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151. Signs of late infall and possible planet formation around DR Tau using VLT/SPHERE and LBTI/LMIRCam

Author: Mesa, D., primary, Ginski, C., additional, Gratton, R., additional, Ertel, S., additional, Wagner, K., additional, Bonavita, M., additional, Fedele, D., additional, Meyer, M., additional, Henning, T., additional, Langlois, M., additional, Garufi, A., additional, Antoniucci, S., additional, Claudi, R., additional, Defrère, D., additional, Desidera, S., additional, Janson, M., additional, Pawellek, N., additional, Rigliaco, E., additional, Squicciarini, V., additional, Zurlo, A., additional, Boccaletti, A., additional, Bonnefoy, M., additional, Cantalloube, F., additional, Chauvin, G., additional, Feldt, M., additional, Hagelberg, J., additional, Hugot, E., additional, Lagrange, A.-M., additional, Lazzoni, C., additional, Maurel, D., additional, Perrot, C., additional, Petit, C., additional, Rouan, D., additional, and Vigan, A., additional
Published: 2022
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152. Orbital and dynamical analysis of the system around HR 8799

Author: Zurlo, A., Go??dziewski, K., Lazzoni, C., Mesa, D., Nogueira, P., Desidera, S., Gratton, R., Marzari, F., Langlois, M., Pinna, E., Chauvin, G., Delorme, P., Girard, J. H., Hagelberg, J., Henning, Th., Janson, M., Rickman, E., Kervella, P., Avenhaus, H., Bhowmik, T., Biller, B., Boccaletti, A., Bonaglia, M., Bonavita, M., Bonnefoy, M., Cantalloube, F., Cheetham, A., Claudi, R., D???orazi, V., Feldt, M., Galicher, R., Ghose, E., Lagrange, A. -M., le Coroller, H., Ligi, R., Kasper, M., Maire, A. -L., Medard, F., Meyer, M., Peretti, S., Perrot, C., Puglisi, A. T., Rossi, F., Rothberg, B., Schmidt, T., Sissa, E., Vigan, A., and Wahhaj, Z.
Published: 2022

153. PYRAMIR: Exploring the On-Sky Performance of the World’s First Near-Infrared Pyramid Wavefront Sensor

Author: Peter, D., Feldt, M., Henning, T., Hippler, S., Aceituno, J., Montoya, L., Costa, J., and Dorner, B.
Published: 2010
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154. 22q11.2 duplications: Expanding the clinical presentation

Author: Bartik, Lauren E., primary, Hughes, Susan S., additional, Tracy, Meghan, additional, Feldt, M. Max, additional, Zhang, Lei, additional, Arganbright, Jill, additional, and Kaye, Alison, additional
Published: 2021
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155. The SPHERE infrared survey for exoplanets (SHINE)

Author: Langlois, M., Gratton, R., Lagrange, A.-M., Delorme, P., Boccaletti, A., Bonnefoy, M., Maire, A.-L., Mesa, D., Chauvin, G., Desidera, S., Vigan, A., Cheetham, A., Hagelberg, J., Feldt, M., Meyer, M., Rubini, P., Le Coroller, H., Cantalloube, F., Biller, B., Bonavita, M., Bhowmik, T., Brandner, W., Daemgen, S., D’orazi, V., Flasseur, O., Fontanive, C., Galicher, R., Girard, J., Janin-Potiron, P., Janson, M., Keppler, M., Kopytova, T., Lagadec, E., Lannier, J., Lazzoni, C., Ligi, R., Meunier, N., Perreti, A., Perrot, C., Rodet, L., Romero, C., Rouan, D., Samland, M., Salter, G., Sissa, E., Schmidt, T., Zurlo, A., Mouillet, D., Denis, L., Thiébaut, E., Milli, J., Wahhaj, Z., Beuzit, J.-L., Dominik, C., Henning, Th., Ménard, F., Müller, A., Schmid, H. M., Turatto, M., Udry, S., Abe, L., Antichi, J., Allard, F., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., de Caprio, V., Delboulbé, A., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, Thierry, Gigan, P., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Messina, S., Möller-Nilsson, O., Mugnier, Laurent, Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, Cyril, Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J.-F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Rickman, E., 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 Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Max-Planck-Institut, Department of Biochemistry and Molecular Biology, Mayo Clinic, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Max Planck Institute for Radio Astronomy, University of Michigan [Ann Arbor], University of Michigan System, Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Pixyl Medical [Grenoble], Max Planck Institute for Astronomy (MPIA), University of Edinburgh, Center for Space and Habitability (CSH), University of Bern, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Centre d'Etudes pour le Développement des Territoires et l'Environnement (CEDETE), Université d'Orléans (UO), Laboratoire Hubert Curien [Saint Etienne] (LHC), Institut d'Optique Graduate School (IOGS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Biomécanique et Mécanique des Chocs (LBMC UMR T9406 ), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Université Gustave Eiffel, Laboratoire des Sciences de l'Ingénieur pour l'Environnement - UMR 7356 (LaSIE), La Rochelle Université (ULR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), CHU Tenon [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), Département Médico-Universitaire APPROCHES, Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), CHU Pitié-Salpêtrière [AP-HP], Laboratoire Hippolyte Fizeau (FIZEAU), INAF - Osservatorio Astronomico di Capodimonte (OAC), Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen], European Southern Observatory (ESO), Environnements et Paléoenvironnements OCéaniques (EPOC), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Catania (OACT), NASA Goddard Space Flight Center (GSFC), Centre Hospitalier Henri Duffaut (Avignon), This work is supported by the French National Research Agency in the framework of the Investissements d’Avenir program (ANR-15-IDEX-02), through the funding of the 'Origin of Life' project of the Univ. Grenoble-Alpes. This work is jointly supported by the French National Programms (PNP and PNPS) and by the Action Spécifique Haute Résolution Angulaire (ASHRA) of CNRS/INSU co-funded by CNES.AV acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 757561). A.-M.L. acknowledges funding from French National Research Agency (GIPSE project). C.P. acknowledges financial support from Fondecyt (grant 3190691) and financial support from the ICM (Iniciativa Científica Milenio) via the Núcleo Milenio de Formación Planetaria grant, from the Universidad de Valparaíso. T.H. acknowledges support from the European Research Council under the Horizon 2020 Framework Program via the ERC Advanced Grant Origins 83 24 28., ANR-15-IDEX-0002,UGA,IDEX UGA(2015), Sciences, EDP, and IDEX UGA - - UGA2015 - ANR-15-IDEX-0002 - IDEX - VALID
Subjects: planets and satellites: detection, methods: statistical, instrumentation: high angular resolution, planets and satellites: formation, techniques: image processing, methods: observational, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Context. In recent decades, direct imaging has confirmed the existence of substellar companions (exoplanets or brown dwarfs) on wide orbits (>10 au) around their host stars. In striving to understand their formation and evolution mechanisms, in 2015 we initiated the SPHERE infrared survey for exoplanets (SHINE), a systematic direct imaging survey of young, nearby stars that is targeted at exploring their demographics.Aims. We aim to detect and characterize the population of giant planets and brown dwarfs beyond the snow line around young, nearby stars. Combined with the survey completeness, our observations offer the opportunity to constrain the statistical properties (occurrence, mass and orbital distributions, dependency on the stellar mass) of these young giant planets.Methods. In this study, we present the observing and data analysis strategy, the ranking process of the detected candidates, and the survey performances for a subsample of 150 stars that are representative of the full SHINE sample. Observations were conducted in a homogeneous way between February 2015 and February 2017 with the dedicated ground-based VLT/SPHERE instrument equipped with the IFS integral field spectrograph and the IRDIS dual-band imager, covering a spectral range between 0.9 and 2.3 μm. We used coronographic, angular, and spectral differential imaging techniques to achieve the best detection performances for this study, down to the planetary mass regime.Results. We processed, in a uniform manner, more than 300 SHINE observations and datasets to assess the survey typical sensitivity as a function of the host star and of the observing conditions. The median detection performance reached 5σ-contrasts of 13 mag at 200 mas and 14.2 mag at 800 mas with the IFS (YJ and YJH bands), and of 11.8 mag at 200 mas, 13.1 mag at 800 mas, and 15.8 mag at 3 as with IRDIS in H band, delivering one of the deepest sensitivity surveys thus far for young, nearby stars. A total of sixteen substellar companions were imaged in this first part of SHINE: seven brown dwarf companions and ten planetary-mass companions.These include two new discoveries, HIP 65426 b and HIP 64892 B, but not the planets around PDS70 that had not been originally selected for the SHINE core sample. A total of 1483 candidates were detected, mainly in the large field of view that characterizes IRDIS. The color-magnitude diagrams, low-resolution spectrum (when available with IFS), and follow-up observations enabled us to identify the nature (background contaminant or comoving companion) of about 86% of our subsample. The remaining cases are often connected to crowded-field follow-up observations that were missing. Finally, even though SHINE was not initially designed for disk searches, we imaged twelve circumstellar disks, including three new detections around the HIP 73145, HIP 86598, and HD 106906 systems.Conclusions. Nowadays, direct imaging provides a unique opportunity to probe the outer part of exoplanetary systems beyond 10 au to explore planetary architectures, as highlighted by the discoveries of: one new exoplanet, one new brown dwarf companion, and three new debris disks during this early phase of SHINE. It also offers the opportunity to explore and revisit the physical and orbital properties of these young, giant planets and brown dwarf companions (relative position, photometry, and low-resolution spectrum in near-infrared, predicted masses, and contrast in order to search for additional companions). Finally, these results highlight the importance of finalizing the SHINE systematic observation of about 500 young, nearby stars for a full exploration of their outer part to explore the demographics of young giant planets beyond 10 au and to identify the most interesting systems for the next generation of high-contrast imagers on very large and extremely large telescopes.
Published: 2021

156. The SPHERE infrared survey for exoplanets (SHINE)

Author: Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G.-D., Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Le Coroller, H., Maire, A.-L., Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A.-M., Langlois, M., Bonnefoy, M., Beuzit, J.-L., Boccaletti, A., D��Orazi, V., Delorme, P., Dominik, C., Henning, Th., Janson, M., Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., M��ller, A., Perrot, C., Samland, M., Schmid, H. M., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A. J., Brown Sevilla, S., Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulb��, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J. H., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., M��ller-Nilsson, O., Mouillet, D., Moulin, T., Orign��, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E. L., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J.-F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., Wildi, F., 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, 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: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 530 Physics, 520 Astronomy, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 620 Engineering, Astrophysics::Galaxy Astrophysics
Abstract: International audience; The SpHere INfrared Exoplanet (SHINE) project is a 500-star survey performed with SPHERE on the Very Large Telescope for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. Here we present an initial statistical analysis for a subsample of 150 stars spanning spectral types from B to M that are representative of the full SHINE sample. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 M Jup and semimajor axes between 5 and 300 au. For this purpose, we adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Based on the results obtained for each star and on the 13 detections in the sample, we use a Markov chain Monte Carlo tool to compare our observations to two different types of models. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are 23.0 −9.7 +13.5 , 5.8 −2.8 +4.7 , and 12.6 −7.1 +12.9 % for BA, FGK, and M stars, respectively. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1–75 M Jup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using our population model and restricting our sample to FGK stars, we derive a frequency of 5.7 −2.8 +3.8 %, consistent with predictions from the parametric model. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies.
Published: 2021

157. The SPHERE infrared survey for exoplanets (SHINE)

Author: Desidera, S., Chauvin, G., Bonavita, M., Messina, S., LeCoroller, H., Schmidt, T., Gratton, R., Lazzoni, C., Meyer, M., Schlieder, J., Cheetham, A., Hagelberg, J., Bonnefoy, M., Feldt, M., Lagrange, A.-M., Langlois, M., Vigan, A., Tan, T. G., Hambsch, F.-J., Millward, M., Alcalá, J., Benatti, S., Brandner, W., Carson, J., Covino, E., Delorme, P., D’Orazi, V., Janson, M., Rigliaco, E., Beuzit, J.-L., Biller, B., Boccaletti, A., Dominik, C., Cantalloube, F., Fontanive, C., Galicher, R., Henning, Th., Lagadec, E., Ligi, R., Maire, A.-L., Menard, F., Mesa, D., Müller, A., Samland, M., Schmid, H. M., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Asensio-Torres, R., Kopytova, T., Rickman, E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbé, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J.-F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU]Sciences of the Universe [physics], 530 Physics, 520 Astronomy, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: International audience; Context. Large surveys with new-generation high-contrast imaging instruments are needed to derive the frequency and properties of exoplanet populations with separations from ~5 to 300 au. A careful assessment of the stellar properties is crucial for a proper understanding of when, where, and how frequently planets form, and how they evolve. The sensitivity of detection limits to stellar age makes this a key parameter for direct imaging surveys. Aims. We describe the SpHere INfrared survey for Exoplanets (SHINE), the largest direct imaging planet-search campaign initiated at the VLT in 2015 in the context of the SPHERE Guaranteed Time Observations of the SPHERE consortium. In this first paper we present the selection and the properties of the complete sample of stars surveyed with SHINE, focusing on the targets observed during the first phase of the survey (from February 2015 to February 2017). This early sample composed of 150 stars is used to perform a preliminary statistical analysis of the SHINE data, deferred to two companion papers presenting the survey performance, main discoveries, and the preliminary statistical constraints set by SHINE. Methods. Based on a large database collecting the stellar properties of all young nearby stars in the solar vicinity (including kinematics, membership to moving groups, isochrones, lithium abundance, rotation, and activity), we selected the original sample of 800 stars that were ranked in order of priority according to their sensitivity for planet detection in direct imaging with SPHERE. The properties of the stars that are part of the early statistical sample wererevisited, including for instance measurements from the Gaia Data Release 2. Rotation periods were derived for the vast majority of the late-type objects exploiting TESS light curves and dedicated photometric observations. Results. The properties of individual targets and of the sample as a whole are presented.
Published: 2021

158. A multiwavelength analysis of the spiral arms in the protoplanetary disk around WaOph 6

Author: Brown-Sevilla, S. B., primary, Keppler, M., additional, Barraza-Alfaro, M., additional, Melon Fuksman, J. D., additional, Kurtovic, N., additional, Pinilla, P., additional, Feldt, M., additional, Brandner, W., additional, Ginski, C., additional, Henning, Th., additional, Klahr, H., additional, Asensio-Torres, R., additional, Cantalloube, F., additional, Garufi, A., additional, van Holstein, R. G., additional, Langlois, M., additional, Ménard, F., additional, Rickman, E., additional, Benisty, M., additional, Chauvin, G., additional, Zurlo, A., additional, Weber, P., additional, Pavlov, A., additional, Ramos, J., additional, Rochat, S., additional, and Roelfsema, R., additional
Published: 2021
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159. Revealing asymmetrical dust distribution in the inner regions of HD 141569

Author: Singh, G., primary, Bhowmik, T., additional, Boccaletti, A., additional, Thébault, P., additional, Kral, Q., additional, Milli, J., additional, Mazoyer, J., additional, Pantin, E., additional, van Holstein, R. G., additional, Olofsson, J., additional, Boukrouche, R., additional, Di Folco, E., additional, Janson, M., additional, Langlois, M., additional, Maire, A.-L., additional, Vigan, A., additional, Benisty, M., additional, Augereau, J.-C., additional, Perrot, C., additional, Gratton, R., additional, Henning, T., additional, Ménard, F., additional, Rickman, E., additional, Wahhaj, Z., additional, Zurlo, A., additional, Biller, B., additional, Bonnefoy, M., additional, Chauvin, G., additional, Delorme, P., additional, Desidera, S., additional, D’Orazi, V., additional, Feldt, M., additional, Hagelberg, J., additional, Keppler, M., additional, Kopytova, T., additional, Lagadec, E., additional, Lagrange, A.-M., additional, Mesa, D., additional, Meyer, M., additional, Rouan, D., additional, Sissa, E., additional, Schmidt, T. O. B., additional, Jaquet, M., additional, Fusco, T., additional, Pavlov, A., additional, and Rabou, P., additional
Published: 2021
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160. Investigating point sources in MWC 758 with SPHERE

Author: Boccaletti, A., primary, Pantin, E., additional, Ménard, F., additional, Galicher, R., additional, Langlois, M., additional, Benisty, M., additional, Gratton, R., additional, Chauvin, G., additional, Ginski, C., additional, Lagrange, A.-M., additional, Zurlo, A., additional, Biller, B., additional, Bonavita, M., additional, Bonnefoy, M., additional, Brown-Sevilla, S., additional, Cantalloube, F., additional, Desidera, S., additional, D’Orazi, V., additional, Feldt, M., additional, Hagelberg, J., additional, Lazzoni, C., additional, Mesa, D., additional, Meyer, M., additional, Perrot, C., additional, Vigan, A., additional, Sauvage, J.-F., additional, Ramos, J., additional, Rousset, G., additional, and Magnard, Y., additional
Published: 2021
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161. Perturbers: SPHERE detection limits to planetary-mass companions in protoplanetary disks

Author: Asensio-Torres, R., primary, Henning, Th., additional, Cantalloube, F., additional, Pinilla, P., additional, Mesa, D., additional, Garufi, A., additional, Jorquera, S., additional, Gratton, R., additional, Chauvin, G., additional, Szulágyi, J., additional, van Boekel, R., additional, Dong, R., additional, Marleau, G.-D., additional, Benisty, M., additional, Villenave, M., additional, Bergez-Casalou, C., additional, Desgrange, C., additional, Janson, M., additional, Keppler, M., additional, Langlois, M., additional, Ménard, F., additional, Rickman, E., additional, Stolker, T., additional, Feldt, M., additional, Fusco, T., additional, Gluck, L., additional, Pavlov, A., additional, and Ramos, J., additional
Published: 2021
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162. METIS: The Mid-infrared ELT Imager and Spectrograph

Author: Brandl, B.R., Bettonvil, F.C.M., Boekel, R. van, Glauser, A., Quanz, S., Absil, O., Amorim, A., Feldt, M., Glasse, A., Güdel, M., Ho, P., Labadie, L., Meyer, M., Pantin, E., Winckel, H. van, and METIS Consortium
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The Mid-infrared ELT Imager and Spectrograph (METIS) will provide the Extremely Large Telescope (ELT) with a unique window to the thermal- and mid-infrared (3 - 13 microns). Its single-conjugate adaptive optics (SCAO) system will enable high contrast imaging and integral field unit (IFU) spectroscopy (R~100,000) at the diffraction limit of the ELT. This article describes the science drivers, conceptual design, observing modes, and expected performance of METIS., 5 pages, 3 figures, published in the ESO Messenger
Published: 2021

163. The Structure of Pre-Transitional Protoplanetary Disks. II Azimuthal Asymmetries, Different Radial Distributions of Large and Small Dust Grains in PDS 70

Author: Hashimoto, J, Tsukagoshi, T, Brown, J. M, Dong, R, Muto, T, Zhu, Z, Wisniewski, J, Ohashi, N, Kudo, T, Kusakabe, N, Abe, L, Akiyama, E, Brandner, W, Brandt, T, Carson J, Currie, T, Egner, S, Feldt, M, Grady, Carol A, Guyon, O, Hayano, Y, Hayashi, M, Hayashi, S, Henning, T, Hodapp, K, Ishii, M, Iye, M, Janson, M, Kandori, R, Knapp, G, Kuzuhara, M, Kwon, J, Matsuo, T, McElwain, M. W, and Mayama, S
Subjects: 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-micron 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 Submillimeter Array observations of the dust continuum at 1.3 mm and CO-12 J = 2 yields 1 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 approx. 65 AU at NIR wavelengths. However, we found a larger gap in the disk with a radius of approx. 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.
Published: 2015
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164. The SPHERE Infrared Survey for Exoplanets (SHINE): II. Observations, Data Reduction and Analysis, Detection Performances, and Initial Results

Author: Langlois, M., Gratton, R., Lagrange, A. -M., Delorme, P., Boccaletti, A., Bonnefoy, M., Maire, A. -L., Mesa, D., Chauvin, G., Desidera, S., Vigan, A., Cheetham, A., Hagelberg, J., Feldt, M., Meyer, M., Rubini, P., Le, Coroller, H., Cantalloube, F., Biller, B., Bonavita, M., Bhowmik, T., Brandner, W., Daemgen, S., D'Orazi, V., Flasseur, O., Fontanive, C., Galicher, R., Girard, J., Janin-Potiron, P., Janson, M., Keppler, M., Kopytova, T., Lagadec, E., Lannier, J., Lazzoni, C., Ligi, R., Meunier, N., Perreti, A., Perrot, C., Rodet, L., Romero, C., Rouan, D., Samland, M., Salter, G., Sissa, E., Schmidt, T., Zurlo, A., Mouillet, D., Denis, L., Thiébaut, E., Milli, J., Wahhaj, Z., Beuzit, J. -L., Dominik, C., Henning, T., Ménard, F., Müller, A., Schmid, H. M., Turatto, M., Udry, S., Abe, L., Antichi, J., Allard, F., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbé, A., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Messina, S., Möller-Nilsson, O., Mugnier, L., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., and Rickman, E.
Subjects: STATISTICAL [METHODS], IMAGING TECHNIQUES, INFRARED DEVICES, FORMATION [PLANETS AND SATELLITES], DETECTION PERFORMANCE, IMAGE PROCESSING [TECHNIQUES], EXTREMELY LARGE TELESCOPES, COLOR MAGNITUDE DIAGRAMS, ANALYSIS STRATEGIES, FORMATION AND EVOLUTIONS, SEARCH ENGINES, OBSERVATIONAL [METHODS], STATISTICAL PROPERTIES, HIGH ANGULAR RESOLUTION [INSTRUMENTATION], DETECTION [PLANETS AND SATELLITES], ORBITS, LARGE FIELD OF VIEWS, POPULATION STATISTICS, SURVEYS, INTEGRAL FIELD SPECTROGRAPH, STARS, EXTRASOLAR PLANETS
Abstract: Context. In recent decades, direct imaging has confirmed the existence of substellar companions (exoplanets or brown dwarfs) on wide orbits (>10 au) around their host stars. In striving to understand their formation and evolution mechanisms, in 2015 we initiated the SPHERE infrared survey for exoplanets (SHINE), a systematic direct imaging survey of young, nearby stars that is targeted at exploring their demographics. Aims. We aim to detect and characterize the population of giant planets and brown dwarfs beyond the snow line around young, nearby stars. Combined with the survey completeness, our observations offer the opportunity to constrain the statistical properties (occurrence, mass and orbital distributions, dependency on the stellar mass) of these young giant planets. Methods. In this study, we present the observing and data analysis strategy, the ranking process of the detected candidates, and the survey performances for a subsample of 150 stars that are representative of the full SHINE sample. Observations were conducted in a homogeneous way between February 2015 and February 2017 with the dedicated ground-based VLT/SPHERE instrument equipped with the IFS integral field spectrograph and the IRDIS dual-band imager, covering a spectral range between 0.9 and 2.3 μm. We used coronographic, angular, and spectral differential imaging techniques to achieve the best detection performances for this study, down to the planetary mass regime. Results. We processed, in a uniform manner, more than 300 SHINE observations and datasets to assess the survey typical sensitivity as a function of the host star and of the observing conditions. The median detection performance reached 5σ-contrasts of 13 mag at 200 mas and 14.2 mag at 800 mas with the IFS (YJ and YJH bands), and of 11.8 mag at 200 mas, 13.1 mag at 800 mas, and 15.8 mag at 3 as with IRDIS in H band, delivering one of the deepest sensitivity surveys thus far for young, nearby stars. A total of sixteen substellar companions were imaged in this first part of SHINE: seven brown dwarf companions and ten planetary-mass companions.These include two new discoveries, HIP 65426 b and HIP 64892 B, but not the planets around PDS70 that had not been originally selected for the SHINE core sample. A total of 1483 candidates were detected, mainly in the large field of view that characterizes IRDIS. The color-magnitude diagrams, low-resolution spectrum (when available with IFS), and follow-up observations enabled us to identify the nature (background contaminant or comoving companion) of about 86% of our subsample. The remaining cases are often connected to crowded-field follow-up observations that were missing. Finally, even though SHINE was not initially designed for disk searches, we imaged twelve circumstellar disks, including three new detections around the HIP 73145, HIP 86598, and HD 106906 systems. Conclusions. Nowadays, direct imaging provides a unique opportunity to probe the outer part of exoplanetary systems beyond 10 au to explore planetary architectures, as highlighted by the discoveries of: one new exoplanet, one new brown dwarf companion, and three new debris disks during this early phase of SHINE. It also offers the opportunity to explore and revisit the physical and orbital properties of these young, giant planets and brown dwarf companions (relative position, photometry, and low-resolution spectrum in near-infrared, predicted masses, and contrast in order to search for additional companions). Finally, these results highlight the importance of finalizing the SHINE systematic observation of about 500 young, nearby stars for a full exploration of their outer part to explore the demographics of young giant planets beyond 10 au and to identify the most interesting systems for the next generation of high-contrast imagers on very large and extremely large telescopes. © M. Langlois et al. 2021. SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF – Osservatorio di Padova (Italy), Observatoire de Genève (Switzerland), ETH Zürich (Switzerland), NOVA (Netherlands), ONERA (France) and ASTRON (Netherlands) in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland) and NOVA (Netherlands). SPHERE also received funding from the European CommissionSixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004-2008), grant number 226604 for FP7 (2009-2012) and grant number 312430 for FP7 (2013-2016). This paper is based on observations collected at the European Southern Observatory under ESO programmes 198.C-0209, 097.C-0865, 095.C-0298, 095.C-0309,096.C-0241. This work has made use of the SPHERE Data Centre, jointly operated by OSUG/IPAG (Grenoble), PYTHEAS/LAM/CeSAM (Marseille), OCA/Lagrange (Nice), Observatoire de Paris/LESIA (Paris), and Observatoire de Lyon (OSUL/CRAL). This work is supported by the French National Research Agency in the framework of the Investissements d’Avenir program (ANR-15-IDEX-02), through the funding of the “Origin of Life” project of the Univ. Grenoble-Alpes. This work is jointly supported by the French National Programms (PNP and PNPS) and by the Action Spécifique Haute Résolution Angulaire (ASHRA) of CNRS/INSU co-funded by CNES. We also thank the anonymous referee for her/his careful reading of the manuscript as well as her/his insightful comments and suggestions. AV acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 757561). A.-M.L. acknowledges funding from French National Research Agency (GIPSE project). C.P. acknowledges financial support from Fondecyt (grant 3190691) and financial support from the ICM (Iniciativa Científica Milenio) via the Núcleo Milenio de Formación Planetaria grant, from the Universidad de Valparaíso. T.H. acknowledges support from the European Research Council under the Horizon 2020 Framework Program via the ERC Advanced Grant Origins 832428.
Published: 2021

165. METIS: The Mid-infrared ELT Imager and Spectrograph

Author: Brandl, B.R. (author), Bettonvil, F. (author), van Boekel, R. (author), Glauser, A. (author), Quanz, S. (author), Absil, O. (author), Amorim, A. (author), Feldt, M. (author), Ho, P. (author), Meyer, M. (author), Brandl, B.R. (author), Bettonvil, F. (author), van Boekel, R. (author), Glauser, A. (author), Quanz, S. (author), Absil, O. (author), Amorim, A. (author), Feldt, M. (author), Ho, P. (author), and Meyer, M. (author)
Abstract: The Mid-infrared ELT Imager and Spectrograph (METIS) will provide the Extremely Large Telescope (ELT) with a unique window to the thermal- and mid-infrared (3–13 µm). Its single-conjugate adaptive optics (SCAO) system will enable high contrast imaging and integral field unit (IFU) spectroscopy (R ~ 100 000) at the diffraction limit of the ELT. This article describes the science drivers, conceptual design, observing modes, and expected performance of METIS., Astrodynamics & Space Missions
Published: 2021
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166. The SPHERE infrared survey for exoplanets (SHINE) : III. The demographics of young giant exoplanets below 300 au with SPHERE

Author: Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G-D, Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Le Coroller, H., Maire, A-L, Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A-M, Langlois, M., Bonnefoy, M., Beuzit, J-L, Boccaletti, A., D'Orazi, V, Delorme, P., Dominik, C., Henning, Th, Janson, Markus, Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., Muller, A., Perrot, C., Samland, Matthias, Schmid, H. M., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A. J., Sevilla, S. Brown, Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V, Delboulbe, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J. H., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Moller-Nilsson, O., Mouillet, D., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E. L., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J-F, Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., Wildi, F., Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G-D, Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Le Coroller, H., Maire, A-L, Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A-M, Langlois, M., Bonnefoy, M., Beuzit, J-L, Boccaletti, A., D'Orazi, V, Delorme, P., Dominik, C., Henning, Th, Janson, Markus, Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., Muller, A., Perrot, C., Samland, Matthias, Schmid, H. M., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A. J., Sevilla, S. Brown, Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V, Delboulbe, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J. H., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Moller-Nilsson, O., Mouillet, D., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E. L., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J-F, Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., and Wildi, F.
Abstract: The SpHere INfrared Exoplanet (SHINE) project is a 500-star survey performed with SPHERE on the Very Large Telescope for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. Here we present an initial statistical analysis for a subsample of 150 stars spanning spectral types from B to M that are representative of the full SHINE sample. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 MJup and semimajor axes between 5 and 300 au. For this purpose, we adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Based on the results obtained for each star and on the 13 detections in the sample, we use a Markov chain Monte Carlo tool to compare our observations to two different types of models. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are 23.0−9.7+13.5, 5.8−2.8+4.7, and 12.6−7.1+12.9% for BA, FGK, and M stars, respectively. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1–75 MJup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using our population model and restricting our sample to FGK stars, we derive a frequency of 5.7−2.8+3.8%, consistent with predictions from the parametric model. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies.
Published: 2021
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167. Revealing asymmetrical dust distribution in the inner regions of HD 141569

Author: Singh, G., Bhowmik, T., Boccaletti, A., Thebault, P., Kral, Q., Milli, J., Mazoyer, J., Pantin, E., van Holstein, R. G., Olofsson, J., Boukrouche, R., Di Folco, E., Janson, Markus, Langlois, M., Maire, A.-L., Vigan, A., Benisty, M., Augereau, J.-C., Perrot, C., Gratton, R., Henning, T., Menard, F., Rickman, E., Wahhaj, Z., Zurlo, A., Biller, B., Bonnefoy, M., Chauvin, G., Delorme, P., Desidera, S., D'Orazi, V., Feldt, M., Hagelberg, J., Keppler, M., Kopytova, T., Lagadec, E., Lagrange, A.-M., Mesa, D., Meyer, M., Rouan, D., Sissa, E., Schmidt, T. O. B., Jaquet, M., Fusco, T., Pavlov, A., Rabou, P., Singh, G., Bhowmik, T., Boccaletti, A., Thebault, P., Kral, Q., Milli, J., Mazoyer, J., Pantin, E., van Holstein, R. G., Olofsson, J., Boukrouche, R., Di Folco, E., Janson, Markus, Langlois, M., Maire, A.-L., Vigan, A., Benisty, M., Augereau, J.-C., Perrot, C., Gratton, R., Henning, T., Menard, F., Rickman, E., Wahhaj, Z., Zurlo, A., Biller, B., Bonnefoy, M., Chauvin, G., Delorme, P., Desidera, S., D'Orazi, V., Feldt, M., Hagelberg, J., Keppler, M., Kopytova, T., Lagadec, E., Lagrange, A.-M., Mesa, D., Meyer, M., Rouan, D., Sissa, E., Schmidt, T. O. B., Jaquet, M., Fusco, T., Pavlov, A., and Rabou, P.
Abstract: Context. The combination of high-contrast imaging with spectroscopy and polarimetry offers a pathway to studying the grain distribution and properties of debris disks in exquisite detail. Here, we focus on the case of a gas-rich debris disk around HD 141569A, which features a multiple-ring morphology first identified with SPHERE in the near-infrared. Aims. We obtained polarimetric differential imaging with SPHERE in the H-band to compare the scattering properties of the innermost ring at 44 au with former observations in total intensity with the same instrument. In polarimetric imaging, we observed that the intensity of the ring peaks in the south-east, mostly in the forward direction, whereas in total intensity imaging, the ring is detected only at the south. This noticeable characteristic suggests a non-uniform dust density in the ring. With these two sets of images, we aim to study the distribution of the dust to solve for the actual dust distribution. Methods. We implemented a density function varying azimuthally along the ring and generated synthetic images both in polarimetry and in total intensity, which are then compared to the actual data. The search for the best-fit model was performed both with a grid-based and an MCMC approach. Using the outcome of this modelization, we further measured the polarized scattering phase function for the observed scattering angle between 33 degrees and 147 degrees as well as the spectral reflectance of the southern part of the ring between 0.98 and 2.1 mu m. We tentatively derived the grain properties by comparing these quantities with MCFOST models and assuming Mie scattering. Results. We find that the dust density peaks in the south-west at an azimuthal angle of 220 degrees similar to 238 degrees with a rather broad width of 61 degrees similar to 127 degrees. The difference in the intensity distributions observed in polarimetry and total intensity is the result of this particular morphology. Although there are still uncert
Published: 2021
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168. Limits on the presence of planets in systems with debris discs : HD92945 and HD107146

Author: Mesa, D., Marino, S., Bonavita, M., Lazzoni, C., Fontanive, C., Pérez, S., D'Orazi, V, Desidera, S., Gratton, R., Engler, N., Henning, T., Janson, Markus, Kral, Q., Langlois, M., Messina, S., Milli, J., Pawellek, N., Perrot, C., Rigliaco, E., Rickman, E., Squicciarini, V, Vigan, A., Wahhaj, Z., Zurlo, A., Boccaletti, A., Bonnefoy, M., Chauvin, G., De Caprio, V, Feldt, M., Gluck, L., Hagelberg, J., Keppler, M., Lagrange, A-M, Launhardt, R., Maire, A-L, Meyer, M., Moeller-Nilsson, O., Pavlov, A., Samland, Matthias, Schmidt, T., Weber, L., Mesa, D., Marino, S., Bonavita, M., Lazzoni, C., Fontanive, C., Pérez, S., D'Orazi, V, Desidera, S., Gratton, R., Engler, N., Henning, T., Janson, Markus, Kral, Q., Langlois, M., Messina, S., Milli, J., Pawellek, N., Perrot, C., Rigliaco, E., Rickman, E., Squicciarini, V, Vigan, A., Wahhaj, Z., Zurlo, A., Boccaletti, A., Bonnefoy, M., Chauvin, G., De Caprio, V, Feldt, M., Gluck, L., Hagelberg, J., Keppler, M., Lagrange, A-M, Launhardt, R., Maire, A-L, Meyer, M., Moeller-Nilsson, O., Pavlov, A., Samland, Matthias, Schmidt, T., and Weber, L.
Abstract: Recent observations of resolved cold debris discs at tens of au have revealed that gaps could be a common feature in these Kuiper-belt analogues. Such gaps could be evidence for the presence of planets within the gaps or closer in near the edges of the disc. We present SPHERE observations of HD 92945 and HD 107146, two systems with detected gaps. We constrained the mass of possible companions responsible for the gap to 1–2 MJup for planets located inside the gap and to less than 5 MJup for separations down to 20 au from the host star. These limits allow us to exclude some of the possible configurations of the planetary systems proposed to explain the shape of the discs around these two stars. In order to put tighter limits on the mass at very short separations from the star, where direct-imaging data are less effective, we also combined our data with astrometric measurements from Hipparcos and Gaia and radial-velocity measurements. We were able to limit the separation and the mass of the companion potentially responsible for the proper-motion anomaly of HD 107146 to values of 2–7 au and 2–5 MJup, respectively.
Published: 2021
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169. SPHERE+: Imaging young Jupiters down to the snowline

Author: Augereau, J. -C., Baudino, J. -L., Beuzit, J. -L., Bouret, J. -C., Desert, J. -M., Delisle, J. -B., Orazi, V. D, Gonzalez, J. -F., Lagrange, A. -M., Coroller, H. Le, Arena, G. Muro, Diaye, M. N, Sauvage, J. -F., Schmid, H. -M., Boccaletti, A., Chauvin, G., Mouillet, D., Absil, O., Allard, F., Antoniucci, S., Augereau, J.-C, Barge, P., Baruffolo, A., Baudino, J.-L, Baudoz, P., Beaulieu, M., Benisty, M., Beuzit, J.-L, Bianco, A., Biller, B., Bonavita, B., Bonnefoy, M., Bos, S., Bouret, J.-C, Brandner, W., Buchschache, N., Carry, B., Cantalloube, F., Cascone, E., Carlotti, A., Charnay, B., Chiavassa, A., Choquet, E., Clenet, Y., Crida, A., De Boer, J., De Caprio, V., Desidera, S., Desert, J.-M, Delisle, J.-B, Delorme, P., Dohlen, K., Doelman, D., Dominik, C., D'orazi, V, Dougados, C., Douté, S., Fedele, D., Feldt, M., Ferreira, F., Fontanive, C., Fusco, T., Galicher, R., Garufi, A., Gendron, E., Ghedina, A., Ginski, C., Gonzalez, J.-F, Gratadour, D., Gratton, R., Guillot, T., Haffert, S., Hagelberg, J., Henning, T., Huby, E., Janson, M., Kamp, I., Keller, C. U., Kenworthy, M., Kervella, P., Kral, Q., Kuhn, J., Lagadec, E., Laibe, G., Langlois, M., Lagrange, A.-M, Launhardt, R., Leboulleux, L., Le Coroller, H, Causi, G. Li, Loupias, M., Maire, A. L., Marleau, G., Martinache, F., Martinez, P., Mary, D., Mattioli, M., Mazoyer, J., Meheut, H., Ménard, F., Mesa, D., Meunier, N., Miguel, Y., Milli, J., Min, M., Molliere, P., Mordasini, C., Moretto, G., Mugnier, L., Muro Arena, G, Nardetto, N., N'Diaye, M, Nesvadba, N., Pedichini, F., Pinilla, P., Por, E., Potier, A., Quanz, S., Rameau, J., Roelfsema, R., Rouan, D., Rigliaco, E., Salasnich, B., Samland, M., Sauvage, J.-F, Schmid, H.-M, Segransan, D., Snellen, I., Snik, F., Soulez, F., Stadler, E., Stam, D., Tallon, M., Thebault, P., Thiebaut, E., Tschudi, C., Udry, S., van Holstein, R., Vernazza, P, Vidal, F., Vigan, A., Waters, R., Wildi, F., Willson, M., Zanutta, A., Zavagno, Annie, Zurlo, A., 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), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Cte d’Azur, 96 Boulevard de l’Observatoire, Nice, 06300, France, Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Département de Recherche sur la Fusion Contrôlée (DRFC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), 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), 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, Department of Biochemistry and Molecular Biology, Mayo Clinic, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Université Côte d'Azur (UCA), University of Arizona, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), NOVA Optical Infrared Instrumentation Group, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), 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), SRON Netherlands Institute for Space Research (SRON), Croissance et propriétés de systèmes hybrides en couches minces (INSP-E8), Institut des Nanosciences de Paris (INSP), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Unité de recherche d'Économie et Sociologie Rurales (ESR), Institut National de la Recherche Agronomique (INRA), INAF - Osservatorio Astronomico di Roma (OAR), Universität Greifswald - University of Greifswald, European Southern Observatory [Santiago] (ESO), Immunopathologie et chimie thérapeutique (ICT), Institut de biologie moléculaire et cellulaire (IBMC), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, INAF - Osservatorio Astronomico di Capodimonte (OAC), Hôpital Cochin [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), DOTA, ONERA, Université Paris Saclay [Palaiseau], Department of Astronomy, Stockholm University, Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-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), Sterrewacht Leiden, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), 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, 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université 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), Centre National de la Recherche Scientifique (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)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), 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), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Universiteit Leiden
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: SPHERE (Beuzit et al,. 2019) has now been in operation at the VLT for more than 5 years, demonstrating a high level of performance. SPHERE has produced outstanding results using a variety of operating modes, primarily in the field of direct imaging of exoplanetary systems, focusing on exoplanets as point sources and circumstellar disks as extended objects. The achievements obtained thus far with SPHERE (~200 refereed publications) in different areas (exoplanets, disks, solar system, stellar physics...) have motivated a large consortium to propose an even more ambitious set of science cases, and its corresponding technical implementation in the form of an upgrade. The SPHERE+ project capitalizes on the expertise and lessons learned from SPHERE to push high contrast imaging performance to its limits on the VLT 8m-telescope. The scientific program of SPHERE+ described in this document will open a new and compelling scientific window for the upcoming decade in strong synergy with ground-based facilities (VLT/I, ELT, ALMA, and SKA) and space missions (Gaia, JWST, PLATO and WFIRST). While SPHERE has sampled the outer parts of planetary systems beyond a few tens of AU, SPHERE+ will dig into the inner regions around stars to reveal and characterize by mean of spectroscopy the giant planet population down to the snow line. Building on SPHERE's scientific heritage and resounding success, SPHERE+ will be a dedicated survey instrument which will strengthen the leadership of ESO and the European community in the very competitive field of direct imaging of exoplanetary systems. With enhanced capabilities, it will enable an even broader diversity of science cases including the study of the solar system, the birth and death of stars and the exploration of the inner regions of active galactic nuclei., White paper submitted to ESO on Feb. 20th, 2020
Published: 2020

170. Limits on the presence of planets in systems with debris discs: HD 92945 and HD 107146

Author: Mesa, D, primary, Marino, S, additional, Bonavita, M, additional, Lazzoni, C, additional, Fontanive, C, additional, Pérez, S, additional, D’Orazi, V, additional, Desidera, S, additional, Gratton, R, additional, Engler, N, additional, Henning, T, additional, Janson, M, additional, Kral, Q, additional, Langlois, M, additional, Messina, S, additional, Milli, J, additional, Pawellek, N, additional, Perrot, C, additional, Rigliaco, E, additional, Rickman, E, additional, Squicciarini, V, additional, Vigan, A, additional, Wahhaj, Z, additional, Zurlo, A, additional, Boccaletti, A, additional, Bonnefoy, M, additional, Chauvin, G, additional, De Caprio, V, additional, Feldt, M, additional, Gluck, L, additional, Hagelberg, J, additional, Keppler, M, additional, Lagrange, A-M, additional, Launhardt, R, additional, Maire, A-L, additional, Meyer, M, additional, Moeller-Nilsson, O, additional, Pavlov, A, additional, Samland, M, additional, Schmidt, T, additional, and Weber, L, additional
Published: 2021
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171. Investigating three Sirius-like systems with SPHERE

Author: Gratton, R., primary, D’Orazi, V., additional, Pacheco, T. A., additional, Zurlo, A., additional, Desidera, S., additional, Meléndez, J., additional, Mesa, D., additional, Claudi, R., additional, Janson, M., additional, Langlois, M., additional, Rickman, E., additional, Samland, M., additional, Moulin, T., additional, Soenke, C., additional, Cascone, E., additional, Ramos, J., additional, Rigal, F., additional, Avenhaus, H., additional, Beuzit, J. L., additional, Biller, B., additional, Boccaletti, A., additional, Bonavita, M., additional, Bonnefoy, M., additional, Brandner, W., additional, Chauvin, G., additional, Cudel, M., additional, Daemgen, S., additional, Delorme, P., additional, Desgrange, C., additional, Engler, N., additional, Feldt, M., additional, Fontanive, C., additional, Galicher, R., additional, Garufi, A., additional, Gasparri, D., additional, Ginski, C., additional, Girard, J., additional, Hagelberg, J., additional, Hunziker, S., additional, Kasper, M., additional, Keppler, M., additional, Lagrange, A.-M., additional, Lannier, J., additional, Lazzoni, C., additional, Le Coroller, H., additional, Ligi, R., additional, Lombart, M., additional, Maire, A.-L., additional, Mayer, M. R., additional, Mazevet, S., additional, Ménard, F., additional, Mouillet, D., additional, Perrot, C., additional, Peretti, S., additional, Petrus, S., additional, Potier, A., additional, Rouan, D., additional, Schmid, H. M., additional, Schmidt, T. O. B., additional, Sissa, E., additional, Stolker, T., additional, Salter, G., additional, Vigan, A., additional, and Wildi, F., additional
Published: 2021
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172. Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70

Author: Keppler, M, Benisty, M, Müller, A, Henning, T, Van Boekel, R, Cantalloube, F, Ginski, C, Van Holstein, RG, Maire, AL, Pohl, A, Samland, M, Avenhaus, H, Baudino, JL, Boccaletti, A, De Boer, J, Bonnefoy, M, Chauvin, G, Desidera, S, Langlois, M, Lazzoni, C, Marleau, GD, Mordasini, C, Pawellek, N, Stolker, T, Vigan, A, Zurlo, A, Birnstiel, T, Brandner, W, Feldt, M, Flock, M, Girard, J, Gratton, R, Hagelberg, J, Isella, A, Janson, M, Juhasz, A, Kemmer, J, Kral, Q, Lagrange, AM, Launhardt, R, Matter, A, Ménard, F, Milli, J, Mollière, P, Olofsson, J, Pérez, L, Pinilla, P, Pinte, C, Quanz, SP, Schmidt, T, Udry, S, Wahhaj, Z, Williams, JP, Buenzli, E, Cudel, M, Dominik, C, Galicher, R, Kasper, M, Lannier, J, Mesa, D, Mouillet, D, Peretti, S, Perrot, C, Salter, G, Sissa, E, Wildi, F, Abe, L, Antichi, J, Augereau, JC, Baruffolo, A, Baudoz, P, Bazzon, A, Beuzit, JL, Blanchard, P, Brems, SS, Buey, T, De Caprio, V, Carbillet, M, Carle, M, Cascone, E, Cheetham, A, Claudi, R, Costille, A, Delboulbé, A, Dohlen, K, Fantinel, D, Feautrier, P, Fusco, T, Giro, E, Gluck, L, Gry, C, Hubin, N, Hugot, E, Jaquet, M, Le Mignant, D, Llored, M, Madec, F, Magnard, Y, Martinez, P, Maurel, D, Pawellek, Nicole [0000-0002-9385-9820], and Apollo - University of Cambridge Repository
Subjects: planets and satellites: detection, stars: individual: PDS 70, radiative transfer, protoplanetary disks, scattering, Astrophysics::Solar and Stellar Astrophysics, techniques: high angular resolution, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Young circumstellar disks are of prime interest to understand the physical and chemical conditions under which planet formation takes place. Only very few detections of planet candidates within these disks exist, and most of them are currently suspected to be disk features. In this context, the transition disk around the young star PDS 70 is of particular interest, due to its large gap identified in previous observations, indicative of ongoing planet formation. We aim to search for the presence of planets and search for disk structures indicative for disk-planet interactions and other evolutionary processes. We analyse new and archival near-infrared (NIR) images of the transition disk PDS 70 obtained with the VLT/SPHERE, VLT/NaCo and Gemini/NICI instruments in polarimetric differential imaging (PDI) and angular differential imaging (ADI) modes. We detect a point source within the gap of the disk at about 195 mas (about 22 au) projected separation. The detection is confirmed at five different epochs, in three filter bands and using different instruments. The astrometry results in an object of bound nature, with high significance. The comparison of the measured magnitudes and colours to evolutionary tracks suggests that the detection is a companion of planetary mass. We confirm the detection of a large gap of about 54 au in size within the disk in our scattered light images, and detect a signal from an inner disk component. We find that its spatial extent is very likely smaller than about 17 au in radius. The images of the outer disk show evidence of a complex azimuthal brightness distribution which may in part be explained by Rayleigh scattering from very small grains. Future observations of this system at different wavelengths and continuing astrometry will allow us to test theoretical predictions regarding planet-disk interactions, planetary atmospheres and evolutionary models.
Published: 2020
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173. Polarimetric imaging mode of VLT/SPHERE/IRDIS

Author: van Holstein, R., Girard, J., De Boer, J., Snik, F., Milli, J., Stam, D., Ginski, C., Mouillet, D., Wahhaj, Z., Keller, C. U., Schmid, H., Langlois, M., Dohlen, K., Vigan, Arthur, Pohl, A., Carbillet, M., Fantinel, D., Maurel, D., Origne, A., Petit, C., Ramos, J., Rigal, F, Sevin, A., Boccaletti, A., Le Coroller, H., Dominik, C., Henning, T., Lagadec, E., Menard, F., Turatto, M., Udry, S., Chauvin, G., Feldt, M., Beuzit, J.-L., 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, 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), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), SRON Netherlands Institute for Space Research (SRON), European Southern Observatory (ESO), 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), Laboratoire Hippolyte Fizeau (FIZEAU), 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), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut d’Électronique, de Microélectronique et de Nanotechnologie (IEMN) - UMR 8520 (IEMN), Ecole Centrale de Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF), University of Copenhagen = Københavns Universitet (KU), Anton Pannekoek Institute for Astronomy, University of Amsterdam [Amsterdam] (UvA), Anthropologie Moléculaire et Imagerie de Synthèse (AMIS), Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées, 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), 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), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Observatoire Astronomique de l'Université de Genève (ObsGE), and Université de Genève (UNIGE)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics
Abstract: International audience; Context. Circumstellar disks and self-luminous giant exoplanets or companion brown dwarfs can be characterized through direct-imaging polarimetry at near-infrared wavelengths. SPHERE/IRDIS at the Very Large Telescope has the capabilities to perform such measurements, but uncalibrated instrumental polarization effects limit the attainable polarimetric accuracy. Aims. We aim to characterize and correct the instrumental polarization effects of the complete optical system, that is, the telescope and SPHERE/IRDIS. Methods. We created a detailed Mueller matrix model in the broadband filters Y, J, H, and K s and calibrated the model using measurements with SPHERE’s internal light source and observations of two unpolarized stars. We developed a data-reduction method that uses the model to correct for the instrumental polarization effects, and applied it to observations of the circumstellar disk of T Cha. Results. The instrumental polarization is almost exclusively produced by the telescope and SPHERE’s first mirror and varies with telescope altitude angle. The crosstalk primarily originates from the image derotator (K-mirror). At some orientations, the derotator causes severe loss of signal (> 90% loss in the H - and K s -band) and strongly offsets the angle of linear polarization. With our correction method we reach, in all filters, a total polarimetric accuracy of ≲0.1% in the degree of linear polarization and an accuracy of a few degrees in angle of linear polarization. Conclusions. The correction method enables us to accurately measure the polarized intensity and angle of linear polarization of circumstellar disks, and is a vital tool for detecting spatially unresolved (inner) disks and measuring the polarization of substellar companions. We have incorporated the correction method in a highly-automated end-to-end data-reduction pipeline called IRDAP, which we made publicly available online.
Published: 2020

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

Author: Brandt, Timothy D, Kuzuhara, Masayuki, McElwain, Michael W, Schlieder, Joshua E, Wisniewski, John P, Turner, Edwin L, Carson, J, Matsuo, T, Biller, B, Bonnefoy, M, Dressing, C, Janson, M, Knapp, G. R, Moro-Martin, A, Thalmann, C, Kudo, T, Kusakabe, N, Hashimoto, J, Abe, L, Brandner, W, Currie, T, Egner, S, Feldt, M, Golota, T, Goto, M, Brady, C. A, Guyon, O, Hayano, Y, Hyashi, M, Hayashi, S, Henning, T, Hodapp, W, Ishi, M, Iye, M, and Kandori, R
Subjects: Astrophysics
Abstract: We present results from the first three years of observations of moving group (MG) targets in the Strategic Exploration of Exoplanets and Disks with Subaru (SEEDS) high-contrast imaging survey of exoplanets and disks using the Subaru telescope. We achieve typical contrasts of (is) approximately10(exp 5) at 1" and (is) approximately 10(exp 6) beyond 2" around 63 proposed members of nearby kinematic MGs. We review each of the kinematic associations to which our targets belong, concluding that five, beta Pictoris ((is) approximately 20 Myr), AB Doradus ((is) approximately 100 Myr), Columba ((is) approximately 30 Myr), Tucana-Horogium ((is) approximately 30 Myr), and TW Hydrae ((is) approximately 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 MGs. For all of our targets, we combine proposed MG 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.
Published: 2014
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175. Transitional Disks Associated With Intermediate-mass Stars: Results of the SEEDS YSO survey

Author: Grady, Carol A, Fukagawa, M, Maruta, Y, Ohta, Y, Wisniewski, J, Hashimoto, J, Okamoto, Y, Momose, M, Currie, T, Mcelwain, Michael W, Muto, T, Kotani, T, Kusakabe, Nb, Follette, K, Bonnefoy, M, Feldt, M, Sitko, M, Takami, M, Karr, J, and Tamura, M
Subjects: Astrophysics
Abstract: As part of the Strategic Exploration of Exoplanets and Disks with Subaru YSO survey, we have surveyed a number of Herbig B-F stars at H-band using Polarimetric Differential Imaging+Angular differential imaging. Historically, Herbig stars have been sorted based on their IR SEDs into those with SEDS which can be fit by powerlaws over 1-200 μm (Meeus et al. 2001, group II), and those which can be interpreted as a powerlaw + a blackbody component (Meeus group I) or powerlaw+missing warm thermal emission, which is one of the criteria for identification of gapped or transitional disks. Meeus group II disks, when imaged with HiCIAO show featureless disks with depolarization along the projection of the disk semi-minor axis (Kusakabe et al. 2012). This is what we had expected to see for the Meeus group I disks, except for the addition of wide gaps or central cavities. Instead we find wild diversity, suggesting that transitional disks are highly perturbed compared to Meeus group II disks.
Published: 2014

176. Transitional Disks Associated with Intermediate-Mass Stars: Results of the SEEDS YSO Survey

Author: Grady, C, Fukagawa, M, Maruta, Y, Ohta, Y, Wisniewski, J, Hashimoto, J, Okamoto, Y, Momose, M, Currie, T, McElwain, M, Muto, T, Kotani, T, Kusakabe, N. B, Follette, K, Bonnefoy, M, Feldt, M, Sitko, M, Takami, M, Karr, J, and Tamura, M
Subjects: Astronomy
Abstract: Protoplanetary disks are where planets form, grow, and migrate to produce the diversity of exoplanet systems we observe in mature systems. Disks where this process has advanced to the stage of gap opening, and in some cases central cavity formation, have been termed pre-transitional and transitional disks in the hope that they represent intermediate steps toward planetary system formation. Recent reviews have focussed on disks where the star is of solar or sub-solar mass. In contrast to the sub-millimeter where cleared central cavities predominate, at H-band some T Tauri star transitional disks resemble primordial disks in having no indication of clearing, some show a break in the radial surface brightness profile at the inner edge of the outer disk, while others have partially to fully cleared gaps or central cavities. Recently, the Meeus Group I Herbig stars, intermediate-mass PMS stars with IR spectral energy distributions often interpreted as flared disks, have been proposed to have transitional and pre-transitional disks similar to those associated with solar-mass PMS stars, based on thermal-IR imaging, and sub-millimeter interferometry. We have investigated their appearance in scattered light as part of the Strategic Exploration of Exoplanets and Disks with Subaru (SEEDS), obtaining H-band polarimetric imagery of 10 intermediate-mass stars with Meeus Group I disks. Augmented by other disks with imagery in the literature, the sample is now sufficiently large to explore how these disks are similar to and differ from T Tauri star disks. The disk morphologies seen in the Tauri disks are also found for the intermediate-mass star disks, but additional phenomena are found; a hallmark of these disks is remarkable individuality and diversity which does not simply correlate with disk mass or stellar properties, including age, including spiral arms in remnant envelopes, arms in the disk, asymmetrically and potentially variably shadowed outer disks, gaps, and one disk where only half of the disk is seen in scattered light at H. We will discuss our survey results in terms of spiral arm theory, dust trapping vortices, and systematic differences in the relative scale height of these disks compared to those around Solar-mass stars. For the disks with spiral arms we discuss the planet-hosting potential, and limits on where giant planets can be located. We also discuss the implications for imaging with extreme adaptive optics instruments. Grady is supported under NSF AST 1008440 and through the NASA Origins of Solar Systems program on NNG13PB64P. JPW is supported NSF AST 100314. 0) in marked contrast to protoplanetary disks, transitional disks exhibit wide range of structural features1) arm visibility correlated with relative scale height in disk2) asymmetric and possibly variable shadowing of outer portions some transitional disks3) confirm pre-transitional disk nature of Oph IRS 48, MWC 758, HD 169142, etc.
Published: 2014

177. Gap, shadows, spirals, and streamers : SPHERE observations of binary-disk interactions in GG Tauri A

Author: Keppler, M., Penzlin, A., Benisty, M., van Boekel, R., Henning, T., van Holstein, R. G., Kley, W., Garufi, A., Ginski, C., Brandner, W., Bertrang, G. H.-M., Boccaletti, A., de Boer, J., Bonavita, M., Brown Sevilla, S., Chauvin, G., Dominik, C., Janson, Markus, Langlois, M., Lodato, G., Maire, A.-L., Ménard, F., Pantin, E., Pinte, C., Stolker, T., Szulágyi, J., Thebault, P., Villenave, M., Zurlo, A., Rabou, P., Feautrier, P., Feldt, M., Madec, F., Wildi, F., Keppler, M., Penzlin, A., Benisty, M., van Boekel, R., Henning, T., van Holstein, R. G., Kley, W., Garufi, A., Ginski, C., Brandner, W., Bertrang, G. H.-M., Boccaletti, A., de Boer, J., Bonavita, M., Brown Sevilla, S., Chauvin, G., Dominik, C., Janson, Markus, Langlois, M., Lodato, G., Maire, A.-L., Ménard, F., Pantin, E., Pinte, C., Stolker, T., Szulágyi, J., Thebault, P., Villenave, M., Zurlo, A., Rabou, P., Feautrier, P., Feldt, M., Madec, F., and Wildi, F.
Abstract: Context. A large portion of stars is found to be part of binary or higher-order multiple systems. The ubiquity of planets found around single stars raises the question of whether and how planets in binary systems form. Protoplanetary disks are the birthplaces of planets, and characterizing them is crucial in order to understand the planet formation process. Aims. Our goal is to characterize the morphology of the GG Tau A disk, one of the largest and most massive circumbinary disks. We also aim to trace evidence for binary-disk interactions. Methods. We obtained observations in polarized scattered light of GG Tau A using the SPHERE/IRDIS instrument in the H-band filter. We analyzed the observed disk morphology and substructures. We ran 2D hydrodynamical models to simulate the evolution of the circumbinary ring over the lifetime of the disk. Results. The disk and also the cavity and the inner region are highly structured, with several shadowed regions, spiral structures, and streamer-like filaments. Some of these are detected here for the first time. The streamer-like filaments appear to connect the outer ring with the northern arc. Their azimuthal spacing suggests that they may be generated through periodic perturbations by the binary, which tear off material from the inner edge of the outer disk once during each orbit. By comparing observations to hydrodynamical simulations, we find that the main features, in particular, the gap size, but also the spiral and streamer filaments, can be qualitatively explained by the gravitational interactions of a binary with a semimajor axis of similar to 35 au on an orbit coplanar with the circumbinary ring.
Published: 2020
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178. High contrast imaging with ELT/METIS: The wind driven halo, from SPHERE to METIS

Author: Cantalloube, F., Absil, O., Bertram, T., Wolfgang Brandner, Delacroix, C., Feldt, M., Kenworthy, M. A., Kulas, M., Milli, J., Neureuther, P., Xivry, O. G., Pathak, P., Por, E., Scheithauer, S., Steuer, H., Boekel, R., Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), and Universität Stuttgart [Stuttgart]
Subjects: ELT/METIS, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], AO4ELT-6 proceeding, Post-processing, High-contrast imaging, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Adaptive Optics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Coronagraphy
Abstract: METIS is one of the three first-light instruments planned for the ELT, mainly dedicated to high contrast imaging in the mid-infrared. On the SPHERE high-contrast instrument currently installed at the VLT, we observe that one of the main contrast limitations is the wind driven halo, due to the limited AO running speed with respect to the atmospheric turbulence temporal evolution. From this observation, we extrapolate this signature to the ELT/METIS instrument, which is equipped with a single conjugated adaptive optics system and with several coronagraphic devices. By making use of an analytic AO simulator, we compare the amount of wind driven halo observed with SPHERE and with METIS, under the same turbulence conditions., AO4ELT6 Conference Proceedings, 12 pages, 8 figures
Published: 2019

179. Upgrading the high contrast imaging facility SPHERE: science drivers and instrument choices

Author: Evans, Christopher J., Bryant, Julia J., Motohara, Kentaro, Boccaletti, A., Chauvin, G., Wildi, F., Milli, J., Stadler, E., Diolaiti, E., Gratton, R., Vidal, F., Loupias, M., Langlois, M., Cantalloube, F., N’Diaye, M., Gratadour, D., Ferreira, F., Tallon, M., Mazoyer, J., Segransan, D., Mouillet, D., Beuzit, J.-L., Bonnefoy, M., Galicher, R., Vigan, A., Snellen, I., Feldt, M., Desidera, S., Rousseau, S., Baruffolo, A., Goulas, C., Baudoz, P., Bechet, C., Benisty, M., Bianco, A., Carry, B., Cascone, E., Charnay, B., Choquet, E., Christiaens, V., Cortecchia, F., Di Capprio, V., De Rosa, A., Desgrange, C., D'Orazi, V., Douté, S., Frangiamore, M., Gendron, E., Ginski, C., Huby, E., Keller, C., Kulcsár, C., Landman, R., Lagarde, S., Lagadec, E., Lagrange, A.-M., Lombini, M., Kasper, M., Ménard, F., Magnard, Y., Malaguti, G., Maurel, D., Mesa, D., Morgante, G., Pantin, E., Pichon, T., Potier, A., Rabou, P., Rochat, S., Terenzi, l., Thiébaut, E., Tallon-Bosc, I., Raynaud, H.-F, Rouan, D., Sevin, A., Schiavone, F., Schrieber, L., and Zanutta, A.
Published: 2022
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180. 22q11.2 duplications: Expanding the clinical presentation.

Author: Bartik, Lauren E., Hughes, Susan S., Tracy, Meghan, Feldt, M. Max, Zhang, Lei, Arganbright, Jill, and Kaye, Alison
Abstract: 22q11.2 duplication syndrome has a frequency of ~1/700 in the intellectual disability population. Despite this frequency, there is limited information on the variable clinical presentation. Although the phenotype and incidence of congenital anomalies are well described for 22q11.2 deletion syndrome, they are not as well understood for individuals with 22q11.2 duplication syndrome. This study is a single‐center, retrospective review of patients diagnosed with 22q11.2 duplication syndrome designed to categorize the variable phenotype seen in these individuals. The data suggest that the incidence of congenital anomalies may be higher than previously reported for this syndrome. Affected individuals are at increased risk for a variety of problems including gastrointestinal complications, endocrine dysfunction, ophthalmologic abnormalities, palatal anomalies, congenital heart disease, musculoskeletal differences, and neurologic abnormalities. Individuals with 22q11.2 duplication syndrome would benefit from care coordinated by a multidisciplinary team and managed according to the 22q11.2 deletion syndrome guidelines. [ABSTRACT FROM AUTHOR]
Published: 2022
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181. Direct Imaging Discovery of A Super-Jupiter Around the Late B-Type Star K And*

Author: Carson, J, Thalmann, C, Janson, M, Kozakis, T, Bonnefoy, M, Biller, B, Schlieder, J, Currie, T, McElwain, M, Goto, M, Henning, T, Brandner, W, Feldt, M, Kandori, R, Kuzuhara, M, Stevens, L, Wong, P, Gainey, K, Fukagawa, M, Kuwada, Y, Brandt, T, Kwon, J, Abe, L, Egner, S, Grady, C, Guyon, O, Hashimoto, J, Hayano, Y, Hayashi, M, Hayashi, S, Hodapp, K, Ishii, M, Iye, M, Knapp, G, Kudo, T, Kusakabe, N, Matsuo, T, Miyama, S, Morino, J, Moro-Martin, A, Nishimura, T, Pyo, T, Serabyn, E, Suto, H, Suzuki, R, Takami, M, Takato, N, Terada, H, Tomono, D, Turner, E, Watanabe, M, Wisniewski, J, Yamada, T, Takami, H, Usuda, T, and Tamura, M
Subjects: Astrophysics
Abstract: We present the direct imaging discovery of an extrasolar planet, or possible low-mass brown dwarf, at a projected separation of 55 plus or minus 2 AU (1."058 plus or minus 0."007) from the B9-type star K And. The planet was detected with Subaru/HiCIAO (Subaru/High Contrast Instrument for the Subaru Next Generation Adaptive Optics) during the SEEDS (Strategic Exploration of Exoplanets and Disks with Subaru Telescope/HiCIAO) survey and confirmed as a bound companion via common proper motion measurements. Observed near-infrared magnitudes of J equals 16.3 plus or minus 0.3, H equals 15.2 plus or minus 0.2, K (sub s) = 14.6 plus or minus 0.4, and L prime equals 13.12 plus or minus 0.09 indicate a temperature of approximately 1700 degrees Kelvin. The galactic kinematics of the host star are consistent with membership in the Columba Association, implying a corresponding age of 30 (exp from plus 20 to minus10) Myr. The systems age, combined with the companion photometry, points to a model-dependent companion mass approximately 12.8 times the mass of Jupiter. The host stars estimated mass of 2.4 to 2.5 times the mass of the sun places it among the most massive stars ever known to harbor an extrasolar planet or low-mass brown dwarf. While the mass of the companion is close to the deuterium burning limit, its mass ratio, orbital separation, and likely planet-like formation scenario imply that it may be best defined as a super-Jupiter with properties similar to other recently discovered companions to massive stars.
Published: 2013
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182. Spiral Arms in the Asymmetrically Illuminated Disk of MWC 758 and Constraints on Giant Planets

Author: Grady, C. A, Muto, T, Hashimoto, J, Fukagawa, M, Currie, T, Biller, B, Thalmann, C, Sitko, M. L, Russell, R, Wisniewski, J, Dong, R, Kwon, J, Sai, S, Hornbeck, J, Schneider, G, Hines, D, Moro Martin, A, Feldt, M, Henning, Th, Pott, J.-U, Bonnefoy, M, Bouwman, J, Lacour, S, McElwain, M, and Serabyn, G
Subjects: Astronomy
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 micrometer Hubble Space Telescope/NICMOS data. While submillimeter 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 that asymmetrically shadow the outer disk. We model one of the spirals using spiral density wave theory, and derive a disk aspect ratio of h approximately 0.18, indicating a dynamically warm disk. If the spiral pattern is excited by a perturber, we estimate its mass to be 5(exp +3)(sub -4) M(sub J), 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 M(sub J) at 1".0 and 2 M(sub J) at 1".55, using the COND models. Collectively, these data strengthen the case for MWC 758 already being a young planetary system.
Published: 2013
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183. Relationship between Serum 25-Hydroxyvitamin D and IgE: National Health and Nutrition Examination Survey 2-Year Results: 573

Author: Jacobs, Z. D., Dai, H., Feldt, M., and Dinakar, C.
Published: 2011

184. The search for disks or planetary objects around directly imaged companions: a candidate around DH Tauri B

Author: Lazzoni, C., primary, Zurlo, A., additional, Desidera, S., additional, Mesa, D., additional, Fontanive, C., additional, Bonavita, M., additional, Ertel, S., additional, Rice, K., additional, Vigan, A., additional, Boccaletti, A., additional, Bonnefoy, M., additional, Chauvin, G., additional, Delorme, P., additional, Gratton, R., additional, Houllé, M., additional, Maire, A. L., additional, Meyer, M., additional, Rickman, E., additional, Spalding, E. A., additional, Asensio-Torres, R., additional, Langlois, M., additional, Müller, A., additional, Baudino, J-L., additional, Beuzit, J.-L., additional, Biller, B., additional, Brandner, W., additional, Buenzli, E., additional, Cantalloube, F., additional, Cheetham, A., additional, Cudel, M., additional, Feldt, M., additional, Galicher, R., additional, Janson, M., additional, Hagelberg, J., additional, Henning, T., additional, Kasper, M., additional, Keppler, M., additional, Lagrange, A.-M., additional, Lannier, J., additional, LeCoroller, H., additional, Mouillet, D., additional, Peretti, S., additional, Perrot, C., additional, Salter, G., additional, Samland, M., additional, Schmidt, T., additional, Sissa, E., additional, and Wildi, F., additional
Published: 2020
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185. K-Stacker: an algorithm to hack the orbital parameters of planets hidden in high-contrast imaging

Author: Le Coroller, H., primary, Nowak, M., additional, Delorme, P., additional, Chauvin, G., additional, Gratton, R., additional, Devinat, M., additional, Bec-Canet, J., additional, Schneeberger, A., additional, Estevez, D., additional, Arnold, L., additional, Beust, H., additional, Bonnefoy, M., additional, Boccaletti, A., additional, Desgrange, C., additional, Desidera, S., additional, Galicher, R., additional, Lagrange, A. M., additional, Langlois, M., additional, Maire, A. L., additional, Menard, F., additional, Vernazza, P., additional, Vigan, A., additional, Zurlo, A., additional, Fenouillet, T., additional, Lambert, J. C., additional, Bonavita, M., additional, Cheetham, A., additional, D’orazi, V., additional, Feldt, M., additional, Janson, M., additional, Ligi, R., additional, Mesa, D., additional, Meyer, M., additional, Samland, M., additional, Sissa, E., additional, Beuzit, J.-L., additional, Dohlen, K., additional, Fusco, T., additional, Le Mignant, D., additional, Mouillet, D., additional, Ramos, J., additional, Rochat, S., additional, and Sauvage, J. F., additional
Published: 2020
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186. Gap, shadows, spirals, and streamers: SPHERE observations of binary-disk interactions in GG Tauri A

Author: Keppler, M., primary, Penzlin, A., additional, Benisty, M., additional, van Boekel, R., additional, Henning, T., additional, van Holstein, R. G., additional, Kley, W., additional, Garufi, A., additional, Ginski, C., additional, Brandner, W., additional, Bertrang, G. H.-M., additional, Boccaletti, A., additional, de Boer, J., additional, Bonavita, M., additional, Brown Sevilla, S., additional, Chauvin, G., additional, Dominik, C., additional, Janson, M., additional, Langlois, M., additional, Lodato, G., additional, Maire, A.-L., additional, Ménard, F., additional, Pantin, E., additional, Pinte, C., additional, Stolker, T., additional, Szulágyi, J., additional, Thebault, P., additional, Villenave, M., additional, Zurlo, A., additional, Rabou, P., additional, Feautrier, P., additional, Feldt, M., additional, Madec, F., additional, and Wildi, F., additional
Published: 2020
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187. Searching for the near-infrared counterpart of Proxima c using multi-epoch high-contrast SPHERE data at VLT

Author: Gratton, R., primary, Zurlo, A., additional, Le Coroller, H., additional, Damasso, M., additional, Del Sordo, F., additional, Langlois, M., additional, Mesa, D., additional, Milli, J., additional, Chauvin, G., additional, Desidera, S., additional, Hagelberg, J., additional, Lagadec, E., additional, Vigan, A., additional, Boccaletti, A., additional, Bonnefoy, M., additional, Brandner, W., additional, Brown, S., additional, Cantalloube, F., additional, Delorme, P., additional, D’Orazi, V., additional, Feldt, M., additional, Galicher, R., additional, Henning, T., additional, Janson, M., additional, Kervella, P., additional, Lagrange, A.-M., additional, Lazzoni, C., additional, Ligi, R., additional, Maire, A.-L., additional, Ménard, F., additional, Meyer, M., additional, Mugnier, L., additional, Potier, A., additional, Rickman, E. L., additional, Rodet, L., additional, Romero, C., additional, Schmidt, T., additional, Sissa, E., additional, Sozzetti, A., additional, Szulágyi, J., additional, Wahhaj, Z., additional, Antichi, J., additional, Fusco, T., additional, Stadler, E., additional, Suarez, M., additional, and Wildi, F., additional
Published: 2020
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188. HD 117214 debris disk: scattered-light images and constraints on the presence of planets

Author: Engler, N., primary, Lazzoni, C., additional, Gratton, R., additional, Milli, J., additional, Schmid, H. M., additional, Chauvin, G., additional, Kral, Q., additional, Pawellek, N., additional, Thébault, P., additional, Boccaletti, A., additional, Bonnefoy, M., additional, Brown, S., additional, Buey, T., additional, Cantalloube, F., additional, Carle, M., additional, Cheetham, A., additional, Desidera, S., additional, Feldt, M., additional, Ginski, C., additional, Gisler, D., additional, Henning, Th., additional, Hunziker, S., additional, Lagrange, A. M., additional, Langlois, M., additional, Mesa, D., additional, Meyer, M. R., additional, Moeller-Nilsson, O., additional, Olofsson, J., additional, Petit, C., additional, Petrus, S., additional, Quanz, S. P., additional, Rickman, E., additional, Stadler, E., additional, Stolker, T., additional, Vigan, A., additional, Wildi, F., additional, and Zurlo, A., additional
Published: 2020
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189. RefPlanets: Search for reflected light from extrasolar planets with SPHERE/ZIMPOL

Author: Hunziker, S., primary, Schmid, H. M., additional, Mouillet, D., additional, Milli, J., additional, Zurlo, A., additional, Delorme, P., additional, Abe, L., additional, Avenhaus, H., additional, Baruffolo, A., additional, Bazzon, A., additional, Boccaletti, A., additional, Baudoz, P., additional, Beuzit, J. L., additional, Carbillet, M., additional, Chauvin, G., additional, Claudi, R., additional, Costille, A., additional, Daban, J.-B., additional, Desidera, S., additional, Dohlen, K., additional, Dominik, C., additional, Downing, M., additional, Engler, N., additional, Feldt, M., additional, Fusco, T., additional, Ginski, C., additional, Gisler, D., additional, Girard, J. H., additional, Gratton, R., additional, Henning, Th., additional, Hubin, N., additional, Kasper, M., additional, Keller, C. U., additional, Langlois, M., additional, Lagadec, E., additional, Martinez, P., additional, Maire, A. L., additional, Menard, F., additional, Meyer, M. R., additional, Pavlov, A., additional, Pragt, J., additional, Puget, P., additional, Quanz, S. P., additional, Rickman, E., additional, Roelfsema, R., additional, Salasnich, B., additional, Sauvage, J.-F., additional, Siebenmorgen, R., additional, Sissa, E., additional, Snik, F., additional, Suarez, M., additional, Szulágyi, J., additional, Thalmann, Ch., additional, Turatto, M., additional, Udry, S., additional, van Holstein, R. G., additional, Vigan, A., additional, and Wildi, F., additional
Published: 2020
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190. Polarimetric imaging mode of VLT/SPHERE/IRDIS

Author: de Boer, J., primary, Langlois, M., additional, van Holstein, R. G., additional, Girard, J. H., additional, Mouillet, D., additional, Vigan, A., additional, Dohlen, K., additional, Snik, F., additional, Keller, C. U., additional, Ginski, C., additional, Stam, D. M., additional, Milli, J., additional, Wahhaj, Z., additional, Kasper, M., additional, Schmid, H. M., additional, Rabou, P., additional, Gluck, L., additional, Hugot, E., additional, Perret, D., additional, Martinez, P., additional, Weber, L., additional, Pragt, J., additional, Sauvage, J.-F., additional, Boccaletti, A., additional, Le Coroller, H., additional, Dominik, C., additional, Henning, T., additional, Lagadec, E., additional, Ménard, F., additional, Turatto, M., additional, Udry, S., additional, Chauvin, G., additional, Feldt, M., additional, and Beuzit, J.-L., additional
Published: 2020
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191. Interferometry of M8E-IR with MIDI - Resolving the Dust Emission

Author: Feldt, M., primary, Pascucci, I., additional, Chesneau, O., additional, Apai, D., additional, Henning, Th., additional, Leinert, Ch., additional, Linz, H., additional, Men’shchikov, A., additional, and Stecklum, B., additional
Published: 2007
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192. Polarimetric Imaging of Large Cavity Structures in the Pre-transitional Protoplanetary Disk Around PDS 70: Observations of the Disk

Author: Hashimoto, J, Dong, R, Kudo, T, Honda, M, McClure, M. K, Zhu, Z, Muto, T, Wisniewski, J, Abe, L, Brandner, W, Brandt, T, Carson, J, Egner, S, Feldt, M, Fukagawa, M, Goto, M, Grady, C. A, Guyon, O, Hayano, Y, Hayashi, M, Hayashi, S, Henning, T, Hodapp, K, Ishii, M, and McElwain, M. W
Subjects: Astrophysics
Abstract: We present high-resolution H-band polarized intensity (FWHM=0".1:14AU) 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 approx.70 AU. Our data show that the geometric center of the disk shifts by approx.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 spectral energy distribution 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 of approx.30 to approx.50 M(sub J) on the mass of companions within the gap. Taking into account 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. Key words: planetary systems - polarization - protoplanetary disks - stars: individual (PDS 70) - stars: pre-main sequence.
Published: 2012
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193. Discovery of Small-Scale Spiral Structures in the Disk of SAO 206462 (HD 135344B)(exp 1): Implications for the Physical State of the Disk from Spiral Density Wave Theory

Author: Muto, T, Grady, C. A, Hashimoto, J, Fukagawa, M, Hornbeck, J. B, Sitko, M, Russell, R, Werren, C, Cure, M, Currie, T, Ohashi, N, Okamoto, Y, Momose, M, Honda, M, Inutsuka, S, Takeuchi, T, Dong, R, Abe, L, Brandner, W, Brandt, T, Carson, J, Egner, S, Feldt, M, Fukue, T, and Goto, M
Subjects: Astronomy
Abstract: We present high-resolution, H-band, imaging observations, collected with Subaru /HiCIAO, of the scattered light from the transitional disk around SAO 206462 (HD 1353448). Although previous sub-mm imagery suggested the existence of the dust-depleted cavity at r <= 46 AU, our observations reveal the presence of scattered light components as close as O".2 (approx 28 AU) from the star. Moreover , we have discovered two small-scale spiral structures lying within 0".5 (approx 70 AU). We present models for the spiral structures using the spiral density wave theory, and derive a disk aspect ratio of h approx. 0.1, which is consistent with previous sub-mm observations. This model can potentially give estimates of the temperature and rotation profiles of the disk based on dynamical processes. independently from sub-nun observations. It also predicts the evolution of the spiral structures, which can be observable on timescales of 10-20 years, providing conclusive tests of the model. While we cannot uniquely identify the origin of these spirals, planets embedded in the disk may be capable of exciting the observed morphology. Assuming that this is the case, we can make predictions on the locations and, possibly, the masses of the unseen planets. Such planets may be detected by future multi-wavelengths observations
Published: 2012

194. Images of the Extended Outer Regions of the Debris Ring around HR 4796 A

Author: Thalmann, C, Janson, M, Buenzli, E, Brandt, T. D, Wisniewski, J. P, Moro-Martin, A, Usuda, T, Schneider, G, Carson, J, McElwain, M. W, Grady, C. A, Goto, M, Abe, L, Brandner, W, Dominik, C, Egner, S, Feldt, M, Fukue, T, Golota, T, Guyon, O, Hashimoto, J, Hayano, Y, Hayashi, M, Hayashi, S, and Serabyn, E
Subjects: Astronomy
Abstract: We present high-contrast images of HR 4796 A taken with Subaru/HiCIAO in H-band, resolving the debris disk in scattered light. The application of specialized angular differential imaging methods (ADI) allows us to trace the inner edge of the disk with high precision, and reveals a pair of "streamers" extending radially outwards from the ansae. Using a simple disk model with a power-law surface brightness profile, we demonstrate that the observed streamers can be understood as part of the smoothly tapered outer boundary of the debris disk, which is most visible at the ansae. Our observations are consistent with the expected result of a narrow planetesimal ring being ground up in a collisional cascade, yielding dust with a wide range of grain sizes. Radiation forces leave large grains in the ring and push smaller grains onto elliptical, or even hyperbolic trajectories. We measure and characterize the disk's surface brightness profile, and confirm the previously suspected offset of the disk's center from the star's position along the ring's major axis. Furthermore, we present first evidence for an offset along the minor axis. Such offsets are commonly viewed as signposts for the presence of unseen planets within a disk's cavity. Our images also offer new constraints on the presence of companions down to the planetary mass regime (approx 9 M(sub Jup) at 0".5, approx 3 M(sub Jup) at 1").
Published: 2012

195. New Techniques for High-Contrast Imaging with ADI: The ACORNS-ADI SEEDS Data Reduction Pipeline

Author: Brandt, Timothy D, McElwain, Michael W, Turner, Edwin L, Abe, L, Brandner, W, Carson, J, Egner, S, Feldt, M, Golota, T, Grady, C. A, Guyon, O, Hashimoto, J, Hayano, Y, Hayashi, M, Hayashi, S, Henning, T, Hodapp, K. W, Ishil, M, Lye, M, Janson, M, Kandori, R, Knapp, G. R, Kudo, T, Kusakabe, N, and Kuzuhara, M
Subjects: Astronomy
Abstract: We describe Algorithms for Calibration, Optimized Registration, and Nulling the Star in Angular Differential Imaging (ACORNS-ADI), a new, parallelized software package to reduce high-contrast imaging data, and its application to data from the Strategic Exploration of Exoplanets and Disks (SEEDS) survey. We implement seyeral new algorithms, includbg a method to centroid saturated images, a trimmed mean for combining an image sequence that reduces noise by up to approx 20%, and a robust and computationally fast method to compute the sensitivitv of a high-contrast obsen-ation everywhere on the field-of-view without introducing artificial sources. We also include a description of image processing steps to remove electronic artifacts specific to Hawaii2-RG detectors like the one used for SEEDS, and a detailed analysis of the Locally Optimized Combination of Images (LOCI) algorithm commonly used to reduce high-contrast imaging data. ACORNS-ADI is efficient and open-source, and includes several optional features which may improve performance on data from other instruments. ACORNS-ADI is freely available for download at www.github.com/t-brandt/acorns_-adi under a BSD license
Published: 2012

196. VLT/SPHERE exploration of the young multiplanetary system PDS70

Author: Mesa, D., primary, Keppler, M., additional, Cantalloube, F., additional, Rodet, L., additional, Charnay, B., additional, Gratton, R., additional, Langlois, M., additional, Boccaletti, A., additional, Bonnefoy, M., additional, Vigan, A., additional, Flasseur, O., additional, Bae, J., additional, Benisty, M., additional, Chauvin, G., additional, de Boer, J., additional, Desidera, S., additional, Henning, T., additional, Lagrange, A.-M., additional, Meyer, M., additional, Milli, J., additional, Müller, A., additional, Pairet, B., additional, Zurlo, A., additional, Antoniucci, S., additional, Baudino, J.-L., additional, Brown Sevilla, S., additional, Cascone, E., additional, Cheetham, A., additional, Claudi, R. U., additional, Delorme, P., additional, D’Orazi, V., additional, Feldt, M., additional, Hagelberg, J., additional, Janson, M., additional, Kral, Q., additional, Lagadec, E., additional, Lazzoni, C., additional, Ligi, R., additional, Maire, A.-L., additional, Martinez, P., additional, Menard, F., additional, Meunier, N., additional, Perrot, C., additional, Petrus, S., additional, Pinte, C., additional, Rickman, E. L., additional, Rochat, S., additional, Rouan, D., additional, Samland, M., additional, Sauvage, J.-F., additional, Schmidt, T., additional, Udry, S., additional, Weber, L., additional, and Wildi, F., additional
Published: 2019
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197. SPHERE: the exoplanet imager for the Very Large Telescope

Author: Beuzit, J.-L., primary, Vigan, A., additional, Mouillet, D., additional, Dohlen, K., additional, Gratton, R., additional, Boccaletti, A., additional, Sauvage, J.-F., additional, Schmid, H. M., additional, Langlois, M., additional, Petit, C., additional, Baruffolo, A., additional, Feldt, M., additional, Milli, J., additional, Wahhaj, Z., additional, Abe, L., additional, Anselmi, U., additional, Antichi, J., additional, Barette, R., additional, Baudrand, J., additional, Baudoz, P., additional, Bazzon, A., additional, Bernardi, P., additional, Blanchard, P., additional, Brast, R., additional, Bruno, P., additional, Buey, T., additional, Carbillet, M., additional, Carle, M., additional, Cascone, E., additional, Chapron, F., additional, Charton, J., additional, Chauvin, G., additional, Claudi, R., additional, Costille, A., additional, De Caprio, V., additional, de Boer, J., additional, Delboulbé, A., additional, Desidera, S., additional, Dominik, C., additional, Downing, M., additional, Dupuis, O., additional, Fabron, C., additional, Fantinel, D., additional, Farisato, G., additional, Feautrier, P., additional, Fedrigo, E., additional, Fusco, T., additional, Gigan, P., additional, Ginski, C., additional, Girard, J., additional, Giro, E., additional, Gisler, D., additional, Gluck, L., additional, Gry, C., additional, Henning, T., additional, Hubin, N., additional, Hugot, E., additional, Incorvaia, S., additional, Jaquet, M., additional, Kasper, M., additional, Lagadec, E., additional, Lagrange, A.-M., additional, Le Coroller, H., additional, Le Mignant, D., additional, Le Ruyet, B., additional, Lessio, G., additional, Lizon, J.-L., additional, Llored, M., additional, Lundin, L., additional, Madec, F., additional, Magnard, Y., additional, Marteaud, M., additional, Martinez, P., additional, Maurel, D., additional, Ménard, F., additional, Mesa, D., additional, Möller-Nilsson, O., additional, Moulin, T., additional, Moutou, C., additional, Origné, A., additional, Parisot, J., additional, Pavlov, A., additional, Perret, D., additional, Pragt, J., additional, Puget, P., additional, Rabou, P., additional, Ramos, J., additional, Reess, J.-M., additional, Rigal, F., additional, Rochat, S., additional, Roelfsema, R., additional, Rousset, G., additional, Roux, A., additional, Saisse, M., additional, Salasnich, B., additional, Santambrogio, E., additional, Scuderi, S., additional, Segransan, D., additional, Sevin, A., additional, Siebenmorgen, R., additional, Soenke, C., additional, Stadler, E., additional, Suarez, M., additional, Tiphène, D., additional, Turatto, M., additional, Udry, S., additional, Vakili, F., additional, Waters, L. B. F. M., additional, Weber, L., additional, Wildi, F., additional, Zins, G., additional, and Zurlo, A., additional
Published: 2019
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198. Orbital and spectral analysis of the benchmark brown dwarf HD 4747B

Author: Peretti, S., primary, Ségransan, D., additional, Lavie, B., additional, Desidera, S., additional, Maire, A.-L., additional, D’Orazi, V., additional, Vigan, A., additional, Baudino, J.-L., additional, Cheetham, A., additional, Janson, M., additional, Chauvin, G., additional, Hagelberg, J., additional, Menard, F., additional, Heng, Kevin, additional, Udry, S., additional, Boccaletti, A., additional, Daemgen, S., additional, Le Coroller, H., additional, Mesa, D., additional, Rouan, D., additional, Samland, M., additional, Schmidt, T., additional, Zurlo, A., additional, Bonnefoy, M., additional, Feldt, M., additional, Gratton, R., additional, Lagrange, A.-M., additional, Langlois, M., additional, Meyer, M., additional, Carbillet, M., additional, Carle, M., additional, De Caprio, V., additional, Gluck, L., additional, Hugot, E., additional, Magnard, Y., additional, Moulin, T., additional, Pavlov, A., additional, Pragt, J., additional, Rabou, P., additional, Ramos, J., additional, Rousset, G., additional, Sevin, A., additional, Soenke, C., additional, Stadler, E., additional, Weber, L., additional, and Wildi, F., additional
Published: 2019
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199. High-fidelity Imaging of the Inner AU Mic Debris Disk: Evidence of Differential Wind Sculpting?

Author: Molaverdikhani, K., Trifonov, T., Mollière, P., Frankel, N., Messina, S., Biller, B. A., Roux, A., Damasso, M., Del Sordo, F., Brandner, W., Kervella, P., Mugnier, L., Romero, C., Sozzetti, A., Antichi, J., Huby, E., N’Diaye, M., Kitzmann, D., Tang, Y. W., Habart, E., Beck, T. L., Potier, A., Singh, G., Di Folco, E., Péricaud, J., Dutrey, A., Chapillon, E., Guilloteau, S., Piétu, V., Pawellek, N., Brown, S., Buey, T., Moeller-Nilsson, O., Stolker, T., Hunziker, S., Abe, L., Avenhaus, H., Baruffolo, A., Bazzon, A., Costille, A., Daban, J.-B., Downing, M., Engler, N., Gisler, D., Hubin, N., Puget, P., Quanz, S. P., Roelfsema, R., Salasnich, B., Siebenmorgen, R., Suarez, M., Szulágyi, J., Thalmann, Ch., Pohl, A., Fantinel, D., Maurel, D., Origné, A., Petit, C., Rigal, F., Girard, J. H., Mouillet, D., Dohlen, K., Snik, F., Keller, C. U., Ginski, C., Stam, D. M., Wahhaj, Z., Kasper, M., Schmid, H. M., Perret, D., Dominik, C., Turatto, M., Beuzit, J.-L., Keppler, M., Rodet, L., Charnay, B., Bae, J., De Boer, J., Müller, A., Pairet, B., Antoniucci, S., Brown Sevilla, S., Cascone, E., Claudi, R. U., Lagadec, E., Martinez, P., Meunier, N., Petrus, S., Pinte, C., Rochat, S., Sauvage, J.-F., Peretti, S., Ségransan, D., Lavie, B., Baudino, J.-L., Janson, M., Heng, Kevin, Udry, S., Daemgen, S., Le Coroller, H., Samland, M., Carbillet, M., Carle, M., Hugot, E., Magnard, Y., Moulin, T., Pavlov, A., Pragt, J., Rabou, P., Rousset, G., Sevin, A., Soenke, C., Stadler, E., Weber, L., Wildi, F., Bhowmik, T., Thébault, P., Kral, Q., Mazoyer, J., van Holstein, R. G., Baudoz, P., Galicher, R., Olofsson, J., Pantin, E., Perrot, C., Mesa, D., Langlois, M., Garufi, A., Gratton, R., Desidera, S., D'Orazi, V., Flasseur, O., Barbieri, M., Benisty, M., Henning, Th., Ligi, R., Sissa, E., Vigan, A., Zurlo, A., Bonnefoy, M., Cantalloube, F., Chauvin, G., Cheetham, A. C., De Caprio, V., Delorme, P., Feldt, M., Fusco, T., Gluck, L., Hagelberg, J., Lazzoni, C., Madec, F., Maire, A.-L., Ménard, F., Meyer, M. R., Ramos, J., Rickman, E. L., Rouan, D., Schmidt, T., van der Plas, G., D’Orazi, V., De Caprio, V, Van der Plas, G, Wisniewski, John P., Kowalski, Adam F., Davenport, James R. A., Schneider, Glenn, Grady, Carol A., Hebb, Leslie, Lawson, Kellen D., Augereau, Jean-Charles, Boccaletti, A., Brown, Alexander, Debes, John H., Gaspar, Andras, Henning, Thomas K., Hines, Dean C., Kuchner, Marc J., Lagrange, Anne-Marie, Milli, Julien, Sezestre, Elie, Stark, Christopher C., Thalmann, Christian, Wisniewski, John, Kowalski, Adam, Davenport, James, Grady, Carol, Lawson, Kellen, Debes, John, Henning, Thomas, Hines, Dean, Kuchner, Marc, Stark, Christopher, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and 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)
Subjects: planets and satellites: detection, 010504 meteorology & atmospheric sciences, planets and satellites: dynamical evolution and stability, stars: individual: HD 117214, stars: individual: AB Aur, techniques: image processing, Astrophysics, M dwarf stars, 01 natural sciences, stars: individual: HD 19467, accretion, Debris disks, Astrophysics::Solar and Stellar Astrophysics, infrared: planetary systems, 010303 astronomy & astrophysics, instrumentation: spectrographs, Physics, Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: atmospheres, [PHYS]Physics [physics], planet-disk interactions, accretion disks, stars: individual: HD 32297, protoplanetary disks, stars: individual: Proxima, Exoplanet, Astrophysics - Solar and Stellar Astrophysics, binaries: general, techniques: imaging spectroscopy, techniques: interferometric, stars individual: HIP 65875, planets and satellites: individual: Proxima c, Astrophysics::Earth and Planetary Astrophysics, methods: observational, radio lines: stars, binaries: spectroscopic, brown dwarfs, (stars:) planetary systems, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Brown dwarf, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, stars: pre-main sequence, instrumentation: adaptive optics, planets and satellites: terrestrial planets, stars: individual: PDS70, instrumentation: high angular resolution, 0103 physical sciences, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Debris disk, polarization, HD 163296, Stellar rotation, Starspot, techniques: high angular resolution, Astronomy and Astrophysics, Planetary system, methods: data analysis, binaries: visual, Starspots, techniques: polarimetric, Polar wind, Space and Planetary Science, Circumstellar disks, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Heliosphere, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Astrophysical Journal Letters, 883 (1), ISSN:1967-2014, ISSN:2041-8213
Published: 2019

200. A search for accreting young companions embedded in circumstellar disks

Author: Cugno, G, Quanz, S P, Hunziker, S, Stolker, T, Schmid, H M, Avenhaus, H, Baudoz, P, Bohn, A J, Bonnefoy, M, Buenzli, E, Chauvin, G, Cheetham, A, Desidera, S, Dominik, C, Feautrier, P, Feldt, M, Ginski, C, Girard, J H, Gratton, R, Hagelberg, J, Hugot, E, Janson, M, Lagrange, A-M, Langlois, M, Magnard, Y, Maire, A-L, Menard, F, Meyer, M, Milli, J, Mordasini, C, et al, University of Zurich, and Cugno, G
Subjects: 1912 Space and Planetary Science, 530 Physics, Space and Planetary Science, 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics, Astronomy and Astrophysics
Published: 2019

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