Author: "Feldt M" / Language: undetermined - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Feldt M"' showing total 45 results

Start Over Author "Feldt M" Language undetermined

45 results on '"Feldt M"'

1. METIS: final design of the Imager sub-system

Author: Bizenberger, P., Baumeister, H., Barriere, J.-C., Bertram, T., Böhm, A., Brandl, B., Cárdenas Vázquez, M.C., Chamorro, E., Feldt, M., Glauser, A.M., Henning, T., Laun, W., Lesman, D., Mohr, L., Raskin, G., Rohloff, R.-R., Scheithauer, S., Serra, B., Stepien, P., Stuik, R., Todd, S., Boekel, R. van, Evans, C.J., Bryant, J.J., Motohara, K., Evans, C.J., Bryant, J.J., and Motohara, K.
Published: 2022

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

Author: Boccaletti, A., Chauvin, G., Wildi, F., Milli, J., Stadler, E., Diolaiti, E., Gratton, R., Vidal, F., Loupias, M., Langlois, M., Cantalloube, F., N'Diaye, M., Gratadour, D., Ferreira, F., Tallon, M., Mazoyer, J., Segransan, D., Mouillet, D., Beuzit, J.-L., Bonnefoy, M., Galicher, R., Vigan, A., Snellen, I.A.G., Feldt, M., Desidera, S., Rousseau, S., Baruffolo, A., Goulas, C., Baudoz, P., Bechet, C., Benisty, M., Bianco, A., Carry, B., Cascone, E., Charnay, B., Choquet, E., Christiaens, V., Cortecchia, F., Di Capprio, V., De Rosa, A., Desgrange, C., D'Orazi, V., Douté, S., Frangiamore, M., Gendron, E., Ginski, C., Huby, E., Keller, C.U., Kulcsár, C., Landman, R., Lagarde, S., Lagadec, E., Lagrange, A.-M., Lombini, M., Kasper, M., Ménard, F., Magnard, Y., Malaguti, G., Maurel, D., Mesa, D., Morgante, G., Pantin, E., Pichon, T., Potier, A., Rabou, P., Rochat, S., Terenzi, . l ., Thiébaut, E., Tallon-Bosc, I., Raynaud, H.-F., Rouan, D., Sevin, A., Schiavone, F., Schrieber, L., Zanutta, A., Evans, C.J., Bryant, J.J., Motohara, K., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = 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)-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), Pôle Planétologie du LESIA, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Universidad de Chile = University of Chile [Santiago] (UCHILE), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), 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, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Padova (OAPD), 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), 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), Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), High Contrast Imaging, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Exoplanets, FOS: Physical sciences, Adaptive Optics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics, Coronagraphy
Abstract: SPHERE+ is a proposed upgrade of the SPHERE instrument at the VLT, which is intended to boost the current performances of detection and characterization for exoplanets and disks. SPHERE+ will also serve as a demonstrator for the future planet finder (PCS) of the European ELT. The main science drivers for SPHERE+ are 1/ to access the bulk of the young giant planet population down to the snow line ($3-10$ au), to bridge the gap with complementary techniques (radial velocity, astrometry); 2/ to observe fainter and redder targets in the youngest ($1-10$\,Myr) associations compared to those observed with SPHERE to directly study the formation of giant planets in their birth environment; 3/ to improve the level of characterization of exoplanetary atmospheres by increasing the spectral resolution in order to break degeneracies in giant planet atmosphere models. Achieving these objectives requires to increase the bandwidth of the xAO system (from $\sim$1 to 3\,kHz) as well as the sensitivity in the infrared (2 to 3\,mag). These features will be brought by a second stage AO system optimized in the infrared with a pyramid wavefront sensor. As a new science instrument, a medium resolution integral field spectrograph will provide a spectral resolution from 1000 to 5000 in the J and H bands. This paper gives an overview of the science drivers, requirements and key instrumental trade-off that were done for SPHERE+ to reach the final selected baseline concept., To appear in the Proceedings of the SPIE Astronomical Telescopes + Instrumentation (2022), 13 pages, 6 figure
Published: 2022

3. Status update on the development of METIS, the mid-infrared ELT imager and spectrograph

Author: Brandl, B.R., Bettonvil, F.C.M., Van Boekel, R., Glauser, A., Quanz, S.P., Absil, O., Feldt, M., Garcia, P.J.V., Glasse, A., Guedel, M., Labadie, L., Meyer, M., Pantin, E., Wang, S.-Y., Van Winckel, H., Agócs, T., Amorim, A., Bertram, T., Burtscher, L.H., Delacroix, C., Laun, W., Lesman, D., Raskin, G., Salo, C., Scheithauer, S., Stuik, R., Todd, S., Haupt, C., Siebenmorgen, R., Evans, C.J., Bryant, J.J., and Motohara, K.
Published: 2022

4. Revisiting the atmosphere of the exoplanet 51 Eridani b with VLT/SPHERE

Author: Brown-Sevilla, S. B., Maire, A. -L., Mollière, P., Samland, M., Feldt, M., Brandner, W., Henning, Th., Gratton, R., Janson, M., Stolker, T., Hagelberg, J., Zurlo, A., Cantalloube, F., Boccaletti, A., Bonnefoy, M., Chauvin, G., Desidera, S., D'Orazi, V., Lagrange, A. -M., Langlois, M., Menard, F., Mesa, D., Meyer, M., Pavlov, A., Petit, C., Rochat, S., Rouan, D., Schmidt, T., Vigan, A., and Weber, L.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: [Full abstract in the paper] We aim to better constrain the atmospheric properties of the directly imaged exoplanet 51~Eri~b by using a retrieval approach on higher signal-to-noise data than previously reported. In this context, we also compare the results of using the atmospheric retrieval code \texttt{petitRADTRANS} vs a self-consistent model to fit atmospheric parameters. We present a higher signal-to-noise $YH$ spectrum of the planet and revised $K1K2$ photometry (M$_{K1} = 15.11 \pm 0.04$ mag, M$_{K2} = 17.11 \pm 0.38$ mag). The best-fit parameters obtained using an atmospheric retrieval differ from previous results using self-consistent models. In general, we find that our solutions tend towards cloud-free atmospheres (e.g. log $\tau_{\rm clouds} = -5.20 \pm 1.44$). For our ``nominal'' model with new data, we find a lower metallicity ([Fe/H] $= 0.26\pm$0.30 dex) and C/O ratio ($0.38\pm0.09$), and a slightly higher effective temperature (T$_{\rm{eff}} = 807\pm$45 K) than previous studies. The surface gravity (log $g = 4.05\pm0.37$) is in agreement with the reported values in the literature within uncertainties. We estimate the mass of the planet to be between 2 and 4 M$_{\rm{Jup}}$. When comparing with self-consistent models, we encounter a known correlation between the presence of clouds and the shape of the $P-T$ profiles. Our findings support the idea that results from atmospheric retrievals should not be discussed in isolation, but rather along with self-consistent temperature structures obtained using the retrieval's best-fit parameters., Comment: Accepted for publication in A&A. 21 pages, 7 figures in the main text and 9 figures in the Appendix
Published: 2023

5. Peering into the Young Planetary System AB Pic. Atmosphere, Orbit, Obliquity & Second Planetary Candidate

Author: Palma-Bifani, P., Chauvin, G., Bonnefoy, M., Rojo, P. M., Petrus, S., Rodet, L., Langlois, M., Allard, F., Charnay, B., Desgrange, C., Homeier, D., Lagrange, A. -M., Beuzit, J. -L., Baudoz, P., Boccaletti, A., Chomez, A., Delorme, P., Desidera, S., Feldt, M., Ginski, C., Gratton, R., Maire, A. -L., Meyer, M., Samland, M., Snellen, I., Vigan, A., and Zhang, Y.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences
Abstract: We aim to revisit the system AB Pic which has a known companion at the exoplanet/ brown-dwarf boundary. We based this study on a rich set of observations to investigate the companion's orbit and atmosphere. We composed a spectrum of AB Pic b merging archival VLT/SINFONI K-band data, with published spectra at J and H-band (SINFONI) and Lp-band (Magellan-AO), and photometric measurements (HST and Spitzer). We modeled the spectrum with ForMoSA, based on two atmospheric models: ExoREM and BT-SETTL13. We determined the orbital properties of b fitting the astrometric measurements from NaCo (2003 and 2004) and SPHERE (2015). The orbital solutions favor a semi-major axis of $\sim$190au viewed edge-on. With Exo-REM, we derive a T$_{eff}$ of 1700$\pm$50K and surface gravity of 4.5$\pm$0.3dex, consistent with previous works, and we report for the first time a C/O ratio of 0.58$\pm$0.08 ($\sim$solar). The posteriors are sensitive to the wavelength interval and the family of models used. Given the 2.1hr rotation period and our vsin(i) of $\sim$73km/s, we estimate for the first time the true obliquity to be $\sim$45 or $\sim$135deg, indicating a significant misalignment between the planet's spin and orbit orientations. Finally, a proper motion anomaly between the Hipparcos and Gaia eDR3 compared to our SPHERE detection limits and adapted radial velocity limits indicate the existence of a $\sim$6M$_{Jup}$ inner planet orbiting from 2 to 10au (40-200mas). The possible existence of an inner companion and the likely miss-alignment of the spin axis orientation strongly favor a formation path by gravitational instability or core accretion within a disk closer inside followed by dynamical interactions. Confirmation and characterization of planet c and access to a broader wavelength coverage for planet b will be essential to probe the uncertainties associated with the parameters., 17 pages, 13 Figures, 6 Tables
Published: 2022
Full Text: View/download PDF

6. The high-albedo, low polarization disk around HD 114082 harbouring a Jupiter-sized transiting planet

Author: Engler, N., Milli, J., Gratton, R., Ulmer-Moll, S., Vigan, A., Lagrange, A. -M., Kiefer, F., Rubini, P., Grandjean, A., Schmid, H. M., Messina, S., Squicciarini, V., Olofsson, J., Thébault, P., van Holstein, R. G., Janson, M., Ménard, F., Marshall, J. P., Chauvin, G., Lendl, M., Bhowmik, T., Boccaletti, A., Bonnefoy, M., del Burgo, C., Choquet, E., Desidera, S., Feldt, M., Fusco, T., Girard, J., Gisler, D., Hagelberg, J., Langlois, M., Maire, A. -L., Mesa, D., Meyer, M. R., Rabou, P., Rodet, L., Schmidt, T., and Zurlo, A.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present new optical and near-IR images of debris disk around the F-type star HD 114082. We obtained direct imaging observations and analysed the TESS photometric time series data of this target with a goal to search for planetary companions and to characterise the morphology of the debris disk and the scattering properties of dust particles. HD 114082 was observed with the VLT/SPHERE instrument: the IRDIS camera in the K band together with the IFS in the Y, J and H band using the ADI technique as well as IRDIS in the H band and ZIMPOL in the I_PRIME band using the PDI technique. The scattered light images were fitted with a 3D model for single scattering in an optically thin dust disk. We performed aperture photometry in order to derive the scattering and polarized phase functions, polarization fraction and spectral scattering albedo for the dust particles in the disk. This method was also used to obtain the reflectance spectrum of the disk to retrieve the disk color and study the dust reflectivity in comparison to the debris disk HD 117214. We also performed the modeling of the HD 114082 light curve measured by TESS using the models for planet transit and stellar activity to put constraints on radius of the detected planet and its orbit. The debris disk appears as an axisymmetric debris belt with a radius of ~0.37$"$ (35 au), inclination of ~83$^\circ$ and a wide inner cavity. Dust particles in HD 114082 have a maximum polarization fraction of ~17% and a high reflectivity which results in a spectral scattering albedo of 0.65. The analysis of TESS photometric data reveals a transiting planetary companion to HD 114082 with a radius of $\sim$1~$\rm R_{J}$ on an orbit with a semi-major axis of $0.7 \pm 0.4$ au. Combining different data, we reach deep sensitivity limits in terms of companion masses down to ~5$M_{\rm Jup}$ at 50 au, and ~10 $M_{\rm Jup}$ at 30 au from the central star., Comment: 27 pages
Published: 2022
Full Text: View/download PDF

7. In-depth direct imaging and spectroscopic characterization of the young Solar System analog HD 95086

Author: Desgrange, C., Chauvin, G., Christiaens, V., Cantalloube, F., Lefranc, L.-X., Le Coroller, H., Rubini, P., Otten, G. P. P. L., Beust, H., Bonavita, M., Delorme, P., Devinat, M., Gratton, R., Lagrange, A.-M., Langlois, M., Mesa, D., Milli, J., Szulágyi, J., Nowak, M., Rodet, L., Rojo, P., Petrus, S., Janson, M., Henning, T., Kral, Q., van Holstein, R. G., Ménard, F., Beuzit, J.-L., Biller, B., Boccaletti, A., Bonnefoy, M., Brown, S., Costille, A., Delboulbe, A., Desidera, S., D’Orazi, V., Feldt, M., Fusco, T., Galicher, R., Hagelberg, J., Lazzoni, C., Ligi, R., Maire, A.-L., Messina, S., Meyer, M., Potier, A., Ramos, J., Rouan, D., Schmidt, T., Vigan, A., Zurlo, A., Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL), 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), 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), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de Astronomía, Universidad de Chile = University of Chile [Santiago] (UCHILE), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Pixyl Medical [Grenoble], INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Department of Biochemistry and Molecular Biology, Mayo Clinic, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Cornell Center for Astrophysics and Planetary Science (CCAPS), Cornell University [New York], and Observatoire de Paris
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], instrumentation: high angular resolution, [SDU]Sciences of the Universe [physics], Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, stars: individual: HD95086, methods: observational, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], instrumentation: adaptive optics, planetary systems, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. HD 95086 is a young nearby Solar System analog hosting a giant exoplanet orbiting at 57 au from the star between an inner and outer debris belt. The existence of additional planets has been suggested as the mechanism that maintains the broad cavity between the two belts. Aims. We present a dedicated monitoring of HD 95086 with the VLT/SPHERE instrument to refine the orbital and atmospheric properties of HD 95086 b, and to search for additional planets in this system. Methods. SPHERE observations, spread over ten epochs from 2015 to 2019 and including five new datasets, were used. Combined with archival observations, from VLT/NaCo (2012-2013) and Gemini/GPI (2013-2016), the extended set of astrometric measurements allowed us to refine the orbital properties of HD 95086 b. We also investigated the spectral properties and the presence of a circumplanetary disk around HD 95086 b by using the special fitting tool exploring the diversity of several atmospheric models. In addition, we improved our detection limits in order to search for a putative planet c via the K-Stacker algorithm. Results. We extracted for the first time the JH low-resolution spectrum of HD 95086 b by stacking the six best epochs, and confirm its very red spectral energy distribution. Combined with additional datasets from GPI and NaCo, our analysis indicates that this very red color can be explained by the presence of a circumplanetary disk around planet b, with a range of high-temperature solutions (1400-1600 K) and significant extinction (Av > 10 mag), or by a super-solar metallicity atmosphere with lower temperatures (800-1300 K), and small to medium amount of extinction (Av < 10 mag). We do not find any robust candidates for planet c, but give updated constraints on its potential mass and location., 29 pages, 20 figures, A&A, accepted
Published: 2022

8. An extended scattered light disk around AT Pyx

Author: Ginski, C., Gratton, R., Bohn, A.J., Dominik, C., Jorquera, S., Chauvin, G., Milli, J., Rodriguez, M., Benisty, M., Launhardt, R., Müller, A., Cugno, G., Holstein, R.G. van, Boccaletti, A., Muro-Arena, G.A., Desidera, S., Keppler, M., Zurlo, A., Sissa, E., Henning, T., Janson, M., Langlois, M., Bonnefoy, M., Cantalloube, F., D'Orazi, V., Feldt, M., Hagelberg, J., Ségransan, D., Lagrange, A.-M., Lazzoni, C., Meyer, M., Romero, C., Schmidt, T.O.B., Vigan, A., Petit, C., Roelfsema, R., Pragt, J., Weber, L., 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 = 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), 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), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, and Low Energy Astrophysics (API, FNWI)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], protoplanetary disks, FOS: Physical sciences, Astronomy and Astrophysics, instrumentation: adaptive optics, techniques: polarimetric, Astrophysics - Solar and Stellar Astrophysics, instrumentation: high angular resolution, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, planets and satellites: formation, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: To understand how the multitude of planetary systems that have been discovered come to be, we need to study systems at different evolutionary stages, with different central stars but also in different environments. The most challenging environment for planet formation may be the harsh UV radiation field of nearby massive stars which quickly erodes disks by external photo-evaporation. We have observed the AT Pyx system, located in the head of a cometary globule in the Gum Nebula, to search for signs of ongoing planet formation. We used the extreme adaptive optics imager VLT/SPHERE to observe AT Pyx in polarized light as well as total intensity in the J, H and K-band. Additionally we employed VLT/NACO to observe the system in the L-band. We resolve the disk around AT Pyx in scattered light across multiple wavelengths. We find an extended (>126 au) disk, with an intermediate inclination between 35 deg and 42 deg. The disk shows complex sub-structure and we identify 2 and possibly 3 spiral-like features. Depending on the precise geometry of the disk (which we can not unambiguously infer from our data) the disk may be eccentric with an eccentricity of ~0.16 or partially self-shadowed. The spiral features and possible eccentricity are both consistent with signatures of an embedded gas giant planet equal in mass to Jupiter. Our own observations can rule out brown dwarf companions embedded in the resolved disk, but are not sensitive enough to detect gas giants. AT Pyx is the first disk in a cometray globule in the Gum Nebula which is spatially resolved. By comparison with disks in the Orion Nebula Cluster we note that the extension of the disk may be exceptional for this environment if the external UV radiation field is comparable to other cometary globules in the region. The signposts of ongoing planet formation are intriguing and need to be followed up with higher sensitivity., 11 pages, 9 figures, accepted for publication in A&A
Published: 2022

9. 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
Full Text: View/download PDF

10. SPHERE dynamical and spectroscopic characterization of HD 142527B

Author: Claudi, R., Maire, A.-L., Mesa, D., Cheetham, A., Fontanive, C., Gratton, R., Zurlo, A., Avenhaus, H., Bhowmik, T., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Cascone, E., Chauvin, G., Delboulbé, A., Desidera, S., D'Orazi, V., Feautrier, P., Feldt, M., Flammini Dotti, F., Girard, J. H., Giro, E., Janson, M., Hagelberg, J., Keppler, M., Kopytova, T., Lacour, S., Lagrange, A.-M., Langlois, M., Lannier, J., Le Coroller, H., Ménard, F., Messina, S., Meyer, M., Millward, M., Olofsson, J., PAVLOV, A., Peretti, S., Perrot, C., Pinte, C., Pragt, J., Ramos, J., Rochat, S., Rodet, L., Roelfsema, R., Rouan, D., Salter, G., Schmidt, T., Sissa, E., Thebault, P., Udry, S., Vigan, Arthur, D’Orazi, V., Girard, H., INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Capodimonte (OAC), Stockholm University, Geneva Observatory, University of Geneva [Switzerland], NOVA Optical Infrared Instrumentation Group, Universidade de Lisboa (ULISBOA), 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), 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), Observatoire de Paris, Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Universidade de Lisboa = University of Lisbon (ULISBOA)
Subjects: 010504 meteorology & atmospheric sciences, media_common.quotation_subject, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), Type (model theory), 01 natural sciences, Omega, Spectral line, instrumentation: high angular resolution, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Eccentricity (behavior), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Orbital elements, Earth and Planetary Astrophysics (astro-ph.EP), stars: formation, Accretion (meteorology), protoplanetary disks, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, techniques: imaging spectroscopy, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], stars: individual: HD 142527, Energy (signal processing), Astrophysics - Earth and Planetary Astrophysics
Abstract: We detect the accreting low-mass companion HD142527B at a separation of 73 mas (11.4 au) from the star. No other companions with mass greater than 10 MJ are visible in the field of view of IFS (\sim 100 au centered on the star) or in the IRDIS field of view (\sim 400 au centered on the star). Measurements from IFS, SAM IFS, and IRDIS suggest an M6 spectral type for HD142527B, with an uncertainty of one spectral subtype, compatible with an object of M=0.11 \pm 0.06 MSun and R=0.15 \pm 0.07 RSun. The determination of the mass remains a challenge using contemporary evolutionary models, as they do not account for the energy input due to accretion from infalling material. We consider that the spectral type of the secondary may also be earlier than the type we derived from IFS spectra. From dynamical considerations, we further constrain the mass to 0.26^{+0.16}_{-0.14} MSun , which is consistent with both our spectroscopic analysis and the values reported in the literature. Following previous methods, the lower and upper dynamical mass values correspond to a spectral type between M2.5 and M5.5 for the companion. By fitting the astrometric points, we find the following orbital parameters: a period of P=35-137 yr; an inclination of i=121-130 deg.; , a value of Omega=124-135 deg for the longitude of node, and an 68% confidence interval of \sim 18 - 57 au for the separation at periapsis. Eccentricity and time at periapsis passage exhibit two groups of values: \sim0.2-0.45 and \sim0.45-0.7 for e, and \sim 2015-2020 and \sim2020-2022 for T_0. While these orbital parameters might at first suggest that HD142527B is not the companion responsible for the outer disk truncation, a previous hydrodynamical analysis of this system showed that they are compatible with a companion that is able to produce the large cavity and other observed features., Comment: 15, pages, 11 figures, Accepted for publication on Astronomy and Astrophysics
Published: 2019

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

Author: Cugno, G., Quanz, S. P., Hunziker, S., Stolker, T., Schmid, H. M., Avenhaus, H., Baudoz, P., Bohn, A. J., Bonnefoy, M., Buenzli, E., Chauvin, G., Cheetham, A., Desidera, S., Dominik, C., Feautrier, P., Feldt, M., Ginski, C., Girard, J. H., Gratton, R., Hagelberg, J., Hugot, E., Janson, M., Lagrange, A.-M., Langlois, M., Magnard, Y., Maire, A.-L., Menard, F., Meyer, M., Milli, J., Mordasini, C., Pinte, C., Pragt, J., Roelfsema, R., Rigal, F., Szulágyi, J., van Boekel, R., van der Plas, G., Vigan, A., Wahhaj, Z., and Zurlo, A.
Subjects: 530 Physics
Published: 2019
Full Text: View/download PDF

12. The SPHERE view of the jet and the envelope of RY Tau

Author: Garufi, A., Podio, L., Bacciotti, F., Antoniucci, S., Boccaletti, A., Codella, C., Dougados, C., Menard, F., Mesa, D., Meyer, M., Nisini, B., Schmid, H. M., Stolker, T., Baudino, J. L., Biller, B., Bonavita, M., Bonnefoy, M., Cantalloube, F., Chauvin, G., Cheetham, A., Desidera, S., D'Orazi, V., Feldt, M., Galicher, R., Grandjean, A., Gratton, R., Hagelberg, J., Lagrange, A. M., Langlois, M., Lannier, J., Lazzoni, C., Maire, A. L., Perrot, C., Rickman, E., Schmidt, T., Vigan, A., Zurlo, A., Delboulbe, A., Mignant, D. Le, Fantinel, D., Moeller-Nilsson, O., Weber, L., and Sauvage, J. -F.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: Jets are rarely associated with pre-main-sequence intermediate-mass stars. Optical and near-IR observations of jet-driving sources are often hindered by the presence of a natal envelope. Jets around partly embedded sources are a useful diagnostic to constrain the geometry of the concealed protoplanetary disk. In fact, the jet-driving mechanisms are affected by both spatial anisotropies and episodic variations at the (sub-)au scale from the star. We obtained a rich set of high-contrast VLT/SPHERE observations from 0.6 micron to 2.2 micron of the young intermediate-mass star RY Tau. Given the proximity to the Sun of this source, our images have the highest spatial resolution ever obtained for an atomic jet. Optical observations in polarized light show no sign of the protoplanetary disk detected by ALMA. Instead, we observed a diffuse signal resembling a remnant envelope with an outflow cavity. The jet is detected in four spectral lines. The jet appears to be wiggling and its radial width increasing with the distance is complementary to the shape of the outflow cavity suggesting a strong jet/envelope interaction. Through the estimated tangential velocity, we revealed a possible connection between the launching time of the jet sub-structures and the stellar activity of RY Tau. RY Tau is at an intermediate stage toward the dispersal of the natal envelope. This source shows episodic increases of mass accretion/ejection similarly to other known intermediate-mass stars. The amount of observed jet wiggle is consistent with the presence of a precessing disk warp or misaligned inner disk that would be induced by an unseen planetary/sub-stellar companion at sub-/few-au scales. The high disk mass of RY Tau and of two other jet-driving intermediate-mass stars, HD163296 and MWC480, suggests that massive, full disks are more efficient at launching prominent jets., Comment: 15 pages, 9 figures. Accepted for publication by A\&A
Published: 2019
Full Text: View/download PDF

13. Post-conjunction detection of Œ≤ Pictoris b with VLT/SPHERE

Author: Lagrange, A., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, M., Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Le Coroller, H., Ligi, R., Maire, A., Mesa, D., Messina, S., Müeller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Ménard, F., Schmid, H., Turatto, M., Udry, S., Bohn, A., Charnay, B., Gomez Gonzales, C., Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., and Wildi, F.
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Context. With an orbital distance comparable to that of Saturn in the solar system, Œ≤ Pictoris b is the closest (semi-major axis ‚âÉ9 au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to Œ≤ Pictoris have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet's orbital parameters. Aims: We aimed at further constraining Œ≤ Pictoris b orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. Methods: We used SPHERE at the VLT to precisely monitor the orbital motion of beta Œ≤ Pictoris b since first light of the instrument in 2014. Results: We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6 au) and prevented further detection. We redetected Œ≤ Pictoris b on the northeast side of the disk at a separation of 139 mas and a PA of 30¬∞ in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of a = 9.0 ¬± 0.5 au (1œÉ), it definitely excludes previously reported possible long orbital periods, and excludes Œ≤ Pictoris b as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away. Based on observations collected at the European Southern Observatory under programmes 198.C-0209, 1100.C-0481.
Published: 2019

14. Status of the mid-IR ELT imager and spectrograph (METIS)

Author: Brandl, B., Absil, O., Agócs, T., Baccichet, N., Bertram, T., Bettonvil, F., van Boekel, R., Burtscher, L., van Dishoeck, E., Feldt, M., Garcia, P., Glasse, A., Glauser, A., Güdel, M., Haupt, C., Kenworthy, M., Labadie, L., Laun, W., Lesman, D., Pantin, E., Quanz, S., Snellen, I., Siebenmorgen, R., and van Winckel, H.
Abstract: The Mid-Infrared ELT Imager and Spectrograph (METIS) is one of three first light instruments on the ELT. It will provide high-contrast imaging and medium resolution, slit-spectroscopy from 3 - 19um, as well as high resolution (R 100,000) integral field spectroscopy from 2.9-5.3µm. All modes observe at the diffraction limit of the ELT, by means of adaptive optics, yielding angular resolutions of a few tens of milliarcseconds. The range of METIS science is broad, from Solar System objects to active galactic nuclei (AGN). We will present an update on the main science drivers for METIS: circum-stellar disks and exoplanets. The METIS project is now in full steam, approaching its preliminary design review (PDR) in 2018. In this paper we will present the current status of its optical, mechanical and thermal design as well as operational aspects. We will also discuss the challenges of building an instrument for the ELT, and the required technologies.
Published: 2018

15. High-Contrast study of the candidate planets and protoplanetary disk around HD~100546

Author: Sissa, E., Gratton, R., Garufi, A., Rigliaco, E., Zurlo, A., Mesa, D., Langlois, M., De Boer, J., Desidera, S., Ginski, C., Lagrange, A.-M., Maire, A.-L., Vigan, Arthur, Dima, M., Antichi, J., Baruffolo, A., Bazzon, A., Benisty, M., Beuzit, J.-L., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Brandner, W., Bruno, P., Buenzli, E., Cascone, E., Chauvin, G., Cheetham, A., Claudi, R. U., Cudel, M., De Caprio, V., Dominik, C., Fantinel, D., Farisato, G., Feldt, M., Fontanive, C., Galicher, R., Giro, E., Hagelberg, J., Incorvaia, S., Janson, M., Kasper, M., Keppler, M., Kopytova, T., Lagadec, E., Lannier, J., Lazzoni, C., LeCoroller, H., Lessio, L., Ligi, R., Marzari, F., Ménard, F., Meyer, M. R., Mouillet, D., Peretti, S., Perrot, C., Potiron, P. J., Rouan, D., Salasnich, B., Salter, G., Samland, M., Schmidt, T., Scuderi, S., Wildi, F., Meyer, R., Potiron, J., INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Biochemistry and Molecular Biology, Mayo Clinic, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], 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]), Department of Bentho-pelagic processes, Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), INAF - Osservatorio Astrofisico di Arcetri (OAA), 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Erosion torrentielle neige et avalanches (UR ETGR (ETNA)), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), INAF - Osservatorio Astronomico di Capodimonte (OAC), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Stockholm University, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica, Universita degli Studi di Padova, Université libre de Bruxelles (ULB), Geneva Observatory, University of Geneva [Switzerland], Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - 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), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Centre National de la Recherche Scientifique (CNRS), Université Libre de Bruxelles [Bruxelles] (ULB), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden, Université de Genève = University of Geneva (UNIGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Padova = University of Padua (Unipd), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Low Energy Astrophysics (API, FNWI), Universidad Autonónoma de Madrid, Institute of Astronomy [ETH Zürich], Observatoire de Paris, Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: planets and satellites: detection, Be star, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, Protoplanetary disk, 01 natural sciences, 010309 optics, Planet, 0103 physical sciences, Substellar object, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], protoplanetary disks, techniques: high angular resolution, Astronomy and Astrophysics, Planets and satellites: detection, Protoplanetary disks, Stars: individual: HD 100546, Techniques: high angular resolution, Techniques: polarimetric, Astrometry, Wavelength, techniques: polarimetric, 13. Climate action, Space and Planetary Science, Orbital motion, stars: individual: HD 100546, Astrophysics::Earth and Planetary Astrophysics, Protoplanet, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: The nearby Herbig Be star HD100546 is known to be a laboratory for the study of protoplanets and their relation with the circumstellar disk that is carved by at least 2 gaps. We observed the HD100546 environment with high contrast imaging exploiting several different observing modes of SPHERE, including datasets with/without coronagraphs, dual band imaging, integral field spectroscopy and polarimetry. The picture emerging from these different data sets is complex. Flux-conservative algorithms images clearly show the disk up to 200au. More aggressive algorithms reveal several rings and warped arms overlapping the main disk. The bright parts of this ring lie at considerable height over the disk mid-plane at about 30au. Our images demonstrate that the brightest wings close to the star in the near side of the disk are a unique structure, corresponding to the outer edge of the intermediate disk at ~40au. Modeling of the scattered light from the disk with a geometrical algorithm reveals that a moderately thin structure can well reproduce the light distribution in the flux-conservative images. We suggest that the gap between 44 and 113 au span between the 1:2 and 3:2 resonance orbits of a massive body located at ~70au that might coincide with the candidate planet HD100546b detected with previous thermal IR observations. In this picture, the two wings can be the near side of a ring formed by disk material brought out of the disk at the 1:2 resonance with the same massive object. While we find no clear evidence confirming detection of the planet candidate HD100546c in our data, we find a diffuse emission close to the expected position of HD100546b. This source can be described as an extremely reddened substellar object surrounded by a dust cloud or its circumplanetary disk. Its astrometry is broadly consistent with a circular orbital motion on the disk plane., Comment: Accepted by A&A on 30/08/2018
Published: 2018
Full Text: View/download PDF

16. Subaru/HiCIAO HK s Imaging of LKHa 330: Multi-band Detection of the Gap and Spiral-like Structures

Author: Uyama, T., Hashimoto, J., Muto, T., Akiyama, E., Dong, R., de Leon, J., Sakon, I., Kudo, T., Kusakabe, N., Kuzuhara, M., Bonnefoy, M., Abe, L., Brandner, W., Brandt, T., Carson, J., Currie, T., Egner, S., Feldt, M., Fung, J., Goto, M., Grady, C., Guyon, O., Hayano, Y., Hayashi, M., Hayashi, S., Henning, T., Hodapp, K., Ishii, M., Iye, M., Janson, M., Kandori, R., Knapp, G., Kwon, J., Matsuo, T., Mayama, S., Mcelwain, M., Miyama, S., Morino, J., Moro-Martin, A., Nishimura, T., Pyo, T., Serabyn, E., Sitko, M., Suenaga, T., Suto, H., Suzuki, R., Takahashi, Y., Takami, M., Takato, N., Terada, H., Thalmann, C., Turner, E., Watanabe, M., Wisniewski, J., Yamada, T., Yang, Y., Takami, H., Usuda, T., and Tamura, M.
Subjects: Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present H- and K s-bands observations of the LkHα 330 disk with a multi-band detection of the large gap and spiral-like structures. The morphology of the outer disk (r ̃ 0.″3) at PA = 0°-45° and PA° = 180-290° is likely density wave-induced spirals, and comparison between our observational results and simulations suggests a planet formation. We have also investigated the azimuthal profiles at the ring and the outer-disk regions as well as radial profiles in the directions of the spiral-like structures and semimajor axis. Azimuthal analysis shows a large variety in wavelength and implies that the disk has non- axisymmetric dust distributions. The radial profiles in the major-axis direction (PA = 271°) suggest that the outer region (r ≥ 0.″25) may be influenced by shadows of the inner region of the disk. The spiral-like directions (PA = 10° and 230°) show different radial profiles, which suggests that the surfaces of the spiral-like structures are highly flared and/or have different dust properties. Finally, a color map of the disk shows a lack of an outer eastern region in the H-band disk, which may hint at the presence of an inner object that casts a directional shadow onto the disk.
Published: 2018

17. Orbital characterization of GJ1108A system, and comparison of dynamical mass with model-derived mass for resolved binaries

Author: Mede, K., Schlieder, J. E., Janson, M., Brandt, T. D., Hirano, T., Narita, N., Wisniewski, J., Biller, B., Bonnefoy, M., Carson, J. C., McElwain, M. W., Turner, E. L., Mayama, S., Akiyama, E., Uyama, T., Kudo, T., Hashimoto, J., Abe, Lyu, Brander, W., Egner, S., Feldt, M., Grady, C. A., Guyon, O., Henning, T., Hodapp, K. W., Knapp, G. R., Mono-Martin, A., Pyo, T., Serabyn, E., Suenaga, Takuya, Takahashi, Yasuhiro H., Takami, M., Thalmann, C., Mizuki, Toshiyuki, Kuzuhara, Masayuki, Yamada, Toru, Matsuo, Taro, Nakagawa, Takao, Kusakabe, Nobuhiko, Goto, Miwa, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Ishii, Miki, Iye, Masanori, Kandori, R., Kwon, Jungmi, Miyama, Shoken, Morino, Jun-ichi, Moro-Martin, A., Nishimura, Tetsuo, Suto, Hiroshi, Suzuki, Ryuji, Takato, Naruhisa, Terada, Hiroshi, Watanabe, Makoto, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide
Subjects: 010504 meteorology & atmospheric sciences, Phase (waves), FOS: Physical sciences, Astrophysics, 01 natural sciences, stars: individual (GJ1108A), stars: low-mass, 0103 physical sciences, Binary system, Adaptive optics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Accretion (meteorology), Astronomy and Astrophysics, Astrometry, Mass comparison, binaries: visual, stars: imaging, Radial velocity, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, binaries: spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract: 著者人数: 58名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 水木, 敏幸; 山田, 亨; 中川, 貴雄; 權, 靜美), Accepted: 2018-08-13, 資料番号: SA1180204000
Published: 2018
Full Text: View/download PDF

18. SPHERE/ZIMPOL high resolution polarimetric imager

Author: Schmid, Hans Martin, Bazzon, Andreas, Roelfsema, Ronald, Mouillet, David, Milli, Julien, Menard, François, Gisler, Daniel, Hunziker, Sandra, Pragt, Johan, Dominik, Carsten, Boccaletti, Anthony, Ginski, Christian, Abe, L., Antoniucci, S., Avenhaus, H., Baruffolo, A., Baudoz, P., Beuzit, J.L., Carbillet, M., Chauvin, G., Claudi, R., Costille, A., Daban, J.B., de Haan, M., Desidera, S., Dohlen, K., Downing, M., Elswijk, E., Engler, N., Feldt, M., Fusco, Thierry, Girard, J., Gratton, R., Hanenburg, H., Henning, T., Hubin, N., Joos, F., Kasper, M., Keller, C., Langlois, M., Lagadec, E., Martinez, P., Mulder, E., PAVLOV, A., Podio, L., Puget, P., Quanz, S., Rigal, F., Salasnich, B., Sauvage, Jean-François, Schuil, M., Siebenmorgen, R., Sissa, E., Snik, F., Suarez, M., Thalmann, C., Turatto, M., Udry, S., van Duin, A., van Holstein, R., Vigan, A., Wildi, F., 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), NOVA Optical Infrared Instrumentation Group, 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), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Istituto Ricerche Solari Locarno, Kiepenheuer-Institut für Sonnenphysik (KIS), 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), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Padova (OAPD), 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), Universidad de Chile, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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), Universiteit Leiden, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidad de Chile = University of Chile [Santiago] (UCHILE), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Genève = University of Geneva (UNIGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: [PHYS]Physics [physics], INSTRUMENTATION:POLARIMETERS, [SPI]Engineering Sciences [physics], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], instrumentation: high angular resolution, instrumentation: detectors, instrumentation: polarimeters, adaptive optics, Instrumentation: high angular resolution, Instrumentation: polarimeters, Instrumentation: detectors, Planetary systems, Circumstellar matter [Instrumentation], instrumentation: adaptive optics, planetary systems, circumstellar matter
Abstract: International audience; Context . The SPHERE “planet finder” is an extreme adaptive optics (AO) instrument for high resolution and high contrast observations at the Very Large Telescope (VLT). We describe the Zurich Imaging Polarimeter (ZIMPOL), the visual focal plane subsystem of SPHERE, which pushes the limits of current AO systems to shorter wavelengths, higher spatial resolution, and much improved polarimetric performance. Aims . We present a detailed characterization of SPHERE/ZIMPOL which should be useful for an optimal planning of observations and for improving the data reduction and calibration. We aim to provide new benchmarks for the performance of high contrast instruments, in particular for polarimetric differential imaging. Methods . We have analyzed SPHERE/ZIMPOL point spread functions (PSFs) and measure the normalized peak surface brightness, the encircled energy, and the full width half maximum (FWHM) for different wavelengths, atmospheric conditions, star brightness, and instrument modes. Coronagraphic images are described and the peak flux attenuation and the off-axis flux transmission are determined. Simultaneous images of the coronagraphic focal plane and the pupil plane are analyzed and the suppression of the diffraction rings by the pupil stop is investigated. We compared the performance at small separation for different coronagraphs with tests for the binary α Hyi with a separation of 92 mas and a contrast of Δ m ≈ 6 m . For the polarimetric mode we made the instrument calibrations using zero polarization and high polarization standard stars and here we give a recipe for the absolute calibration of polarimetric data. The data show small (< 1 mas) but disturbing differential polarimetric beam shifts, which can be explained as Goos-Hähnchen shifts from the inclined mirrors, and we discuss how to correct this effect. The polarimetric sensitivity is investigated with non-coronagraphic and deep, coronagraphic observations of the dust scattering around the symbiotic Mira variable R Aqr. Results . SPHERE/ZIMPOL reaches routinely an angular resolution (FWHM) of 22−28 mas, and a normalized peak surface brightness of SB 0 − m star ≈ −6.5 m arcsec −2 for the V -, R - and I -band. The AO performance is worse for mediocre ≳1.0″ seeing conditions, faint stars m R ≳ 9 m , or in the presence of the “low wind” effect (telescope seeing). The coronagraphs are effective in attenuating the PSF peak by factors of > 100, and the suppression of the diffracted light improves the contrast performance by a factor of approximately two in the separation range 0.06″−0.20″. The polarimetric sensitivity is Δ p < 0.01% and the polarization zero point can be calibrated to better than Δ p ≈ 0.1%. The contrast limits for differential polarimetric imaging for the 400 s I -band data of R Aqr at a separation of ρ = 0.86″ are for the surface brightness contrast SB pol ( ρ )− m star ≈ 8 m arcsec −2 and for the point source contrast m pol ( ρ )− m star ≈ 15 m and much lower limits are achievable with deeper observations. Conclusions . SPHERE/ZIMPOL achieves imaging performances in the visual range with unprecedented characteristics, in particular very high spatial resolution and very high polarimetric contrast. This instrument opens up many new research opportunities for the detailed investigation of circumstellar dust, in scattered and therefore polarized light, for the investigation of faint companions, and for the mapping of circumstellar H α emission.
Published: 2018

19. Post conjunction detection of $��$ Pictoris b with VLT/SPHERE

Author: Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, M., Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Coroller, H. Le, Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Mueller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Menard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., de Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Moller-Nilsson, O., Llored, M., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., and Wildi, F.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract: With an orbital distance comparable to that of Saturn in the solar system, \bpic b is the closest (semi-major axis $\simeq$\,9\,au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to \bpic have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet's orbital parameters. We aimed at further constraining \bpic b orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. We used SPHERE at the VLT to precisely monitor the orbital motion of beta \bpic b since first light of the instrument in 2014. We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6\,au) and prevented further detection. We redetected \bpic b on the northeast side of the disk at a separation of 139\,mas and a PA of 30$^{\circ}$ in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of $a = 9.0 \pm 0.5$ au (1 $��$), it definitely excludes previously reported possible long orbital periods, and excludes \bpic b as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away., accepted by A&A
Published: 2018
Full Text: View/download PDF

20. Gearing up SPHERE

Author: Kasper M., Beuzit J.-L., Feldt M., Dohlen K., Mouillet D., Puget P., Wildi F., Abe L., and Bar
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract: Direct imaging and spectral characterisation of exoplanets is one of the most exciting but also one of the most challenging areas in modern astronomy. The challenge is to overcome the very large contrast between the host star and its planet seen at very small angular separations. This article reports on the progress made in the construction of the second generation VLT instrument SPHERE the Spectro Polarimetric High contrast Exoplanet REsearch instrument. SPHERE is expected to be commissioned on the VLT in 2013.
Published: 2013

21. Azimuthal asymmetries in the debris disk around HD61005

Author: Olofsson, J., Samland, M., Avenhaus, H., Caceres, C., Henning, Th, Moor, A., Milli, J., Canovas, H., Quanz, S., Schreiber, M. R., Augereau, J. -C, Bayo, A., Bazzon, A., Beuzit, J. -L, Boccaletti, A., Buenzli, E., Casassus, S., Chauvin, G., Dominik, C., Desidera, S., Feldt, M., Gratton, R., Janson, M., Lagrange, A. -M, Langlois, M., Lannier, J., Maire, A. -L, Mesa, D., Pinte, C., Rouan, D., Salter, G., Thalmann, C., and Arthur Vigan
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: Debris disks offer valuable insights into the latest stages of circumstellar disk evolution, and can possibly help us to trace the outcomes of planetary formation processes. In the age range 10 to 100\,Myr, most of the gas is expected to have been removed from the system, giant planets (if any) must have already been formed, and the formation of terrestrial planets may be on-going. Pluto-sized planetesimals, and their debris released in a collisional cascade, are under their mutual gravitational influence, which may result into non-axisymmetric structures in the debris disk. High angular resolution observations are required to investigate these effects and constrain the dynamical evolution of debris disks. Furthermore, multi-wavelength observations can provide information about the dust dynamics by probing different grain sizes. Here we present new VLT/SPHERE and ALMA observations of the debris disk around the 40\,Myr-old solar-type star HD\,61005. We resolve the disk at unprecedented resolution both in the near-infrared (in scattered and polarized light) and at millimeter wavelengths. Thanks to the new observations, we propose a solution for both the radial and azimuthal distribution of the dust grains in the debris disk. We find that the disk has a moderate eccentricity ($e \sim 0.1$) and that the dust density is two times larger at the pericenter compared to the apocenter. With no giant planets detected in our observations, we investigate alternative explanations besides planet-disk interactions to interpret the inferred disk morphology. We postulate that the morphology of the disk could be the consequence of a massive collision between $\sim$\,1000\,km-sized bodies at $\sim$\,61\,au. If this interpretation holds, it would put stringent constraints on the formation of massive planetesimals at large distances from the star., Comment: Accepted by A&A
Published: 2016
Full Text: View/download PDF

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

Author: Reggiani, M., Meyer, M. R., Chauvin, G., Vigan, A., Quanz, S. P., Biller, B., Bonavita, M., Desidera, S., Delorme, P., Hagelberg, J., Maire, A.-L., Boccaletti, A., Beuzit, J.-L., Buenzli, E., Carson, J., Covino, E., Feldt, M., Girard, J., Gratton, R., Henning, T., Kasper, M., Lagrange, A.-M., Mesa, D., Messina, S., Montagnier, G., Mordasini, Christoph, Mouillet, D., Schlieder, J. E., Segransan, D., Thalmann, C., and Zurlo, A.
Subjects: 530 Physics
Published: 2016
Full Text: View/download PDF

23. Characterization of the gaseous companion �� Andromedae b: New Keck and LBTI high-contrast observations

Author: Bonnefoy, M., Currie, T., Marleau, G. -D., Schlieder, J. E., Wisniewski, J., Carson, J., Covey, K. R., Henning, T., Biller, B., Hinz, P., Klahr, H., Boyer, A. N. Marsh, Zimmerman, N., Janson, M., McElwain, M., Mordasini, C., Skemer, A., Bailey, V., Defr��re, D., Thalmann, C., Skrutskie, M., Allard, F., Homeier, D., Tamura, M., Feldt, M., Cumming, A., Grady, C., Brandner, W., Kandori, R., Kuzuhara, M., Fukagawa, M., Kwon, J., Kudo, T., Hashimoto, J., Kusakabe, N., Abe, L., Brandt, T., Egner, S., Guyon, O., Hayano, Y., Hayashi, M., Hayashi, S., Hodapp, K., Ishii, M., Iye, M., Knapp, G., Matsuo, T., Mede, K., Miyama, M., Morino, J. -I., Moro-Martin, A., Nishimura, T., Pyo, T., Serabyn, E., Suenaga, T., Suto, H., Suzuki, R., Takahashi, Takami, M., Takato, N., Terada, H., Tomono, D., Turner, E., Watanabe, M., Yamada, T., Takami, H., and Usuda, T.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We previously reported the direct detection of a low mass companion at a projected separation of 55+-2 AU around the B9 type star �� Andromedae. The properties of the system (mass ratio, separation) make it a benchmark for the understanding of the formation and evolution of gas giant planets and brown dwarfs on wide-orbits. We present new angular differential imaging (ADI) images of the Kappa Andromedae system at 2.146 (Ks), 3.776 (L'), 4.052 (NB 4.05) and 4.78 ��m (M') obtained with Keck/NIRC2 and LBTI/LMIRCam, as well as more accurate near-infrared photometry of the star with the MIMIR instrument. We derive a more accurate J = 15.86 +- 0.21, H = 14.95 +- 0.13, Ks = 14.32 +- 0.09 mag for �� And b. We redetect the companion in all our high contrast observations. We confirm previous contrasts obtained at Ks and L' band. We derive NB 4.05 = 13.0 +- 0.2 and M' = 13.3 +- 0.3 mag and estimate Log10(L/Lsun) = -3.76 +- 0.06. We build the 1-5 microns spectral energy distribution of the companion and compare it to seven PHOENIX-based atmospheric models in order to derive Teff = 1900+100-200 K. Models do not set constrains on the surface gravity. ``Hot-start" evolutionary models predict masses of 14+25-2 MJup based on the luminosity and temperature estimates, and considering a conservative age range for the system (30+120-10 Myr). ``warm-start" evolutionary tracks constrain the mass to M >= 11 MJup. Therefore, the mass of �� Andromedae b mostly falls in the brown-dwarf regime, due to remaining uncertainties in age and mass-luminosity models. According to the formation models, disk instability in a primordial disk could account for the position and a wide range of plausible masses of �� And b., 20 pages, 16 figures, accepted for publication in Astronomy and Astrophysics on August 6, 2013
Published: 2013
Full Text: View/download PDF

24. The ZIMPOL high contrast imaging polarimeter for SPHERE: sub-system test results

Author: Roelfsema, R., Gisler, D., Pragt, J., Schmid, H.M., Bazzon, A., Dominik, C., Baruffolo, A., Beuzit, J.-L., Charton, J., Dohlen, K., Downing, M., Elswijk, E., Feldt, M., de Haan, M., Hubin, N., Kasper, M., Keller, C., Lizon, J.-L., Mouillet, D., Pavlov, A., Puget, P., Rochat, S., Salasnich, B., Steiner, P., Thalmann, C., Waters, R., Wildi, F., Shaklan, S., and Low Energy Astrophysics (API, FNWI)
Subjects: 010309 optics, Physics, Optics, business.industry, 0103 physical sciences, System testing, Polarimeter, High contrast imaging, business, 010303 astronomy & astrophysics, 01 natural sciences
Abstract: SPHERE (Spectro-Polarimetric High Contrast Exoplanet Research) is one of the first instruments which aim for the direct detection from extra-solar planets. The instrument will search for direct light from old planets with orbital periods of several months to several years as we know them from our solar system. These are planets which are in or close to the habitable zone. ZIMPOL (Zurich Imaging Polarimeter) is the high contrast imaging polarimeter subsystem of the ESO SPHERE instrument. ZIMPOL is dedicated to detect the very faint reflected and hence polarized visible light from extrasolar planets. The search for reflected light from extra-solar planets is very demanding because the signal decreases rapidly with the orbital separation. For a Jupiter-sized object and a separation of 1 AU the planet/star contrast to be achieved is on the order of 10-8 for a successful detection. This is much more demanding than the direct imaging of young self-luminous planets. ZIMPOL is located behind an extreme AO system (SAXO) and a stellar coronagraph. SPHERE is foreseen to have first light at the VLT at the end of 2012. ZIMPOL is currently in the subsystem testing phase. We describe the results of verification and performance testing done at the NOVA-ASTRON lab. We will give an overview of the system noise performance, the polarimetric accuracy and the high contrast testing. For the high contrast testing we will describe the impact of crucial system parameters on the contrast performance. SPHERE is an instrument designed and built by a consortium consisting of IPAG, MPIA, LAM, LESIA, Fizeau, INAF, Observatoire de Genève, ETH, NOVA, ONERA and ASTRON in collaboration with ESO.
Published: 2011

25. CHEOPS NIR IFS: exploring stars neighborhood spectroscopically

Author: Claudi, R.U., Turatto, M., Gratton, R., Antichi, J., Buson, S., Pernechele, C., Desidera, S., Baruffolo, A., Lima, J., Alcalà, J., Cascone, E., Piotto, G., Ortolani, S., Schmid, H.M., Feldt, M., Neuhauser, R., Waters, R., Berton, A., Bagnara, P., Moorwood, A.F.M., Iye, M., and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimetry, Strehl ratio, Astronomy, Field of view, Astrophysics::Cosmology and Extragalactic Astrophysics, Exoplanet, Optics, Integral field spectrograph, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, Adaptive optics, Spectrograph, Astrophysics::Galaxy Astrophysics
Abstract: CHEOPS is a 2nd generation VLT instrument for the direct detection of extrasolar planets. The project is currently in its Phase A. It consists of an high order adaptive optics system which provides the necessary Strehl ratio for the differential polarimetric imager (ZIMPOL) and an Integral Field Spectrograph (IFS). The IFS is a very low resolution spectrograph (R~15) which works in the near IR (0.95-1.7 mum), an ideal wavelength range for the ground based detection of planetary features. In our baseline design, the Integral Field Unit (IFU) is a microlens array of about 250x250 elements which will cover a field of view of about 3.5x3.5 arcsecs2 in proximity of the target star. In this paper we describe the instrument, its preliminary optical design and the basic requirements about detectors. In a separate contribution to this conference, we present the very low resolution disperser.
Published: 2004

26. CHEOPS/ZIMPOL: a VLT instrument study for the polarimetric search of scattered light from extrasolar planets

Author: Gisler, D., Schmid, H.M., Thalmann, C., Povel, H.P., Stenflo, J.O., Joos, F., Feldt, M., Lenzen, R., Tinbergen, J., Gratton, R., Stuik, R., Stam, D.M., Brandner, W., Hippler, S., Turatto, M., Neuhauser, R., Dominik, C., Hatzes, A., Henning, T., Lima, J., Quirrenbach, A., Waters, L.B.F.M., Wuchterl, G., Zinnecker, H., Moorwood, A.F.M., Iye, M., and Low Energy Astrophysics (API, FNWI)
Subjects: Physics, Ccd camera, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimetry, Astronomy, Polarimeter, Polarization (waves), Exoplanet, Optics, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Scattered light, business
Abstract: We present results from a phase A study supported by ESO for a VLT instrument for the search and investigation of extrasolar planets. The envisaged CHEOPS (CHaracterizing Extrasolar planets by Opto-infrared Polarization and Spectroscopy) instrument consists of an extreme AO system, a spectroscopic integral field unit and an imaging polarimeter. This paper describes the conceptual design of the imaging polarimeter which is based on the ZIMPOL (Zurich IMaging POLarimeter) technique using a fast polarization modulator combined with a demodulating CCD camera. ZIMPOL is capable of detecting polarization signals on the order of p=0.001% as demonstrated in solar applications. We discuss the planned implementation of ZIMPOL within the CHEOPS instrument, in particular the design of the polarization modulator. Further we describe strategies to minimize the instrumental effects and to enhance the overall measuring efficiency in order to achieve the very demanding science goals.
Published: 2004

27. The Planet Finder: Proposal for a 2nd Generation VLT Instrument

Author: Feldt, M., Hippler, S., Henning, T., Gratton, R., Turatto, M., Waters, L.B.F.M., Quirrenbach, A., Deming, D., Seager, S., and Low Energy Astrophysics (API, FNWI)
Published: 2003

28. The astrophysical potentials of the MIDI VLTI instrument

Author: Lopez, B., Leinert, C., Graser, U., Waters, L.B.F.M., Perrin, G., Herbst, T., Rottgering, H., Rouan, D., Stecklum, B., Mundt, R., Zinnecker, H., de Laverny, P., Feldt, M., Meisner, J., Dutrey, Th., Henning, T., Vakili, F., Lena, P.J., Quirrenbach, A., and Low Energy Astrophysics (API, FNWI)
Published: 2000

29. Orbital and atmospheric characterization of the planet within the gap of the PDS 70 transition disk

Author: Müller, A, Keppler, M, Henning, T, Samland, M, Chauvin, G, Beust, H, Maire, AL, Molaverdikhani, K, Van Boekel, R, Benisty, M, Boccaletti, A, Bonnefoy, M, Cantalloube, F, Charnay, B, Baudino, JL, Gennaro, M, Long, ZC, Cheetham, A, Desidera, S, Feldt, M, Fusco, T, Girard, J, Gratton, R, Hagelberg, J, Janson, M, Lagrange, AM, Langlois, M, Lazzoni, C, Ligi, R, Ménard, F, Mesa, D, Meyer, M, Mollière, P, Mordasini, C, Moulin, T, Pavlov, A, Pawellek, N, Quanz, SP, Ramos, J, Rouan, D, Sissa, E, Stadler, E, Vigan, A, Wahhaj, Z, Weber, L, and Zurlo, A
Subjects: planets and satellites: atmospheres, 13. Climate action, Astrophysics::Solar and Stellar Astrophysics, planets and satellites: individual: PDS 70, astrometry, Astrophysics::Earth and Planetary Astrophysics, methods: observational, Astrophysics::Galaxy Astrophysics, techniques: spectroscopic
Abstract: 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 years which allows 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 to 3.8 micrometer). 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 ~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 between 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_jupiter 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 dataset 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 for young giant planets. The detailed atmospheric analysis indicates that a circumplanetary disk may contribute to the total planet flux.

30. CHEOPS: a second generation VLT instrument for the direct detection of exo-planets

Author: Claudi, R. U., Costa, J., Feldt, M., Gratton, R., Amorim, A., Henning, Th, Hippler, S., Neuhäuser, R., claudio pernechele, Turatto, M., Schmid, H. M., Waters, R., and Zinnecker, H.

31. A 'planet finder' instrument for the ESO VLT

Author: Feldt, M., Turatto, M., Schmid, H. M., Waters, R., Neuhäuser, R., and Antonio Amorim

32. VizieR Online Data Catalog: NIR spectrum of exoplanet HIP 65426b (Chauvin+, 2017)

Author: Chauvin, G., Desidera, S., Lagrange, A. -M, Arthur Vigan, Gratton, R., Langlois, M., Bonnefoy, M., Beuzit, J. -L, Feldt, M., Mouillet, D., Meyer, M., Cheetham, A., Biller, B., Boccaletti, A., D Orazi, V., Galicher, R., Hagelberg, J., Maire, A. -L, Mesa, D., Olofsson, J., Samland, M., Schmidt, T. O. B., Sissa, E., Bonavita, M., Charnay, B., Cudel, M., Daemgen, S., Delorme, P., Janin-Potiron, P., Janson, M., Keppler, M., Le Coroller, H., Ligi, R., Marleau, G. D., Messina, S., Molliere, P., Mordasini, C., Muller, A., Peretti, S., Perrot, C., Rodet, L., Rouan, D., Zurlo, A., Dominik, C., Henning, T., Menard, F., Schmid, H. -M, Turatto, M., Udry, S., Vakili, F., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignan, T. D., Mol Ler-Nilsson, O., Llored, M., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, R., 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., Antoniucci, S., Augereau, J. -C, Baudino, J. -L, Brandner, W., Engler, N., Girard, J., Gry, C., Kral, Q., Kopytova, T., Lagadec, E., Milli, J., Moutou, C., Schlieder, J., Szulagyi, J., Thalmann, C., and Wahhaj, Z.

33. Dynamical models to explain observations with SPHERE in planetary systems with double debris belts

Author: Lazzoni, C, Desidera, S, Marzari, F, Boccaletti, A, Langlois, M, Mesa, D, Gratton, R, Kral, Q, Pawellek, N, Olofsson, J, Bonnefoy, M, Chauvin, G, Lagrange, AM, Vigan, A, Sissa, E, Antichi, J, Avenhaus, H, Baruffolo, A, Baudino, JL, Bazzon, A, Beuzit, JL, Biller, B, Bonavita, M, Brandner, W, Bruno, P, Buenzli, E, Cantalloube, F, Cascone, E, Cheetham, A, Claudi, RU, Cudel, M, Daemgen, S, Caprio, VD, Delorme, P, Fantinel, D, Farisato, G, Feldt, M, Galicher, R, Ginski, C, Girard, J, Giro, E, Janson, M, Hagelberg, J, Henning, T, Incorvaia, S, Kasper, M, Kopytova, T, Lecoroller, H, Lessio, L, Ligi, R, Maire, AL, Ménard, F, Meyer, M, Milli, J, Mouillet, D, Peretti, S, Perrot, C, Rouan, D, Samland, M, Salasnich, B, Salter, G, Schmidt, T, Scuderi, S, Sezestre, E, Turatto, M, Udry, S, Wildi, F, and Zurlo, A
Subjects: planet-disk interactions, 13. Climate action, instrumentation: high angular resolution, Kuiper belt: general, techniques: image processing, Astrophysics::Earth and Planetary Astrophysics, methods: observational, methods: analytical
Abstract: A large number of systems harboring a debris disk show evidence for a double belt architecture. One hypothesis for explaining the gap between the belts is the presence of one or more planets dynamically carving it. This work aims to investigate this scenario in systems harboring two components debris disks. All the targets in the sample were observed with the SPHERE instrument which performs high-contrast direct imaging. Positions of the inner and outer belts were estimated by SED fitting of the infrared excesses or, when available, from resolved images of the disk. Very few planets have been observed so far in debris disks gaps and we intended to test if such non-detections depend on the observational limits of the present instruments. This aim is achieved by deriving theoretical predictions of masses, eccentricities and semi-major axes of planets able to open the observed gaps and comparing such parameters with detection limits obtained with SPHERE. The relation between the gap and the planet is due to the chaotic zone around the orbit of the planet. The radial extent of this zone depends on the mass ratio between the planet and the star, on the semi-major axis and on the eccentricity of the planet and it can be estimated analytically. We apply the formalism to the case of one planet on a circular or eccentric orbit. We then consider multi-planetary systems: 2 and 3 equal-mass planets on circular orbits and 2 equal-mass planets on eccentric orbits in a packed configuration. We then compare each couple of values (M,a), derived from the dynamical analysis of single and multiple planetary models, with the detection limits obtained with SPHERE. Our results show that the apparent lack of planets in gaps between double belts could be explained by the presence of a system of two or more planets possibly of low mass and on an eccentric orbits whose sizes are below the present detection limits.

34. The Planet Finder: Proposal for a 2nd Generation VLT Instrument

Author: Feldt, M., Stefan Hippler, Henning, Th, Gratton, R., Turatto, M., Waters, R., and Quirrenbach, A.

35. Investigating the young solar system analog HD 95086

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

36. SPHERE: exo-planets science with the new frontier of high contrast imaging

Author: Claudi, R., Beuzit, J. -L, Feldt, M., Mouillet, D., Dohlen, K., Puget, P., Wildi, F., Baruffolo, A., Charton, J., Antichi, J., Boccaletti, A., Desidera, S., Fusco, T., Raffaele Gratton, Langlois, M., Mesa, D., Pragt, J., Raboub, P., Roelfsema, R., Saisse, M., Schmid, H. -M, Turatto, M., Moutou, C., Henning, T., Udry, S., Vakili, F., Waters, R., 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), Pôle Astronomie du LESIA, 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Ingénieurs, Techniciens et Administratifs
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience

37. Simulation of planet detection with the SPHERE IFS

Author: Mesa, D., Gratton, R., Berton, A., Antichi, J., Verinaud, C., Boccaletti, A., Kasper, M., Claudi, R. U., Desidera, S., Giro, E., Beuzit, J. -L, Dohlen, K., Feldt, M., Mouillet, D., Chauvin, G., and Arthur Vigan
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: Aims. We present simulations of the perfomances of the future SPHERE IFS instrument designed for imaging extrasolar planets in the near infrared (Y, J, and H bands). Methods. We used the IDL package code for adaptive optics simulation (CAOS) to prepare a series of input point spread functions (PSF). These feed an IDL tool (CSP) that we designed to simulate the datacube resulting from the SPHERE IFS. We performed simulations under different conditions to evaluate the contrast that IFS will be able to reach and to verify the impact of physical propagation within the limits of the near field of the aperture approximation (i.e. Fresnel propagation). We then performed a series of simulations containing planet images to test the capability of our instrument to correctly classify the found objects. To this purpose we developed a separated IDL tool. Results. We found that using the SPHERE IFS instrument and appropriate analysis techniques, such as multiple spectral differential imaging (MDI), spectral deconvolution (SD), and angular differential imaging (ADI), we should be able to image companion objects down to a luminosity contrast of ? 10-7 with respect to the central star in favorable cases. Spectral deconvolution resulted in the most effective method for reducing the speckle noise. We were then able to find most of the simulated planets (more than 90% with the Y-J-mode and more than the 95% with the Y-H-mode) for contrasts down to 3 \times 10-7 and separations between 0.3 and 1.0 arcsec. The spectral classification is accurate but seems to be more precise for late T-type spectra than for earlier spectral types. A possible degeneracy between early L-type companion objects and field objects (flat spectra) is highlighted. The spectral classification seems to work better using the Y-H-mode than with the Y-J-mode., Comment: 11 pages, 11 figures

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

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

39. Direct Detection of Giant Extrasolar Planets with SPHERE on the VLT

Author: Beuzit, J. -L, Boccaletti, A., Feldt, M., Dohlen, K., Mouillet, D., Puget, P., Wildi, F., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Carbillet, M., Charton, J., Claudi, R., Desidera, S., Downing, M., Fabron, C., Feautrier, P., Fedrigo, E., Fusco, T., Gach, J. -L, Giro, E., Gratton, R., Henning, T., Hubin, N., Joos, F., Kasper, M., Lagrange, A. -M, Langlois, M., Lenzen, R., Moutou, C., Pavlov, A., Petit, C., Pragt, J., Rabou, P., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Saisse, M., Schmid, H. -M, Stadler, E., Thalmann, C., Turatto, M., Udry, S., Vakili, F., Arthur Vigan, and Waters, R.

40. SPHERE system analysis predictions

Author: Dohlen, K., Wildi, F., Beuzit, J. L., Puget, P., Mouillet, D., Baruffolo, A., Boccaletti, A., Charton, J., Claudi, R., Costille, A., Feautrier, P., Feldt, M., Fusco, T., Raffaele Gratton, Kasper, M., Langlois, M., Le Mignant, D., Lizon, J. L., Hubin, N., Pavlov, A., Petit, C., Pragt, J., Rabou, P., Rochat, S., Roelfsema, R., Sauvage, J. F., and Schmid, H. M.
Subjects: ADAPTIVE OPTICS, WAVEFRONT CORRECTORS, REAL-TIME CONTROL, Astrophysics::Instrumentation and Methods for Astrophysics, POST-PROCESSING, Astrophysics::Cosmology and Extragalactic Astrophysics, INSTRUMENTS, EXTREMELY LARGE TELESCOPES, PATHFINDERS, ATMOSPHERIC TURBULENCE, MODELING, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, WAVEFRONT SENSING, Astrophysics::Galaxy Astrophysics, LASER GUIDE STAR SYSTEMS
Abstract: SPHERE is an extra-solar planet imager instrument for ESO's VLT telescope. Scheduled for first light in 2012, aims to detect giant extra-solar planet in the vicinity of bright stars and to characterise the objects found through spectroscopic and polarimetric observations. The observations will be done both within the Y, J, H and Ks atmospheric windows (~0.95 – 2.32μm) by the aid of a dual imaging camera (IRDIS) and an integral field spectrograph (IFS), and in the visible using a fast-modulating polarizing camera (ZIMPOL). The instrument employs an extreme-AO turbulence compensation system, focal plane tip-tilt correction, and interferential coronagraphs. The aim of this paper is to analyse the approach taken for system analysis and implementation in the light of forthcoming instruments of this type to be design and built for ELT-class telescopes.

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

Author: Lagrange, A., Kasper, M., Mordasini, C., Thalmann, C., Segransan, D., Reggiani, M., Moutou, C., Mouillet, D., Montagnier, G., Meyer, M., Messina, S., Mesa, D., Coroller, H., Gratton, R., Girard, J., Feldt, M., Buenzli, E., Boccaletti, A., Beuzit, J., Zurlo, A., Quanz, S., Janson, M., Henning, T., Hagelberg, J., Covino, E., Carson, J., Bonnefoy, M., Schlieder, J., Delorme, P., Meunier, J., Desidera, S., Chauvin, G., Rice, K., Forgan, D., Biller, B., Bonavita, M., Vigan, A., Beuzit, J.-L., Lagrange, A.-M., Meunier, J.-C., Le Coroller, H., Lagrange, M., Girard, H., and Meunier, C.
Abstract: Understanding the formation and evolution of giant planets ($\ge$1 $M_{Jup}$) at wide orbital separation ($\ge$5 AU) is one of the goals of direct imaging. Over the past 15 years, many surveys have placed strong constraints on the occurrence rate of wide-orbit giants, mostly based on non-detections, but very few have tried to make a direct link with planet formation theories. In the present work, we combine the results of our previously published VLT/NaCo large program with the results of 12 past imaging surveys to constitute a statistical sample of 199 FGK stars within 100 pc, including 3 stars with sub-stellar companions. Using Monte Carlo simulations and assuming linear flat distributions for the mass and semi-major axis of planets, we estimate the sub-stellar companion frequency to be within 0.75-5.7% at the 68% confidence level (CL) within 20-300 AU and 0.5-75 $M_{Jup}$, which is compatible with previously published results. We also compare our results with the predictions of state-of-the-art population synthesis models based on the gravitational instability (GI) formation scenario by Forgan & Rice (2013), with and without scattering. We estimate that in both the scattered and non-scattered populations, we would be able to detect more than 30% of companions in the 1-75 $M_{Jup}$ range (95% CL). With the 3 sub-stellar detections in our sample, we estimate the fraction of stars that host a planetary system formed by GI to be within 1.0-8.6% (95% CL). We also conclude that even though GI is not common, it predicts a mass distribution of wide-orbit massive companions that is much closer to what is observed than what the core accretion scenario predicts. Finally, we associate the present paper with the release of the Direct Imaging Virtual Archive (DIVA, http://cesam.lam.fr/diva/), a public database that aims at gathering the results of past, present, and future direct imaging surveys. Comment: 20 pages, 11 figures. Accepted for publication in A&A

42. SPHERE: A Planet Finder Instrument for the VLT

Author: L Beuzit, J., Feldt, M., Dohlen, K., Mouillet, D., Puget, P., Antichi, J., Baudoz, P., Boccaletti, A., Carbillet, M., Charton, J., Claudi, R., Thierry Fusco, Gratton, R., Henning, T., Hubin, N., Joos, F., Kasper, M., Langlois, M., Moutou, C., Pragt, J., Rabou, P., Saisse, M., Schmid, H. M., Turatto, M., Udry, S., Vakili, F., Waters, R., Wildi, F., Laboratoire Hippolyte Fizeau (FIZEAU), 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 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)
Abstract: Proceedings of the conference In the Spirit of Bernard Lyot: The Direct Detection of Planets and Circumstellar Disks in the 21st Century, ed. P. Kalas, n/a, (2007); International audience

43. High-resolution near-infrared polarimetry of a circumstellar disk around UXTauA

Author: Tanii, R., Itoh, Y., Kudo, T., Hioki, T., Oasa, Y., Gupta, R., Sen, A. K., Wisniewski, J. P., Muto, T., Grady, C. A., Hashimoto, J., Fukagawa, M., Mayama, S., Hornbeck, J., Sitko, M. L., Russell, R. W., Werren, C., Cure, M., Currie, T., Ohashi, N., Okamoto, Y., Momose, M., Honda, M., Inutsuka, S. -I, Takeuchi, T., Dong, R., Abe, L., Brandner, W., Brandt, T. D., Carson, J., Egner, S. E., Feldt, M., Fukue, T., Goto, M., Guyon, O., Hayano, Y., Hayashi, M., Hayashi, S. S., Henning, T., Hodapp, K. W., Ishii, M., Iye, M., Janson, M., Kandori, R., Knapp, G. R., Kusakabe, N., Kuzuhara, M., Matsuo, T., Mcelwain, M. W., Miyama, S., Morino, J. -I, Moro-Martin, A., Nishimura, T., Pyo, T. -S, Serabyn, E., Suto, H., Suzuki, R., Takami, M., Takato, N., Terada, H., Thalmann, C., Tomono, D., Turner, E. L., Makoto Watanabe, Yamada, T., Takami, H., Usuda, T., and Tamura, M.

44. VizieR Online Data Catalog: HR 8799e and HR 8799d spectra (Zurlo+, 2016)

Author: Zurlo, A., Arthur Vigan, Galicher, R., Maire, A. -L, Mesa, D., Gratton, R., Chauvin, G., Kasper, M., Moutou, C., Bonnefoy, M., Desidera, S., Abe, L., Apai, D., Baruffolo, A., Baudoz, P., Baudrand, J., Beuzit, J. -L, Blancard, P., Boccaletti, A., Cantalloube, F., Carle, M., Cascone, E., Charton, J., Claudi, R. U., Costille, A., Caprio, V., Dohlen, K., Dominik, C., Fantinel, D., Feautrier, P., Feldt, M., Fusco, T., Gigan, P., Girard, J. H., Gisler, D., Gluck, L., Gry, C., Henning, T., Hugot, E., Janson, M., Jaquet, M., Lagrange, A. -M, Langlois, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mawet, D., Meyer, M. R., Milli, J., Moeller-Nilsson, O., Mouillet, D., Origne, A., Pavlov, A., Petit, C., Puget, P., Quanz, S. P., Rabou, P., Ramos, J., Rousset, G., Roux, A., Salasnich, B., Salter, G., Sauvage, J. -F, Schmid, H. M., Soenke, C., Stadler, E., Suarez, M., Turatto, M., Udry, S., Vakili, F., Wahhaj, Z., Wildi, F., and Antichi, J.

45. The ultracompact H II region G45.45+0.06. A pearl necklace in the sky

Author: Feldt, M., Stecklum, B., Henning, Th, Hayward, T. L., Lehmann, Th, and Randolf Klein

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Journal

Database

Publisher

45 results on '"Feldt M"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources