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

Author

Lagrange, A., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, M., Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Le Coroller, H., Ligi, R., Maire, A., Mesa, D., Messina, S., Müeller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Ménard, F., Schmid, H., Turatto, M., Udry, S., Bohn, A., Charnay, B., Gomez Gonzales, C., Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J., 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., Deboulbe, 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., Szulagyi, J., and Wildi, F.

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Context. With an orbital distance comparable to that of Saturn in the solar system, β Pictoris b is the closest (semi-major axis ≃9 au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to β Pictoris have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet's orbital parameters. Aims: We aimed at further constraining β Pictoris b orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. Methods: We used SPHERE at the VLT to precisely monitor the orbital motion of beta β Pictoris b since first light of the instrument in 2014. Results: We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6 au) and prevented further detection. We redetected β Pictoris b on the northeast side of the disk at a separation of 139 mas and a PA of 30° in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of a = 9.0 ± 0.5 au (1σ), it definitely excludes previously reported possible long orbital periods, and excludes β Pictoris b as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away. Based on observations collected at the European Southern Observatory under programmes 198.C-0209, 1100.C-0481.

Published
2019

52. Hint of curvature in the orbital motion of the exoplanet 51 Eridani b using 3 yr of VLT/SPHERE monitoring

Author

Maire, A-L, Rodet, L., Cantalloube, F., Galicher, R., Brandner, W., Messina, S., Lazzoni, C., Mesa, D., Melnick, D., Carson, J., Samland, M., Biller, B. A., Boccaletti, A., Wahhaj, Z., Beust, H., Bonnefoy, M., Chauvin, G., Desidera, S., Langlois, M., Henning, T., Janson, Markus, Olofsson, J., Rouan, D., Menard, F., Lagrange, A-M, Gratton, R., Vigan, A., Meyer, M. R., Cheetham, A., Beuzit, J-L, Dohlen, K., Avenhaus, H., Bonavita, M., Claudi, R., Cudel, M., Daemgen, S., D'Orazi, V, Fontanive, C., Hagelberg, J., Le Coroller, H., Perrot, C., Rickman, E., Schmidt, T., Sissa, E., Udry, S., Zurlo, A., Abe, L., Origne, A., Rigal, F., Rousset, G., Roux, A., Weber, L., Maire, A-L, Rodet, L., Cantalloube, F., Galicher, R., Brandner, W., Messina, S., Lazzoni, C., Mesa, D., Melnick, D., Carson, J., Samland, M., Biller, B. A., Boccaletti, A., Wahhaj, Z., Beust, H., Bonnefoy, M., Chauvin, G., Desidera, S., Langlois, M., Henning, T., Janson, Markus, Olofsson, J., Rouan, D., Menard, F., Lagrange, A-M, Gratton, R., Vigan, A., Meyer, M. R., Cheetham, A., Beuzit, J-L, Dohlen, K., Avenhaus, H., Bonavita, M., Claudi, R., Cudel, M., Daemgen, S., D'Orazi, V, Fontanive, C., Hagelberg, J., Le Coroller, H., Perrot, C., Rickman, E., Schmidt, T., Sissa, E., Udry, S., Zurlo, A., Abe, L., Origne, A., Rigal, F., Rousset, G., Roux, A., and Weber, L.

Abstract

Context. The 51 Eridani system harbors a complex architecture with its primary star forming a hierarchical system with the binary GJ 3305AB at a projected separation of 2000 au, a giant planet orbiting the primary star at 13 au, and a low-mass debris disk around the primary star with possible cold and warm components inferred from the spectral energy distribution. Aims. We aim to better constrain the orbital parameters of the known giant planet. Methods. We monitored the system over three years from 2015 to 2018 with the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) instrument at the Very Large Telescope (VET). Results. We measure an orbital motion for the planet of similar to 130 mas with a slightly decreasing separation (similar to 10 mas) and find a hint of curvature. This potential curvature is further supported at 3 sigma significance when including literature Gemini Planet Imager (GPI) astrometry corrected for calibration systematics. Fits of the SPHERE and GPI data using three complementary approaches provide broadly similar results. The data suggest an orbital period of 32(-9)(+17) yr (i.e., 12(-2)(+4), au in semi-major axis), an inclination of 133(-7)(+1)(4) deg, an eccentricity of 0.45(-0.15)(+0.10), and an argument of periastron passage of 87(-30)(+34) deg [mod 180 degrees]. The time at periastron passage and the longitude of node exhibit bimodal distributions because we do not yet detect whether the planet is accelerating or decelerating along its orbit. Given the inclinations of the orbit and of the stellar rotation axis (134-144 degrees), we infer alignment or misalignment within 18 degrees for the star-planet spin-orbit. Further astrometric monitoring in the next 3-4 yr is required to confirm at a higher significance the curvature in the motion of the planet, determine if the planet is accelerating or decelerating on its orbit, and further constrain its orbital parameters and the star-planet spin-orbit.

Published
2019
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53. SPHERE dynamical and spectroscopic characterization of HD142527B

Author

Claudi, R., Maire, A. -L., Mesa, D., Cheetham, A., Fontanive, C., Gratton, R., Zurlo, A., Avenhaus, H., Bhowmik, T., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Cascone, E., Chauvin, G., Delboulbe, A., Desidera, S., D'Orazi, V., Feautrier, P., Feldt, M., Dotti, F. Flammini, Girard, J. H., Giro, E., Janson, Markus, Hagelberg, J., Keppler, M., Kopytova, T., Lacour, S., Lagrange, A. -M., Langlois, M., Lannier, J., Le Coroller, H., Menard, F., Messina, S., Meyer, M., Millward, M., Olofsson, J., Pavlov, A., Peretti, S., Perrot, C., Pinte, C., Pragt, J., Ramos, J., Rochat, S., Rodet, L., Roelfsema, R., Rouan, D., Salter, G., Schmidt, T., Sissa, E., Thebault, P., Udry, S., Vigan, A., Claudi, R., Maire, A. -L., Mesa, D., Cheetham, A., Fontanive, C., Gratton, R., Zurlo, A., Avenhaus, H., Bhowmik, T., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Cascone, E., Chauvin, G., Delboulbe, A., Desidera, S., D'Orazi, V., Feautrier, P., Feldt, M., Dotti, F. Flammini, Girard, J. H., Giro, E., Janson, Markus, Hagelberg, J., Keppler, M., Kopytova, T., Lacour, S., Lagrange, A. -M., Langlois, M., Lannier, J., Le Coroller, H., Menard, F., Messina, S., Meyer, M., Millward, M., Olofsson, J., Pavlov, A., Peretti, S., Perrot, C., Pinte, C., Pragt, J., Ramos, J., Rochat, S., Rodet, L., Roelfsema, R., Rouan, D., Salter, G., Schmidt, T., Sissa, E., Thebault, P., Udry, S., and Vigan, A.

Abstract

Aims. HD142527 is one of the most frequently studied Herbig Ae/Be stars with a transitional disk that hosts a large cavity that is up to about 100 au in radius. For this reason, it has been included in the guaranteed time observation (GTO) SpHere INfrared survey for Exoplanets (SHINE) as part of the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) at the Very Large Telescope (VLT) in order to search for low-mass companions that might explain the presence of the gap. SHINE is a large survey within about 600 young nearby stars are observed with SPHERE with the aim to constrain the occurrence and orbital properties of the giant planet population at large (>5 au) orbital separation around young stars. Methods. We used the IRDIFS observing mode of SPHERE (IRDIS short for infrared dual imaging and spectrograph plus IFS or integral field spectrograph) without any coronagraph in order to search for and characterize companions as close as 30 mas of the star. Furthermore, we present the first observations that ever used the sparse aperture mask (SAM) for SPHERE both in IRDIFS and IRDIFS_EXT modes. All the data were reduced using the dedicated SPHERE pipeline and dedicated algorithms that make use of the principal component analysis (PCA) and reference differential imaging (RDI) techniques. Results. We detect the accreting low-mass companion HD142527B at a separation of 73 mas (11.4 au) from the star. No other companions with mass greater than 10 M-J are visible in the field of view of IFS (similar to 100 au centered on the star) or in the IRDIS field of view (similar to 400 au centered on the star). Measurements from IFS, SAM IFS, and IRDIS suggest an M6 spectral type for HD142527B, with an uncertainty of one spectral subtype, compatible with an object of M = 0.11 +/- 0.06 M-circle dot and R = 0.15 +/- 0.07 R-circle dot. The determination of the mass remains a challenge using contemporary evolutionary models, as they do not account for the energy input due to

Published
2019
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54. Post-conjunction detection of beta Pictoris b with VLT/SPHERE

Author

Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, Markus, Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Le Coroller, H., Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Müeller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Ménard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. 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., Deboulbe, 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., Szulagyi, J., Wildi, F., Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, Markus, Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Le Coroller, H., Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Müeller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Ménard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. 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., Deboulbe, 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., Szulagyi, J., and Wildi, F.

Abstract

Context. With an orbital distance comparable to that of Saturn in the solar system, beta Pictoris b is the closest (semi-major axis similar or equal to 9 au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to beta Pictoris have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet's orbital parameters. Aims. We aimed at further constraining beta Pictoris b orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. Methods. We used SPHERE at the VLT to precisely monitor the orbital motion of beta beta Pictoris b since first light of the instrument in 2014. Results. We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6 au) and prevented further detection. We redetected beta Pictoris b on the northeast side of the disk at a separation of 139 mas and a PA of 30 degrees in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of a = 9.0 +/- 0.5 au (1 sigma), it definitely excludes previously reported possible long orbital periods, and excludes beta Pictoris b as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away.

Published
2019
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55. Investigating the young solar system analog HD 95086

Author

Chauvin, G., Gratton, R., Bonnefoy, M., Lagrange, A. -M, Boer, J., Arthur Vigan, Beust, H., Lazzoni, C., Boccaletti, A., Galicher, R., Desidera, S., Delorme, P., Keppler, M., Lannier, J., Maire, A. -L, Mesa, D., Meunier, N., Kral, Q., Henning, T., Menard, F., Moor, A., Avenhaus, H., Bazzon, A., Janson, M., Beuzit, J. -L, Bhowmik, T., Bonavita, M., Borgniet, S., Brandner, W., Cheetham, A., Cudel, M., Feldt, M., Fontanive, C., Ginski, C., Hagelberg, J., Janin-Potiron, P., Lagadec, E., Langlois, M., Le Coroller, H., Messina, S., Meyer, M., Mouillet, D., Peretti, S., Perrot, C., Rodet, L., Samland, M., Sissa, E., Olofsson, J., Salter, G., Schmidt, T., Zurlo, A., Milli, J., Boekel, R., Quanz, S., Wilson, P. A., Feautrier, P., Le Mignant, D., Perret, D., Ramos, J., Rochat, S., Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Universidad de Chile (UCHILE), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Department of Astronomy, Stockholm University, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), INAF - Osservatorio Astrofisico di Catania (OACT), Laboratoire d'interaction du rayonnement X avec la matière (LIXAM), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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), 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), Universidad de Chile = University of Chile [Santiago] (UCHILE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden, Université de Genève = University of Geneva (UNIGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, 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), and We acknowledge financial support from the Programme National de Planétologie (PNP) and the Programme National de Physique Stellaire (PNPS) of CNRS-INSU. This work has also been supported by a grant from the French Labex OSUG@2020 (Investissements d’avenir – ANR10 LABX56). The project is supported by CNRS, by the Agence Nationale de la Recherche (ANR-14-CE33-0018).A (Germany), INAF (Italy), FINES (Switzerland) and NOVA (Netherlands). SPHERE also received funding from the European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004–2008), grant number 226604 for FP7 (2009–2012) and grant number 312430 for FP7 (2013–2016).

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Earth and Planetary Astrophysics
Abstract

HD95086 (A8V, 17Myr) hosts a rare planetary system for which a multi-belt debris disk and a giant planet of 4-5MJup have been directly imaged. Our study aims to characterize the physical and orbital properties of HD95086b, search for additional planets at short and wide orbits and image the cold outer debris belt in scattered light. We used HARPS at the ESO 3.6m telescope to monitor the radial velocity of HD95086 over 2 years and investigate the existence of giant planets at less than 3au orbital distance. With the IRDIS dual-band imager and the IFS integral field spectrograph of SPHERE at VLT, we imaged the faint circumstellar environment beyond 10au at six epochs between 2015 and 2017. We do not detect additional giant planets around HD95086. We identified the nature (bound companion or background contaminant) of all point-like sources detected in the IRDIS field of view. None of them correspond to the ones recently discovered near the edge of the cold outer belt by ALMA. HD95086b is resolved for the first time in J-band with IFS. Its near-infrared spectral energy distribution is well fitted by a few dusty and/or young L7-L9 dwarf spectral templates. The extremely red 1-4um spectral distribution is typical of low-gravity objects at the L/T spectral type transition. The planet's orbital motion is resolved between January 2015 and May 2017. Together with past NaCo measurements properly re-calibrated, our orbital fitting solutions favor a retrograde low to moderate-eccentricity orbit e=0.2 (0.0 to 0.5), with a semi-major axis 52au corresponding to orbital periods of 288$ yrs and an inclination that peaks at i = 141deg, which is compatible with a planet-disk coplanar configuration. Finally, we report the detection in polarimetric differential imaging of the cold outer debris belt between 100 and 300au, consistent in radial extent with recent ALMA 1.3mm resolved observations., Comment: 23 pages, 19 figures, accepted in A&A (Dec 28th, 2017)

Published
2018
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56. Investigating the young solar system analog HD 95086. A combined HARPS and SPHERE exploration

Author

Chauvin, G., Gratton, R., Bonnefoy, M., Lagrange, A. -M., de Boer, J., Vigan, A., Beust, H., Lazzoni, C., Boccaletti, A., Galicher, R., Desidera, S., Delorme, P., Keppler, M., Lannier, J., Maire, A. -L., Mesa, D., Meunier, N., Kral, Q., Henning, T., Menard, F., Moor, A., Avenhaus, H., Bazzon, A., Janson, M., Beuzit, J. -L., Bhowmik, T., Bonavita, M., Borgniet, S., Brandner, W., Cheetham, A., Cudel, M., Feldt, M., Fontanive, C., Ginski, C., Hagelberg, J., Janin-Potiron, P., Lagadec, E., Langlois, M., Le Coroller, H., Messina, S., Meyer, M., Mouillet, D., Peretti, S., Perrot, C., Rodet, L., Samland, M., Sissa, E., Olofsson, J., Salter, G., Schmidt, T., Zurlo, A., Milli, J., van Boekel, R., Quanz, S., Feautrier, P., Le Mignant, D., Perret, D., and Rochat, J. Ramos and S.

Published
2018

58. Hint of curvature in the orbital motion of the exoplanet 51 Eridani b using 3 yr of VLT/SPHERE monitoring

Author

Maire, A.-L., primary, Rodet, L., additional, Cantalloube, F., additional, Galicher, R., additional, Brandner, W., additional, Messina, S., additional, Lazzoni, C., additional, Mesa, D., additional, Melnick, D., additional, Carson, J., additional, Samland, M., additional, Biller, B. A., additional, Boccaletti, A., additional, Wahhaj, Z., additional, Beust, H., additional, Bonnefoy, M., additional, Chauvin, G., additional, Desidera, S., additional, Langlois, M., additional, Henning, T., additional, Janson, M., additional, Olofsson, J., additional, Rouan, D., additional, Ménard, F., additional, Lagrange, A.-M., additional, Gratton, R., additional, Vigan, A., additional, Meyer, M. R., additional, Cheetham, A., additional, Beuzit, J.-L., additional, Dohlen, K., additional, Avenhaus, H., additional, Bonavita, M., additional, Claudi, R., additional, Cudel, M., additional, Daemgen, S., additional, D’Orazi, V., additional, Fontanive, C., additional, Hagelberg, J., additional, Le Coroller, H., additional, Perrot, C., additional, Rickman, E., additional, Schmidt, T., additional, Sissa, E., additional, Udry, S., additional, Zurlo, A., additional, Abe, L., additional, Origné, A., additional, Rigal, F., additional, Rousset, G., additional, Roux, A., additional, and Weber, L., additional

Published
2019
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60. High-contrast study of the candidate planets and protoplanetary disk around HD 100546

Author

Sissa, E., Gratton, R., Garufi, A., Rigliaco, E., Zurlo, A., Mesa, D., Langlois, M., de Boer, J., Desidera, S., Ginski, C., Lagrange, A. -M., Maire, A. -L., Vigan, A., Dima, M., Antichi, J., Baruffolo, A., Bazzon, A., Benisty, M., Beuzit, J. -L., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Brandner, W., Bruno, P., Buenzli, E., Cascone, E., Chauvin, G., Cheetham, A., Claudi, R. U., Cudel, M., De Caprio, V., Dominik, C., Fantinel, D., Farisato, G., Feldt, M., Fontanive, C., Galicher, R., Giro, E., Hagelberg, J., Incorvaia, S., Janson, Markus, Kasper, M., Keppler, M., Kopytova, T., Lagadec, E., Lannier, J., Lazzoni, C., LeCoroller, H., Lessio, L., Ligi, R., Marzari, F., Menard, F., Meyer, M. R., Mouillet, D., Peretti, S., Perrot, C., Potiron, P. J., Rouan, D., Salasnich, B., Salter, G., Samland, M., Schmidt, T., Scuderi, S., Wildi, F., Sissa, E., Gratton, R., Garufi, A., Rigliaco, E., Zurlo, A., Mesa, D., Langlois, M., de Boer, J., Desidera, S., Ginski, C., Lagrange, A. -M., Maire, A. -L., Vigan, A., Dima, M., Antichi, J., Baruffolo, A., Bazzon, A., Benisty, M., Beuzit, J. -L., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Brandner, W., Bruno, P., Buenzli, E., Cascone, E., Chauvin, G., Cheetham, A., Claudi, R. U., Cudel, M., De Caprio, V., Dominik, C., Fantinel, D., Farisato, G., Feldt, M., Fontanive, C., Galicher, R., Giro, E., Hagelberg, J., Incorvaia, S., Janson, Markus, Kasper, M., Keppler, M., Kopytova, T., Lagadec, E., Lannier, J., Lazzoni, C., LeCoroller, H., Lessio, L., Ligi, R., Marzari, F., Menard, F., Meyer, M. R., Mouillet, D., Peretti, S., Perrot, C., Potiron, P. J., Rouan, D., Salasnich, B., Salter, G., Samland, M., Schmidt, T., Scuderi, S., and Wildi, F.

Abstract

The nearby Herbig Be star HD 100546 is known to be a laboratory for the study of protoplanets and their relation with the circum stellar disk, which is carved by at least two gaps. We observed the HD 100546 environment with high-contrast imaging exploiting several different observing modes of SPHERE, including data sets with and without coronagraphs, dual band imaging, integral field spectroscopy and polarimetry. The picture emerging from these different data sets is complex. Flux-conservative algorithm images clearly show the disk up to 200 au. More aggressive algorithms reveal several rings and warped arms that are seen overlapping the main disk. Some of these structures are found to lie at considerable height over the disk mid-plane at about 30 au. Our images demon-strate that the brightest wings close to the star in the near side of the disk are a unique structure, corresponding to the outer edge of the intermediate disk at similar to 40 au. Modeling of the scattered light from the disk with a geometrical algorithm reveals that a moderately thin structure (H/r = 0.18 at 40 au) can well reproduce the light distribution in the flux-conservative images. We suggest that the gap between 44 and 113 au spans between the 1:2 and 3:2 resonance orbits of a massive body located at similar to 70 au, which might coincide with the candidate planet HD 100546b detected with previous thermal infrared (IR) observations. In this picture, the two wings can be the near side of a ring formed by disk material brought out of the disk at the 1:2 resonance with the same massive object. While we find no clear evidence confirming detection of the planet candidate HD 100546c in our data, we find a diffuse emission close to the expected position of HD 100546b. This source can be described as an extremely reddened substellar object surrounded by a dust cloud or its circumplanetary disk. Its astrometry is broadly consistent with a circular orbital motion on the disk plane, a result that could

Published
2018
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61. The Y dwarf population with HST: unlocking the secrets of our coolest neighbours – I. Overview and first astrometric results.

Author

Fontanive, C, Bedin, L R, and Bardalez Gagliuffi, D C

Subjects
*BROWN dwarf stars, *SPACE telescopes, *PARALLAX, *SECRECY, *NEIGHBORS
Abstract

In this paper, we present our project that aims at determining accurate distances and proper motions for the Y brown dwarf population using the Hubble Space Telescope. We validate the program with our first results, using a single new epoch of observations of the Y0pec dwarf WISE J163940.83−684738.6. These new data allowed us to refine its proper motion and improve the accuracy of its parallax by a factor of three compared to previous determinations, now constrained to ϖ = 211.11 ± 0.56 mas. This newly derived absolute parallax corresponds to a distance of 4.737 ± 0.013 pc, an exquisite and unprecedented precision for faint ultracool Y dwarfs. [ABSTRACT FROM AUTHOR]

Published
2021
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62. Orbiting a binary: SPHERE characterisation of the HD 284149 system

Author

Bonavita, M., d'Orazi, V., Mesa, D., Fontanive, C., Desidera, S., Messina, S., Daemgen, S., Gratton, R., Vigan, Arthur, Bonnefoy, M., Zurlo, A., Antichi, J., Avenhaus, H., Baruffolo, A., Baudino, J. L., Beuzit, J. L., Boccaletti, A., Bruno, P., Buey, T., Carbillet, M., Cascone, E., Chauvin, G., Claudi, R. U., de Caprio, V., Fantinel, D., Farisato, G., Feldt, M., Galicher, R., Giro, E., Gry, C., Hagelberg, J., Incorvaia, S., Janson, M., Jaquet, M., Lagrange, A. M., Langlois, M., Lannier, J., Le Coroller, H., Lessio, L., Ligi, R., Maire, A. L., Meyer, M., Menard, F., Perrot, C., Peretti, S., Petit, C., Ramos, J., Roux, A., Salasnich, B., Salter, G., Samland, M., Scuderi, S., Schlieder, J., Surez, M., Turatto, M., Weber, L., INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), SUPA, Institute for Astronomy, University of Edinburgh, Monash University [Melbourne], Institute for Astronomy [Edinburgh] (IfA), INAF - Osservatorio Astrofisico di Catania (OACT), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Universidad Diego Portales [Santiago] (UDP), INAF - Osservatorio Astrofisico di Arcetri (OAA), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Oxford, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Capodimonte (OAC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Milano (OAM), Department of Astronomy, Stockholm University, Max Planck Institute for Radio Astronomy, Département de Physique Nucléaire (ex SPhN) (DPHN), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Franco-Chilien d'Astronomie (LFCA), Universidad de Chile = University of Chile [Santiago] (UCHILE)-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción - University of Concepcion [Chile], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), ONERA, NASA Goddard Space Flight Center (GSFC), Centre de Recherche en Acquisition et Traitement de l'Image pour la Santé (CREATIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), 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), University of Oxford [Oxford], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Chile, Université de Genève (UNIGE), Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL)

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], stars: individual: HD 284149, stars: rotation, techniques: high angular resolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], binaries: visual, brown dwarfs
Abstract

International audience; Aims. In this paper we present the results of the SPHERE observation of the HD 284149 system, aimed at a more detailed characterisation of both the primary and its brown dwarf companion. Methods. We observed HD 284149 in the near-infrared with SPHERE, using the imaging mode (IRDIS+IFS) and the long-slit spectroscopy mode (IRDIS-LSS). The data were reduced using the dedicated SPHERE pipeline, and algorithms such as PCA and TLOCI were applied to reduce the speckle pattern. Results. The IFS images revealed a previously unknown low-mass (~0.16 M ⊙ ) stellar companion ( HD 294149 B) at ~0.1′′, compatible with previously observed radial velocity differences, as well as proper motion differences between Gaia and Tycho -2 measurements. The known brown dwarf companion ( HD 284149 b) is clearly visible in the IRDIS images. This allowed us to refine both its photometry and astrometry. The analysis of the medium resolution IRDIS long slit spectra also allowed a refinement of temperature and spectral type estimates. A full reassessment of the age and distance of the system was also performed, leading to more precise values of both mass and semi-major axis. Conclusions. As a result of this study, HD 284149 ABb therefore becomes the latest addition to the (short) list of brown dwarfs on wide circumbinary orbits, providing new evidence to support recent claims that object in such configuration occur with a similar frequency to wide companions to single stars.

Published
2017
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63. High-contrast study of the candidate planets and protoplanetary disk around HD 100546

Author

Sissa, E., primary, Gratton, R., additional, Garufi, A., additional, Rigliaco, E., additional, Zurlo, A., additional, Mesa, D., additional, Langlois, M., additional, de Boer, J., additional, Desidera, S., additional, Ginski, C., additional, Lagrange, A.-M., additional, Maire, A.-L., additional, Vigan, A., additional, Dima, M., additional, Antichi, J., additional, Baruffolo, A., additional, Bazzon, A., additional, Benisty, M., additional, Beuzit, J.-L., additional, Biller, B., additional, Boccaletti, A., additional, Bonavita, M., additional, Bonnefoy, M., additional, Brandner, W., additional, Bruno, P., additional, Buenzli, E., additional, Cascone, E., additional, Chauvin, G., additional, Cheetham, A., additional, Claudi, R. U., additional, Cudel, M., additional, De Caprio, V., additional, Dominik, C., additional, Fantinel, D., additional, Farisato, G., additional, Feldt, M., additional, Fontanive, C., additional, Galicher, R., additional, Giro, E., additional, Hagelberg, J., additional, Incorvaia, S., additional, Janson, M., additional, Kasper, M., additional, Keppler, M., additional, Kopytova, T., additional, Lagadec, E., additional, Lannier, J., additional, Lazzoni, C., additional, LeCoroller, H., additional, Lessio, L., additional, Ligi, R., additional, Marzari, F., additional, Menard, F., additional, Meyer, M. R., additional, Mouillet, D., additional, Peretti, S., additional, Perrot, C., additional, Potiron, P. J., additional, Rouan, D., additional, Salasnich, B., additional, Salter, G., additional, Samland, M., additional, Schmidt, T., additional, Scuderi, S., additional, and Wildi, F., additional

Published
2018
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65. Orbiting a binary

Author

Bonavita, M., primary, D’Orazi, V., additional, Mesa, D., additional, Fontanive, C., additional, Desidera, S., additional, Messina, S., additional, Daemgen, S., additional, Gratton, R., additional, Vigan, A., additional, Bonnefoy, M., additional, Zurlo, A., additional, Antichi, J., additional, Avenhaus, H., additional, Baruffolo, A., additional, Baudino, J. L., additional, Beuzit, J. L., additional, Boccaletti, A., additional, Bruno, P., additional, Buey, T., additional, Carbillet, M., additional, Cascone, E., additional, Chauvin, G., additional, Claudi, R. U., additional, De Caprio, V., additional, Fantinel, D., additional, Farisato, G., additional, Feldt, M., additional, Galicher, R., additional, Giro, E., additional, Gry, C., additional, Hagelberg, J., additional, Incorvaia, S., additional, Janson, M., additional, Jaquet, M., additional, Lagrange, A. M., additional, Langlois, M., additional, Lannier, J., additional, Le Coroller, H., additional, Lessio, L., additional, Ligi, R., additional, Maire, A. L., additional, Meyer, M., additional, Menard, F., additional, Perrot, C., additional, Peretti, S., additional, Petit, C., additional, Ramos, J., additional, Roux, A., additional, Salasnich, B., additional, Salter, G., additional, Samland, M., additional, Scuderi, S., additional, Schlieder, J., additional, Surez, M., additional, Turatto, M., additional, and Weber, L., additional

Published
2017
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66. Shadows and spirals in the protoplanetary disk HD 100453

Author

Benisty, M., primary, Stolker, T., additional, Pohl, A., additional, de Boer, J., additional, Lesur, G., additional, Dominik, C., additional, Dullemond, C. P., additional, Langlois, M., additional, Min, M., additional, Wagner, K., additional, Henning, T., additional, Juhasz, A., additional, Pinilla, P., additional, Facchini, S., additional, Apai, D., additional, van Boekel, R., additional, Garufi, A., additional, Ginski, C., additional, Ménard, F., additional, Pinte, C., additional, Quanz, S. P., additional, Zurlo, A., additional, Boccaletti, A., additional, Bonnefoy, M., additional, Beuzit, J. L., additional, Chauvin, G., additional, Cudel, M., additional, Desidera, S., additional, Feldt, M., additional, Fontanive, C., additional, Gratton, R., additional, Kasper, M., additional, Lagrange, A.-M., additional, LeCoroller, H., additional, Mouillet, D., additional, Mesa, D., additional, Sissa, E., additional, Vigan, A., additional, Antichi, J., additional, Buey, T., additional, Fusco, T., additional, Gisler, D., additional, Llored, M., additional, Magnard, Y., additional, Moeller-Nilsson, O., additional, Pragt, J., additional, Roelfsema, R., additional, Sauvage, J.-F., additional, and Wildi, F., additional

Published
2016
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67. Investigating the young solar system analog HD 95086

Author

Chauvin, G., Gratton, R., Bonnefoy, M., Boer, J., Beust, H., Lazzoni, C., Boccaletti, A., Galicher, R., Desidera, S., Delorme, P., Keppler, M., Lannier, J., Maire, A., Mesa, D., Meunier, N., Kral, Q., Henning, T., Menard, F., Moor, A., Avenhaus, H., Bazzon, A., Janson, M., Beuzit, J., Bhowmik, T., Bonavita, M., Borgniet, S., Brandner, W., Cheetham, A., Cudel, M., Feldt, M., Fontanive, C., Ginski, C., Hagelberg, J., Janin-Potiron, P., Eric Lagadec, M. Langlois, Le Coroller, H., Messina, S., Meyer, M., Mouillet, D., Peretti, S., Perrot, C., Rodet, L., Samland, M., Sissa, E., Olofsson, J., Salter, G., Schmidt, T., Zurlo, A., Milli, J., Boekel, R., Quanz, S., Feautrier, P., Le Mignant, D., Perret, D., Ramos, J., Rochat, S., Arthur Vigan, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, University of Cambridge [UK] (CAM), Universidad de Chile = University of Chile [Santiago] (UCHILE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'interaction du rayonnement X avec la matière (LIXAM), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Groupe d'Acoustique de l'Université de Sherbrooke (GAUS), Département de génie mécanique [Sherbrooke] (UdeS), Université de Sherbrooke (UdeS)-Université de Sherbrooke (UdeS), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Universidad de Chile (UCHILE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Centre National de la Recherche Scientifique (CNRS), Département de génie mécanique [Sherbrooke], Université de Sherbrooke [Sherbrooke]-Université de Sherbrooke [Sherbrooke], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

68. SPHERE+: Imaging young Jupiters down to the snowline

Author

Boccaletti, A., Chauvin, G., Mouillet, D., Absil, O., Allard, F., Antoniucci, S., C Augereau, J., Barge, P., Baruffolo, A., L Baudino, J., Baudoz, P., Beaulieu, M., Benisty, M., L Beuzit, J., Bianco, A., Biller, B., Bonavita, B., Bonnefoy, M., Bos, S., C Bouret, J., Brandner, W., Buchschache, N., Carry, B., Cantalloube, F., Cascone, E., Carlotti, A., Charnay, B., Chiavassa, A., Choquet, E., Clenet, Y., Crida, A., Boer, J., Caprio, V., Desidera, S., M Desert, J., B Delisle, J., Delorme, P., Dohlen, K., Doelman, D., Dominik, C., Orazi, V. D., Dougados, C., Doute, S., Fedele, D., Feldt, M., Ferreira, F., Fontanive, C., Thierry Fusco, Galicher, R., Garufi, A., Gendron, E., Ghedina, A., Ginski, C., F Gonzalez, J., Gratadour, D., Gratton, R., Guillot, T., Haffert, S., Hagelberg, J., Henning, T., Huby, E., Janson, M., Kamp, I., Keller, C., Kenworthy, M., Kervella, P., Kral, Q., Kuhn, J., Lagadec, E., Laibe, G., Langlois, M., M Lagrange, A., Launhardt, R., Leboulleux, L., Le Coroller, H., Li Causi, G., Loupias, M., Maire, A. L., Marleau, G., Martinache, F., Martinez, P., Mary, D., Mattioli, M., Mazoyer, J., Meheut, H., Menard, F., Mesa, D., Meunier, N., Miguel, Y., Milli, J., Min, M., Molliere, P., Mordasini, C., Moretto, G., Mugnier, L., Muro Arena, G., Nardetto, N., Diaye, M. N., Nesvadba, N., Pedichini, F., Pinilla, P., Por, E., Potier, A., Quanz, S., Rameau, J., Roelfsema, R., Rouan, D., Rigliaco, E., Salasnich, B., Samland, M., F Sauvage, J., M Schmid, H., Segransan, D., Snellen, I., Snik, F., Soulez, F., Stadler, E., Stam, D., Tallon, M., Thebault, P., Thiebaut, E., Tschudi, C., Udry, S., Holstein, R., Vernazza, P., Vidal, F., Vigan, A., Waters, R., Wildi, F., Willson, M., Zanutta, A., Annie Zavagno, and Zurlo, A.

69. Constraining masses and separations of unseen companions to five accelerating nearby stars

Author

Mesa, D., Bonavita, M., Benatti, S., Gratton, R., Marino, S., Kervella, P., D’ Orazi, V., Desidera, S., Henning, T., Janson, M., Langlois, M., Rickman, E., Vigan, A., Zurlo, A., Baudino, J.-L., Biller, B., Boccaletti, A., Bonnefoy, M., Brandner, W., Buenzli, E., Cantalloube, F., Fantinel, D., Fontanive, C., Galicher, R., Ginski, C., Girard, J., Hagelberg, J., Kopytova, T., Lagrange, A.-M., Lazzoni, C., Le Coroller, H., Ligi, R., Llored, M., Maire, A.-L., Mouillet, D., Perrot, C., Rochat, S., Romero, C., Rouan, D., Samland, M., Schmidt, T. O. B., Sissa, E., Wildi, F., Mesa, D., Bonavita, M., Benatti, S., Gratton, R., Marino, S., Kervella, P., D’ Orazi, V., Desidera, S., Henning, T., Janson, M., Langlois, M., Rickman, E., Vigan, A., Zurlo, A., Baudino, J.-L., Biller, B., Boccaletti, A., Bonnefoy, M., Brandner, W., Buenzli, E., Cantalloube, F., Fantinel, D., Fontanive, C., Galicher, R., Ginski, C., Girard, J., Hagelberg, J., Kopytova, T., Lagrange, A.-M., Lazzoni, C., Le Coroller, H., Ligi, R., Llored, M., Maire, A.-L., Mouillet, D., Perrot, C., Rochat, S., Romero, C., Rouan, D., Samland, M., Schmidt, T. O. B., Sissa, E., and Wildi, F.

Abstract

Aims. In this work, we aim to constrain the masses and separations of potential substellar companions to five accelerating stars (HIP 1481, HIP 88399, HIP 96334, HIP 30314, and HIP 116063) using multiple data sets acquired with different techniques. Methods. Our targets were originally observed as part of the SPHERE/SHINE survey, and radial velocity (RV) archive data were also available for four of the five objects. No companions were originally detected in any of these data sets, but the presence of significant proper motion anomalies (PMas) for all the stars strongly suggested the presence of a companion. Combining the information from the PMas with the limits derived from the RV and SPHERE data, we were able to put constraints on the characteristics of the unseen companions. Results. Our analysis led to relatively strong constraints for both HIP 1481 and HIP 88399, narrowing down the companion masses to 2–5 MJup and 3–5 MJup and separations within 2–15 au and 3–9 au, respectively. Because of the large age uncertainties for HIP 96334, the poor observing conditions for the SPHERE epochs of HIP 30314, and the lack of RV data for HIP 116063, the results for these targets were not as well defined, but we were still able to constrain the properties of the putative companions within a reasonable confidence level. Conclusions. For all five targets, our analysis reveals that the companions responsible for the PMa signal would be well within reach for future instruments planned for the ELT (e.g., MICADO), which would easily achieve the required contrast and angular resolution. Our results therefore represent yet another confirmation of the power of multi-technique approaches for both the discovery and characterisation of planetary systems.

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