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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. High-fidelity Imaging of the Inner AU Mic Debris Disk: Evidence of Differential Wind Sculpting?

Author: John P. Wisniewski, Adam F. Kowalski, James R. A. Davenport, Glenn Schneider, Carol A. Grady, Leslie Hebb, Kellen D. Lawson, Jean-Charles Augereau, Anthony Boccaletti, Alexander Brown, John H. Debes, Andras Gaspar, Thomas K. Henning, Dean C. Hines, Marc J. Kuchner, Anne-Marie Lagrange, Julien Milli, Elie Sezestre, Christopher C. Stark, and Christian Thalmann
Subjects: Astrophysics
Abstract: We present new high-fidelity optical coronagraphic imagery of the inner ∼50 au of AU Mic's edge-on debris disk using the BAR5 occulter of the Hubble Space Telescope Imaging Spectrograph (HST/STIS) obtained on 2018 July 26–27. This new imagery reveals that "feature A," residing at a projected stellocentric separation of 14.2 au on the southeast side of the disk, exhibits an apparent "loop-like" morphology at the time of our observations. The loop has a projected width of 1.5 au and rises 2.3 au above the disk midplane. We also explored Transiting Exoplanet Survey Satellite photometric observations of AU Mic that are consistent with evidence of two starspot complexes in the system. The likely co-alignment of the stellar and disk rotational axes breaks degeneracies in detailed spot modeling, indicating that AU Mic's projected magnetic field axis is offset from its rotational axis. We speculate that small grains in AU Mic's disk could be sculpted by a time-dependent wind that is influenced by this offset magnetic field axis, analogous to co-rotating solar interaction regions that sculpt and influence the inner and outer regions of our own Heliosphere. Alternatively, if the observed spot modulation is indicative of a significant misalignment of the stellar and disk rotational axes, we suggest that the disk could still be sculpted by the differential equatorial versus polar wind that it sees with every stellar rotation.
Published: 2019
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4. 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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5. 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

6. 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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7. The Eroding Disk of AU Mic

Author: Anthony Boccaletti, Marc J. Kuchner, Carol A. Grady, Andras Gaspar, Christopher C. Stark, Jean-Charles Augereau, Christian Thalmann, Thomas Henning, John H. Debes, Glenn Schneider, Julien Milli, John P. Wisniewski, Dean C. Hines, E. Sezestre, and Anne-Marie Lagrange
Subjects: Physics, Stellar wind, 010308 nuclear & particles physics, Space and Planetary Science, Mass transfer, 0103 physical sciences, Astronomy and Astrophysics, Astrophysics, Space (mathematics), 010303 astronomy & astrophysics, 01 natural sciences
Published: 2020

8. SPHERE / ZIMPOL high resolution polarimetric imager. I. System overview, PSF parameters, coronagraphy, and polarimetry

Author: Carsten Dominik, Anthony Boccaletti, François Ménard, Riccardo Claudi, Mark Downing, Hans Martin Schmid, S. Antoniucci, Kjetil Dohlen, A. van Duin, J.-L. Beuzit, E. Sissa, Christoph U. Keller, Markus Kasper, Thierry Fusco, Sascha P. Quanz, Ronald Roelfsema, E. Mulder, Ralf Siebenmorgen, Arthur Vigan, N. Engler, David Mouillet, Marcos Suarez, Julien Girard, Eric Lagadec, H. Hanenburg, M. de Haan, Norbert Hubin, G. Chauvin, Raffaele Gratton, Johan Pragt, Eddy Elswijk, Patrice Martinez, D. Gisler, Andrea Baruffolo, Marcel Carbillet, Stéphane Udry, Jean-François Sauvage, A. Bazzon, F. Rigal, Christian Ginski, Franco Joos, Linda Podio, Anne Costille, Bernardo Salasnich, Maud Langlois, Silvano Desidera, Frans Snik, Francois Wildi, A. Pavlov, S. Hunziker, Lyu Abe, Henning Avenhaus, M. Feldt, J.-B. Daban, R. G. van Holstein, Pierre Baudoz, M. Schuil, Julien Milli, Thomas Henning, Christian Thalmann, Massimo Turatto, Pascal Puget, Low Energy Astrophysics (API, FNWI), ITA, FRA, DEU, CHL, NLD, CHE, Institute for Astronomy, Department of Physics, ETH Zürich, Netherlands Institute for Radio Astronomy (ASTRON), 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, European Southern Observatory, Istituto Ricerche Solari Locarno, Astronomical Institute Anton Pannekoek, University of Amsterdam, 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), Haute résolution angulaire en astrophysique, 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), Leiden Observatory, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), INAF-Osservatorio Astronomico di Roma (INAF-OAR), Max-Planck-Institut für Astronomie (MPIA), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Franco-Chilien d'Astronomie, UMI 3386, European Southern Observatory (ESO), ONERA, 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), INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Firenze, Italy, and Geneva Observatory, University of Geneva, Chemin des Mailettes 51, 1290, Versoix, Switzerland
Subjects: Brightness, Polarimetry, FOS: Physical sciences, instrumentation: adaptive optics, 01 natural sciences, Encircled energy, circumstellar matter, 010309 optics, Optics, instrumentation: high angular resolution, 0103 physical sciences, Surface brightness, 010303 astronomy & astrophysics, Image resolution, planetary systems, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Mira variable, business.industry, instrumentation: detectors, instrumentation: polarimeters, Astronomy and Astrophysics, Polarimeter, Space and Planetary Science, Circumstellar dust, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We describe the Zurich Imaging Polarimeter (ZIMPOL), the visual focal plane subsystem of the SPHERE "VLT planet finder", which pushes the limits of current AO systems to shorter wavelengths, higher spatial resolution, and much improved polarimetric performance. We provide new benchmarks for the performance of high contrast instruments, in particular for polarimetric differential imaging. We have analyzed SPHERE/ZIMPOL point spread functions and measure the peak surface brightness, the encircled energy, and the full width half maximum (FWHM) for different wavelengths, atmospheric conditions, star brightness, and instrument modes. Coronagraphic images are described and analized and the performance for different coronagraphs is compared with tests for the binary alpha Hyi with a separation of 92 mas and a contrast of 6 mag. For the polarimetric mode we made the instrument calibrations using zero polarization and high polarization standard stars and here we give a recipe for the absolute calibration of polarimetric data. The data show a small, 38 pages with 33 figurs, accepted for publication in Astron. Astrophys
Published: 2018

9. 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

10. Assessing the Sustainability Performance of Organic and Low-Input Conventional Farms from Eastern Poland with the RISE Indicator System

Author: Adam Kleofas Berbeć, Beata Feledyn-Szewczyk, Christian Thalmann, Rebekka Wyss, Jan Grenz, Jerzy Kopiński, Jarosław Stalenga, and Paweł Radzikowski
Subjects: Environmental sciences, Environmental effects of industries and plants, sustainability assessment, TJ807-830, GE1-350, RISE, organic farms, TD194-195, conventional farms, Renewable energy sources, biodiversity
Abstract: The aim of this study was to examine the sustainability performance of organic and low-input conventional farms with the sustainability assessment tool—RISE 3.0. It is an indicator-based method for holistic assessment of sustainability of agricultural production at farm level. Ten organic and 10 conventional farms from eastern Poland, Lublin province were assessed. According to the thresholds levels of the RISE method, organic farms performed positively for 7 out of 10 themes, while the values of the other 3 topics, biodiversity, working conditions, and economic viability, were at medium level. Conventional farms reached positive scores for 9 out of 10 themes. The only middle-performing theme was biodiversity. None of the two farm types had the lowest, problematic scores for examined themes. For the theme biodiversity and two indicators (greenhouse gas balance and intensity of agricultural production), significant differences between farming systems were found. Biodiversity performance, an important indicator of sustainability, estimated with the RISE system, was highly correlated with measured on-field weed flora and Orthoptera biodiversity of farms. High soil acidity and low crop productivity, improper weed regulation, and energy management were the most common problems in both types of farms. Working hours and wage and income levels were also assessed as being low. Recommendations to improve the sustainability of both organic and conventional farms are presented.
Published: 2018
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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. 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

13. 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

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

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

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

Author: Gael Chauvin, Johan Olofsson, Alice Zurlo, Dino Mesa, Thomas Henning, Carsten Dominik, Anthony Boccaletti, Mickael Bonnefoy, J. Lannier, François Ménard, Antonio Garufi, Sebastian Daemgen, Markus Feldt, E. Sissa, Raffaele Gratton, Christian Thalmann, N. Engler, Markus Janson, Anne-Marie Lagrange, H. M. Schmid, H. Le Coroller, Myriam Benisty, Silvano Desidera, Gijs D. Mulders, Michael R. Meyer, Christophe Pinte, Graeme Salter, Maud Langlois, Sascha P. Quanz, R. Ligi, Arthur Vigan, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), GDFSuez, Laboratoire Franco-Chilien d'Astronomie (LFCA), Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Chile, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universidad de Chile = University of Chile [Santiago] (UCHILE)-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción - University of Concepcion [Chile], Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Low Energy Astrophysics (API, FNWI), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Universidad de Chile-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Brightness, Scattering, Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, 010309 optics, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Substructure, Surface brightness, Astrophysics::Earth and Planetary Astrophysics, Protoplanet, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: LkCa 15 hosts a pre-transitional disk as well as at least one accreting protoplanet orbiting in its gap. Previous disk observations have focused mainly on the outer disk, which is cleared inward of ~50 au. The planet candidates, on the other hand, reside at orbital radii around 15 au, where disk observations have been unreliable until recently. Here we present new J-band imaging polarimetry of LkCa 15 with SPHERE IRDIS, yielding the most accurate and detailed scattered-light images of the disk to date down to the planet-hosting inner regions. We find what appear to be persistent asymmetric structures in the scattering material at the location of the planet candidates, which could be responsible at least for parts of the signals measured with sparse-aperture masking. These images further allow us to trace the gap edge in scattered light at all position angles and search the inner and outer disks for morphological substructure. The outer disk appears smooth with slight azimuthal variations in polarized surface brightness, which may be due to shadowing from the inner disk or a two-peaked polarized phase function. We find that the near-side gap edge revealed by polarimetry matches the sharp crescent seen in previous ADI imaging very well. Finally, the ratio of polarized disk to stellar flux is more than six times larger in J-band than in the RI bands., 6 pages, 4 figures, 1 table; accepted for publication in ApJ Letters
Published: 2016

16. 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

17. 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

18. 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

19. 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

20. 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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21. SPOTS: The Search for Planets Orbiting Two Stars: II. First constraints on the frequency of sub-stellar companions on wide circumbinary orbits

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

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

23. SPOTS: The Search for Planets Orbiting Two Stars

Author: Michael Meyer, Francesco Marzari, Ruben Asensio-Torres, Masayuki Kuzuhara, Markus Janson, Silvano Desidera, Mariangela Bonavita, Per Calissendorff, Taichi Uyama, Christian Thalmann, and Thomas Henning
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Stellar population, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrometry, Astrophysics, Planetary system, 01 natural sciences, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Binary star, Circumbinary planet, 010303 astronomy & astrophysics, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: Binary stars constitute a large percentage of the stellar population, yet relatively little is known about the planetary systems orbiting them. Most constraints on circumbinary planets (CBPs) so far come from transit observations with the Kepler telescope, which is sensitive to close-in exoplanets but does not constrain planets on wider orbits. However, with continuous developments in high-contrast imaging techniques, this population can now be addressed through direct imaging. We present the full survey results of the Search for Planets Orbiting Two Stars (SPOTS) survey, which is the first direct imaging survey targeting CBPs. The SPOTS observational program comprises 62 tight binaries that are young and nearby, and thus suitable for direct imaging studies, with VLT/NaCo and VLT/SPHERE. Results from SPOTS include the resolved circumbinary disk around AK Sco, the discovery of a low-mass stellar companion in a triple packed system, the relative astrometry of up to 9 resolved binaries, and possible indications of non-background planetary-mass candidates around HIP 77911. We did not find any CBP within 300 AU, which implies a frequency upper limit on CBPs (1--15 $M_{\rm Jup}$) of 6--10 % between 30-300 AU. Coupling these observations with an archival dataset for a total of 163 stellar pairs, we find a best-fit CBP frequency of 1.9 % (2--15 $M_{\rm Jup}$) between 1--300 AU with a 10.5 % upper limit at a 95 % confidence level. This result is consistent with the distribution of companions around single stars., 27 pages, 13 Figures, 7 Tables. Accepted for publication in A&A
Published: 2018

24. 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

25. 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

26. 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

27. 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

28. 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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29. 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

30. 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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31. 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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32. A narrow, edge-on disk resolved around HD 106906 with SPHERE

Author: Matthias Samland, Thomas Henning, Lyu Abe, S. Peretti, Anne-Lise Maire, Hervé Beust, H. Le Coroller, F. Madec, Clément Perrot, Raphael Galicher, Johan Olofsson, Gael Chauvin, Mickael Bonnefoy, Christian Thalmann, Cyril Petit, A-M. Lagrange, Maud Langlois, Markus Janson, Dino Mesa, Graeme Salter, E. Sissa, Julien Girard, J. L. Beuzit, L. Weber, Wolfgang Brandner, Raffaele Gratton, Matthew A. Kenworthy, Julien Milli, J. Lannier, Silvano Desidera, François Ménard, Markus Feldt, D. Perret, C. Soenke, Anthony Boccaletti, P. Rabou, David Mouillet, Esther Buenzli, Vanessa P. Bailey, Anthony Cheetham, Arthur Vigan, Zahed Wahhaj, Surace, Christian, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Steward Observatory, University of Arizona, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre scientifique et Technique Jean Feger (CSTJF), TOTAL FINA ELF, Sterrewacht Leiden, Universiteit Leiden [Leiden], Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Department of Astronomy, Stockholm University, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), De la Molécule aux Nanos-objets : Réactivité, Interactions et Spectroscopies (MONARIS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), ESO, Physics Department [Garching], Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM)-Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), European Synchrotron Radiation Facility (ESRF), Centre de Recherche en Acquisition et Traitement de l'Image pour la Santé (CREATIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Hospices Civils de Lyon (HCL)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble [2011-2019] (IPAG [2011-2019]), Observatoire des Sciences de l'Univers de Grenoble [1985-2015] (OSUG [1985-2015]), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Instituto de Fisica y Astronomia, ICM nucleus on protoplanetary disks, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Franco-Chilien d'Astronomie (LFCA), Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Chile, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), ONERA - The French Aerospace Lab [Châtillon], Université Paris Saclay (COmUE)-ONERA, Université Joseph Fourier - Grenoble 1 (UJF), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), TOTAL-Scientific and Technical Center Jean Féger (CSTJF), University of Geneva [Switzerland], Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Technical University of Munich (TUM)-Technical University of Munich (TUM), Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble [1985-2015] (OSUG [1985-2015]), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Universidad de Chile-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Universiteit Leiden, Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA), ONERA, and université J.Fourier
Subjects: Brightness, 010504 meteorology & atmospheric sciences, HD 106906, FOS: Physical sciences, Astrophysics, 01 natural sciences, [SDU] Sciences of the Universe [physics], Planet, 0103 physical sciences, PLANETARY SYSTEMS, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Debris disk, Spectrometer, Plane (geometry), HIGH ANGULAR RESOLUTION, Astronomy and Astrophysics, Planetary system, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Orbit, Astrophysics - Solar and Stellar Astrophysics, Radiation pressure, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: HD~106906AB is so far the only young binary system around which a planet has been imaged and a debris disk evidenced thanks to a strong IR excess. As such, it represents a unique opportunity to study the dynamics of young planetary systems. We aim at further investigating the close (tens of au scales) environment of the HD~106906AB system. We used the extreme AO fed, high contrast imager SPHERE recently installed on the VLT to observe HD~106906. Both the IRDIS imager and the Integral Field Spectrometer were used. We discovered a very inclined, ring-like disk at a distance of 65~au from the star. The disk shows a strong brightness asymmetry with respect to its semi-major axis. It shows a smooth outer edge, compatible with ejection of small grains by the stellar radiation pressure. We show furthermore that the planet's projected position is significantly above the disk's PA. Given the determined disk inclination, it is not excluded though that the planet could still orbit within the disk plane if at a large separation (2000--3000 au). We identified several additional point sources in the SPHERE/IRDIS field-of-view, that appear to be background objects. We compare this system with other debris disks sharing similarities, and we briefly discuss the present results in the framework of dynamical evolution., Comment: 7 pages, 6 figures, accepted by Astronomy & Astrophysics
Published: 2015
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33. Effects of defoliation by horse chestnut leafminer ( Cameraria ohridella ) on reproduction in Aesculus hippocastanum

Author: Sven Bacher, Christian Thalmann, Jona Freise, and Werner Heitland
Subjects: Aesculus hippocastanum, Herbivore, Ecology, biology, Physiology, food and beverages, Forestry, Plant Science, 580 Plants (Botany), biology.organism_classification, medicine.disease_cause, Hippocastanaceae, Lepidoptera genitalia, Horticulture, Inflorescence, Infestation, Botany, medicine, 570 Life sciences, 590 Animals (Zoology), PEST analysis, Gracillariidae
Abstract: In large parts of Europe horse chestnut trees (Aesculus hippocastanum) suffer from severe defoliation by an alien invasive species, the specialist leaf mining moth Cameraria ohridella (Lepidoptera; Gracillariidae). Heavily infested trees have a drastically shortened period for photosynthesis. We quantified the effect of moth infestation on reproduction of horse chestnut trees in two different cities in central Europe, Bern and Munich. C. ohridella negatively affected seed and fruit weight of A. hippocastanum at both locations. In Munich, seed weight of heavily damaged trees was reduced by almost half. However, the number of seeds per fruit, the number of fruits per inflorescence, and the number of inflorescences per tree did not change due to herbivory. We conclude that C. ohridella mining affects seed quality but not seed quantity. The reduced seed weight may severely impair growth and survival of horse chestnut seedlings and thus may endanger the long-term persistence of A. hippocastanum in its endemic forests in south-east Europe.
Published: 2003

34. 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

35. 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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36. 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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37. 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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38. On-Sky Speckle Nulling Demonstration at Small Angular Separation with SCExAO

Author: Christophe Clergeon, Frantz Martinache, Olivier Guyon, Nemanja Jovanovic, Motohide Tamura, Tomoyuki Kudo, Christian Thalmann, Garima Singh, Michael W. McElwain, Thayne Currie, Low Energy Astrophysics (API, FNWI), Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Nice, France, 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, California Institute of Technology (CALTECH), Observatoire de Paris, Université Paris sciences et lettres (PSL), 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), Subaru Telescope, National Astronomical Observatory of Japan (NAOJ), 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), NASA, 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, 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: Dynamic speckle, Physics, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], business.industry, Angular distance, media_common.quotation_subject, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), 01 natural sciences, 010309 optics, Speckle pattern, Optics, Space and Planetary Science, Sky, 0103 physical sciences, Halo, Subaru Telescope, Adaptive optics, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), ComputingMilieux_MISCELLANEOUS, media_common
Abstract: This paper presents the first on-sky demonstration of speckle nulling, which was achieved at the Subaru Telescope in the context of the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) Project. Despite the absence of a high-order high-bandwidth closed-loop AO system, observations conducted with SCExAO show that even in poor-to-moderate observing conditions, speckle nulling can be used to suppress static and slow speckles even in the presence of a brighter dynamic speckle halo, suggesting that more advanced high-contrast imaging algorithms developed in the laboratory can be applied to ground-based systems., Comment: 5 figures, accepted for publication by PASP
Published: 2014

39. 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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40. 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

41. 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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42. 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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43. Mapping H-band Scattered Light Emission in the Mysterious SR21 Transitional Disk

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

44. The Moving Group Targets of the SEEDS High-Contrast Imaging Survey of Exoplanets and Disks: Results and Observations from the First Three Years

Author: Shoken Miyama, Thomas Henning, Masayuki Kuzuhara, Beth Biller, Eugene Serabyn, Hiroshi Terada, Carol A. Grady, Tetsuro Nishimura, Michihiro Takami, Courtney D. Dressing, Jun-Ichi Morino, Tomoyuki Kudo, Mickael Bonnefoy, Hiroshi Suto, Masanori Iye, Takuya Suenaga, Miwa Goto, Hideki Takami, Makoto Watanabe, Naruhisa Takato, Nobuhiko Kusakabe, Taras Golota, Markus Janson, Wolfgang Brandner, Masahiko Hayashi, Joseph C. Carson, Miki Ishii, D. Tomono, Lyu Abe, Edwin L. Turner, Motohide Tamura, Joshua E. Schlieder, Toru Yamada, John P. Wisniewski, Sebastian Egner, Markus Feldt, Saeko S. Hayashi, Tae-Soo Pyo, Yasuhiro H. Takahashi, Christian Thalmann, Olivier Guyon, Ryuji Suzuki, Tomonori Usuda, Taro Matsuo, Ryo Kandori, Klaus W. Hodapp, Timothy D. Brandt, Amaya Moro-Martin, Yutaka Hayano, Thayne Currie, Gillian R. Knapp, Kyle Mede, Michael W. McElwain, Jungmi Kwon, Jun Hashimoto, and Low Energy Astrophysics (API, FNWI)
Subjects: Rotation period, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Posterior probability, myr, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Exoplanet, Space and Planetary Science, 0103 physical sciences, Probability distribution, Beta Pictoris, TW Hydrae, Subaru Telescope, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present results from the first three years of observations of moving group targets in the SEEDS high-contrast imaging survey of exoplanets and disks using the Subaru telescope. We achieve typical contrasts of ~10^5 at 1" and ~10^6 beyond 2" around 63 proposed members of nearby kinematic moving groups. We review each of the kinematic associations to which our targets belong, concluding that five, \beta Pictoris (~20 Myr), AB Doradus (~100 Myr), Columba (~30 Myr), Tucana-Horogium (~30 Myr), TW Hydrae (~10 Myr), are sufficiently well-defined to constrain the ages of individual targets. Somewhat less than half of our targets are high-probability members of one of these moving groups. For all of our targets, we combine proposed moving group membership with other age indicators where available, including Ca II HK emission, X-ray activity, and rotation period, to produce a posterior probability distribution of age. SEEDS observations discovered a substellar companion to one of our targets, \kappa And, a late B star. We do not detect any other substellar companions, but do find seven new close binary systems, of which one still needs to be confirmed. A detailed analysis of the statistics of this sample, and of the companion mass constraints given our age probability distributions and exoplanet cooling models, will be presented in a forthcoming paper., Comment: 26 pages, 4 figures, 6 tables. Replaced with published ApJ version
Published: 2013
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45. Spiral Arms in the Asymmetrically Illuminated Disk of MWC 758 and Constraints on Giant Planets

Author: Carol A. Grady, Tetsuro Nishimura, Edwin L. Turner, Lyu Abe, Motohide Tamura, Jeremy Hornbeck, Toru Yamada, Th. Henning, Sebastian Egner, Ruobing Dong, Jordy Bouwman, Nobuhiko Kusakabe, Klaus W. Hodapp, Satoshi Mayama, M. Bonnefoy, Jungmi Kwon, Michael L. Sitko, M. Hayashi, J.-U. Pott, G. Serabyn, Wolfgang Brandner, John P. Wisniewski, Sylvestre Lacour, Michihiro Takami, Saeko S. Hayashi, Timothy D. Brandt, Takayuki Muto, Hannah Jang-Condell, Masanori Iye, Markus Janson, Masayuki Kuzuhara, Miwa Goto, A. Crida, David J. Wilner, Tomoyuki Kudo, Jun-Ichi Morino, Jun Hashimoto, Katherine B. Follette, Joseph C. Carson, G. R. Knapp, Christian Thalmann, Miki Ishii, Ryo Kandori, Amaya Moro-Martin, Tomonori Usuda, Michael W. McElwain, Sean M. Andrews, Yutaka Hayano, Glenn Schneider, S. Sai, T. Currie, Adam L. Kraus, Makoto Watanabe, Hiroshi Suto, Gael Chauvin, Naruhisa Takato, Beth Biller, Thomas P. Robitaille, Dean C. Hines, Taro Matsuo, Daigo Tomono, Tae-Soo Pyo, Ray W. Russell, Olivier Guyon, Markus Feldt, Attila Juhasz, Scott Dahm, Ryuji Suzuki, A. Mueller, Hideki Takami, Hiroshi Terada, Misato Fukagawa, Shoken Miyama, Eiji Akiyama, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Low Energy Astrophysics (API, FNWI), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Density wave theory, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [PHYS]Physics [physics], Spiral galaxy, Astronomy and Astrophysics, Planetary system, Exoplanet, Accretion (astrophysics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the first near-IR scattered light detection of the transitional disk associated with the Herbig Ae star MWC 758 using data obtained as part of the Strategic Exploration of Exoplanets and Disks with Subaru, and 1.1 micron HST/NICMOS data. While sub-millimeter studies suggested there is a dust-depleted cavity with r=0.35, we find scattered light as close as 0.1 (20-28 AU) from the star, with no visible cavity at H, K', or Ks. We find two small-scaled spiral structures which asymmetrically shadow the outer disk. We model one of the spirals using spiral density wave theory, and derive a disk aspect ratio of h ~ 0.18, indicating a dynamically warm disk. If the spiral pattern is excited by a perturber, we estimate its mass to be 5+3,-4 Mj, in the range where planet filtration models predict accretion continuing onto the star. Using a combination of non-redundant aperture masking data at L' and angular differential imaging with Locally Optimized Combination of Images at K' and Ks, we exclude stellar or massive brown dwarf companions within 300 mas of the Herbig Ae star, and all but planetary mass companions exterior to 0.5. We reach 5-sigma contrasts limiting companions to planetary masses, 3-4 MJ at 1.0 and 2 MJ at 1.55 using the COND models. Collectively, these data strengthen the case for MWC 758 already being a young planetary system., 45 pages, 9 figures; ApJ in press
Published: 2013

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

Author: Andreas Bazzon, E. Lagadec, Massimo Turatto, Catherine Dougados, E. Sissa, Francesca Bacciotti, Simone Antoniucci, Christian Thalmann, T. Giannini, Linda Podio, H. M. Schmid, Mickael Bonnefoy, Gael Chauvin, Raffaele Gratton, A. La Camera, Brunella Nisini, Maud Langlois, Silvano Desidera, ITA, FRA, CHE, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Be star, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Binary number, stars: pre-main sequence, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, circumstellar matter, 01 natural sciences, outflows, Collimated light, stars: individual: Z CMa, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, stars: variables: T Tauri, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Herbig Ae/Be, techniques: high angular resolution, Astronomy and Astrophysics, Accretion (astrophysics), 3. Good health, Stars, T Tauri star, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, stars: winds, Orbital motion, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Deconvolution
Abstract: Crucial information on the mass accretion-ejection in young stars can be obtained from high spatial resolution images of jets in sources with recurrent accretion outbursts. Using the SPHERE/ZIMPOL instrument, we observed the young binary Z CMa that is composed of a Herbig Be star and a FUor object, both driving a jet. We analyse the structure of the two jets in relation with previous accretion events observed in this target. We obtained optical images in the Halpha and OI 6300A lines at the unprecedented angular resolution of ~0.03 arcsec, on which we have performed both continuum subtraction and deconvolution, thereby deriving results that are consistent with each other. Our images reveal extended emission from both sources: a fairly compact and poorly collimated emission SW of the Herbig component and an extended collimated and precessing jet from the FUor component. The compact emission from the Herbig star is compatible with a wide-angle wind and is possibly connected to the recent outburst events shown by this component. The FUor jet is traced down to 70 mas (80 AU) from the source and is highly collimated with a width of 26-48 AU at distances 100-200 AU, which is similar to the width of jets from T Tauri stars. This strongly suggests that the same magneto-centrifugal jet-launching mechanism also operates in FUors. The observed jet wiggle can be modelled as originating from an orbital motion with a period of 4.2 yr around an unseen companion with mass between 0.48 and 1 Msun. The jet mass loss rate Mloss was derived from the OI luminosity and is in the range 1E-8 and 1E-6 Msun/yr. This is the first direct Mloss measurement from a jet in a FUor. If we assume previous Macc estimates obtained through modelling of the accretion disk, the derived range of Mloss would imply a very low mass-ejection efficiency (Mloss/Macc < 0.02), which is lower than that typical of T Tauri stars., Letter to Astronomy and Astrophysics
Published: 2016

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

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

48. Extreme asymmetry in the polarized disk of V1247 Orionis

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

49. VLT/SPHERE deep insight of NGC 3603’s core: Segregation or confusion?

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

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

Author: Michael W. McElwain, Tomonori Usuda, Mitsuhiko Honda, Zhaohuan Zhu, Melissa McClure, Carol A. Grady, Markus Janson, Lyu Abe, Miki Ishii, Yutaka Hayano, Masao Hayashi, Ryuji Suzuki, Takuya Suenaga, Naruhisa Takato, John P. Wisniewski, Edwin L. Turner, Jungmi Kwon, Christian Thalmann, Klaus W. Hodapp, Yasuhiro H. Takahashi, Taro Matsuo, Michihiro Takami, Tomoyuki Kudo, Gene Serabyn, Timothy D. Brandt, Misato Fukagawa, Shoken Miyama, Masanori Iye, Masayuki Kuzuhara, Hiroshi Terada, Tetsuro Nishimura, Saeko S. Hayashi, Satoshi Mayama, Joseph C. Carson, Ryo Kandori, Makoto Watanabe, Miwa Goto, Markus Feldt, Hideki Takami, Tae-Soo Pyo, Olivier Guyon, Hiroshi Suto, Motohide Tamura, Toru Yamada, G. R. Knapp, Nobuhiko Kusakabe, Jun-Ichi Morino, Jun Hashimoto, Daigo Tomono, Takayuki Muto, Thomas Henning, Sebastian Egner, Amaya Moro-Martin, Wolfgang Brandner, Ruobing Dong, and Low Energy Astrophysics (API, FNWI)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, Proper motion, 010308 nuclear & particles physics, Monte Carlo method, Brown dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Protoplanetary disk, 01 natural sciences, T Tauri star, Full width at half maximum, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present high resolution H-band polarized intensity (PI; FWHM = 0."1: 14 AU) and L'-band imaging data (FWHM = 0."11: 15 AU) of the circumstellar disk around the weak-lined T Tauri star PDS 70 in Centaurus at a radial distance of 28 AU (0."2) up to 210 AU (1."5). In both images, a giant inner gap is clearly resolved for the first time, and the radius of the gap is ~70 AU. Our data show that the geometric center of the disk shifts by ~6 AU toward the minor axis. We confirm that the brown dwarf companion candidate to the north of PDS 70 is a background star based on its proper motion. As a result of SED fitting by Monte Carlo radiative transfer modeling, we infer the existence of an optically thick inner disk at a few AU. Combining our observations and modeling, we classify the disk of PDS 70 as a pre-transitional disk. Furthermore, based on the analysis of L'-band imaging data, we put an upper limit mass of companions at ~30 to ~50MJ within the gap. Taking account of the presence of the large and sharp gap, we suggest that the gap could be formed by dynamical interactions of sub-stellar companions or multiple unseen giant planets in the gap., accepted by APJL
Published: 2012

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