Author: "Wahhaj, Z." - Searchworks@Jio Institute Digital Library Search Results

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291 results on '"Wahhaj, Z."'

51. Empirical contrast model for high-contrast imaging. A VLT/SPHERE case study

Author: Courtney-Barrer, B., primary, De Rosa, R., additional, Kokotanekova, R., additional, Romero, C., additional, Jones, M., additional, Milli, J., additional, and Wahhaj, Z., additional
Published: 2023
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52. The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds: VI. Perseus Observed with MIPS

Author: Rebull, L. M., Stapelfeldt, K. R., Evans II, N. J., Joergensen, J. K., Harvey, P. M., Brooke, T. Y., Bourke, T. L., Padgett, D. L., Chapman, N. L., Lai, S. -P., Spiesmann, W. J., Noreiga-Crespo, A., Merin, B., Huard, T., Allen, L. E., Blake, G. A., Jarrett, T., Koerner, D. W., Mundy, L. G., Myers, P. C., Sargent, A. I., van Dishoeck, E. F., Wahhaj, Z., and Young, K. E.
Subjects: Astrophysics
Abstract: We present observations of 10.6 square degrees of the Perseus molecular cloud at 24, 70, and 160 microns with the Spitzer Space Telescope Multiband Imaging Photometer for Spitzer (MIPS). The image mosaics show prominent, complex extended emission dominated by illuminating B stars on the East side of the cloud, and by cold filaments of 160 micron emission on the West side. Of 3950 point sources identified at 24 microns, 1141 have 2MASS counterparts. A quarter of these populate regions of the Ks vs. Ks-[24] diagram that are distinct from stellar photospheres and background galaxies, and thus are likely to be cloud members with infrared excess. Nearly half (46%) of these 24 micron excess sources are distributed outside the IC 348 and NGC 1333 clusters. NGC 1333 shows the highest fraction of stars with flat or rising spectral energy distributions (28%), while Class II SEDs are most common in IC 348. These results are consistent with previous relative age determinations for the two clusters. The intercluster region contains several tightly clumped (r~0.1 pc) young stellar aggregates whose members exhibit a wide variety of infrared spectral energy distributions characteristic of different circumstellar environments. One possible explanation is a significant age spread among the aggregate members, such that some have had time to evolve more than others. Alternatively, if the aggregate members all formed at roughly the same time, then remarkably rapid circumstellar evolution would be required to account for the association of Class I and Class III sources at ages <~1 Myr. We highlight important results for several other objects as well (full abstract in the paper)., Comment: 82 pages, 32 figures, accepted to ApJS; ALL figures (even line drawings) had to be degraded to be accepted by the system here; the full-res figures are available in the version linked from the 'publications' area available at http://peggysue.as.utexas.edu/SIRTF/
Published: 2007
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53. High-Resolution Imaging of the Dust Disk around 49 Ceti

Author: Wahhaj, Z., Koerner, D. W., and Sargent, A. I.
Subjects: Astrophysics
Abstract: Sub-arcsecond scale Keck images of the young A1V star, 49 Ceti, resolve emission at lambda = 12.5 and 17.9 microns from a disk with long axis at PA 125 pm 10 degrees and inclination phi = 60 pm 15 degrees . At 17.9 microns, the emission is brighter and more extended toward the NW than the SE. Modeling of the mid-infrared images combined with flux densities from the literature indicate that the bulk of the mid-infrared emission comes from very small grains (a ~ 0.1 microns) confined between 30 and 60 AU from the star. This population of dust grains contributes negligibly to the significant excess observed in the spectral energy distribution. Most of the non- photospheric energy is radiated at longer wavelengths by an outer disk of larger grains (a ~ 15 microns), inner radius ~ 60 AU, and outer radius ~ 900 AU. Global properties of the 49 Cet disk show more affinity with the Beta Pic and HR 4796A disks than with other debris disks. This may be because they are all very young (t < 20 Myr), adding strength to the argument that they are transitional objects between Herbig Ae and "Vega-like" A stars with more tenuous circumstellar disks., Comment: 19 pages, 6 figures. Accepted for publicaion in ApJ
Published: 2007
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54. The Spitzer c2d Survey of Nearby Dense Cores: I: First Direct Detection of the Embedded Source in IRAM 04191+1522

Author: Dunham, M. M., Evans II, N. J., Bourke, T. L., Dullemond, C. P., Young, C. H., Brooke, T. Y., Chapman, N., Myers, P. C., Porras, A., Spiesman, W., Teuben, P. J., and Wahhaj, Z.
Subjects: Astrophysics
Abstract: We report the first detections of the Class 0 protostellar source IRAM 04191+1522 at wavelengths shortward of 60 microns with the Spitzer Space Telescope. We see extended emission in the Spitzer images that suggests the presence of an outflow cavity in the circumstellar envelope. We combine the Spitzer observations with existing data to form a complete dataset ranging from 3.6 to 1300 microns and use these data to construct radiative transfer models of the source. We conclude that the internal luminosity of IRAM 04191+1522, defined to be the sum of the luminosity from the internal sources (a star and a disk), is L_int = 0.08 +/- 0.04 L_sun, placing it among the lowest luminosity protostars known. Though it was discovered before the launch of the Spitzer Space Telescope, IRAM 04191+1522 falls within a new class of Very Low Luminosity Objects being discovered by Spitzer. Unlike the two other well-studied objects in this class, which are associated either with weak, compact outflows or no outflows at all, IRAM 04191+1522 has a well-defined molecular outflow with properties consistent with those expected based on relations derived from higher luminosity (L_int > 1 L_sun) protostars. We discuss the difficulties in understanding IRAM 04191+1522 in the context of the standard model of star formation, and suggest a possible explanation for the very low luminosity of this source., Comment: Accepted for publication in the Astrophysical Journal. 39 pages, 9 figures. See http://peggysue.as.utexas.edu/SIRTF/ for high-resolution figures
Published: 2006
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55. Weak-line T Tauri Star Disks I. Initial Spitzer Results from the Cores to Disks Legacy Project

Author: Padgett, D. L., Cieza, L., Stapelfeldt, K. R., Evans, N. J., Koerner, D., Sargent, A., Fukagawa, M., van Dishoek, E. F., Augereau, J., Allen, L., Blake, G., Brooke, T., Chapman, N., Harvey, P., Porras, A., Lai, S., Mundy, L., Myers, P. C., Spiesman, W., and Wahhaj, Z.
Subjects: Astrophysics
Abstract: Using the Spitzer Space Telescope, we have observed 90 weak-line and classical T Tauri stars in the vicinity of the Ophiuchus, Lupus, Chamaeleon, and Taurus star-forming regions as part of the Cores to Disks (c2d) Spitzer Legacy project. In addition to the Spitzer data, we have obtained contemporaneous optical photometry to assist in constructing spectral energy distributions. These objects were specifically chosen as solar-type young stars with low levels of H alpha emission, strong X-ray emission, and lithium absorption i.e. weak-line T Tauri stars, most of which were undetected in the mid-to-far IR by the IRAS survey. Weak-line T Tauri stars are potentially extremely important objects in determining the timescale over which disk evolution may take place. Our objective is to determine whether these young stars are diskless or have remnant disks which are below the detection threshold of previous infrared missions. We find that only 5/83 weak-line T Tauri stars have detectable excess emission between 3.6 and 70 micron which would indicate the presence of dust from the inner few tenths of an AU out to the planet-forming regions a few tens of AU from the star. Of these sources, two have small excesses at 24 microns consistent with optically thin disks; the others have optically thick disks already detected by previous IR surveys. All of the seven classical T Tauri stars show excess emission at 24 and 70 micron, although their properties vary at the shorter wavelengths. Our initial results show that disks are rare among young stars selected for their weak H alpha emission., Comment: 29 pages, 9 figures, accepted for publication in ApJ
Published: 2006

56. The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds. I. Chamaeleon II Observed with MIPS

Author: Young, K. E., Harvey, P. M., Brooke, T. Y., Chapman, N., Kauffmann, J., Bertoldi, F., Lai, S. -P., Alcala', J., Bourke, T. L., Spiesman, W., Allen, L. E., Blake, G. A., Evans II, N. J., Koerner, D. W., Mundy, L. G., Myers, P. C., Padgett, D. L., Salinas, A., Sargent, A. I., Stapelfeldt, K. R., Teuben, P., van Dishoeck, E. F., and Wahhaj, Z.
Subjects: Astrophysics
Abstract: We present maps of over 1.5 square degrees in Chamaeleon (Cha) II at 24, 70, and 160 micron observed with the Spitzer Space Telescope Multiband Imaging Photometer for Spitzer (MIPS) and a 1.2 square degree millimeter map from SIMBA on the Swedish-ESO Submillimetre Telescope (SEST). The c2d Spitzer Legacy Team's data reduction pipeline is described in detail. Over 1500 24 micron sources and 41 70 micron sources were detected by MIPS with fluxes greater than 10-sigma. More than 40 potential YSOs are identified with a MIPS and 2MASS color-color diagram and by their spectral indices, including two previously unknown sources with 24 micron excesses. Our new SIMBA millimeter map of Cha II shows that only a small fraction of the gas is in compact structures with high column densities. The extended emission seen by MIPS is compared with previous CO observations. Some selected interesting sources, including two detected at 1 mm, associated with Cha II are discussed in detail and their SEDs presented. The classification of these sources using MIPS data is found to be consistent with previous studies., Comment: 44 pages, 12 figures (1 color), to be published in ApJ
Published: 2005
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57. Radial Distribution of Dust Grains Around HR 4796A

Author: Wahhaj, Z., Koerner, D. W., Backman, D. E., Werner, M. W., Serabyn, E., Ressler, M. E., and Lis, D. C.
Subjects: Astrophysics
Abstract: We present high-dynamic-range images of circumstellar dust around HR 4796A that were obtained with MIRLIN at the Keck II telescope at lambda = 7.9, 10.3, 12.5 and 24.5 um. We also present a new continuum measurement at 350 um obtained at the Caltech Submillimeter Observatory. Emission is resolved in Keck images at 12.5 and 24.5 um with PSF FWHM's of 0.37" and 0.55", respectively, and confirms the presence of an outer ring centered at 70 AU. Unresolved excess infrared emission is also detected at the stellar position and must originate well within 13 AU of the star. A model of dust emission fit to flux densities at 12.5, 20.8, and 24.5 um indicates dust grains are located 4(+3/-2) AU from the star with effective size, 28+/-6 um, and an associated temperature of 260+/-40 K. We simulate all extant data with a simple model of exozodiacal dust and an outer exo-Kuiper ring. A two-component outer ring is necessary to fit both Keck thermal infrared and HST scattered-light images. Bayesian parameter estimates yield a total cross-sectional area of 0.055 AU^2 for grains roughly 4 AU from the star and an outer-dust disk composed of a narrow large-grain ring embedded within a wider ring of smaller grains. The narrow ring is 14+/-1 AU wide with inner radius 66+/-1 AU and total cross-sectional area 245 AU^2. The outer ring is 80+/-15 AU wide with inner radius 45+/-5 AU and total cross-sectional area 90 AU^2. Dust grains in the narrow ring are about 10 times larger and have lower albedos than those in the wider ring. These properties are consistent with a picture in which radiation pressure dominates the dispersal of an exo-Kuiper belt., Comment: Accepted by Astrophysical Journal (Part1) on September 9, 2004. 13 pages, 10 figures, 2 tables
Published: 2004
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58. A 'Starless' Core that Isn't: Detection of a Source in the L1014 Dense Core with the Spitzer Space Telescope

Author: Young, C. H., Joergensen, J. K., Shirley, Y. L., Kauffmann, J., Huard, T., Lai, S. -P., Lee, C. W., Crapsi, A., Bourke, T. L., Dullemond, C. P., Brooke, T. Y., Porras, A., Spiesman, W., Allen, L. E., Blake, G. A., Evans II, N. J., Harvey, P. M., Koerner, D. W., Mundy, L. G., Myers, P. C., Padgett, D. L., Sargent, A. I., Stapelfeldt, K. R., van Dishoeck, E. F., Bertoldi, F., Chapman, N., Cieza, L., DeVries, C. H., Ridge, N. A., and Wahhaj, Z.
Subjects: Astrophysics
Abstract: We present observations of L1014, a dense core in the Cygnus region previously thought to be starless, but data from the Spitzer Space Telescope shows the presence of an embedded source. We propose a model for this source that includes a cold core, heated by the interstellar radiation field, and a low-luminosity internal source. The low luminosity of the internal source suggests a substellar object. If L1014 is representative, other "starless" cores may turn out to harbor central sources., Comment: 7 pages, To appear in the ApJS Spitzer Special Edition
Published: 2004
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59. The Inner Rings of Beta Pictoris

Author: Wahhaj, Z., Koerner, D. W., Ressler, M. E., Werner, M. W., Backman, D. E., and Sargent, A. I.
Subjects: Astrophysics
Abstract: We present Keck images of the dust disk around Beta Pictoris at 17.9 microns that reveal new structure in its morphology. Within 1" (19 AU) of the star, the long axis of the dust emission is rotated by more than 10 degrees with respect to that of the overall disk. This angular offset is more pronounced than the warp detected at 3.5" by HST, and in the opposite direction. By contrast, the long axis of the emission contours at ~ 1.5" from the star is aligned with the HST warp. Emission peaks between 1.5" and 4" from the star hint at the presence of rings similar to those observed in the outer disk at ~ 25" with HST/STIS. A deconvolved image strongly suggests that the newly detected features arise from a system of four non-coplanar rings. Bayesian estimates based on the primary image lead to ring radii of 14+/-1 AU, 28+/-3 AU, 52+/-2 AU and 82+/-2 AU, with orbital inclinations that alternate in orientation relative to the overall disk and decrease in magnitude with increasing radius. We believe these new results make a strong case for the existence of a nascent planetary system around Beta Pic., Comment: 5 pages, 2 figures, PDF format. Published in ApJL, December 20,2002
Published: 2002
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60. SPHERE adaptive optics performance for faint targets

Author: Jones, M. I., primary, Milli, J., additional, Blanchard, I., additional, Wahhaj, Z., additional, De Rosa, R. J., additional, Romero, C., additional, and Ihanec, N., additional
Published: 2022
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61. Orbital and dynamical analysis of the system around HR 8799

Author: Zurlo, A., primary, Goździewski, K., additional, Lazzoni, C., additional, Mesa, D., additional, Nogueira, P., additional, Desidera, S., additional, Gratton, R., additional, Marzari, F., additional, Langlois, M., additional, Pinna, E., additional, Chauvin, G., additional, Delorme, P., additional, Girard, J. H., additional, Hagelberg, J., additional, Henning, Th., additional, Janson, M., additional, Rickman, E., additional, Kervella, P., additional, Avenhaus, H., additional, Bhowmik, T., additional, Biller, B., additional, Boccaletti, A., additional, Bonaglia, M., additional, Bonavita, M., additional, Bonnefoy, M., additional, Cantalloube, F., additional, Cheetham, A., additional, Claudi, R., additional, D’Orazi, V., additional, Feldt, M., additional, Galicher, R., additional, Ghose, E., additional, Lagrange, A.-M., additional, le Coroller, H., additional, Ligi, R., additional, Kasper, M., additional, Maire, A.-L., additional, Medard, F., additional, Meyer, M., additional, Peretti, S., additional, Perrot, C., additional, Puglisi, A. T., additional, Rossi, F., additional, Rothberg, B., additional, Schmidt, T., additional, Sissa, E., additional, Vigan, A., additional, and Wahhaj, Z., additional
Published: 2022
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62. Increasing the raw contrast of VLT/SPHERE with the dark hole technique

Author: Potier, A., primary, Mazoyer, J., additional, Wahhaj, Z., additional, Baudoz, P., additional, Chauvin, G., additional, Galicher, R., additional, and Ruane, G., additional
Published: 2022
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63. Calibration of quasi-static aberrations in exoplanet direct-imaging instruments with a Zernike phase-mask sensor

Author: Vigan, A., primary, Dohlen, K., additional, N’Diaye, M., additional, Cantalloube, F., additional, Girard, J. H., additional, Milli, J., additional, Sauvage, J.-F., additional, Wahhaj, Z., additional, Zins, G., additional, Beuzit, J.-L., additional, Caillat, A., additional, Costille, A., additional, Le Merrer, J., additional, Mouillet, D., additional, and Tourenq, S., additional
Published: 2022
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64. 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

65. 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

66. 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

67. 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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68. 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

69. 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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70. 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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71. 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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72. A search for a fifth planet around HR 8799 using the star-hopping RDI technique at VLT/SPHERE

Author: Wahhaj, Z., primary, Milli, J., additional, Romero, C., additional, Cieza, L., additional, Zurlo, A., additional, Vigan, A., additional, Peña, E., additional, Valdes, G., additional, Cantalloube, F., additional, Girard, J., additional, and Pantoja, B., additional
Published: 2021
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73. 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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74. A survey of the linear polarization of directly imaged exoplanets and brown dwarf companions with SPHERE-IRDIS

Author: van Holstein, R.G., primary, Stolker, T., additional, Jensen-Clem, R., additional, Ginski, C., additional, Milli, J., additional, de Boer, J., additional, Girard, J.H., additional, Wahhaj, Z., additional, Bohn, A.J., additional, Millar-Blanchaer, M.A., additional, Benisty, M., additional, Bonnefoy, M., additional, Chauvin, G., additional, Dominik, C., additional, Hinkley, S., additional, Keller, C.U., additional, Keppler, M., additional, Langlois, M., additional, Marino, S., additional, Ménard, F., additional, Perrot, C., additional, Schmidt, T.O.B., additional, Vigan, A., additional, Zurlo, A., additional, and Snik, F., additional
Published: 2021
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75. 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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76. 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

77. A triple star in disarray

Author: Kasper, Marcus, Santhakumari, Kalyan, Herbst, Tom, Van Boekel, Roy, Ménard, F., Gratton, Raffaele, van Holstein, Rob, Langlois, M., Ginski, Christian, Boccaletti, A., Benisty, M., De Boer, J., Delorme, P., Desidera, S., Dominik, C., Hagelberg, J., Henning, T., Heidt, J., Köhler, R., Mesa, D., Messina, S., Pavlov, A., Petit, Cyril, Rickman, E., Roux, A., Rigal, F., Vigan, A., Wahhaj, Z., Zurlo, A., European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Max Planck Institute for Medical Research [Heidelberg], Max-Planck-Gesellschaft, 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, Leiden Observatory [Leiden], Universiteit Leiden, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'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), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Université de Genève = University of Geneva (UNIGE), Max-Planck-Institut für Astronomie (MPIA), Universität Wien, INAF - Osservatorio Astrofisico di Catania (OACT), DOTA, ONERA, Université Paris Saclay [Palaiseau], 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), European Southern Observatory [Santiago] (ESO), Universidad Diego Portales [Santiago] (UDP), ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016), 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), Universiteit Leiden [Leiden], École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'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), and Université de Genève (UNIGE)
Subjects: High angular resolution astronomy, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Star formation, Star wind, Multiple star
Abstract: International audience; Aims. T Tauri remains an enigmatic triple star for which neither the evolutionary state of the stars themselves, nor the geometry of the complex outflow system is completely understood. Eight-meter class telescopes equipped with state-of-the-art adaptive optics provide the spatial resolution necessary to trace tangential motion of features over a timescale of a few years, and they help to associate them with the different outflows.Methods. We used J-, H-, and K-band high-contrast coronagraphic imaging with VLT-SPHERE recorded between 2016 and 2018 to map reflection nebulosities and obtain high precision near-infrared (NIR) photometry of the triple star. We also present H2 emission maps of the ν = 1-0 S(1) line at 2.122 μm obtained with LBT-LUCI during its commissioning period at the end of 2016.Results. The data reveal a number of new features in the system, some of which are seen in reflected light and some are seen in H2 emission; furthermore, they can all be associated with the main outflows. The tangential motion of the features provides compelling evidence that T Tauri Sb drives the southeast–northwest outflow. T Tauri Sb has recently faded probably because of increased extinction as it passes through the southern circumbinary disk. While Sb is approaching periastron, T Tauri Sa instead has brightened and is detected in all our J-band imagery for the first time.
Published: 2020

78. Unveiling the beta Pictoris system, coupling high contrast imaging, interferometric, and radial velocity data

Author: Lagrange, A. M., Rubini, P., Nowak, M., Lacour, S., Grandjean, A., Boccaletti, A., Langlois, M., Delorme, P., Gratton, R., Wang, J., Flasseur, O., Galicher, R., Kral, Q., Meunier, N., Beust, H., Babusiaux, C., Le Coroller, H., Thebault, P., Kervella, P., Zurlo, A., Maire, A.-L., Wahhaj, Z., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J. P., Bonnefoy, M., Brandner, W., Cantalloube, F., Charnay, B., Chauvin, G., Choquet, E., Clenet, Y., Christiaens, V., Coude du Foresto, V., de Zeeuw, P. T., Desidera, S., Duvert, G., Eckart, A., Eisenhauer, F., Galland, F., Gao, F., Garcia, P., Garcia Lopez, R., Gendron, E., Genzel, R., Gillessen, S., Girard, J., Hagelberg, J., Haubois, X., Henning, T., Heissel, G., Hippler, S., Horrobin, M., Janson, Markus, Kammerer, J., Kenworthy, M., Keppler, M., Kreidberg, L., Lapeyrere, V., Le Bouquin, J.-B., Lena, P., Merand, A., Messina, S., Molliere, P., Monnier, J. D., Ott, T., Otten, G., Paumard, T., Paladini, C., Perraut, K., Perrin, G., Pueyo, L., Pfuhl, O., Rodet, L., Rodriguez-Coira, G., Rousset, G., Samland, M., Shangguan, J., Schmidt, T., Straub, O., Straubmeier, C., Stolker, T., Vigan, A., Vincent, F., Widmann, F., Woillez, J., Lagrange, A. M., Rubini, P., Nowak, M., Lacour, S., Grandjean, A., Boccaletti, A., Langlois, M., Delorme, P., Gratton, R., Wang, J., Flasseur, O., Galicher, R., Kral, Q., Meunier, N., Beust, H., Babusiaux, C., Le Coroller, H., Thebault, P., Kervella, P., Zurlo, A., Maire, A.-L., Wahhaj, Z., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J. P., Bonnefoy, M., Brandner, W., Cantalloube, F., Charnay, B., Chauvin, G., Choquet, E., Clenet, Y., Christiaens, V., Coude du Foresto, V., de Zeeuw, P. T., Desidera, S., Duvert, G., Eckart, A., Eisenhauer, F., Galland, F., Gao, F., Garcia, P., Garcia Lopez, R., Gendron, E., Genzel, R., Gillessen, S., Girard, J., Hagelberg, J., Haubois, X., Henning, T., Heissel, G., Hippler, S., Horrobin, M., Janson, Markus, Kammerer, J., Kenworthy, M., Keppler, M., Kreidberg, L., Lapeyrere, V., Le Bouquin, J.-B., Lena, P., Merand, A., Messina, S., Molliere, P., Monnier, J. D., Ott, T., Otten, G., Paumard, T., Paladini, C., Perraut, K., Perrin, G., Pueyo, L., Pfuhl, O., Rodet, L., Rodriguez-Coira, G., Rousset, G., Samland, M., Shangguan, J., Schmidt, T., Straub, O., Straubmeier, C., Stolker, T., Vigan, A., Vincent, F., Widmann, F., and Woillez, J.
Abstract: Context. The nearby and young beta Pictoris system hosts a well resolved disk, a directly imaged massive giant planet orbiting at similar or equal to 9 au, as well as an inner planet orbiting at similar or equal to 2.7 au, which was recently detected through radial velocity (RV). As such, it offers several unique opportunities for detailed studies of planetary system formation and early evolution. Aims. We aim to further constrain the orbital and physical properties of beta Pictoris b and c using a combination of high contrast imaging, long base-line interferometry, and RV data. We also predict the closest approaches or the transit times of both planets, and we constrain the presence of additional planets in the system. Methods. We obtained six additional epochs of SPHERE data, six additional epochs of GRAVITY data, and five additional epochs of RV data. We combined these various types of data in a single Markov-chain Monte Carlo analysis to constrain the orbital parameters and masses of the two planets simultaneously. The analysis takes into account the gravitational influence of both planets on the star and hence their relative astrometry. Secondly, we used the RV and high contrast imaging data to derive the probabilities of presence of additional planets throughout the disk, and we tested the impact of absolute astrometry. Results. The orbital properties of both planets are constrained with a semi-major axis of 9.8 0.4 au and 2.7 +/- 0.02 au for b and c, respectively, and eccentricities of 0.09 +/- 0.1 and 0.27 +/- 0.07, assuming the HIPPARCOS distance. We note that despite these low fitting error bars, the eccentricity of beta Pictoris c might still be over-estimated. If no prior is provided on the mass of beta Pictoris b, we obtain a very low value that is inconsistent with what is derived from brightness-mass models. When we set an evolutionary model motivated prior to the mass of beta Pictoris b, we find a solution in the 10-11 M-Jup range. Conversely, beta P
Published: 2020
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79. Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A close low-mass companion to ET Cha

Author: Ginski, C., primary, Ménard, F., additional, Rab, Ch., additional, Mamajek, E. E., additional, van Holstein, R. G., additional, Benisty, M., additional, Manara, C. F., additional, Asensio Torres, R., additional, Bohn, A., additional, Birnstiel, T., additional, Delorme, P., additional, Facchini, S., additional, Garufi, A., additional, Gratton, R., additional, Hogerheijde, M., additional, Huang, J., additional, Kenworthy, M., additional, Langlois, M., additional, Pinilla, P., additional, Pinte, C., additional, Ribas, Á., additional, Rosotti, G., additional, Schmidt, T. O. B., additional, van den Ancker, M., additional, Wahhaj, Z., additional, Waters, L. B. F. M., additional, Williams, J., additional, and Zurlo, A., additional
Published: 2020
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80. 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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81. Increasing the raw contrast of VLT/SPHERE with the dark hole technique

Author: Potier, A., primary, Galicher, R., additional, Baudoz, P., additional, Huby, E., additional, Milli, J., additional, Wahhaj, Z., additional, Boccaletti, A., additional, Vigan, A., additional, N’Diaye, M., additional, and Sauvage, J.-F., additional
Published: 2020
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82. 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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83. 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

84. The B-Star Exoplanet Abundance Study: a co-moving 16–25 M Jup companion to the young binary system HIP 79098

Author: Carbillet, M., Maurel, D., Origné, A., Rigal, F., Sevin, A., De Boer, J., van Holstein, R. G., Dohlen, K., Snik, F., Keller, C. U., Ginski, C., Stam, D. M., Wahhaj, Z., Kasper, M., Rabou, P., Hugot, E., Perret, D., Martinez, P., Pragt, J., Coroller, H. Le, Dominik, C., Turatto, M., Udry, S., Beuzit, J. -L., Le Coroller, H., Mennesson, B., Bailey, V., Kasdin, J., Trauger, J., Absil, O., Akeson, R., Armus, L., Baudoz, P., Bellini, A., Bennett, D., Berriman, B., Calchi-Novati, S., Carpenter, K., Chen, C., Danchi, W., Debes, J., Defrere, D., Ertel, S., Frerking, M., Gelino, C., Girard, J. H., Groff, T., Kane, S., Helou, G., Kalirai, J., Krist, J., Kruk, J., Hasegawa, Y., Laine, S., Lowrance, P., Malhotra, S., Mandell, A., Marshall, P., McElwain, M., Meshkat, T., Millan-Gabet, R., Moustakas, L., Nemati, B., Paladini, R., Postman, M., Pueyo, L., Quintana, E., Ramirez, S., Rhodes, J., Riggs, A. J. E., Rizzo, M., Soummer, R., Stapelfeldt, K., Stark, C., Turnbull, M., van der Marel, R., Ygouf, M., Wyatt, M., Zhao, F., Zimmerman, N., Loh, Alan, Messina, Sergio, Brandner, Wolfgang, Buenzli, Esther, Daemgen, Sebastien, Lagadec, Eric, Mouillet, David, Peretti, Sébastien, Janin-Potiron, Pierre, Salter, Graeme, Roux, Alain, Llored, Marc, Buey, Jean-Tristan, Pavlov, Alexei, Petit, C., Pawellek, Nicole, Moór, Attila, Milli, Julien, Kóspál, Ágnes, Olofsson, Johan, Ábrahám, Péter, Keppler, Miriam, Kral, Quentin, Pohl, Adriana, Augereau, Jean-Charles, Choquet, Elodie, Engler, Natalia, Lee, Eve J., Thebault, Philippe, Lee, Eve, Podio, L., Bacciotti, F., Antoniucci, S., Codella, C., Dougados, C., Nisini, B., Schmid, H. M., Stolker, T., Baudino, J. L., Biller, Beth, Bonavita, M., Galicher, R., Grandjean, A., Lagrange, Anne-Marie, Lannier, Justine, Maire, Anne-Lise, Perrot, Clément, Delboulbé, A., Mignant, D. Le, Fantinel, D., Moeller-Nilsson, O., Weber, Luc, Sauvage, J. -F., Le Mignant, D., Möller-Nilsson, O., Mesa, Dino, Garufi, A., D'Orazi, V., Flasseur, O., Barbieri, M., Benisty, M., Henning, Thomas, Ligi, R., Sissa, Elena, Zurlo, Alice, Boccaletti, Anthony, Cantalloube, F., Cheetham, Anthony, De Caprio, V., Feldt, Markus, Fusco, T., Gluck, L., Hagelberg, J., Lagrange, A. -M., Lazzoni, C., Madec, F., Maire, A. -L., Ménard, F., Meyer, M., Ramos, J., Rickman, E. L., Rouan, D., Schmidt, T., van der Plas, G., D’Orazi, V., De Caprio, V, Lagrange, A-M, Maire, A-L, Van der Plas, G, Janson, Markus, Asensio-Torres, Ruben, André, Damien, Bonnefoy, Mickaël, Delorme, Philippe, Reffert, Sabine, Desidera, Silvano, Langlois, M, Chauvin, G., Gratton, Raffaele, Bohn, Alexander J., Eriksson, Simon C., Marleau, Gabriel-Dominique, Mamajek, Eric E., Vigan, Arthur, Carson, Joseph C., Bohn, Alexander, Eriksson, Simon, Mamajek, Eric, Carson, Joseph, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], 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), Faculty of Aerospace Engineering [Delft], Delft University of Technology (TU Delft), Department of International Development, University of Oxford [Oxford], 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]), JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY PASADENA USA, Partenaires IRSTEA, Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, 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, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), European Southern Observatory (ESO), 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), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Roma (OAR), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Biochemistry and Molecular Biology, Mayo Clinic, INAF - Osservatorio Astronomico di Padova (OAPD), 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), Collège de France (CdF (institution)), 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, Axe 4 : céramiques sous contraintes environnementales (SPCTS-AXE4), Science des Procédés Céramiques et de Traitements de Surface (SPCTS), Université de Limoges (UNILIM)-Ecole Nationale Supérieure de Céramique Industrielle (ENSCI)-Institut des Procédés Appliqués aux Matériaux (IPAM), Université de Limoges (UNILIM)-Université de Limoges (UNILIM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Limoges (UNILIM)-Ecole Nationale Supérieure de Céramique Industrielle (ENSCI)-Institut des Procédés Appliqués aux Matériaux (IPAM), Université de Limoges (UNILIM)-Université de Limoges (UNILIM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Landessternwarte Königstuhl [ZAH] (LSW), Universität Heidelberg [Heidelberg], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Stockholm University, Universität Heidelberg [Heidelberg] = Heidelberg University, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de Ingeniería Matemática [Santiago] (DIM), Universidad de Chile = University of Chile [Santiago] (UCHILE)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden, Institut für Astronomie und Astrophysik [Tübingen] (IAAT), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Department of Physics and Astronomy [Rochester], University of Rochester [USA], College of Charleston, ANR-10-LABX-0056,OSUG@2020,Innovative strategies for observing and modelling natural systems(2010), and European Project: 678194,H2020,ERC-2015-STG,FALCONER(2016)
Subjects: planets and satellites: detection, Proper motion, 010504 meteorology & atmospheric sciences, Stellar mass, Brown dwarf, FOS: Physical sciences, Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Mass ratio, stars: early-type, Exoplanet, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Circumbinary planet, Astrophysics - Earth and Planetary Astrophysics, brown dwarfs
Abstract: Wide low-mass substellar companions are known to be very rare among low-mass stars, but appear to become increasingly common with increasing stellar mass. However, B-type stars, which are the most massive stars within ~150 pc of the Sun, have not yet been examined to the same extent as AFGKM-type stars in that regard. In order to address this issue, we launched the ongoing B-star Exoplanet Abundance Study (BEAST) to examine the frequency and properties of planets, brown dwarfs, and disks around B-type stars in the Scorpius-Centaurus (Sco-Cen) association; we also analyzed archival data of B-type stars in Sco-Cen. During this process, we identified a candidate substellar companion to the B9-type spectroscopic binary HIP 79098 AB, which we refer to as HIP 79098 (AB)b. The candidate had been previously reported in the literature, but was classified as a background contaminant on the basis of its peculiar colors. Here we demonstrate that the colors of HIP 79098 (AB)b are consistent with several recently discovered young and low-mass brown dwarfs, including other companions to stars in Sco-Cen. Furthermore, we show unambiguous common proper motion over a 15-year baseline, robustly identifying HIP 79098 (AB)b as a bona fide substellar circumbinary companion at a 345+/-6 AU projected separation to the B9-type stellar pair. With a model-dependent mass of 16-25 Mjup yielding a mass ratio of, 9 pages, 6 figures, accepted for publication in A&A
Published: 2019

85. 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., Ménard, F., Meyer, M., Milli, J., Mordasini, C., Pinte, C., Pragt, J., Roelfsema, R., Rigal, F, Szulagyi, J., Van Boekel, R., van der Plas, G., Vigan, Arthur, Wahhaj, Z., Zurlo, A., Girard, H., Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), 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), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), 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), 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Stockholm University, European Southern Observatory (ESO), Physikalisches Institut [Bern], Universität Bern [Bern], NOVA Optical Infrared Instrumentation Group, 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), 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), 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]), Université de Genève = University of Geneva (UNIGE), Universiteit Leiden, Universität Bern [Bern] (UNIBE), and ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016)
Subjects: planet-disk interactions, planets and satellites: detection, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], techniques: high angular resolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], planetary systems
Abstract: International audience; Context. In recent years, our understanding of giant planet formation progressed substantially. There have even been detections of a few young protoplanet candidates still embedded in the circumstellar disks of their host stars. The exact physics that describes the accretion of material from the circumstellar disk onto the suspected circumplanetary disk and eventually onto the young, forming planet is still an open question. Aims: We seek to detect and quantify observables related to accretion processes occurring locally in circumstellar disks, which could be attributed to young forming planets. We focus on objects known to host protoplanet candidates and/or disk structures thought to be the result of interactions with planets. Methods: We analyzed observations of six young stars (age 3.5-10 Myr) and their surrounding environments with the SPHERE/ZIMPOL instrument on the Very Large Telescope (VLT) in the Hα filter (656 nm) and a nearby continuum filter (644.9 nm). We applied several point spread function (PSF) subtraction techniques to reach the highest possible contrast near the primary star, specifically investigating regions where forming companions were claimed or have been suggested based on observed disk morphology. Results: We redetect the known accreting M-star companion HD142527 B with the highest published signal to noise to date in both Hα and the continuum. We derive new astrometry (r=62.8-2.7+2.1 mas and PA=(98.7±1.8)°) and photometry (ΔN_Ha = 6.3-0.3+0.2 mag, ΔB_Ha = 6.7 ± 0.2 mag and ΔCnt_Ha = 7.3-0.2+0.3 mag) for the companion in agreement with previous studies, and estimate its mass accretion rate (Ṁ ≈ 1-2 × 10-10 M⊙yr-1). A faint point-like source around HD135344 B (SAO206462) is also investigated, but a second deeper observation is required to reveal its nature. No other companions are detected. In the framework of our assumptions we estimate detection limits at the locations of companion candidates around HD100546, HD169142, and MWC 758 and calculate that processes involving Hα fluxes larger than 8 × 10-14-10-15 erg s-1 cm-2 (Ṁ > 10-10-10-12 M⊙yr-1) can be excluded. Furthermore, flux upper limits of 10-14-10-15 erg s-1 cm-2 (Ṁ < 10-11-10-12 M⊙yr-1) are estimated within the gaps identified in the disks surrounding HD135344 B and TW Hya. The derived luminosity limits exclude Hα signatures at levels similar to those previously detected for the accreting planet candidate LkCa15 b. Based on observations collected at the Paranal Observatory, ESO (Chile). Program ID: 096.C-0248(B), 096.C-0267(A),096.C-0267(B), 095.C-0273(A), 095.C-0298(A).The reduced images (FITS files) are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/622/A156
Published: 2019

86. 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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87. A search for accreting young companions embedded in circumstellar disks High-contrast H alpha imaging with VLT/SPHERE

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, Markus, Lagrange, A. -M., Langlois, M., Magnard, Y., Maire, A. -L., Menard, F., Meyer, M., Milli, J., Mordasini, C., Pinte, C., Pragt, J., Roelfsema, R., Rigal, F., Szulagyi, J., van Boekel, R., van der Plas, G., Vigan, A., Wahhaj, Z., Zurlo, A., 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, Markus, Lagrange, A. -M., Langlois, M., Magnard, Y., Maire, A. -L., Menard, F., Meyer, M., Milli, J., Mordasini, C., Pinte, C., Pragt, J., Roelfsema, R., Rigal, F., Szulagyi, J., van Boekel, R., van der Plas, G., Vigan, A., Wahhaj, Z., and Zurlo, A.
Abstract: Context. In recent years, our understanding of giant planet formation progressed substantially. There have even been detections of a few young protoplanet candidates still embedded in the circumstellar disks of their host stars. The exact physics that describes the accretion of material from the circumstellar disk onto the suspected circumplanetary disk and eventually onto the young, forming planet is still an open question. Aims. We seek to detect and quantify observables related to accretion processes occurring locally in circumstellar disks, which could be attributed to young forming planets. We focus on objects known to host protoplanet candidates and/or disk structures thought to be the result of interactions with planets. Methods. We analyzed observations of six young stars (age 3.5-10 Myr) and their surrounding environments with the SPHERE/ZIMPOL instrument on the Very Large Telescope (VLT) in the H alpha filter (656 nm) and a nearby continuum filter (644.9 nm). We applied several point spread function (PSF) subtraction techniques to reach the highest possible contrast near the primary star, specifically investigating regions where forming companions were claimed or have been suggested based on observed disk morphology. Results. We redetect the known accreting M-star companion HD142527 B with the highest published signal to noise to date in both H alpha and the continuum. We derive new astrometry (r = 62.8(-2.7)(+2.1)mas and PA = (98.7 +/- 1.8)degrees) and photometry (Delta N_Ha = 6.3-(+0.2)(0.3) mag, Delta B_Ha = 6.7 +/- 0.2 mag and Delta Cnt_Ha= 7.3(-0.2)(+0.3) mag) for the companion in agreement with previous studies, and estimate its mass accretion rate (M approximate to 1-2 x 10(-10) M-circle dot yr(-1)). A faint point-like source around HD135344 B (SA0206462) is also investigated, but a second deeper observation is required to reveal its nature. No other companions are detected. In the framework of our assumptions we estimate detection limits at the loc
Published: 2019
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88. Characterization of the Low-Mass Companion HD 142527 B

Author: Christiaens, V., Casassus, S., Absil, O., Kimeswenger, S., Gonzalez, C.G., Girard, J., Ramírez, R., Wertz, O., Zurlo, A., Wahhaj, Z., Salinas Poblete, V.N., Jordan, A., and Mawet, D.
Abstract: The circumstellar disk of the Herbig Fe star HD 142527 is host to several remarkable features including a warped inner disk, a 120 au-wide annular gap, a prominent dust trap and several spiral arms. A low-mass companion, HD 142527 B, was also found orbiting the primary star at only ~14 au. This poster presents how we managed to better characterize this companion using VLT/SINFONI in pupil-tracking mode. Using ADI-based post-processing algorithms, we conspicuously re-detected the companion in most spectral channels, enabling us to extract the first medium-resolution spectrum of a low-mass companion within 0.1'' from its central star. Our analysis suggests that HD 142527 B is an M2.5+-1.0 star with an effective temperature of 3500+-100 K, possibly surrounded with a hot (1700 K) inner rim. Based on its location in HR diagrams compared to stellar evolution tracks, we constrain the mass and age to be 0.34+-0.06 MSun and 0.5--3.0 Myr, respectively. The new spectral type makes HD 142527 B a twin of the well known TW Hya T-Tauri star, and new hydro-dynamical simulations considering our revised mass of HD 142527 B show that companion-disk interactions alone are able to account qualitatively for the observed morphology of the disk.
Published: 2018

89. 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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90. Calibration of quasi-static aberrations in exoplanet direct-imaging instruments with a Zernike phase-mask sensor

Author: Vigan, A., primary, N’Diaye, M., additional, Dohlen, K., additional, Sauvage, J.-F., additional, Milli, J., additional, Zins, G., additional, Petit, C., additional, Wahhaj, Z., additional, Cantalloube, F., additional, Caillat, A., additional, Costille, A., additional, Le Merrer, J., additional, Carlotti, A., additional, Beuzit, J.-L., additional, and Mouillet, D., additional
Published: 2019
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91. Separating extended disc features from the protoplanet in PDS 70 using VLT/SINFONI

Author: Christiaens, V, primary, Casassus, S, additional, Absil, O, additional, Cantalloube, F, additional, Gomez Gonzalez, C, additional, Girard, J, additional, Ramírez, R, additional, Pairet, B, additional, Salinas, V, additional, Price, D J, additional, Pinte, C, additional, Quanz, S P, additional, Jordán, A, additional, Mawet, D, additional, and Wahhaj, Z, additional
Published: 2019
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92. 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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93. Orbital and atmospheric characterization of the planet within the gap of the PDS70 transition disk

Author: Mueller, A., Keppler, M., Henning, Th., Samland, M., Chauvin, G., Beust, H., Maire, A. -L., Molaverdikhani, K., van Boekel, R., Benisty, M., Boccaletti, A., Bonnefoy, M., Cantalloube, F., Charnay, B., Baudino, J. -L., Gennaro, M., Long, Z. C., Cheetham, A., Desidera, S., Feldt, M., Fusco, T., Girard, J., Gratton, R., Hagelberg, J., Janson, Markus, Lagrange, A. -M., Langlois, M., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Meyer, M., Molliere, P., Mordasini, C., Moulin, T., Pavlov, A., Pawellek, N., Quanz, S. P., Ramos, J., Rouan, D., Sissa, E., Stadler, E., Vigan, A., Wahhaj, Z., Weber, L., Zurlo, A., Mueller, A., Keppler, M., Henning, Th., Samland, M., Chauvin, G., Beust, H., Maire, A. -L., Molaverdikhani, K., van Boekel, R., Benisty, M., Boccaletti, A., Bonnefoy, M., Cantalloube, F., Charnay, B., Baudino, J. -L., Gennaro, M., Long, Z. C., Cheetham, A., Desidera, S., Feldt, M., Fusco, T., Girard, J., Gratton, R., Hagelberg, J., Janson, Markus, Lagrange, A. -M., Langlois, M., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Meyer, M., Molliere, P., Mordasini, C., Moulin, T., Pavlov, A., Pawellek, N., Quanz, S. P., Ramos, J., Rouan, D., Sissa, E., Stadler, E., Vigan, A., Wahhaj, Z., Weber, L., and Zurlo, A.
Abstract: Context. The observation of planets in their formation stage is a crucial but very challenging step in understanding when, how, and where planets form. PDS 70 is a young pre-main sequence star surrounded by a transition disk, in the gap of which a planetary-mass companion has recently been discovered. This discovery represents the first robust direct detection of such a young planet, possibly still at the stage of formation. Aims. We aim to characterize the orbital and atmospheric properties of PDS 70 b, which was first identified on May 2015 in the course of the SHINE survey with SPHERE, the extreme adaptive-optics instrument at the VLT. Methods. We obtained new deep SPHERE/IRDIS imaging and SPHERE/IFS spectroscopic observations of PDS 70 b. The astrometric baseline now covers 6 yr, which allowed us to perform an orbital analysis. For the first time, we present spectrophotometry of the young planet which covers almost the entire near-infrared range (0.96-3.8 mu m). We use different atmospheric models covering a large parameter space in temperature, log g, chemical composition, and cloud properties to characterize the properties of the atmosphere of PDS 70 b. Results. PDS 70 b is most likely orbiting the star on a circular and disk coplanar orbit at similar to 22 au inside the gap of the disk. We find a range of models that can describe the spectrophotometric data reasonably well in the temperature range 1000-1600 K and log g no larger than 3.5 dex. The planet radius covers a relatively large range between 1.4 and 3.7 R-J with the larger radii being higher than expected from planet evolution models for the age of the planet of 5.4 Myr. Conclusions. This study provides a comprehensive data set on the orbital motion of PDS 70 b, indicating a circular orbit and a motion coplanar with the disk. The first detailed spectral energy distribution of PDS 70 b indicates a temperature typical of young giant planets. The detailed atmospheric analysis indicates that a circumplane
Published: 2018
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94. Investigation of the inner structures around HD 169142 with VLT/SPHERE

Author: Ligi, R., Vigan, A., Gratton, R., de Boer, J., Benisty, M., Boccaletti, A., Quanz, S. P., Meyer, M., Ginski, C., Sissa, E., Gry, C., Henning, T., Beuzit, J. -L., Biller, B., Bonnefoy, M., Chauvin, G., Cheetham, A. C., Cudel, M., Delorme, P., Desidera, S., Feldt, M., Galicher, R., Girard, J., Janson, Markus, Kasper, M., Kopytova, T., Lagrange, A. -M., Langlois, M., Lecoroller, H., Maire, A. -L., Menard, F., Mesa, D., Peretti, S., Perrot, C., Pinilla, P., Pohl, A., Rouan, D., Stolker, T., Samland, M., Wahhaj, Z., Wildi, F., Zurlo, A., Buey, T., Fantinel, D., Fusco, T., Jaquet, M., Moulin, T., Ramos, J., Suarez, M., Weber, L., Ligi, R., Vigan, A., Gratton, R., de Boer, J., Benisty, M., Boccaletti, A., Quanz, S. P., Meyer, M., Ginski, C., Sissa, E., Gry, C., Henning, T., Beuzit, J. -L., Biller, B., Bonnefoy, M., Chauvin, G., Cheetham, A. C., Cudel, M., Delorme, P., Desidera, S., Feldt, M., Galicher, R., Girard, J., Janson, Markus, Kasper, M., Kopytova, T., Lagrange, A. -M., Langlois, M., Lecoroller, H., Maire, A. -L., Menard, F., Mesa, D., Peretti, S., Perrot, C., Pinilla, P., Pohl, A., Rouan, D., Stolker, T., Samland, M., Wahhaj, Z., Wildi, F., Zurlo, A., Buey, T., Fantinel, D., Fusco, T., Jaquet, M., Moulin, T., Ramos, J., Suarez, M., and Weber, L.
Abstract: We present observations of the Herbig Ae star HD 169142 with the VLT/SPHERE instruments InfraRed Dual-band Imager and Spectrograph (IRDIS) (K1K2 and H2H3 bands) and the Integral Field Spectrograph (IFS) (Y, J and H bands). We detect several bright blobs at similar to 180 mas separation from the star, and a faint arc-like structure in the IFS data. Our reference differential imaging (RDI) data analysis also finds a bright ring at the same separation. We show, using a simulation based on polarized light data, that these blobs are actually part of the ring at 180 mas. These results demonstrate that the earlier detections of blobs in the H and K-S bands at these separations in Biller et al. as potential planet/substellar companions are actually tracing a bright ring with a Keplerian motion. Moreover, we detect in the images an additional bright structure at similar to 93 mas separation and position angle of 355 degrees, at a location very close to previous detections. It appears point-like in the YJ and K bands but is more extended in the H band. We also marginally detect an inner ring in the RDI data at similar to 100 mas. Follow-up observations are necessary to confirm the detection and the nature of this source and structure.
Published: 2018
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95. Low wind effect on VLT/SPHERE: impact, mitigation strategy, and results

Author: Close, Laird M., Schreiber, Laura, Schmidt, Dirk, Milli, J., Kasper, M., Bourget, P., Pannetier, C., Mouillet, D., Sauvage, J.-F., Reyes, C., Fusco, T., Cantalloube, F., Tristram, K., Wahhaj, Z., Beuzit, J.-L., Girard, J. H., Mawet, D., Telle, A., Vigan, A., N'Diaye, M., Close, Laird M., Schreiber, Laura, Schmidt, Dirk, Milli, J., Kasper, M., Bourget, P., Pannetier, C., Mouillet, D., Sauvage, J.-F., Reyes, C., Fusco, T., Cantalloube, F., Tristram, K., Wahhaj, Z., Beuzit, J.-L., Girard, J. H., Mawet, D., Telle, A., Vigan, A., and N'Diaye, M.
Abstract: The low wind effect is a phenomenon disturbing the phase of the wavefront in the pupil of a large telescope obstructed by spiders, in the absence of wind. It can be explained by the radiative cooling of the spiders, creating air temperature inhomogeneities across the pupil. Because it is unseen by traditional adaptive optics (AO) systems, thus uncorrected, it significantly degrades the quality of AO-corrected images. We provide a statistical analysis of the strength of this effect as seen by VLT/SPHERE after 4 years of operations. We analyse its dependence upon the wind and temperature conditions. We describe the mitigation strategy implemented in 2017: a specific coating with low thermal emissivity in the mid-infrared was applied on the spiders of Unit Telescope 3. We quantify the improvement in terms of image quality, contrast and wave front error using both focal plane images and measured phase maps.
Published: 2018

96. Three Years of SPHERE: The Latest View of the Morphology and Evolution of Protoplanetary Discs

Author: Garufi, A., Benisty, M., Stolker, T., Avenhaus, H., Boer, J. de, Pohl, A., Quanz, S.P., Dominik, C., Ginski, C., Thalmann, C., Boekel, R., Boccaletti, A., Henning, T., Janson, M., Salter, G., Schmid, H.M., Sissa, E., Langlois, M., Beuzit, J.-L., Chauvin, G., Mouillet, D., Augereau, J.-C., Bazzon, A., Biller, B., Bonnefoy, M., Buenzli, E., Cheetham, A., Daemgen, S., Desidera, S., Engler, N., Feldt, M., Girard, J., Gratton, R., Hagelberg, J., Keller, C.U., Keppler, M., Kenworthy, M.A., Kral, Q., Lopez, B., Maire, A.-L., Menard, F., Mesa, D., Messina, S., Meyer, M.R., Milli, J., Min, M., Muller, A., Olofsson, J., Pawellek, N., Pinte, C., Szulagyi, J., Vigan, A., Wahhaj, Z., Waters, R., Zurlo, A., and Low Energy Astrophysics (API, FNWI)
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Spatially resolving the immediate surroundings of young stars is a key challenge for the planet formation community. SPHERE on the VLT represents an important step forward by increasing the opportunities offered by optical or near-infrared imaging instruments to image protoplanetary discs. The Guaranteed Time Observation Disc team has concentrated much of its efforts on polarimetric differential imaging, a technique that enables the efficient removal of stellar light and thus facilitates the detection of light scattered by the disc within a few au from the central star. These images reveal intriguing complex disc structures and diverse morphological features that are possibly caused by ongoing planet formation in the disc. An overview of the recent advances enabled by SPHERE is presented.
Published: 2017

97. Characterization of low-mass companion HD 142527 B

Author: Christiaens, V., primary, Casassus, S., additional, Absil, O., additional, Kimeswenger, S., additional, Gomez Gonzalez, C. A., additional, Girard, J., additional, Ramírez, R., additional, Wertz, O., additional, Zurlo, A., additional, Wahhaj, Z., additional, Flores, C., additional, Salinas, V., additional, Jordán, A., additional, and Mawet, D., additional
Published: 2018
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98. Orbital and atmospheric characterization of the planet within the gap of the PDS 70 transition disk

Author: Müller, A., primary, Keppler, M., additional, Henning, Th., additional, Samland, M., additional, Chauvin, G., additional, Beust, H., additional, Maire, A.-L., additional, Molaverdikhani, K., additional, van Boekel, R., additional, Benisty, M., additional, Boccaletti, A., additional, Bonnefoy, M., additional, Cantalloube, F., additional, Charnay, B., additional, Baudino, J.-L., additional, Gennaro, M., additional, Long, Z. C., additional, Cheetham, A., additional, Desidera, S., additional, Feldt, M., additional, Fusco, T., additional, Girard, J., additional, Gratton, R., additional, Hagelberg, J., additional, Janson, M., additional, Lagrange, A.-M., additional, Langlois, M., additional, Lazzoni, C., additional, Ligi, R., additional, Ménard, F., additional, Mesa, D., additional, Meyer, M., additional, Mollière, P., additional, Mordasini, C., additional, Moulin, T., additional, Pavlov, A., additional, Pawellek, N., additional, Quanz, S. P., additional, Ramos, J., additional, Rouan, D., additional, Sissa, E., additional, Stadler, E., additional, Vigan, A., additional, Wahhaj, Z., additional, Weber, L., additional, and Zurlo, A., additional
Published: 2018
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99. Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70

Author: Keppler, M., primary, Benisty, M., additional, Müller, A., additional, Henning, Th., additional, van Boekel, R., additional, Cantalloube, F., additional, Ginski, C., additional, van Holstein, R. G., additional, Maire, A.-L., additional, Pohl, A., additional, Samland, M., additional, Avenhaus, H., additional, Baudino, J.-L., additional, Boccaletti, A., additional, de Boer, J., additional, Bonnefoy, M., additional, Chauvin, G., additional, Desidera, S., additional, Langlois, M., additional, Lazzoni, C., additional, Marleau, G.-D., additional, Mordasini, C., additional, Pawellek, N., additional, Stolker, T., additional, Vigan, A., additional, Zurlo, A., additional, Birnstiel, T., additional, Brandner, W., additional, Feldt, M., additional, Flock, M., additional, Girard, J., additional, Gratton, R., additional, Hagelberg, J., additional, Isella, A., additional, Janson, M., additional, Juhasz, A., additional, Kemmer, J., additional, Kral, Q., additional, Lagrange, A.-M., additional, Launhardt, R., additional, Matter, A., additional, Ménard, F., additional, Milli, J., additional, Mollière, P., additional, Olofsson, J., additional, Pérez, L., additional, Pinilla, P., additional, Pinte, C., additional, Quanz, S. P., additional, Schmidt, T., additional, Udry, S., additional, Wahhaj, Z., additional, Williams, J. P., additional, Buenzli, E., additional, Cudel, M., additional, Dominik, C., additional, Galicher, R., additional, Kasper, M., additional, Lannier, J., additional, Mesa, D., additional, Mouillet, D., additional, Peretti, S., additional, Perrot, C., additional, Salter, G., additional, Sissa, E., additional, Wildi, F., additional, Abe, L., additional, Antichi, J., additional, Augereau, J.-C., additional, Baruffolo, A., additional, Baudoz, P., additional, Bazzon, A., additional, Beuzit, J.-L., additional, Blanchard, P., additional, Brems, S. S., additional, Buey, T., additional, De Caprio, V., additional, Carbillet, M., additional, Carle, M., additional, Cascone, E., additional, Cheetham, A., additional, Claudi, R., additional, Costille, A., additional, Delboulbé, A., additional, Dohlen, K., additional, Fantinel, D., additional, Feautrier, P., additional, Fusco, T., additional, Giro, E., additional, Gluck, L., additional, Gry, C., additional, Hubin, N., additional, Hugot, E., additional, Jaquet, M., additional, Le Mignant, D., additional, Llored, M., additional, Madec, F., additional, Magnard, Y., additional, Martinez, P., additional, Maurel, D., additional, Meyer, M., additional, Möller-Nilsson, O., additional, Moulin, T., additional, Mugnier, L., additional, Origné, A., additional, Pavlov, A., additional, Perret, D., additional, Petit, C., additional, Pragt, J., additional, Puget, P., additional, Rabou, P., additional, Ramos, J., additional, Rigal, F., additional, Rochat, S., additional, Roelfsema, R., additional, Rousset, G., additional, Roux, A., additional, Salasnich, B., additional, Sauvage, J.-F., additional, Sevin, A., additional, Soenke, C., additional, Stadler, E., additional, Suarez, M., additional, Turatto, M., additional, and Weber, L., additional
Published: 2018
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100. Debris discs with multiple absorption features in metallic lines: circumstellar or interstellar origin?

Author: Iglesias, D, primary, Bayo, A, additional, Olofsson, J, additional, Wahhaj, Z, additional, Eiroa, C, additional, Montesinos, B, additional, Rebollido, I, additional, Smoker, J, additional, Sbordone, L, additional, Schreiber, M R, additional, and Henning, Th, additional
Published: 2018
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