Hiroshi Terada, Tetsuo Taki, M. Bonnefoy, M. Hayashi, Hauyu Baobabu Liu, Nagayoshi Ohashi, Shoken M. Miyama, Gillian R. Knapp, M. W. McElwain, Sebastian Egner, Ruobing Dong, Tomonori Usuda, Timothy D. Brandt, Tae-Soo Pyo, Eugene Serabyn, Olivier Guyon, Tomoyuki Kudo, Makoto Watanabe, John P. Wisniewski, Eiji Akiyama, Taro Matsuo, D. Tomono, Markus Janson, Miki Ishii, T. Tsukagoshi, Munetake Momose, C. A. Grady, Masayuki Kuzuhara, Wolfgang Brandner, Amaya Moro-Martin, Yasuhiro Hasegawa, Lyu Abe, Jungmi Kwon, Masanori Iye, Joseph C. Carson, Klaus W. Hodapp, Hiroshi Suto, Edwin L. Turner, Y. H. Takahashi, Jun-Ichi Morino, Jun Hashimoto, Satoshi Mayama, N. Kusakabe, Naruhisa Takato, C. Thalmann, Michihiro Takami, R. Suzuki, and Toru Yamada
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Planetesimal, Spiral galaxy, 010504 meteorology & atmospheric sciences, Opacity, Dust particles, FOS: Physical sciences, Astronomy and Astrophysics, Trapping, Astrophysics, 01 natural sciences, Grain growth, Wavelength, Space and Planetary Science, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: Dust trapping accelerates the coagulation of dust particles, and thus it represents an initial step toward the formation of planetesimals. We report $H$-band (1.6 um) linear polarimetric observations and 0.87 mm interferometric continuum observations toward a transitional disk around LkHa 330. As results, a pair of spiral arms were detected in the $H$-band emission and an asymmetric (potentially arm-like) structure was detected in the 0.87 mm continuum emission. We discuss the origin of the spiral arm and the asymmetric structure, and suggest that a massive unseen planet is the most plausible explanation. The possibility of dust trapping and grain growth causing the asymmetric structure was also investigated through the opacity index (beta) by plotting the observed SED slope between 0.87 mm from our SMA observation and 1.3 mm from literature. The results imply that grains are indistinguishable from ISM-like dust in the east side ($beta = 2.0 pm 0.5$), but much smaller in the west side $beta = 0.7^{+0.5}_{-0.4}$, indicating differential dust size distribution between the two sides of the disk. Combining the results of near-infrared and submillimeter observations, we conjecture that the spiral arms exist at the upper surface and an asymmetric structure resides in the disk interior. Future observations at centimeter wavelengths and differential polarization imaging in other bands (Y to K) with extreme AO imagers are required to understand how large dust grains form and to further explore the dust distribution in the disk., 10 pages, 4 figures, AJ accepted for publication
Published: 2016

19. Polarimetry and flux distribution in the debris disk around HD 32297

Author: Jungmi Kwon, Makoto Watanabe, Tomoyuki Kudo, Michihiro Takami, Hideki Takami, Th. Henning, Taro Matsuo, Edwin L. Turner, Tetsuro Nishimura, Takuya Suenaga, Motohide Tamura, Masanori Iye, Carol A. Grady, Toru Yamada, Masahiko Hayashi, Markus Janson, Thayne Currie, Shoken Miyama, Hiroshi Suto, Nobuhiko Kusakabe, Joseph C. Carson, John P. Wisniewski, Eiji Akiyama, Masayuki Kuzuhara, Yasuhiro H. Takahashi, Miki Ishii, Timothy D. Brandt, Jun Hashimoto, Naruhisa Takato, Lyu Abe, Amaya Moro-Martin, Christian Thalmann, Ruben Asensio-Torres, Sebastian Egner, Hiroshi Terada, Michael W. McElwain, Ryo Kandori, Ryuji Suzuki, Jun-Ichi Morino, Esther Buenzli, Klaus W. Hodapp, Tomonori Usuda, Eugene Serabyn, Satoshi Mayama, Wolfgang Brandner, Markus Feldt, Miwa Goto, Yutaka Hayano, Gillian R. Knapp, Saeko S. Hayashi, Tae-Soo Pyo, and Olivier Guyon
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Debris disk, 010504 meteorology & atmospheric sciences, Scattering, Linear polarization, Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Ring (chemistry), 01 natural sciences, Azimuth, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Degree (angle), Surface brightness, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present high-contrast angular differential imaging (ADI) observations of the debris disk around HD 32297 in H-band, as well as the first polarimetric images for this system in polarized differential imaging (PDI) mode with Subaru/HICIAO. In ADI, we detect the nearly edge-on disk at >5sigma levels from ~0.45 arcsec to ~1.7 arcsec (50-192 AU) from the star and recover the spine deviation from the midplane already found in previous works. We also find for the first time imaging and surface brightness (SB) indications for the presence of a gapped structure on both sides of the disk at distances of ~0.75 arcsec (NE side) and ~0.65 arcsec (SW side). Global forward-modelling work delivers a best-fit model disk and well-fitting parameter intervals that essentially match previous results, with high-forward scattering grains and a ring located at 110 AU. However, this single ring model cannot account for the gapped structure seen in our SB profiles. We create simple double ring models and achieve a satisfactory fit with two rings located at 60 and 95 AU, respectively, low-forward scattering grains and very sharp inner slopes. In polarized light we retrieve the disk extending from ~0.25-1.6 arcsec, although the central region is quite noisy and high S/N are only found in the range ~0.75-1.2 arcsec. The disk is polarized in the azimuthal direction, as expected, and the departure from the midplane is also clearly observed. Evidence for a gapped scenario is not found in the PDI data. We obtain a linear polarization degree of the grains that increases from ~10% at 0.55 arcsec to ~25% at 1.6 arcsec. The maximum is found at scattering angles of ~90degrees, either from the main components of the disk or from dust grains blown out to larger radii., Accepted for publication in Astronomy and Astrophysics
Published: 2016

20. High-Contrast Imaging of Intermediate-Mass Giants with Long-Term Radial Velocity Trends

Author: Eiichiro Kokubo, Yoichi Takeda, Hideki Takami, Takuya Suenaga, Tsuguru Ryu, Taichi Uyama, Tetsuo Nishimura, Hiroyasu Ando, Yasuhiro H. Takahashi, Hiroshi Terada, Michihiro Takami, Michitoshi Yoshida, Toru Yamada, Norio Narita, Bun'ei Sato, Gillian R. Knapp, Miwa Goto, John P. Wisniewski, Ryo Kandori, Amaya Moro-Martin, Yoichi Itoh, Masayuki Kuzuhara, Tomoyuki Kudo, Michael W. McElwain, Jungmi Kwon, Krzysztof G. Hełminiak, Hiroshi Suto, Eiji Kambe, Masashi Omiya, Timothy D. Brandt, Satoshi Mayama, Hideyuki Izumiura, Kyle Mede, Jun-Ichi Morino, Saeko S. Hayashi, Ryuji Suzuki, Jun Hashimoto, Masanori Iye, Masahiko Hayashi, Carol A. Grady, Yutaka Hayano, Klaus W. Hodapp, Taro Matsuo, Wolfgang Brandner, Markus Feldt, Thayne Currie, Tomonori Usuda, Naruhisa Takato, Lyu Abe, Tae-Soo Pyo, Edwin L. Turner, Thomas Henning, Olivier Guyon, Motohide Tamura, Hiroki Harakawa, Joseph C. Carson, Christian Thalmann, Shoken Miyama, Markus Janson, Makoto Watanabe, Miki Ishii, Nobuhiko Kusakabe, Sebastian Egner, Shigeru Ida, and Eugene Serabyn
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Stellar mass, 010308 nuclear & particles physics, media_common.quotation_subject, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Planetary system, 01 natural sciences, Article, Kozai mechanism, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Observatory, Planet, 0103 physical sciences, Eccentricity (behavior), Subaru Telescope, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), media_common, Astrophysics - Earth and Planetary Astrophysics
Abstract: A radial velocity (RV) survey for intermediate-mass giants has been operated for over a decade at Okayama Astrophysical Observatory (OAO). The OAO survey has revealed that some giants show long-term linear RV accelerations (RV trends), indicating the presence of outer companions. Direct imaging observations can help clarify what objects generate these RV trends. We present the results of high-contrast imaging observations or six intermediate-mass giants with long-term RV trends using the Subaru Telescope and HiCIAO camera. We detected co-moving companions to $\gamma$ Hya B ($0.61^{+0.12}_{-0.14} M_\odot$), HD 5608 B ($0.10 \pm 0.01 M_\odot$), and HD 109272 B ($0.28 \pm 0.06 M_\odot$). For the remaining targets($\iota$ Dra, 18 Del, and HD 14067) we exclude companions more massive than 30-60 $M_\mathrm{Jup}$ at projected separations of 1arcsec-7arcsec. We examine whether these directly imaged companions or unidentified long-period companions can account for the RV trends observed around the six giants. We find that the Kozai mechanism can explain the high eccentricity of the inner planets $\iota$ Dra b, HD 5608 b, and HD 14067 b., Comment: 33 pases, 9 figures, accepted to ApJ
Published: 2016

21. 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

22. Discovery of an Inner Disk Component around HD 141569 A

Author: Murray D. Silverstone, Eugene Serabyn, Hiroshi Shibai, Marc J. Kuchner, Erika R. Nesvold, Joseph C. Carson, John H. Debes, Hannah Jang-Condell, Alycia J. Weinberger, Timothy J. Rodigas, Dean C. Hines, Andras Gaspar, Christopher C. Stark, Marshall D. Perrin, Amaya Moro-Martin, Glenn Schneider, Mihoko Konishi, John P. Wisniewski, Motohide Tamura, Michael W. McElwain, Philip M. Hinz, Carol A. Grady, and Thomas Henning
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Spiral galaxy, 010504 meteorology & atmospheric sciences, Scattering, Forward scatter, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Thermal emission, 01 natural sciences, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Surface brightness, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Planetary mass, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of a scattering component around the HD 141569 A circumstellar debris system, interior to the previously known inner ring. The discovered inner disk component, obtained in broadband optical light with HST/STIS coronagraphy, was imaged with an inner working angle of 0".25, and can be traced from 0".4 (~46 AU) to 1".0 (~116 AU) after deprojection using i=55deg. The inner disk component is seen to forward scatter in a manner similar to the previously known rings, has a pericenter offset of ~6 AU, and break points where the slope of the surface brightness changes. It also has a spiral arm trailing in the same sense as other spiral arms and arcs seen at larger stellocentric distances. The inner disk spatially overlaps with the previously reported warm gas disk seen in thermal emission. We detect no point sources within 2" (~232 AU), in particular in the gap between the inner disk component and the inner ring. Our upper limit of 9+/-3 M_J is augmented by a new dynamical limit on single planetary mass bodies in the gap between the inner disk component and the inner ring of 1 M_J, which is broadly consistent with previous estimates., 4 pages, 4 figures, 1 table, accepted for publication in ApJL
Published: 2016

23. 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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24. Multiwavelength study of Chandra X-ray sources in the Antennae

Author: John C. Wilson, Stephen S. Eikenberry, D. M. Clark, Charles P. Henderson, Thomas L. Hayward, Joseph C. Carson, Bernhard R. Brandl, Donald J. Barry, Edward Colbert, and Andy Ptak
Subjects: Physics, 010308 nuclear & particles physics, X-ray binary, X-ray, High density, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Star cluster, Space and Planetary Science, Position (vector), 0103 physical sciences, 010303 astronomy & astrophysics, Galaxy cluster
Abstract: We use WIRC, IR images of the Antennae (NGC 4038/4039) together with the extensive catalogue of 120 X-ray point sources (Zezas et al. 2006) to search for counterpart candidates. Using our proven frame-tie technique, we find 38 X-ray sources with IR counterparts, almost doubling the number of IR counterparts to X-ray sources first identified in Clark et al. (2007). In our photometric analysis, we consider the 35 IR counterparts that are confirmed star clusters. We show that the clusters with X-ray sources tend to be brighter, Ks � 16 mag, with (J − Ks) = 1.1 mag. We then use archival HST images of the Antennae to search for optical counterparts to the X-ray point sources. We employ our previous IR-to-X-ray frame-tie as an intermediary to establish a precise optical-to-X-ray frame-tie with < 0.6 arcsec rms positional uncertainty. Due to the high optical source density near the X-ray sources, we determine that we cannot reliably identify counterparts. Comparing the HST positions to the 35 identified IR star cluster counterparts, we find optical matches for 27 of these sources. Using Bruzual-Charlot spectral evolutionary models, we find that most clusters associated with an X-ray source are massive, � 10 6 M� , young, � 10 6 yr, with moderate metallicities, Z = 0.05.
Published: 2010

25. 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

26. SPITZER/INFRARED ARRAY CAMERA LIMITS TO PLANETARY COMPANIONS OF FOMALHAUT AND ϵ ERIDANI

Author: S. T. Megeath, M. Marengo, M. W. Werner, Joseph C. Carson, Giovanni G. Fazio, Joseph L. Hora, K. R. Stapelfeldt, and M. T. Schuster
Subjects: Physics, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Stable point, law.invention, Telescope, Stars, Fomalhaut, Space and Planetary Science, law, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Fomalhaut and epsilon Eridani are two young, nearby stars that possess extended debris disks whose structures suggest the presence of perturbing planetary objects. With its high sensitivity and stable point spread function, Spitzer/IRAC is uniquely capable of detecting cool, Jupiter-like planetary companions whose peak emission is predicted to occur near 4.5 um. We report on deep IRAC imaging of these two stars, taken at 3.6 and 4.5 um using subarray mode and in all four channels in wider-field full array mode. Observations acquired at two different telescope roll angles allowed faint surrounding objects to be separated from the stellar diffraction pattern. No companion candidates were detected at the reported position of Fomalhaut b with 3 sigma model-dependent mass upper limits of 3 MJ (for an age of 200 Myr). Around epsilon Eridani we instead set a limit of 4 and
Published: 2009

27. A First Estimate of the X‐Ray Binary Frequency as a Function of Star Cluster Mass in a Single Galactic System

Author: Edward Colbert, Stephen S. Eikenberry, D. M. Clark, Andy Ptak, Thomas L. Hayward, Donald J. Barry, Bernhard R. Brandl, Joseph C. Carson, John C. Wilson, and Charles P. Henderson
Subjects: Physics, education.field_of_study, 010308 nuclear & particles physics, Astrophysics (astro-ph), Population, X-ray binary, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Luminosity, Star cluster, Space and Planetary Science, Globular cluster, 0103 physical sciences, Cluster (physics), education, 010303 astronomy & astrophysics
Abstract: We use the previously-identified 15 infrared star-cluster counterparts to X-ray point sources in the interacting galaxies NGC 4038/4039 (the Antennae) to study the relationship between total cluster mass and X-ray binary number. This significant population of X-Ray/IR associations allows us to perform, for the first time, a statistical study of X-ray point sources and their environments. We define a quantity, \eta, relating the fraction of X-ray sources per unit mass as a function of cluster mass in the Antennae. We compute cluster mass by fitting spectral evolutionary models to K_s luminosity. Considering that this method depends on cluster age, we use four different age distributions to explore the effects of cluster age on the value of \eta and find it varies by less than a factor of four. We find a mean value of \eta for these different distributions of \eta = 1.7 x 10^-8 M_\sun^-1 with \sigma_\eta = 1.2 x 10^-8 M_\sun^-1. Performing a \chi^2 test, we demonstrate \eta could exhibit a positive slope, but that it depends on the assumed distribution in cluster ages. While the estimated uncertainties in \eta are factors of a few, we believe this is the first estimate made of this quantity to ``order of magnitude'' accuracy. We also compare our findings to theoretical models of open and globular cluster evolution, incorporating the X-ray binary fraction per cluster., Comment: 20 pages, 6 figures, accepted by ApJ
Published: 2008

28. 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

29. 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

30. SEEDS Adaptive Optics Imaging of the Asymmetric Transition Disk Oph IRS 48 in Scattered Light

Author: Masanori Iye, Thayne Currie, Masayuki Kuzuhara, Jeremy R. Swearingen, Eiji Akiyama, Tomoyuki Kudo, Timothy D. Brandt, Katherine B. Follette, Jun Hashimoto, Ray W. Russell, Gillian R. Knapp, Markus Feldt, Eugene Serabyn, Christian Thalmann, Nobuhiko Kusakabe, Lyu Abe, Wolfgang Brandner, Masahiko Hayashi, Michael W. McElwain, Takuya Suenaga, Jungmi Kwon, Makoto Watanabe, Ryuji Suzuki, Laird M. Close, Carol A. Grady, Marc J. Kuchner, Elizabeth H. Champney, Miwa Goto, Ryo Kandori, Joseph C. Carson, Michael L. Sitko, Daigo Tomono, Klaus W. Hodapp, Markus Janson, Satoshi Mayama, Tetsuo Nishimura, Miki Ishii, Thomas Henning, K. M. Maaskant, Misato Fukagawa, Shoken Miyama, Yutaka Hayano, Hiroshi Suto, Sebastian Egner, Amaya Moro-Martin, John P. Wisniewski, Naruhisa Takato, Taro Matsuo, Tomonori Usuda, Nienke van der Marel, Takayuki Muto, Edwin L. Turner, Motohide Tamura, Toru Yamada, Michiel Min, Tae-Soo Pyo, Hideki Takami, Olivier Guyon, Yasuhiro H. Takahashi, Hiroshi Terada, Jun-Ichi Morino, Michihiro Takami, Saeko S. Hayashi, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Brightness, 010504 meteorology & atmospheric sciences, Stellar mass, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Stellar classification, 01 natural sciences, Astronomical spectroscopy, Luminosity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Spectral energy distribution, Surface brightness, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: We present the first resolved near infrared imagery of the transition disk Oph IRS 48 (WLY 2-48), which was recently observed with ALMA to have a strongly asymmetric sub-millimeter flux distribution. H-band polarized intensity images show a $\sim$60AU radius scattered light cavity with two pronounced arcs of emission, one from Northeast to Southeast and one smaller, fainter and more distant arc in the Northwest. K-band scattered light imagery reveals a similar morphology, but with a clear third arc along the Southwestern rim of the disk cavity. This arc meets the Northwestern arc at nearly a right angle, revealing the presence of a spiral arm or local surface brightness deficit in the disk, and explaining the East-West brightness asymmetry in the H-band data. We also present 0.8-5.4$\mu$m IRTF SpeX spectra of this object, which allow us to constrain the spectral class to A0$\pm$1 and measure a low mass accretion rate of 10$^{-8.5}$M$_{\odot}$/yr, both consistent with previous estimates. We investigate a variety of reddening laws in order to fit the mutliwavelength SED of Oph IRS 48 and find a best fit consistent with a younger, higher luminosity star than previous estimates., Comment: Accepted by ApJ. 19 pages, 15 figures
Published: 2015

31. 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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32. 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

33. 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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34. The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits I. Sample definition and characterization

Author: Joseph C. Carson, Philippe Delorme, Katia Biazzo, Joshua E. Schlieder, Mariangela Bonavita, Markus Feldt, C. M. Zaidi, Damien Ségransan, M. Marmier, Mark Esposito, Janis Hagelberg, Valentina D'Orazi, Mickael Bonnefoy, Silvano Desidera, Gael Chauvin, Michael R. Meyer, A-M. Lagrange, Claudio Melo, C. Moutou, Elvira Covino, Ralf Launhardt, Léo Girardi, Juan M. Alcalá, J. L. Beuzit, Raffaele Gratton, A. C. Lanzafame, Stéphane Udry, S. Messina, David Mouillet, Arthur Vigan, Thomas Henning, INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 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), RN, Sciences pour l'environnement (SPE), Université Pascal Paoli (UPP)-Centre National de la Recherche Scientifique (CNRS)-Université Pascal Paoli (UPP)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, INAF - Osservatorio Astrofisico di Catania (OACT), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Institut de Chimie Moléculaire de l'Université de Bourgogne [Dijon] (ICMUB), Université de Bourgogne (UB)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), 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), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Université de Genève (UNIGE), INAF - Osservatorio Astrofisico di Arcetri ( OAA ), Istituto Nazionale di Astrofisica ( INAF ), Institut de Planétologie et d'Astrophysique de Grenoble ( IPAG ), Observatoire des Sciences de l'Univers de Grenoble ( OSUG ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -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 ) -Centre National de la Recherche Scientifique ( 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'Etudes Spatiales ( CNES ), 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 ), Sciences pour l'environnement ( SPE ), Université Pascal Paoli ( UPP ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Pascal Paoli ( UPP ) -Centre National de la Recherche Scientifique ( CNRS ), Max-Planck-Institut für Astronomie ( MPIA ), INAF - Osservatorio Astrofisico di Catania ( OACT ), European Southern Observatory [Santiago] ( ESO ), European Southern Observatory ( ESO ), Institut de Chimie Moléculaire de l'Université de Bourgogne [Dijon] ( ICMUB ), Université de Bourgogne ( UB ) -Centre National de la Recherche Scientifique ( CNRS ), Canada-France-Hawaii Telescope Corporation ( CFHT ), National Research Council of Canada ( NRC ) -Centre National de la Recherche Scientifique ( CNRS ) -University of Hawaii [Honolulu] ( UH ), Observatoire Astronomique de l'Université de Genève ( ObsGE ), Université de Genève ( UNIGE ), ITA, USA, FRA, DEU, ESP, AUS, CHL, CHE, 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 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 (Grenoble INP )-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 d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Centre National de la Recherche Scientifique (CNRS)-Université Pascal Paoli (UPP)-Centre National de la Recherche Scientifique (CNRS)-Université Pascal Paoli (UPP)
Subjects: stars: fundamental parameters, stars: rotation, stars: activity, Rotation period, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Metallicity, Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Luminosity, Planet, Astrophysics::Solar and Stellar Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy and Astrophysics, Exoplanet, Radial velocity, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: Young, nearby stars are ideal targets to search for planets using the direct imaging technique. The determination of stellar parameters is crucial for the interpretation of imaging survey results particularly since the luminosity of substellar objects has a strong dependence on system age. We have conducted a large program with NaCo at the VLT in order to search for planets and brown dwarfs in wide orbits around 86 stars. A large fraction of the targets observed with NaCo were poorly investigated in the literature. We performed a study to characterize the fundamental properties (age, distance, mass) of the stars in our sample. To improve target age determinations, we compiled and analyzed a complete set of age diagnostics. We measured spectroscopic parameters and age diagnostics using dedicated observations acquired with FEROS and CORALIE spectrographs at La Silla Observatory. We also made extensive use of archival spectroscopic data and results available in the literature. Additionally, we exploited photometric time-series, available in ASAS and Super-WASP archives, to derive rotation period for a large fraction of our program stars. We provided updated characterization of all the targets observed in the VLT NaCo Large program, a survey designed to probe the occurrence of exoplanets and brown dwarfs in wide orbits. The median distance and age of our program stars are 64 pc and 100 Myr, respectively. Nearly all the stars have masses between 0.70 and 1.50sun, with a median value of 1.01 Msun. The typical metallicity is close to solar, with a dispersion that is smaller than that of samples usually observed in radial velocity surveys. Several stars are confirmed or proposed here to be members of nearby young moving groups. Eight spectroscopic binaries are identified., Comment: 64 pages with Appendix, 15 figures, accepted to A&A
Published: 2015

35. 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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36. The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits II. Survey description, results, and performances

Author: Th. Henning, David Mouillet, D. Segransan, Alice Zurlo, Esther Buenzli, G. Montagnier, M. Reggianni, J. L. Beuzit, G. Chauvin, Joseph C. Carson, Janis Hagelberg, Dino Mesa, A. Boccaletti, Sascha P. Quanz, Beth Biller, P. Delorme, R. G. Gratton, Julien Girard, Anne-Marie Lagrange, C. Moutou, Mickael Bonnefoy, C. Mordasini, Michael Meyer, M. Feldt, E. Covino, Joshua E. Schlieder, Mariangela Bonavita, Sergio Messina, C. Thalmann, Arthur Vigan, M. Kasper, Silvano Desidera, 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Max-Planck-Institut für Astronomie (MPIA), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), 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), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Department of Physics and Astronomy, College of Charleston, Geneva Observatory, University of Geneva, Chemin des Mailettes 51, 1290, Versoix, Switzerland, Institute for Astronomy, Department of Physics, ETH Zürich, INAF Osservatorio Astronomico di Capodimonte, via Moiarello 16, 80131, Napoli, Italy, European Southern Observatory, European Southern Observatory, Karl Schwarzschild St, 2, 85748, Garching, Germany, and INAF-Osservatorio Astrofisico di Catania (INAF-OACt)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Brightness, Debris disk, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Brown dwarf, White dwarf, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Exoplanet, Stars, 13. Climate action, Space and Planetary Science, Primary (astronomy), Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: In anticipation of the VLT/SPHERE planet imager guaranteed time programs, we have conducted a preparatory survey of 86 stars between 2009 and 2013 in order to identify new faint comoving companions to ultimately carry out a comprehensive analysis of the occurence of giant planets and brown dwarf companions at wide (10-2000 AU) orbits around young, solar-type stars. We used NaCo at VLT to explore the occurrence rate of giant planets and brown dwarfs between typically 0.1 and 8''. Diffraction-limited observations in H-band combined with angular differential imaging enabled us to reach primary star-companion brightness ratios as small as 10-6 at 1.5''. 12 systems were resolved as new binaries, including the discovery of a new white dwarf companion to the star HD8049. Around 34 stars, at least one companion candidate was detected in the observed field of view. More than 400 faint sources were detected, 90% of them in 4 crowded fields. With the exception of HD8049B, we did not identify any new comoving companions. The survey also led to spatially resolved images of the thin debris disk around HD\,61005 that have been published earlier. Finally, considering the survey detection limits, we derive a preliminary upper limit on the frequency of giant planets for semi-major axes of [10,2000] AU: typically less than 15% between 100 and 500 AU, and less than 10% between 50 and 500 AU for exoplanets more massive than 5 MJup and 10 MJup respectively, considering a uniform input distribution and with a confidence level of 95%., 19 pages, 8 figures, 12 Tables, accepted to A&A
Published: 2015

37. Deep Near‐Infrared Imaging and Photometry of the Antennae Galaxies with WIRC

Author: Joseph C. Carson, John C. Wilson, Stephen S. Eikenberry, Donald J. Barry, Bernhard R. Brandl, Thomas L. Hayward, James R. Houck, Charles P. Henderson, and D. M. Clark
Subjects: Physics, 010308 nuclear & particles physics, Infrared, Astrophysics (astro-ph), Extinction (astronomy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galactic nuclei, 01 natural sciences, Galaxy, Photometry (optics), Star cluster, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Near infrared imaging, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present deep near-infrared images of the Antennae galaxies, taken with the Palomar Wide-Field Infrared Camera WIRC. The images cover a 4.33' x 4.33' (24.7kpc x 24.7kpc) area around the galaxy interaction zone. We derive J and K_s band photometric fluxes for 172 infrared star clusters, and discuss details of the two galactic nuclei and the overlap region. We also discuss the properties of a subset of 27 sources which have been detected with WIRC, HST and the VLA. The sources in common are young clusters of less than 10 Myr, which show no correlation between their infrared colors and 6 cm radio properties. These clusters cover a wide range in infrared color due to extinction and evolution. The average extinction is about A_V~2 mag while the reddest clusters may be reddened by up to 10 magnitudes., Accepted for publication in ApJ; a version at higher resolution can be obtained from http://www.strw.leidenuniv.nl/~brandl/Antennae_WIRC.ps.gz
Published: 2005

38. The Effects of Instrumental Elliptical Polarization on Stellar Point Spread Function Fine Structure

Author: John T. Trauger, James B. Breckinridge, Brian Kern, Joseph C. Carson, Mather, John C., MacEwen, Howard A., and de Graauw, Mattheus W. M.
Subjects: Point spread function, Physics, Wavefront, business.industry, Optical engineering, Numerical analysis, Astronomy and Astrophysics, Elliptical polarization, Laboratory results, Polarization (waves), Terrestrial Planet Finder, Amplitude, Optics, Space and Planetary Science, Terrestrial planet, business
Abstract: We present a status report on a study on the effects of instrumental polarization on the fine structure of the stellar point spread function (PSF). These effects are important to understand because the the aberration caused by instrumental polarization on an otherwise diffraction-limited PSF will likely have have severe consequences for extreme high contrast imaging systems such as NASA's proposed Terrestrial Planet Finder (TPF) mission and the proposed NASA Eclipse mission. The report here, describing our efforts to examine these effects, includes two parts: 1) a numerical analysis of the effect of metallic reflection, with some polarization-specific retardation, on a spherical wavefront; 2) an experimental approach for observing this effect, along with a status report on preliminary laboratory results. The numerical analysis indicates that the inclusion of polarization-specific phase effects (retardation) results in a point spread function (PSF) aberration more severe than the amplitude (reflectivity) effects previously recorded in the literature. Preliminary in-lab results are consistent with our numerical predictions.© (2006) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.
Published: 2005

39. The Ultraluminous X-Ray Source X-37 Is a Background Quasar in the Antennae Galaxies

Author: Chuck Henderson, Donald J. Barry, D. M. Clark, A. F. Ptak, John C. Wilson, S. S. Eikenberry, Thomas L. Hayward, Bernhard R. Brandl, Joseph C. Carson, M. H. Christopher, and Edward Colbert
Subjects: Physics, Ultraluminous X-ray source, 010504 meteorology & atmospheric sciences, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Visible spectrum
Abstract: In this paper we report that a bright, X-ray source in the Antennae galaxies (NGC 4038/9), previously identified as an ultra-luminous X-ray source, is in fact a background quasar. We identify an isolated infrared and optical counterpart within 0.3 ± 0. ′′ 5 the X-ray source X-37. After acquiring an optical spectrum of
Published: 2005

40. CHAOS: The Cornell High-Order Adaptive Optics Survey for Brown Dwarfs

Author: Thomas L. Hayward, Joseph C. Carson, J. C. Wilson, Bernhard R. Brandl, and Stephen S. Eikenberry
Subjects: CHAOS (operating system), Physics, 010504 meteorology & atmospheric sciences, 0103 physical sciences, Brown dwarf, Astronomy, Astrophysics, High order, Adaptive optics, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences
Abstract: The Cornell High-order Adaptive Optics Survey for brown dwarfs (CHAOS), currently about 90% complete, uses the Palomar Hale Telescope's adaptive optics system to survey 80 bright stars out to 13 parsecs. Using the telescope's AO Science camera, brown dwarf companions 4–200 AU can be identified using coronagraphic imaging and spectroscopic modes. We will be using monte carlo simulations to create population models consistent with the CHAOS data set.Currently, we have observed 70 systems out of a target sample of 80. Five candidate companions await follow-up observations. As of now, no systems in the target sample have shown strong evidence of having brown dwarf companions. These early results support previous speculations of a “brown dwarf desert” at orbital separations out to 200 AU.While the target sources revealed no evidence of brown dwarf companions, accompanying observations of calibration stars provided evidence of an early methane dwarf candidate around the binary system HD150451AB. Forty seven parsecs from earth, the candidate indicated a projected orbital separation of 280 AU.
Published: 2003

41. 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

42. 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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43. 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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44. 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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45. Probing for Exoplanets Hiding in Dusty Debris Disks: Disk Imaging, Characterization, and Exploration with HST/STIS Multi-Roll Coronagraphy

Author: Eugene Serabyn, Hannah Jang-Condell, Murray D. Silverstone, Christopher C. Stark, Marshall D. Perrin, Bruce E. Woodgate, Alycia J. Weinberger, John P. Wisniewski, Marc J. Kuchner, Thomas Henning, Motohide Tamura, P. M. Hinz, Dean C. Hines, Carol A. Grady, Glenn Schneider, Timothy J. Rodigas, Amaya Moro-Martin, John H. Debes, and Joseph C. Carson
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Solar System, Giant planet, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Protoplanetary disk, Exoplanet, Space and Planetary Science, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Protoplanet, Instrumentation and Methods for Astrophysics (astro-ph.IM), Space Telescope Imaging Spectrograph, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Cosmic dust
Abstract: Spatially resolved scattered-light images of circumstellar (CS) debris in exoplanetary systems constrain the physical properties and orbits of the dust particles in these systems. They also inform on co-orbiting (but unseen) planets, systemic architectures, and forces perturbing starlight-scattering CS material. Using HST/STIS optical coronagraphy, we have completed the observational phase of a program to study the spatial distribution of dust in ten CS debris systems, and one "mature" protoplanetrary disk all with HST pedigree, using PSF-subtracted multi-roll coronagraphy. These observations probe stellocentric distances > 5 AU for the nearest stars, and simultaneously resolve disk substructures well beyond, corresponding to the giant planet and Kuiper belt regions in our Solar System. They also disclose diffuse very low-surface brightness dust at larger stellocentric distances. We present new results inclusive of fainter disks such as HD92945 confirming, and better revealing, the existence of a narrow inner debris ring within a larger diffuse dust disk. Other disks with ring-like sub-structures, significant asymmetries and complex morphologies include: HD181327 with a posited spray of ejecta from a recent massive collision in an exo-Kuiper belt; HD61005 suggested interacting with the local ISM; HD15115 & HD32297, discussed also in the context of environmental interactions. These disks, and HD15745, suggest debris system evolution cannot be treated in isolation. For AU Mic's edge-on disk, out-of-plane surface brightness asymmetries at > 5 AU may implicate one or more planetary perturbers. Time resolved images of the MP Mus proto-planetary disk provide spatially resolved temporal variability in the disk illumination. These and other new images from our program enable direct inter-comparison of the architectures of these exoplanetary debris systems in the context of our own Solar System., 109 pages, 43 figures, accepted for publication in the Astronomical Journal
Published: 2014
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46. 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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47. High-contrast imaging ofϵEridani with ground-based instruments

Author: Takao Nakagawa, Hideki Takami, Saeko S. Hayashi, Naruhisa Takato, C. Thalmann, Gillian R. Knapp, Th. Henning, Amaya Moro-Martin, Takuya Suenaga, Jungmi Kwon, Ryo Kandori, Masayuki Kuzuhara, Tetsuro Nishimura, Yutaka Hayano, Edwin L. Turner, M. W. McElwain, Tomoyuki Kudo, Shoken Miyama, Lyu Abe, Tomonori Usuda, Michael L. Sitko, Eugene Serabyn, Hiroshi Terada, Miki Ishii, Motohide Tamura, Masanori Iye, Michihiro Takami, Joseph C. Carson, Taro Matsuo, Carol A. Grady, R. Suzuki, W. Brander, J. Nishikawa, Hiroshi Suto, Toshiyuki Mizuki, Jun-Ichi Morino, Jun Hashimoto, Toru Yamada, Tae-Soo Pyo, N. Kusakabe, Olivier Guyon, Yasuhiro H. Takahashi, Markus Janson, Sebastian Egner, Klaus W. Hodapp, M. Hayashi, Makoto Watanabe, Timothy D. Brandt, M. Feldt, Miwa Goto, and John P. Wisniewski
Subjects: Physics, Orbital elements, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Giant planet, Astronomy, Astronomy and Astrophysics, Orbital eccentricity, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Radial velocity, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Eccentricity (behavior), 010303 astronomy & astrophysics, Planetary mass, Astrophysics::Galaxy Astrophysics, Main sequence, 0105 earth and related environmental sciences, media_common
Abstract: epsilon Eridani is one of the nearest solar-type stars. Its proximity and relatively young age allow high-contrast imaging observations to achieve sensitivities to planets at narrow separations down to an inner radius of similar to 5 AU. Previous observational studies of the system report a dust disk with asymmetric morphology as well as a giant planet with large orbital eccentricity, which may require another massive companion to induce the peculiar morphology and to enhance the large orbital eccentricity. In this paper, we report results from deep high-contrast imaging observations to detect the previously reported planet and search for other unseen less massive companions with Subaru/HiCIAO, Gemini-South/NICI, and VLT/NACO. No positive detection was made, but high-contrast measurements with the CH4S narrow-band filter of HiCIAO achieved sensitivities at 14.7 mag differential magnitude level, at an angular separation of 1.0 ''. In terms of planetary mass, as determined by cooling evolutionary models, the highest sensitivities were achieved by the Lp broad-band filter of NACO, resulting in sensitivities corresponding to 1.8, 2.8, and 4.5 M-jup at the projected separation of 3 AU, if 200, 400, and 800 Myr is assumed for the age of the system, respectively. We also discuss origins of the dust disk from the detection sensitivity in the planetary mass and find that a less massive eccentric planet is preferred for disk stirring, which is consistent with the orbital parameters of epsilon Eri b claimed from the previous long-term radial velocity monitoring.
Published: 2016

48. Direct Imaging Search for Extrasolar Planets in the Pleiades

Author: Masayuki Kuzuhara, Misato Fukagawa, Shoken Miyama, Ryo Kandori, Amaya Moro-Martin, Thomas Henning, Joseph C. Carson, Klaus W. Hodapp, Hideki Takami, M. W. McElwain, Carol A. Grady, Sebastian Egner, Yutaka Hayano, John P. Wisniewski, Timothy D. Brandt, Takahiro Sumi, Mihoko Konishi, Jun-Ichi Morino, Ryuji Suzuki, Eugene Serabyn, Yoichi Itoh, Ryoko Tanii, Miwa Goto, Nobuhiko Kusakabe, J. Nishikawa, Taro Matsuo, Saeko S. Hayashi, Masanori Iye, Motohide Tamura, Jun Sudo, Toru Yamada, Christian Thalmann, Naruhisa Takato, Lyu Abe, Masahiko Hayashi, Gillian R. Knapp, Kodai Yamamoto, Edwin Lewis Turner, Markus Feldt, Markus Janson, Miki Ishii, Tomonori Usuda, Tomoyuki Kudo, Makoto Watanabe, Tae-Soo Pyo, Jun Hashimoto, Olivier Guyon, Wolfgang Brandner, Hiroshi Shibai, Jungmi Kwon, Daigo Tomono, Thayne Currie, Hiroshi Terada, Michihiro Takami, Tetsuo Nishimura, Hiroshi Suto, and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Proper motion, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Exoplanet, Stars, Space and Planetary Science, Planet, Pleiades, Subaru Telescope, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: We carried out an imaging survey for extrasolar planets around stars in the Pleiades (125 Myr, 135 pc) in the $H$ and $K_{S}$ bands using HiCIAO combined with the adaptive optics, AO188, on the Subaru telescope. We found 13 companion candidates fainter than 14.5 mag in the $H$ band around 9 stars. Five of these 13 were confirmed to be background stars by measurement of their proper motion. One was not found in the second epoch observation, and thus was not a background or companion object. One had multi-epoch image, but the precision of its proper motion was not sufficient to conclude whether it was background object. Four other candidates are waiting for second epoch observations to determine their proper motion. Finally, the remaining 2 were confirmed to be 60 $M_{J}$ brown dwarf companions orbiting around HD 23514 (G0) and HII 1348 (K5) respectively, as had been reported in previous studies. In our observations, the average detection limit for a point source was 20.3 mag in the $H$ band beyond 1''.5 from the central star. On the basis of this detection limit, we calculated the detection efficiency to be 90% for a planet with 6 to 12 Jovian masses and a semi-major axis of 50--1000 AU. For this we extrapolated the distribution of planet mass and semi-major axis derived from RV observations and adopted the planet evolution model of Baraffe et al. (2003). As there was no detection of a planet, we estimated the frequency of such planets to be less than 17.9% ($2\sigma$) around one star of the Pleiades cluster., Comment: 30 pages, 5 figures, accepted for publication in PASJ
Published: 2013

49. 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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50. 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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