Author: "Le Mignant, D." / Search Limiters: Available in Library Collection - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Le Mignant, D."' showing total 93 results

Start Over Author "Le Mignant, D." Search Limiters Available in Library Collection

93 results on '"Le Mignant, D."'

1. Keck AO survey of Io global volcanic activity between 2 and 5 mu m

Author: Marchis, F, Le Mignant, D, Chaffee, F H, Davies, A G, Kwok, S H, Prange, R, de Pater, I, Amico, P, Campbell, R, Fusco, T, Goodrich, R W, and Conrad, A
Subjects: Io, volcanism, infrared observations
Abstract: We present in this Keck AO paper the first global high angular resolution observations of Io in three broadband near-infrared filters: Kc (2.3 mu m), Lp (3.8 mu m), and Ms (4.7 mu m). The Keck AO observations are composed of 13 data sets taken during short time intervals spanning 10 nights in December, 2001. The MISTRAL deconvolution process, which is specifically aimed for planetary images, was applied to each image. The spatial resolution achieved with those ground-based observations is 150, 240, and 300 km in the Kc, Lp, and Ms band, respectively, making them similar in quality to most of the distant observations of the Galileo/NIMS instrument. Eleven images per filter were selected and stitched together after being deprojected to build a cylindrical map of the entire surface of the satellite. In Kc-band, surface albedc, features, such as paterae (R > 60 km) are easily identifiable. The Babbar region is characterized by extremely low albedo at 2.2 mu m, and shows an absorption band at 0.9 mu m in Galileo/SSI data. These suggest that this region is covered by dark silicate deposits, possibly made of orthopyroxene. In the Lp-Ms (3-5 mu m) bands, the thermal emission from active centers is easily identified. We detected 26 hot spots in both broadband filters over the entire surface of the minor planet; two have never been seen active before, nine more are seen in the Ms band. We focused our study on the hot spots detected in both broadband filters. Using the measurements of their brightness, we derived the temperature and area covered by 100 brightness measurements. Loki displayed a relatively quiescent activity. Dazhbog, a new eruption detected by Galileo/NIMS in August 2001, is a major feature in our survey. We also point out the fading of Tvashtar volcanic activity after more than two years of energetic activity, and the presence of a hot, but small, active center at the location of Surt, possibly a remnant of its exceptional eruption detected in February 2001. Two new active centers, labeled F and V on our data, are detected. Using the best temperature and the surface area derived from the L and M band intensities, we calculated the thermal output of each active center. The most energetic hot spots are Loki and Dazhbog, representing respectively 36 and 19% of the total output calculated from a temperature fit of all hot spots (20.6 x 10(12) W). Based on the temperature derived from hot spots (similar to 400 K), our measurement can unambiguously identify the contribution to the heat flux from the silicate portion of the surface. Because the entire surface was observed, no extrapolation was required to calculate that flux. It is also important to note that we measured the brightness of the individual hot spots when they were located close to the Central Meridian. This minimizes the line-of-sight effect which does not follow strictly a classical cosine law. Finally, we argue that despite the widespread volcanic activity detected, Io was relatively quiescent in December 2001, with a minimum mean total output of 0.4-1.2 W m(-2). This output is at least a factor of two lower than those inferred from observations made at longer wavelengths and at different epochs. (c) 2005 Elsevier Inc. All rights reserved.
Published: 2005

2. Adaptive optics imaging of IRAS 18276-1431: A bipolar preplanetary nebula with circumstellar 'searchlight beams' and 'Arcs'

Author: Contreras, C. Sánchez, Le Mignant, D., Sahai, R., Gil de Paz, Armando, Morris, M., Contreras, C. Sánchez, Le Mignant, D., Sahai, R., Gil de Paz, Armando, and Morris, M.
Abstract: © 2007. The American Astronomical Society. All rights reserved. The authors thank the anonymous referee for his/ her critical comments and valuable suggestions that have significantly improved this paper. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work has been partially performed at the California Institute of Technology and the Department of Molecular and Infrared Astrophysics of the Instituto de Estructura de la Materia, CSIC, and has been partially supported by National Science Foundation grant 9981546 to Owens Valley Radio Observatory and the Spanish MCyT under project DGES/AYA2003- 02785. R. S. is thankful for partial financial support for this work from a NASA/ADP grant. A. G. d. P. is financed by the MAGPOP EU Marie Curie Research Training Network and partially by the Spanish Programa Nacional de Astronomía y Astrofísica under grant AYA2003-01676. M. M. and R. S. acknowledge financial support for this work from NASA LTSA and ADP awards RTOP 399-20-40-06 and RTOP 399-20-00-08, and HST/GO award GO 09101.01-A. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and the NASA Astrophysics Data System., We present high angular resolution images of the post-AGB nebula IRAS 18276-1431 (also known as OH 17.7-2.0) obtained with the Keck II adaptive optics (AO) system in its natural guide star (NGS) mode in the K_P, L_P, and M_S near-infrared bands. We also present supporting optical F606W and F814W HST images as well as interferometric observations of the 12^CO J = 1-0, 13^CO J = 1-0, and 2.6 mm continuum emission with OVRO. The envelope of IRAS 18276-1431 displays a clear bipolar morphology in our optical and NIR images with two lobes separated by a dark waist and surrounded by a faint 4.5'' × 3.4'' halo. Our K_P-band image reveals two pairs of radial "searchlight beams" emerging from the nebula center and several intersecting, arclike features. From our CO data we derive a mass of M > 0.38 (D/3 kpc)^2 M_☉ and an expansion velocity V_exp = 17 km s^-1 for the molecular envelope. The density in the halo follows a radial power law ∝r^-3, which is consistent with a mass-loss rate increasing with time. Analysis of the NIR colors indicates the presence of a compact central source of ~300-500 K dust illuminating the nebula in addition to the central star. Modeling of the thermal IR suggests a two-shell structure in the dust envelope: (1) an outer shell with inner and outer radius R_in ~ 1.6 × 10^16 and R_out ≥1.25 × 10^17 cm, dust temperature T_dust ~ 105-50 K, and a mean mass-loss rate of M ≈ 10^3 M_☉ yr^-1; and (2) an inner shell with R_in ~ 6.3 × 10 cm, T_dust ~ 500-105 K, and M ~ 3 × 10^-5 M_☉ yr^-1. An additional population of big dust grains (radius a ≥0.4 mm) with T_dust = 150-20 K and mass M_dust = (0.16-1.6) × 10^-3 (D/3 kpc)^2 M_☉ can account for the observed submillimeter and millimeter flux excess. The mass of the envelope enclosed within R_out = 1.25 × 10^17 cm derived from SED modeling is ~1 (D/3 kpc)^2 M_☉., W. M. Keck Foundation, National Science Foundation, Owens Valley Radio Observatory, Ministerio de Ciencia y Tecnología, (MCYT), España, Astrophysics Data Analysis program (ADP), NASA, Spanish Programa Nacional de Astronomía y Astrofísica, LTSA (Long Term Space Astrophysics program), NASA, National Aeronautics and Space Administration (NASA), HST/GO award, Unión Europea. FP6, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub
Published: 2023

3. The Keck Interferometer

Author: Colavita, M. M., Wizinowich, P. L., Akeson, R. L., Ragland, S., Woillez, J. M., Millan-Gabet, R., Serabyn, E., Abajian, M., Acton, D. S., Appleby, E., Beletic, J. W., Beichman, C. A., Bell, J., Berkey, B. C., Berlin, J., Boden, A. F., Booth, A. J., Boutell, R., Chaffee, F. H., Chan, D., Chin, J., Chock, J., Cohen, R., Cooper, A., Crawford, S. L., Creech-Eakman, M. J., Dahl, W., Eychaner, G., Fanson, J. L., Felizardo, C., Garcia-Gathright, J. I., Gathright, J. T., Hardy, G., Henderson, H., Herstein, J. S., Hess, M., Hovland, E. E., Hrynevych, M. A., Johansson, E., Johnson, R. L., Kelley, J., Kendrick, R., Koresko, C. D., Kurpis, P., Le Mignant, D., Lewis, H. A., Ligon, E. R., Lupton, W., McBride, D., Medeiros, D. W., Mennesson, B. P., Moore, J. D., Morrison, D., Nance, C., Neyman, C., Niessner, A., Paine, C. G., Palmer, D. L., Panteleeva, T., Papin, M., Parvin, B., Reder, L., Rudeen, A., Saloga, T., Sargent, A., Shao, M., Smith, B., Smythe, R. F., Stomski, P., Summers, K. R., Swain, M. R., Swanson, P., Thompson, R., Tsubota, K., Tumminello, A., Tyau, C., van Belle, G. T., Vasisht, G., Vause, J., Vescelus, F., Walker, J., Wallace, J. K., Wehmeier, U., and Wetherell, E.
Published: 2013
Full Text: View/download PDF

4. Erratum: Euclid preparation: VI. Verifying the Performance of Cosmic Shear Experiments (A&A (2020) 635 A139 DOI: 10.1051/0004-6361/201936980)

Author: Paykari P., Kitching T., Hoekstra H., Azzollini R., Cardone V. F., Cropper M., Duncan C. A. J., Kannawadi A., Miller L., Aussel H., Conti I. F., Auricchio N., Baldi M., Bardelli S., Biviano A., Bonino D., Borsato E., Bozzo E., Branchini E., Brau-Nogue S., Brescia M., Brinchmann J., Burigana C., Camera S., Capobianco V., Carbone C., Carretero J., Casas S., Castander F. J., Castellano M., Cavuoti S., Charles Y., Cledassou R., Colodro-Conde C., Congedo G., Conselice C., Conversi L., Copin Y., Coupon J., Courtois H. M., Da Silva A., Dupac X., Fabbian G., Farrens S., Ferreira P. G., Fosalba P., Fourmanoit N., Frailis M., Fumana M., Galeotta S., Garilli B., Gillard W., Gillis B. R., Giocoli C., Gracia-Carpio J., Grupp F., Hormuth F., Ilic S., Israel H., Jahnke K., Keihanen E., Kermiche S., Kilbinger M., Kirkpatrick C. C., Kubik B., Kunz M., Kurki-Suonio H., Lacasa F., Laureijs R., Le Mignant D., Ligori S., Lilje P. B., Lloro I., MacIaszek T., Maiorano E., Marggraf O., Markovic K., Martinelli M., Martinet N., Marulli F., Massey R., Mauri N., Medinaceli E., Mei S., Mellier Y., Meneghetti M., Metcalf R. B., Moresco M., Moscardini L., Munari E., Neissner C., Nichol R. C., Niemi S., Nutma T., Padilla C., Paltani S., Pasian F., Pettorino V., Pires S., Polenta G., Pourtsidou A., Raison F., Renzi A., Rhodes J., Romelli E., Roncarelli M., Rossetti E., Saglia R., Sakr Z., Sanchez A. G., Sapone D., Scaramella R., Schneider P., Schrabback T., Scottez V., Secroun A., Serrano S., Sirignano C., Sirri G., Stanco L., Starck J. -L., Sureau F., Tallada-Crespi P., Taylor A., Tenti M., Tereno I., Toledo-Moreo R., Torradeflot F., Tutusaus I., Valenziano L., Vannier M., Vassallo T., Zoubian J., Zucca E., Paykari P., Kitching T., Hoekstra H., Azzollini R., Cardone V.F., Cropper M., Duncan C.A.J., Kannawadi A., Miller L., Aussel H., Conti I.F., Auricchio N., Baldi M., Bardelli S., Biviano A., Bonino D., Borsato E., Bozzo E., Branchini E., Brau-Nogue S., Brescia M., Brinchmann J., Burigana C., Camera S., Capobianco V., Carbone C., Carretero J., Casas S., Castander F.J., Castellano M., Cavuoti S., Charles Y., Cledassou R., Colodro-Conde C., Congedo G., Conselice C., Conversi L., Copin Y., Coupon J., Courtois H.M., Da Silva A., Dupac X., Fabbian G., Farrens S., Ferreira P.G., Fosalba P., Fourmanoit N., Frailis M., Fumana M., Galeotta S., Garilli B., Gillard W., Gillis B.R., Giocoli C., Gracia-Carpio J., Grupp F., Hormuth F., Ilic S., Israel H., Jahnke K., Keihanen E., Kermiche S., Kilbinger M., Kirkpatrick C.C., Kubik B., Kunz M., Kurki-Suonio H., Lacasa F., Laureijs R., Le Mignant D., Ligori S., Lilje P.B., Lloro I., MacIaszek T., Maiorano E., Marggraf O., Markovic K., Martinelli M., Martinet N., Marulli F., Massey R., Mauri N., Medinaceli E., Mei S., Mellier Y., Meneghetti M., Metcalf R.B., Moresco M., Moscardini L., Munari E., Neissner C., Nichol R.C., Niemi S., Nutma T., Padilla C., Paltani S., Pasian F., Pettorino V., Pires S., Polenta G., Pourtsidou A., Raison F., Renzi A., Rhodes J., Romelli E., Roncarelli M., Rossetti E., Saglia R., Sakr Z., Sanchez A.G., Sapone D., Scaramella R., Schneider P., Schrabback T., Scottez V., Secroun A., Serrano S., Sirignano C., Sirri G., Stanco L., Starck J.-L., Sureau F., Tallada-Crespi P., Taylor A., Tenti M., Tereno I., Toledo-Moreo R., Torradeflot F., Tutusaus I., Valenziano L., Vannier M., Vassallo T., Zoubian J., Zucca E., Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., Cardone, V. F., Cropper, M., Duncan, C. A. J., Kannawadi, A., Miller, L., Aussel, H., Conti, I. F., Auricchio, N., Baldi, M., Bardelli, S., Biviano, A., Bonino, D., Borsato, E., Bozzo, E., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Burigana, C., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Casas, S., Castander, F. J., Castellano, M., Cavuoti, S., Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H. M., Da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P. G., Fosalba, P., Fourmanoit, N., Frailis, M., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B. R., Giocoli, C., Gracia-Carpio, J., Grupp, F., Hormuth, F., Ilic, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C. C., Kubik, B., Kunz, M., Kurki-Suonio, H., Lacasa, F., Laureijs, R., Le Mignant, D., Ligori, S., Lilje, P. B., Lloro, I., Maciaszek, T., Maiorano, E., Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Marulli, F., Massey, R., Mauri, N., Medinaceli, E., Mei, S., Mellier, Y., Meneghetti, M., Metcalf, R. B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R. C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., Pasian, F., Pettorino, V., Pires, S., Polenta, G., Pourtsidou, A., Raison, F., Renzi, A., Rhodes, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Sanchez, A. G., Sapone, D., Scaramella, R., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J. -L., Sureau, F., Tallada-Crespi, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valenziano, L., Vannier, M., Vassallo, T., Zoubian, J., and Zucca, E.
Subjects: gravitational lensing: weak, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, errata, addenda
Abstract: Aims.Our aim is to quantify the impact of systematic effects on the inference of cosmological parameters from cosmic shear.Methods.We present an ‘end-to-end’ approach that introduces sources of bias in a modelled weak lensing survey on a galaxy-by-galaxy level. Residual biases are propagated through a pipeline from galaxy properties (one end) through to cosmic shear powerspectra and cosmological parameter estimates (the other end), to quantify how imperfect knowledge of the pipeline changes themaximum likelihood values of dark energy parameters.Results.We quantify the impact of an imperfect correction for charge transfer inefficiency (CTI) and modelling uncertainties of thepoint spread function (PSF) forEuclid, and find that the biases introduced can be corrected to acceptable levels.
Published: 2020

5. Euclid near infrared spectrometer and photometer instrument flight model presentation, performance, and ground calibration results summary

Author: Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., E. Coyle, Laura, D. Perrin, Marshall, Maciaszek, T., Ealet, A., Gillard, W., Jahnke, K., Barbier, R., Prieto, E., Bon, W., Bonnefoi, A., Caillat, A., Carle, M., Costille, A., Ducret, F., Fabron, C., Foulon, B., Gimenez, J.-L., Grassi, E., Jaquet, M., Le Mignant, D., Martin, L., Pamplona, T., Sanchez, P., ClÃ©mens, J.-C., Caillat, L., Niclas, M., Secroun, A., Kubik, B., Ferriol, S., Berthe, M., BarriÃ¨re, J.-C., Fontignie, J., Valenziano, L., Auricchio, N., Battaglia, P., De Rosa, A., Farinelli, R., Franceschi, E., Medinaceli, E., Morgante, G., Sortino, F., Trifoglio, M., Corcione, L., Capobianco, V., Ligori, S., Dusini, S., Borsato, E., Dal Corso, F., Laudisio, F., Sirignano, C., Stanco, L., Ventura, S., Patrizii, L., Chiarusi, T., Fornari, F., Giacomini, F., Margiotta, A., Mauri, N., Pasqualini, L., Sirri, G., Spurio, M., Tenti, M., Travaglini, R., Bonoli, C., Bortoletto, F., Balestra, A., Dalessandro, M., Grupp, F., Penka, D., Steinwagner, J., Hormuth, F., Schirmer, M., Seidel, G., Padilla, C., Casas, R., Lloro, Y., Toledo-Moreo, R., Gomez, J., Colodro-Conde, C., LizÃ¡n, D., Diaz, J.-J., Lilje, P., Andersen, M. I., Andersen, J., SÃ¸rensen, A. N., Hornstrup, A., Jessen, N. C., Thizy, C., Holmes, W., Pniel, M., Jhabvala, M., Pravdo, S., Seiffert, M., Waczynski, A., Laureij, R. J., Racca, G., Salvignol, J.-C., Boenke, T., Strada, P., Mellier, Y., Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., E. Coyle, Laura, D. Perrin, Marshall, Maciaszek, T., Ealet, A., Gillard, W., Jahnke, K., Barbier, R., Prieto, E., Bon, W., Bonnefoi, A., Caillat, A., Carle, M., Costille, A., Ducret, F., Fabron, C., Foulon, B., Gimenez, J.-L., Grassi, E., Jaquet, M., Le Mignant, D., Martin, L., Pamplona, T., Sanchez, P., ClÃ©mens, J.-C., Caillat, L., Niclas, M., Secroun, A., Kubik, B., Ferriol, S., Berthe, M., BarriÃ¨re, J.-C., Fontignie, J., Valenziano, L., Auricchio, N., Battaglia, P., De Rosa, A., Farinelli, R., Franceschi, E., Medinaceli, E., Morgante, G., Sortino, F., Trifoglio, M., Corcione, L., Capobianco, V., Ligori, S., Dusini, S., Borsato, E., Dal Corso, F., Laudisio, F., Sirignano, C., Stanco, L., Ventura, S., Patrizii, L., Chiarusi, T., Fornari, F., Giacomini, F., Margiotta, A., Mauri, N., Pasqualini, L., Sirri, G., Spurio, M., Tenti, M., Travaglini, R., Bonoli, C., Bortoletto, F., Balestra, A., Dalessandro, M., Grupp, F., Penka, D., Steinwagner, J., Hormuth, F., Schirmer, M., Seidel, G., Padilla, C., Casas, R., Lloro, Y., Toledo-Moreo, R., Gomez, J., Colodro-Conde, C., LizÃ¡n, D., Diaz, J.-J., Lilje, P., Andersen, M. I., Andersen, J., SÃ¸rensen, A. N., Hornstrup, A., Jessen, N. C., Thizy, C., Holmes, W., Pniel, M., Jhabvala, M., Pravdo, S., Seiffert, M., Waczynski, A., Laureij, R. J., Racca, G., Salvignol, J.-C., Boenke, T., Strada, P., and Mellier, Y.
Abstract: The NISP (Near Infrared Spectrometer and Photometer) is one of the two Euclid instruments (see ref [1]). It operates in the near-IR spectral region (950-2020nm) as a photometer and spectrometer. The instrument is composed of: - a cold (135K) optomechanical subsystem consisting of a Silicon carbide structure, an optical assembly, a filter wheel mechanism, a grism wheel mechanism, a calibration unit and a thermal control system - a detection system based on a mosaic of 16 H2RG with their front-end readout electronic. - a warm electronic system (290K) composed of a data processing / detector control unit and of an instrument control unit that interfaces with the spacecraft via a 1553 bus for command and control and via Spacewire links for science data This paper presents: - the final architecture of the flight model instrument and subsystems - the performances and the ground calibration measurement done at NISP level and at Euclid Payload Module level at operational cold temperature.
Published: 2022

6. Euclid preparation

Author: Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., Cardone, V.F., Cropper, M., Duncan, C.A.J., Kannawadi Jayaraman, A., Miller, L., Aussel, H., Conti, I.F., Auricchio, N., Baldi, M., Bardelli, S., Biviano, A., Bonino, D., Borsato, E., Bozzo, E., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Burigana, C., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Casas, S., Castander, F.J., Castellano, M., Cavuoti, S., Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H.M., Da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P.G., Fosalba, P., Fourmanoit, N., Frailis, M., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B.R., Giocoli, C., Graciá-Carpio, J., Grupp, F., Hormuth, F., Ilić, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C.C., Kubik, B., Kunz, M., Kurki-Suonio, H., Lacasa, F., Laureijs, R., Le Mignant, D., Ligori, S., Lilje, P.B., Lloro, I., Maciaszek, T., Maiorano, E., Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Marulli, F., Massey, R., Mauri, N., Medinaceli, E., Mei, S., Mellier, Y., Meneghetti, M., Metcalf, R.B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R.C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., Pasian, F., Pettorino, V., Pires, S., Polenta, G., Pourtsidou, A., Raison, F., Renzi, A., Rhodes, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Sánchez, A.G., Sapone, D., Scaramella, R., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J.-L., Sureau, F., Tallada-Crespí, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valenziano, L., Vannier, M., Vassallo, T., Zoubian, J., Zucca, E., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Euclid, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astronomy Centre, University of Sussex, Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Max-Planck-Institut für Astronomie (MPIA), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Euclid Collaboration, European Project: 617656,EC:FP7:ERC,ERC-2013-CoG,THEMODS(2014), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), University of Helsinki, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), 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)-CY Cergy Paris Université (CY), 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), Astronomy, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut national de recherches archéologiques préventives (Inrap), Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-CY Cergy Paris Université (CY)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Particle Physics and Astrophysics, Department of Physics, Helsinki Institute of Physics, Science and Technology Facilities Council (UK), Royal Society (UK), Dutch Research Council, Netherlands Organization for Scientific Research, UK Space Agency, Swiss National Science Foundation, European Commission, Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., Cardone, V. F., Cropper, M., Duncan, C. A. J., Kannawadi, A., Miller, L., Aussel, H., Conti, I. F., Auricchio, N., Baldi, M., Bardelli, S., Biviano, A., Bonino, D., Borsato, E., Bozzo, E., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Burigana, C., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H. M., da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P. G., Fosalba, P., Fourmanoit, N., Frailis, M., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B. R., Giocoli, C., Gracia-Carpio, J., Grupp, F., Hormuth, F., Ilic, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C. C., Kubik, B., Kunz, M., Kurki-Suonio, H., Laureijs, R., Le Mignant, D., Ligori, S., Lilje, P. B., Lloro, I., Maciaszek, T., Maiorano, E., Marggraf, O., Markovic, K., Martinet, N., Marulli, F., Massey, R., Mauri, N., Medinaceli, E., Mei, S., Mellier, Y., Meneghetti, M., Metcalf, R. B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R. C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., Pasian, F., Pettorino, V., Pires, S., Polenta, G., Raison, F., Renzi, A., Rhodes, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Sanchez, A. G., Sapone, D., Scaramella, R., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J. -L., Sureau, F., Tallada-Crespi, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valenziano, L., Vannier, M., Vassallo, T., Zoubian, J., Zucca, E., Da Silva, A., Graciá-Carpio, J., Ilić, S., Sánchez, A. G., Starck, J.-L., and Tallada-Crespí, P.
Subjects: Point spread function, Cosmology and Nongalactic Astrophysics (astro-ph.CO), ComputerSystemsOrganization_COMPUTERSYSTEMIMPLEMENTATION, Pipeline (computing), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Residual, 7. Clean energy, 01 natural sciences, gravitational lensing: weak, 0103 physical sciences, Statistical physics, 010303 astronomy & astrophysics, Weak gravitational lensing, Physics, CALIBRATION, CHARGE-TRANSFER INEFFICIENCY, COSMIC cancer database, 010308 nuclear & particles physics, Computer Science::Information Retrieval, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, 115 Astronomy, Space science, Galaxy, Shear (sheet metal), CHALLENGE LIGHTCONE SIMULATION, BIAS, Space and Planetary Science, astro-ph.CO, Dark energy, DARK ENERGY, SENSITIVITY, weak [Gravitational lensing], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], REQUIREMENTS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aims. Our aim is to quantify the impact of systematic effects on the inference of cosmological parameters from cosmic shear. Methods. We present an "end-to-end" approach that introduces sources of bias in a modelled weak lensing survey on a galaxy-by-galaxy level. We propagated residual biases through a pipeline from galaxy properties at one end to cosmic shear power spectra and cosmological parameter estimates at the other end. We did this to quantify how imperfect knowledge of the pipeline changes the maximum likelihood values of dark energy parameters. Results. We quantify the impact of an imperfect correction for charge transfer inefficiency and modelling uncertainties of the point spread function for Euclid, and find that the biases introduced can be corrected to acceptable levels., PP is supported by an STFC consolidated grant. CW is supported by an STFC urgency grant. TDK is supported by a Royal Society University Research Fellowship. HH acknowledges support from Vici grant 639.043.512 and an NWO-G grant financed by the Netherlands Organization for Scientific Research. LM and CD are supported by UK Space Agency grant ST/N001796/1. VFC is funded by Italian Space Agency (ASI) through contract Euclid – IC (I/031/10/0) and acknowledges financial contribution from the agreement ASI/INAF/I/023/12/0. We would like to thank Jérome Amiaux, Koryo Okumura, Samuel Ronayette for running the ZEMAX simulations. AP is a UK Research and Innovation Future Leaders Fellow, grant MR/S016066/1, and also acknowledges support from the UK Science & Technology Facilities Council through grant ST/S000437/1. MK and FL acknowledge financial support from the Swiss National Science Foundation. SI acknowledges financial support from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007–2013)/ERC Grant Agreement No. 617656 “Theories and Models of the Dark Sector: Dark Matter, Dark Energy and Gravity”.
Published: 2020

7. The SPHERE infrared survey for exoplanets (SHINE)

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

8. The SPHERE infrared survey for exoplanets (SHINE)

Author: Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G.-D., Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Le Coroller, H., Maire, A.-L., Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A.-M., Langlois, M., Bonnefoy, M., Beuzit, J.-L., Boccaletti, A., D��Orazi, V., Delorme, P., Dominik, C., Henning, Th., Janson, M., Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., M��ller, A., Perrot, C., Samland, M., Schmid, H. M., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A. J., Brown Sevilla, S., Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulb��, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J. H., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., M��ller-Nilsson, O., Mouillet, D., Moulin, T., Orign��, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E. L., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J.-F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., Wildi, F., Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 530 Physics, 520 Astronomy, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 620 Engineering, Astrophysics::Galaxy Astrophysics
Abstract: International audience; The SpHere INfrared Exoplanet (SHINE) project is a 500-star survey performed with SPHERE on the Very Large Telescope for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. Here we present an initial statistical analysis for a subsample of 150 stars spanning spectral types from B to M that are representative of the full SHINE sample. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 M Jup and semimajor axes between 5 and 300 au. For this purpose, we adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Based on the results obtained for each star and on the 13 detections in the sample, we use a Markov chain Monte Carlo tool to compare our observations to two different types of models. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are 23.0 −9.7 +13.5 , 5.8 −2.8 +4.7 , and 12.6 −7.1 +12.9 % for BA, FGK, and M stars, respectively. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1–75 M Jup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using our population model and restricting our sample to FGK stars, we derive a frequency of 5.7 −2.8 +3.8 %, consistent with predictions from the parametric model. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies.
Published: 2021

9. The SPHERE infrared survey for exoplanets (SHINE)

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

10. The SPHERE Infrared Survey for Exoplanets (SHINE): II. Observations, Data Reduction and Analysis, Detection Performances, and Initial Results

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

11. The SPHERE Infrared Survey for Exoplanets (SHINE): I. Sample Definition and Target Characterization

Author: Desidera, S., Chauvin, G., Bonavita, M., Messina, S., Lecoroller, H., Schmidt, T., Gratton, R., Lazzoni, C., Meyer, M., Schlieder, J., Cheetham, A., Hagelberg, J., Bonnefoy, M., Feldt, M., Lagrange, A. -M., Langlois, M., Vigan, A., Tan, T. G., Hambsch, F. -J., Millward, M., Alcalá, J., Benatti, S., Brandner, W., Carson, J., Covino, E., Delorme, P., D'Orazi, V., Janson, M., Rigliaco, E., Beuzit, J. -L., Biller, B., Boccaletti, A., Dominik, C., Cantalloube, F., Fontanive, C., Galicher, R., Henning, T., Lagadec, E., Ligi, R., Maire, A. -L., Menard, F., Mesa, D., Müller, A., Samland, M., Schmid, H. M., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Asensio-Torres, R., Kopytova, T., Rickman, E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbé, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Desidera, S., Chauvin, G., Bonavita, M., Messina, S., Lecoroller, H., Schmidt, T., Gratton, R., Lazzoni, C., Meyer, M., Schlieder, J., Cheetham, A., Hagelberg, J., Bonnefoy, M., Feldt, M., Lagrange, A. -M., Langlois, M., Vigan, A., Tan, T. G., Hambsch, F. -J., Millward, M., Alcalá, J., Benatti, S., Brandner, W., Carson, J., Covino, E., Delorme, P., D'Orazi, V., Janson, M., Rigliaco, E., Beuzit, J. -L., Biller, B., Boccaletti, A., Dominik, C., Cantalloube, F., Fontanive, C., Galicher, R., Henning, T., Lagadec, E., Ligi, R., Maire, A. -L., Menard, F., Mesa, D., Müller, A., Samland, M., Schmid, H. M., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Asensio-Torres, R., Kopytova, T., Rickman, E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbé, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., and Wildi, F.
Abstract: Large surveys with new-generation high-contrast imaging instruments are needed to derive the frequency and properties of exoplanet populations with separations from ~5 to 300 au. A careful assessment of the stellar properties is crucial for a proper understanding of when, where, and how frequently planets form, and how they evolve. The sensitivity of detection limits to stellar age makes this a key parameter for direct imaging surveys. Aims. We describe the SpHere INfrared survey for Exoplanets (SHINE), the largest direct imaging planet-search campaign initiated at the VLT in 2015 in the context of the SPHERE Guaranteed Time Observations of the SPHERE consortium. In this first paper we present the selection and the properties of the complete sample of stars surveyed with SHINE, focusing on the targets observed during the first phase of the survey (from February 2015 to February 2017). This early sample composed of 150 stars is used to perform a preliminary statistical analysis of the SHINE data, deferred to two companion papers presenting the survey performance, main discoveries, and the preliminary statistical constraints set by SHINE. Methods. Based on a large database collecting the stellar properties of all young nearby stars in the solar vicinity (including kinematics, membership to moving groups, isochrones, lithium abundance, rotation, and activity), we selected the original sample of 800 stars that were ranked in order of priority according to their sensitivity for planet detection in direct imaging with SPHERE. The properties of the stars that are part of the early statistical sample wererevisited, including for instance measurements from the Gaia Data Release 2. Rotation periods were derived for the vast majority of the late-type objects exploiting TESS light curves and dedicated photometric observations. Results. The properties of individual targets and of the sample as a whole are presented. © ESO 2021.
Published: 2021

12. The SPHERE infrared survey for exoplanets (SHINE) : III. The demographics of young giant exoplanets below 300 au with SPHERE

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

13. Erratum. Euclid preparation. VI. Verifying the performance of cosmic shear experiments

Author: Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., Cardone, V.F., Cropper, M., Duncan, C.A.J., Kannawadi Jayaraman, A., Miller, L., Aussel, H., Conti, I.F., Auricchio, N., Baldi, M., Bardelli, S., Biviano, A., Bonino, D., Borsato, E., Bozzo, E., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Burigana, C., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Casas, S., Castander, F.J., Castellano, M., Cavuoti, S., Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H.M., Da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P.G., Fosalba, P., Fourmanoit, N., Frailis, M., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B.R., Giocoli, C., Graciá-Carpio, J., Grupp, F., Hormuth, F., Ilić, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C.C., Kubik, B., Kunz, M., Kurki-Suonio, H., Lacasa, F., Laureijs, R., Le Mignant, D., Ligori, S., Lilje, P.B., Lloro, I., Maciaszek, T., Maiorano, E., Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Marulli, F., Massey, R., Mauri, N., Medinaceli, E., Mei, S., Mellier, Y., Meneghetti, M., Metcalf, R.B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R.C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., Pasian, F., Pettorino, V., Pires, S., Polenta, G., Pourtsidou, A., Raison, F., Renzi, A., Rhodes, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Sánchez, A.G., Sapone, D., Scaramella, R., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J.-L., Sureau, F., Tallada-Crespí, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valenziano, L., Vannier, M., Vassallo, T., Zoubian, J., and Zucca, E.
Abstract: This article is an erratum for:[https://doi.org/10.1051/0004-6361/201936980]
Published: 2020

14. Euclid preparation: VI. Verifying the Performance of Cosmic Shear Experiments (Corrigendum)

Author: Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., Cardone, V. F., Cropper, M., Duncan, C. A. J., Kannawadi, A., Miller, L., Aussel, H., Conti, I. F., Auricchio, N., Baldi, M., Bardelli, S., Biviano, A., Bonino, D., Borsato, E., Bozzo, E., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Burigana, C., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Casas, S., Castander, F. J., Castellano, M., Cavuoti, S., Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H. M., da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P. G., Fosalba, P., Fourmanoit, N., Frailis, M., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B. R., Giocoli, C., Graciá-Carpio, J., Grupp, F., Hormuth, F., Ilić, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C. C., Kubik, B., Kunz, M., Kurki-Suonio, H., Lacasa, F., Laureijs, R., Le Mignant, D., Ligori, S., Lilje, P. B., Lloro, I., Maciaszek, T., Maiorano, E., Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Marulli, F., Massey, R., Mauri, N., Medinaceli, E., Mei, S., Mellier, Y., Meneghetti, M., Metcalf, R. B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R. C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., Pasian, F., Pettorino, V., Pires, S., Polenta, G., Pourtsidou, A., Raison, F., Renzi, A., Rhodes, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Sánchez, A. G., Sapone, D., Scaramella, R., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J.-L., Sureau, F., Tallada-Crespí, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valenziano, L., Vannier, M., Vassallo, T., Zoubian, J., Zucca, E., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-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), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), 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)-CY Cergy Paris Université (CY), Queen Mary University of London (QMUL), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Euclid Collaboration, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], addenda, errata
Abstract: International audience; Authors Lacasa, Martinelli, Pourtsidou, Tutusaus, were inadvertently missed from the original authorship list. This is now corrected.
Published: 2020

15. Euclid preparation: VI. Verifying the performance of cosmic shear experiments [with erratum]

Author: Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., Cardone, V. F., Cropper, M., Duncan, C. A. J., Kannawadi, A., Miller, L., Aussel, H., Conti, I. F., Auricchio, N., Baldi, M., Bardelli, S., Biviano, A., Bonino, D., Borsato, E., Bozzo, E., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Burigana, C., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Casas, S., Castander, F. J., Castellano, M., Cavuoti, S., Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H. M., Da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P. G., Fosalba, P., Fourmanoit, N., Frailis, M., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B. R., Giocoli, C., Graciá-Carpio, J., Grupp, F., Hormuth, F., Ilić, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C. C., Kubik, B., Kunz, M., Kurki-Suonio, H., Lacasa, F., Laureijs, R., Le Mignant, D., Ligori, S., Lilje, P. B., Lloro, I., Maciaszek, T., Maiorano, E., Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Marulli, F., Massey, R., Mauri, N., Medinaceli, E., Mei, S., Mellier, Y., Meneghetti, M., Metcalf, R. B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R. C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., Pasian, F., Pettorino, V., Pires, S., Polenta, G., Pourtsidou, A., Raison, F., Renzi, A., Rhodes, J., Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Sánchez, A. G., Sapone, D., Scaramella, R., Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Starck, J.-L., Sureau, F., Tallada-Crespí, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valenziano, L., Vannier, M., Vassallo, T., Zoubian, J., and Zucca, E.
Subjects: Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: Aims. Our aim is to quantify the impact of systematic effects on the inference of cosmological parameters from cosmic shear. Methods. We present an “end-to-end” approach that introduces sources of bias in a modelled weak lensing survey on a galaxy-by-galaxy level. We propagated residual biases through a pipeline from galaxy properties at one end to cosmic shear power spectra and cosmological parameter estimates at the other end. We did this to quantify how imperfect knowledge of the pipeline changes the maximum likelihood values of dark energy parameters. Results. We quantify the impact of an imperfect correction for charge transfer inefficiency and modelling uncertainties of the point spread function for Euclid, and find that the biases introduced can be corrected to acceptable levels.
Published: 2020

16. Euclid preparation

Author: Euclid Collaboration, Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., CARDONE, Vincenzo Fabrizio, Cropper, M., Duncan, C. A. J., Kannawadi, A., Miller, L., Aussel, H., Polenta, G., Pourtsidou, A., Raison, F., Renzi, A., Rhodes, J., Romelli, Erik, Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Conti, I. F., Sánchez, A. G., Sapone, D., SCARAMELLA, Roberto, Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., AURICCHIO, NATALIA, Stanco, L., Starck, J. -L., Sureau, F., Tallada-Crespí, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Baldi, M., VALENZIANO, LUCA, Vannier, M., Vassallo, T., Zoubian, J., ZUCCA, Elena, BARDELLI, Sandro, Biviano, A., BONINO, Donata, Borsato, E., Bozzo, E., Branchini, Enzo Franco, Brau-Nogue, S., BRESCIA, Massimo, Brinchmann, J., BURIGANA, CARLO, Camera, S., Capobianco, Vito, CARBONE, Carmelita, Carretero, J., Casas, S., Castander, F. J., CASTELLANO, MARCO, CAVUOTI, STEFANO, Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H. M., Da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P. G., Fosalba, P., Fourmanoit, N., FRAILIS, Marco, Fumana, M., GALEOTTA, Samuele, GARILLI, BIANCA MARIA ROSA, Gillard, W., Gillis, B. R., Giocoli, C., Graciá-Carpio, J., Grupp, F., Hormuth, F., Ilić, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C. C., Kubik, B., Kunz, M., Kurki-Suonio, H., Lacasa, F., Laureijs, R., Le Mignant, D., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., Maciaszek, T., MAIORANO, Elisabetta, Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Marulli, F., Massey, R., Mauri, N., MEDINACELI VILLEGAS, EDUARDO, Mei, S., Mellier, Y., MENEGHETTI, MASSIMO, Metcalf, R. B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R. C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., PASIAN, Fabio, Pettorino, V., Pires, S., Astronomy, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-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), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), 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)-CY Cergy Paris Université (CY), Queen Mary University of London (QMUL), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), and Euclid Collaboration
Subjects: Physics, COSMIC cancer database, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, gravitational lensing: weak, Shear (geology), Space and Planetary Science, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, addenda, errata
Abstract: International audience; Authors Lacasa, Martinelli, Pourtsidou, Tutusaus, were inadvertently missed from the original authorship list. This is now corrected.
Published: 2020

17. K-Stacker : an algorithm to hack the orbital parameters of planets hidden in high-contrast imaging

Author: Le Coroller, H., Nowak, M., Delorme, P., Chauvin, G., Gratton, R., Devinat, M., Bec-Canet, J., Schneeberger, A., Estevez, D., Arnold, L., Beust, H., Bonnefoy, M., Boccaletti, A., Desgrange, C., Desidera, S., Galicher, R., Lagrange, A. M., Langlois, M., Maire, A. L., Menard, F., Vernazza, P., Vigan, A., Zurlo, A., Fenouillet, T., Lambert, J. C., Bonavita, M., Cheetham, A., D'orazi, V., Feldt, Markus, Janson, M., Ligi, R., Mesa, D., Meyer, M., Samland, Matthias, Sissa, E., Beuzit, J.-L., Dohlen, K., Fusco, T., Le Mignant, D., Mouillet, D., Ramos, J., Rochat, S., Sauvage, J. F., Le Coroller, H., Nowak, M., Delorme, P., Chauvin, G., Gratton, R., Devinat, M., Bec-Canet, J., Schneeberger, A., Estevez, D., Arnold, L., Beust, H., Bonnefoy, M., Boccaletti, A., Desgrange, C., Desidera, S., Galicher, R., Lagrange, A. M., Langlois, M., Maire, A. L., Menard, F., Vernazza, P., Vigan, A., Zurlo, A., Fenouillet, T., Lambert, J. C., Bonavita, M., Cheetham, A., D'orazi, V., Feldt, Markus, Janson, M., Ligi, R., Mesa, D., Meyer, M., Samland, Matthias, Sissa, E., Beuzit, J.-L., Dohlen, K., Fusco, T., Le Mignant, D., Mouillet, D., Ramos, J., Rochat, S., and Sauvage, J. F.
Abstract: Context. Recent high-contrast imaging surveys, using the Spectro-Polarimetic High contrast imager for Exoplanets REsearch (SPHERE) or the Gemini Planet Imager in search of planets in young, nearby systems, have shown evidence of a small number ofgiant planets at relatively large separation beyond 10–30 au, where those surveys are the most sensitive. Access to smaller physical separations between 5 and 30 au is the next step for future planet imagers on 10 m telescopes and the next generation of extremely large telescopes in order to bridge the gap with indirect techniques such as radial velocity, transit, and soon astrometry with Gaia. In addition to new technologies and instruments, the development of innovative observing strategies combined with optimized data processing tools is participating in the improvement of detection capabilities at very close angular separation. In that context, we recently proposed a new algorithm, Keplerian-Stacker, which combines multiple observations acquired at different epochs and takes into account the orbital motion of a potential planet present in the images to boost the ultimate detection limit. We showed that this algorithm is able to find planets in time series of simulated images of the SPHERE InfraRed Dual-band Imager and Spectrograph (IRDIS) even when a planet remains undetected at one epoch. Aims. Our goal is to test and validate the K-Stacker algorithm performances on real SPHERE datasets to demonstrate the resilience of this algorithm to instrumental speckles and the gain offered in terms of true detection. This will motivate future dedicated multi-epoch observation campaigns of well-chosen, young, nearby systems and very nearby stars carefully selected to search for planets in emitted and reflected light, respectively, to open a new path concerning the observing strategy used with current and future planet imagers. Methods. To test K-Stacker, we injected fake planets and scanned the low signal-to-noise ratio (S/N) regim
Published: 2020
Full Text: View/download PDF

18. K-Stacker: an algorithm to hack the orbital parameters of planets hidden in high-contrast imaging

Author: Le Coroller, H., primary, Nowak, M., additional, Delorme, P., additional, Chauvin, G., additional, Gratton, R., additional, Devinat, M., additional, Bec-Canet, J., additional, Schneeberger, A., additional, Estevez, D., additional, Arnold, L., additional, Beust, H., additional, Bonnefoy, M., additional, Boccaletti, A., additional, Desgrange, C., additional, Desidera, S., additional, Galicher, R., additional, Lagrange, A. M., additional, Langlois, M., additional, Maire, A. L., additional, Menard, F., additional, Vernazza, P., additional, Vigan, A., additional, Zurlo, A., additional, Fenouillet, T., additional, Lambert, J. C., additional, Bonavita, M., additional, Cheetham, A., additional, D’orazi, V., additional, Feldt, M., additional, Janson, M., additional, Ligi, R., additional, Mesa, D., additional, Meyer, M., additional, Samland, M., additional, Sissa, E., additional, Beuzit, J.-L., additional, Dohlen, K., additional, Fusco, T., additional, Le Mignant, D., additional, Mouillet, D., additional, Ramos, J., additional, Rochat, S., additional, and Sauvage, J. F., additional
Published: 2020
Full Text: View/download PDF

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

Author: Carbillet, M., Maurel, D., Origné, A., Rigal, F., Sevin, A., De Boer, J., van Holstein, R. G., Dohlen, K., Snik, F., Keller, C. U., Ginski, C., Stam, D. M., Wahhaj, Z., Kasper, M., Rabou, P., Hugot, E., Perret, D., Martinez, P., Pragt, J., Coroller, H. Le, Dominik, C., Turatto, M., Udry, S., Beuzit, J. -L., Le Coroller, H., Mennesson, B., Bailey, V., Kasdin, J., Trauger, J., Absil, O., Akeson, R., Armus, L., Baudoz, P., Bellini, A., Bennett, D., Berriman, B., Calchi-Novati, S., Carpenter, K., Chen, C., Danchi, W., Debes, J., Defrere, D., Ertel, S., Frerking, M., Gelino, C., Girard, J. H., Groff, T., Kane, S., Helou, G., Kalirai, J., Krist, J., Kruk, J., Hasegawa, Y., Laine, S., Lowrance, P., Malhotra, S., Mandell, A., Marshall, P., McElwain, M., Meshkat, T., Millan-Gabet, R., Moustakas, L., Nemati, B., Paladini, R., Postman, M., Pueyo, L., Quintana, E., Ramirez, S., Rhodes, J., Riggs, A. J. E., Rizzo, M., Soummer, R., Stapelfeldt, K., Stark, C., Turnbull, M., van der Marel, R., Ygouf, M., Wyatt, M., Zhao, F., Zimmerman, N., Loh, Alan, Messina, Sergio, Brandner, Wolfgang, Buenzli, Esther, Daemgen, Sebastien, Lagadec, Eric, Mouillet, David, Peretti, Sébastien, Janin-Potiron, Pierre, Salter, Graeme, Roux, Alain, Llored, Marc, Buey, Jean-Tristan, Pavlov, Alexei, Petit, C., Pawellek, Nicole, Moór, Attila, Milli, Julien, Kóspál, Ágnes, Olofsson, Johan, Ábrahám, Péter, Keppler, Miriam, Kral, Quentin, Pohl, Adriana, Augereau, Jean-Charles, Choquet, Elodie, Engler, Natalia, Lee, Eve J., Thebault, Philippe, Lee, Eve, Podio, L., Bacciotti, F., Antoniucci, S., Codella, C., Dougados, C., Nisini, B., Schmid, H. M., Stolker, T., Baudino, J. L., Biller, Beth, Bonavita, M., Galicher, R., Grandjean, A., Lagrange, Anne-Marie, Lannier, Justine, Maire, Anne-Lise, Perrot, Clément, Delboulbé, A., Mignant, D. Le, Fantinel, D., Moeller-Nilsson, O., Weber, Luc, Sauvage, J. -F., Le Mignant, D., Möller-Nilsson, O., Mesa, Dino, Garufi, A., D'Orazi, V., Flasseur, O., Barbieri, M., Benisty, M., Henning, Thomas, Ligi, R., Sissa, Elena, Zurlo, Alice, Boccaletti, Anthony, Cantalloube, F., Cheetham, Anthony, De Caprio, V., Feldt, Markus, Fusco, T., Gluck, L., Hagelberg, J., Lagrange, A. -M., Lazzoni, C., Madec, F., Maire, A. -L., Ménard, F., Meyer, M., Ramos, J., Rickman, E. L., Rouan, D., Schmidt, T., van der Plas, G., D’Orazi, V., De Caprio, V, Lagrange, A-M, Maire, A-L, Van der Plas, G, Janson, Markus, Asensio-Torres, Ruben, André, Damien, Bonnefoy, Mickaël, Delorme, Philippe, Reffert, Sabine, Desidera, Silvano, Langlois, M, Chauvin, G., Gratton, Raffaele, Bohn, Alexander J., Eriksson, Simon C., Marleau, Gabriel-Dominique, Mamajek, Eric E., Vigan, Arthur, Carson, Joseph C., Bohn, Alexander, Eriksson, Simon, Mamajek, Eric, Carson, Joseph, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Faculty of Aerospace Engineering [Delft], Delft University of Technology (TU Delft), Department of International Development, University of Oxford [Oxford], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), JET PROPULSION LABORATORY CALIFORNIA INSTITUTE OF TECHNOLOGY PASADENA USA, Partenaires IRSTEA, Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), European Southern Observatory (ESO), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Roma (OAR), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Biochemistry and Molecular Biology, Mayo Clinic, INAF - Osservatorio Astronomico di Padova (OAPD), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Collège de France (CdF (institution)), Département de Physique Nucléaire (ex SPhN) (DPHN), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Axe 4 : céramiques sous contraintes environnementales (SPCTS-AXE4), Science des Procédés Céramiques et de Traitements de Surface (SPCTS), Université de Limoges (UNILIM)-Ecole Nationale Supérieure de Céramique Industrielle (ENSCI)-Institut des Procédés Appliqués aux Matériaux (IPAM), Université de Limoges (UNILIM)-Université de Limoges (UNILIM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Limoges (UNILIM)-Ecole Nationale Supérieure de Céramique Industrielle (ENSCI)-Institut des Procédés Appliqués aux Matériaux (IPAM), Université de Limoges (UNILIM)-Université de Limoges (UNILIM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Landessternwarte Königstuhl [ZAH] (LSW), Universität Heidelberg [Heidelberg], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Stockholm University, Universität Heidelberg [Heidelberg] = Heidelberg University, École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de Ingeniería Matemática [Santiago] (DIM), Universidad de Chile = University of Chile [Santiago] (UCHILE)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden, Institut für Astronomie und Astrophysik [Tübingen] (IAAT), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Department of Physics and Astronomy [Rochester], University of Rochester [USA], College of Charleston, ANR-10-LABX-0056,OSUG@2020,Innovative strategies for observing and modelling natural systems(2010), and European Project: 678194,H2020,ERC-2015-STG,FALCONER(2016)
Subjects: planets and satellites: detection, Proper motion, 010504 meteorology & atmospheric sciences, Stellar mass, Brown dwarf, FOS: Physical sciences, Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Mass ratio, stars: early-type, Exoplanet, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Circumbinary planet, Astrophysics - Earth and Planetary Astrophysics, brown dwarfs
Abstract: Wide low-mass substellar companions are known to be very rare among low-mass stars, but appear to become increasingly common with increasing stellar mass. However, B-type stars, which are the most massive stars within ~150 pc of the Sun, have not yet been examined to the same extent as AFGKM-type stars in that regard. In order to address this issue, we launched the ongoing B-star Exoplanet Abundance Study (BEAST) to examine the frequency and properties of planets, brown dwarfs, and disks around B-type stars in the Scorpius-Centaurus (Sco-Cen) association; we also analyzed archival data of B-type stars in Sco-Cen. During this process, we identified a candidate substellar companion to the B9-type spectroscopic binary HIP 79098 AB, which we refer to as HIP 79098 (AB)b. The candidate had been previously reported in the literature, but was classified as a background contaminant on the basis of its peculiar colors. Here we demonstrate that the colors of HIP 79098 (AB)b are consistent with several recently discovered young and low-mass brown dwarfs, including other companions to stars in Sco-Cen. Furthermore, we show unambiguous common proper motion over a 15-year baseline, robustly identifying HIP 79098 (AB)b as a bona fide substellar circumbinary companion at a 345+/-6 AU projected separation to the B9-type stellar pair. With a model-dependent mass of 16-25 Mjup yielding a mass ratio of, 9 pages, 6 figures, accepted for publication in A&A
Published: 2019

20. Post-conjunction detection of β 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., Le Coroller, H., Ligi, R., Maire, A.-L., Mesa, D., Messina, S., Mueeller, 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., Plas, G. van der, Schlieder, J.E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Moeller-Nilsson, O., Llored, M., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., Wildi, F., Low Energy Astrophysics (API, FNWI), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (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), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, University of Michigan [Ann Arbor], University of Michigan System, Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, University of Oxford [Oxford], 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), 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), 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), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Universidad de Chile, European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Université de Genève (UNIGE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), SUPA School of Physics and Astronomy [Edinburgh], Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford [Oxford]-University of Oxford [Oxford], Stockholm University, INAF - Osservatorio Astronomico di Brera (OAB), INAF - Osservatorio Astrofisico di Catania (OACT), Universidad Diego Portales [Santiago] (UDP), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Physikalisches Institut [Bern], Universität Bern [Bern], NASA Goddard Space Flight Center (GSFC), INAF - Osservatorio Astrofisico di Arcetri (OAA), INAF - Osservatorio Astronomico di Capodimonte (OAC), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), NOVA Optical Infrared Instrumentation Group, 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), Universidad de Chile = University of Chile [Santiago] (UCHILE), University of Oxford-University of Oxford, Universiteit Leiden, Universität Bern [Bern] (UNIBE), 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, 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), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010504 meteorology & atmospheric sciences, 530 Physics, Astrophysics, 01 natural sciences, Planet, instrumentation: high angular resolution, 0103 physical sciences, Beta Pictoris, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, planetary systems, individual: HR 2020, instrumentation: high angular resolution [planetary systems, stars], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Orbital elements, stars: individual: HR 2020, Very Large Telescope, Angular distance, 520 Astronomy, Astronomy and Astrophysics, 500 Science, 620 Engineering, Exoplanet, Orbit, Space and Planetary Science, Orbital motion, stars: individual: HR2020, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. With an orbital distance comparable to that of Saturn in the solar system, β Pictoris b is the closest (semi-major axis ≃9 au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to β Pictoris have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet’s orbital parameters. Aims. We aimed at further constraining β Pictoris b orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. Methods. We used SPHERE at the VLT to precisely monitor the orbital motion of beta β Pictoris b since first light of the instrument in 2014. Results. We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6 au) and prevented further detection. We redetected β Pictoris b on the northeast side of the disk at a separation of 139 mas and a PA of 30° in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of a = 9.0 ± 0.5 au (1σ), it definitely excludes previously reported possible long orbital periods, and excludes β Pictoris b as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away., Astronomy & Astrophysics, 621, ISSN:0004-6361, ISSN:1432-0746
Published: 2019

21. 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

22. Interferometric Coupling of the Keck Telescopes with Single-Mode Fibers

Author: Perrin, G., Woillez, J., Lai, O., Guérin, J., Kotani, T., Wizinowich, P. L., Le Mignant, D., Hrynevych, M., Gathright, J., Léna, P., Chaffee, F., Vergnole, S., Delage, L., Reynaud, F., Adamson, A. J., Berthod, C., Brient, B., Collin, C., Crétenet, J., Dauny, F., Deléglise, C., Fédou, P., Goeltzenlichter, T., Guyon, O., Hulin, R., Marlot, C., Marteaud, M., Melse, B.-T., Nishikawa, J., Reess, J.-M., Ridgway, S. T., Rigaut, F., Roth, K., Tokunaga, A. T., and Ziegler, D.
Published: 2006

23. Post-conjunction detection of beta Pictoris b with VLT/SPHERE

Author: Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, Markus, Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Le Coroller, H., Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Müeller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Ménard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., Wildi, F., Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, Markus, Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Le Coroller, H., Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Müeller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Ménard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., and Wildi, F.
Abstract: Context. With an orbital distance comparable to that of Saturn in the solar system, beta Pictoris b is the closest (semi-major axis similar or equal to 9 au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to beta Pictoris have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet's orbital parameters. Aims. We aimed at further constraining beta Pictoris b orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. Methods. We used SPHERE at the VLT to precisely monitor the orbital motion of beta beta Pictoris b since first light of the instrument in 2014. Results. We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6 au) and prevented further detection. We redetected beta Pictoris b on the northeast side of the disk at a separation of 139 mas and a PA of 30 degrees in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of a = 9.0 +/- 0.5 au (1 sigma), it definitely excludes previously reported possible long orbital periods, and excludes beta Pictoris b as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away.
Published: 2019
Full Text: View/download PDF

24. Resolving faint structures in the debris disk around TWA 7

Author: Olofsson, J., van Holstein, R. G., Boccaletti, A., Janson, M., Thebault, P., Gratton, R., Lazzoni, C., Kral, Q., Bayo, A., Canovas, H., Caceres, C., Ginski, C., Pinte, C., Asensio-Torres, R., Chauvin, G., Desidera, S., Henning, Th., Langlois, M., Milli, J., Schlieder, J. E., Schreiber, M. R., Augereau, J.-C., Bonnefoy, M., Buenzli, E., Brandner, W., Durkan, S., Engler, N., Feldt, M., Godoy, N., Grady, C., Hagelberg, J., Lagrange, A.-M., Lannier, J., Ligi, R., Maire, A.-L., Mawet, D., Ménard, F., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Schmidt, T., Sissa, E., Thalmann, C., Vigan, Arthur, Abe, L., Feautrier, P., Le Mignant, D., Moulin, T., PAVLOV, A., Rabou, P., Rousset, G., Roux, A., Schreiber, R., 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), Stockholm University, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Geneva Observatory, University of Geneva [Switzerland], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), 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), Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), 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, 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), 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), ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and 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)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], instrumentation: high angular resolution, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, instrumentation: polarimeters, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, circumstellar matter, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Debris disks are the intrinsic by-products of the star and planet formation processes. Most likely due to instrumental limitations and their natural faintness, little is known about debris disks around low-mass stars, especially when it comes to spatially resolved observations. We present new VLT/SPHERE IRDIS Dual-Polarization Imaging (DPI) observations in which we detect the dust ring around the M2 spectral type star TWA\,7. Combined with additional Angular Differential Imaging observations we aim at a fine characterization of the debris disk and setting constraints on the presence of low-mass planets. We model the SPHERE DPI observations and constrain the location of the small dust grains, as well as the spectral energy distribution of the debris disk, using the results inferred from the observations, and perform simple N-body simulations. We find that the dust density distribution peaks at 25 au, with a very shallow outer power-law slope, and that the disk has an inclination of 13 degrees with a position angle of 90 degrees East of North. We also report low signal-to-noise detections of an outer belt at a distance of ~52 au from the star, of a spiral arm in the Southern side of the star, and of a possible dusty clump at 3.9 au. These findings seem to persist over timescales of at least a year. Using the intensity images, we do not detect any planets in the close vicinity of the star, but the sensitivity reaches Jovian planet mass upper limits. We find that the SED is best reproduced with an inner disk at 7 au and another belt at 25 au. We report the detections of several unexpected features in the disk around TWA\,7. A yet undetected 100 M$_\oplus$ planet with a semi-major axis at 20-30 au could possibly explain the outer belt as well as the spiral arm. We conclude that stellar winds are unlikely to be responsible for the spiral arm., Comment: Accepted by A&A, 17 pages
Published: 2018

25. Investigating the young solar system analog HD 95086

Author: Chauvin, G., Gratton, R., Bonnefoy, M., Lagrange, A. -M, Boer, J., Arthur Vigan, Beust, H., Lazzoni, C., Boccaletti, A., Galicher, R., Desidera, S., Delorme, P., Keppler, M., Lannier, J., Maire, A. -L, Mesa, D., Meunier, N., Kral, Q., Henning, T., Menard, F., Moor, A., Avenhaus, H., Bazzon, A., Janson, M., Beuzit, J. -L, Bhowmik, T., Bonavita, M., Borgniet, S., Brandner, W., Cheetham, A., Cudel, M., Feldt, M., Fontanive, C., Ginski, C., Hagelberg, J., Janin-Potiron, P., Lagadec, E., Langlois, M., Le Coroller, H., Messina, S., Meyer, M., Mouillet, D., Peretti, S., Perrot, C., Rodet, L., Samland, M., Sissa, E., Olofsson, J., Salter, G., Schmidt, T., Zurlo, A., Milli, J., Boekel, R., Quanz, S., Wilson, P. A., Feautrier, P., Le Mignant, D., Perret, D., Ramos, J., Rochat, S., Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Universidad de Chile (UCHILE), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Department of Astronomy, Stockholm University, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), INAF - Osservatorio Astrofisico di Catania (OACT), Laboratoire d'interaction du rayonnement X avec la matière (LIXAM), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Universidad de Chile = University of Chile [Santiago] (UCHILE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden, Université de Genève = University of Geneva (UNIGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and We acknowledge financial support from the Programme National de Planétologie (PNP) and the Programme National de Physique Stellaire (PNPS) of CNRS-INSU. This work has also been supported by a grant from the French Labex OSUG@2020 (Investissements d’avenir – ANR10 LABX56). The project is supported by CNRS, by the Agence Nationale de la Recherche (ANR-14-CE33-0018).A (Germany), INAF (Italy), FINES (Switzerland) and NOVA (Netherlands). SPHERE also received funding from the European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004–2008), grant number 226604 for FP7 (2009–2012) and grant number 312430 for FP7 (2013–2016).
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Earth and Planetary Astrophysics
Abstract: HD95086 (A8V, 17Myr) hosts a rare planetary system for which a multi-belt debris disk and a giant planet of 4-5MJup have been directly imaged. Our study aims to characterize the physical and orbital properties of HD95086b, search for additional planets at short and wide orbits and image the cold outer debris belt in scattered light. We used HARPS at the ESO 3.6m telescope to monitor the radial velocity of HD95086 over 2 years and investigate the existence of giant planets at less than 3au orbital distance. With the IRDIS dual-band imager and the IFS integral field spectrograph of SPHERE at VLT, we imaged the faint circumstellar environment beyond 10au at six epochs between 2015 and 2017. We do not detect additional giant planets around HD95086. We identified the nature (bound companion or background contaminant) of all point-like sources detected in the IRDIS field of view. None of them correspond to the ones recently discovered near the edge of the cold outer belt by ALMA. HD95086b is resolved for the first time in J-band with IFS. Its near-infrared spectral energy distribution is well fitted by a few dusty and/or young L7-L9 dwarf spectral templates. The extremely red 1-4um spectral distribution is typical of low-gravity objects at the L/T spectral type transition. The planet's orbital motion is resolved between January 2015 and May 2017. Together with past NaCo measurements properly re-calibrated, our orbital fitting solutions favor a retrograde low to moderate-eccentricity orbit e=0.2 (0.0 to 0.5), with a semi-major axis 52au corresponding to orbital periods of 288$ yrs and an inclination that peaks at i = 141deg, which is compatible with a planet-disk coplanar configuration. Finally, we report the detection in polarimetric differential imaging of the cold outer debris belt between 100 and 300au, consistent in radial extent with recent ALMA 1.3mm resolved observations., Comment: 23 pages, 19 figures, accepted in A&A (Dec 28th, 2017)
Published: 2018

26. SPHERE: the exoplanet imager for the Very Large Telescope

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

27. SPHERE view of the jet and the envelope of RY Tauri

Author: Garufi, A., primary, Podio, L., additional, Bacciotti, F., additional, Antoniucci, S., additional, Boccaletti, A., additional, Codella, C., additional, Dougados, C., additional, Ménard, F., additional, Mesa, D., additional, Meyer, M., additional, Nisini, B., additional, Schmid, H. M., additional, Stolker, T., additional, Baudino, J. L., additional, Biller, B., additional, Bonavita, M., additional, Bonnefoy, M., additional, Cantalloube, F., additional, Chauvin, G., additional, Cheetham, A., additional, Desidera, S., additional, D’Orazi, V., additional, Feldt, M., additional, Galicher, R., additional, Grandjean, A., additional, Gratton, R., additional, Hagelberg, J., additional, Lagrange, A. M., additional, Langlois, M., additional, Lannier, J., additional, Lazzoni, C., additional, Maire, A. L., additional, Perrot, C., additional, Rickman, E., additional, Schmidt, T., additional, Vigan, A., additional, Zurlo, A., additional, Delboulbé, A., additional, Le Mignant, D., additional, Fantinel, D., additional, Möller-Nilsson, O., additional, Weber, L., additional, and Sauvage, J.-F., additional
Published: 2019
Full Text: View/download PDF

28. Discovery of a brown dwarf companion to the star HIP 64892

Author: Cheetham, A., Bonnefoy, M., Desidera, S., Langlois, M., Vigan, A., Schmidt, T., Olofsson, J., Chauvin, G., Klahr, H., Gratton, R., D'Orazi, V., Henning, T., Janson, M., Biller, B., Peretti, S., Hagelberg, J., Ségransan, D., Udry, S., Mesa, D., Sissa, E., Kral, Q., Schlieder, J., Maire, A. -L., Mordasini, C., Menard, F., Zurlo, A., Beuzit, J. -L., Feldt, M., Mouillet, D., Meyer, M., Lagrange, A. -M., Boccaletti, A., Keppler, M., Kopytova, T., Ligi, R., Rouan, D., Le, Coroller, H., Dominik, C., Lagadec, E., Turatto, M., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Claudi, R., Costille, A., Delboulbé, A., De, Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le, Mignant, D., Möller-Nilsson, O., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Cheetham, A., Bonnefoy, M., Desidera, S., Langlois, M., Vigan, A., Schmidt, T., Olofsson, J., Chauvin, G., Klahr, H., Gratton, R., D'Orazi, V., Henning, T., Janson, M., Biller, B., Peretti, S., Hagelberg, J., Ségransan, D., Udry, S., Mesa, D., Sissa, E., Kral, Q., Schlieder, J., Maire, A. -L., Mordasini, C., Menard, F., Zurlo, A., Beuzit, J. -L., Feldt, M., Mouillet, D., Meyer, M., Lagrange, A. -M., Boccaletti, A., Keppler, M., Kopytova, T., Ligi, R., Rouan, D., Le, Coroller, H., Dominik, C., Lagadec, E., Turatto, M., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Claudi, R., Costille, A., Delboulbé, A., De, Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le, Mignant, D., Möller-Nilsson, O., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., and Wildi, F.
Abstract: We report the discovery of a bright, brown dwarf companion to the star HIP 64892, imaged with VLT/SPHERE during the SHINE exoplanet survey. The host is a B9.5V member of the Lower-Centaurus-Crux subgroup of the Scorpius Centaurus OB association. The measured angular separation of the companion (1.2705 ± 0.0023”) corresponds to a projected distance of 159 ± 12 AU. We observed the target with the dual-band imaging and long-slit spectroscopy modes of the IRDIS imager to obtain its spectral energy distribution (SED) and astrometry. In addition, we reprocessed archival NACO L-band data, from which we also recover the companion. Its SED is consistent with a young (<30 Myr), low surface gravity object with a spectral type of M9γ ± 1. From comparison with the BT-Settl atmospheric models we estimate an effective temperature of Teff = 2600 ± 100 K, and comparison of the companion photometry to the COND evolutionary models yields a mass of ∼29−37 MJ at the estimated age of 16+−157 Myr for the system. The star HIP 64892 is a rare example of an extreme-mass ratio system (q ∼ 0.01) and will be useful for testing models relating to the formation and evolution of such low-mass objects. © ESO 2018
Published: 2018

29. Investigating the young solar system analog HD 95086 A combined HARPS and SPHERE exploration

Author: Chauvin, G., Gratton, R., Bonnefoy, M., Lagrange, A. -M., de Boer, J., Vigan, A., Beust, H., Lazzoni, C., Boccaletti, A., Galicher, R., Desidera, S., Delorme, P., Keppler, M., Lannier, J., Maire, A. -L., Mesa, D., Meunier, N., Kral, Q., Henning, T., Menard, F., Moor, A., Avenhaus, H., Bazzon, A., Janson, Markus, Beuzit, J. -L., Bhowmik, T., Bonavita, M., Borgniet, S., Brandner, W., Cheetham, A., Cudel, M., Feldt, M., Fontanive, C., Ginski, C., Hagelberg, J., Janin-Potiron, P., Lagadec, E., Langlois, M., Le Coroller, H., Messina, S., Meyer, M., Mouillet, D., Peretti, S., Perrot, C., Rodet, L., Samland, M., Sissa, E., Olofsson, J., Salter, G., Schmidt, T., Zurlo, A., Milli, J., van Boekel, R., Quanz, S., Feautrier, P., Le Mignant, D., Perret, D., Ramos, J., Rochat, S., Chauvin, G., Gratton, R., Bonnefoy, M., Lagrange, A. -M., de Boer, J., Vigan, A., Beust, H., Lazzoni, C., Boccaletti, A., Galicher, R., Desidera, S., Delorme, P., Keppler, M., Lannier, J., Maire, A. -L., Mesa, D., Meunier, N., Kral, Q., Henning, T., Menard, F., Moor, A., Avenhaus, H., Bazzon, A., Janson, Markus, Beuzit, J. -L., Bhowmik, T., Bonavita, M., Borgniet, S., Brandner, W., Cheetham, A., Cudel, M., Feldt, M., Fontanive, C., Ginski, C., Hagelberg, J., Janin-Potiron, P., Lagadec, E., Langlois, M., Le Coroller, H., Messina, S., Meyer, M., Mouillet, D., Peretti, S., Perrot, C., Rodet, L., Samland, M., Sissa, E., Olofsson, J., Salter, G., Schmidt, T., Zurlo, A., Milli, J., van Boekel, R., Quanz, S., Feautrier, P., Le Mignant, D., Perret, D., Ramos, J., and Rochat, S.
Abstract: Context. HD 95086 (A8V, 17 Myr) hosts a rare planetary system for which a multi-belt debris disk and a giant planet of 4-5 Mjup have been directly imaged. Aims. Our study aims to characterize the global architecture of this young system using the combination of radial velocity and direct imaging observations. We want to characterize the physical and orbital properties of HD 95086 b, search for additional planets at short and wide orbits and image the cold outer debris belt in scattered light. Methods. We used HARPS at the ESO 3.6 m telescope to monitor the radial velocity of HD 95086 over two years and investigate the existence of giant planets at less than 3 au orbital distance. With the IRDIS dual-band imager and the IFS integral field spectrograph of SPHERE at VLT, we imaged the faint circumstellar environment beyond 10 au at six epochs between 2015 and 2017. Results. We do not detect additional giant planets around HD 95086. We identify the nature (bound companion or background contaminant) of all point-like sources detected in the IRDIS field of view. None of them correspond to the ones recently discovered near the edge of the cold outer belt by ALMA. HD 95086 b is resolved for the first time in J-band with IFS. Its near-infrared spectral energy distribution is well fitted by a few dusty and/or young L7-L9 dwarf spectral templates. The extremely red 1-4 mu m spectral distribution is typical of low-gravity objects at the L/T spectral type transition. The planet's orbital motion is resolved between January 2015 and May 2017. Together with past NaCo measurements properly re-calibrated, our orbital fitting solutions favor a retrograde low to moderate-eccentricity orbit e = 0.2(-0.2)(+0.3), with a semi-major axis similar to 52 au corresponding to orbital periods of similar to 288 yr and an inclination that peaks at i = 141 degrees, which is compatible with a planet-disk coplanar configuration. Finally, we report the detection in polarimetric differential imaging of
Published: 2018
Full Text: View/download PDF

30. Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70

Author: Keppler, M., Benisty, M., Mueller, A., Henning, Th., van Boekel, R., Cantalloube, F., Ginski, C., van Holstein, R. G., Maire, A. -L., Pohl, A., Samland, M., Avenhaus, H., Baudino, J. -L., Boccaletti, A., de Boer, J., Bonnefoy, M., Chauvin, G., Desidera, S., Langlois, M., Lazzoni, C., Marleau, G. -D., 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, Markus, Juhasz, A., Kemmer, J., Kral, Q., Lagrange, A. -M., Launhardt, R., Matter, A., Menard, F., Milli, J., Molliere, P., Olofsson, J., Perez, L., Pinilla, P., Pinte, C., Quanz, S. P., Schmidt, T., Udry, S., Wahhaj, Z., Williams, J. P., 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, J. -C., Baruffolo, A., Baudoz, P., Bazzon, A., Beuzit, J. -L., Blanchard, P., Brems, S. S., Buey, T., De Caprio, V., Carbillet, M., Carle, M., Cascone, E., Cheetham, A., Claudi, R., Costille, A., Delboulbe, 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., Meyer, M., Moeller-Nilsson, O., Moulin, T., Mugnier, L., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramose, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Turatto, M., Weber, L., Keppler, M., Benisty, M., Mueller, A., Henning, Th., van Boekel, R., Cantalloube, F., Ginski, C., van Holstein, R. G., Maire, A. -L., Pohl, A., Samland, M., Avenhaus, H., Baudino, J. -L., Boccaletti, A., de Boer, J., Bonnefoy, M., Chauvin, G., Desidera, S., Langlois, M., Lazzoni, C., Marleau, G. -D., 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, Markus, Juhasz, A., Kemmer, J., Kral, Q., Lagrange, A. -M., Launhardt, R., Matter, A., Menard, F., Milli, J., Molliere, P., Olofsson, J., Perez, L., Pinilla, P., Pinte, C., Quanz, S. P., Schmidt, T., Udry, S., Wahhaj, Z., Williams, J. P., 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, J. -C., Baruffolo, A., Baudoz, P., Bazzon, A., Beuzit, J. -L., Blanchard, P., Brems, S. S., Buey, T., De Caprio, V., Carbillet, M., Carle, M., Cascone, E., Cheetham, A., Claudi, R., Costille, A., Delboulbe, 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., Meyer, M., Moeller-Nilsson, O., Moulin, T., Mugnier, L., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramose, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Turatto, M., and Weber, L.
Abstract: Context. Young circumstellar disks are the birthplaces of planets. Their study is 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. Aims. 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 an embedded young planet and search for disk structures that may be the result of disk-planet interactions and other evolutionary processes. Methods. We analyse new and archival near-infrared images of the transition disk PDS 70 obtained with the VLT/SPHERE, VLT/NaCo, and Gemini/NICI instruments in polarimetric differential imaging and angular differential imaging modes. Results. We detect a point source within the gap of the disk at about 195 mas (similar to 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. The luminosity of the detected object is consistent with that of an L-type dwarf, but its IR colours are redder, possibly indicating the presence of warm surrounding material. Further, we confirm the detection of a large gap of similar to 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 similar to 17 au in radius, and its position angle is consistent with that of the outer disk. The images of the outer disk show evidence of a complex azimuthal brightness distribution which is different at differ
Published: 2018
Full Text: View/download PDF

31. Resolving faint structures in the debris disk around TWA 7 Tentative detections of an outer belt, a spiral arm, and a dusty cloud

Author: Olofsson, J., van Holstein, R. G., Boccaletti, A., Janson, Markus, Thebault, P., Gratton, R., Lazzoni, C., Kral, Q., Bayo, A., Canovas, H., Caceres, C., Ginski, C., Pinte, C., Asensio-Torres, Ruben, Chauvin, G., Desidera, S., Henning, Th, Langlois, M., Milli, J., Schlieder, J. E., Schreiber, M. R., Augereau, J-C, Bonnefoy, M., Buenzli, E., Brandner, W., Durkan, Stephen, Engler, N., Feldt, M., Godoy, N., Grady, C., Hagelberg, J., Lagrange, A-M, Lannier, J., Ligi, R., Maire, A-L, Mawet, D., Menard, F., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Schmidt, T., Sissa, E., Thalmann, C., Vigan, A., Abe, L., Feautrier, P., Le Mignant, D., Moulin, T., Pavlov, A., Rabou, P., Rousset, G., Roux, A., Olofsson, J., van Holstein, R. G., Boccaletti, A., Janson, Markus, Thebault, P., Gratton, R., Lazzoni, C., Kral, Q., Bayo, A., Canovas, H., Caceres, C., Ginski, C., Pinte, C., Asensio-Torres, Ruben, Chauvin, G., Desidera, S., Henning, Th, Langlois, M., Milli, J., Schlieder, J. E., Schreiber, M. R., Augereau, J-C, Bonnefoy, M., Buenzli, E., Brandner, W., Durkan, Stephen, Engler, N., Feldt, M., Godoy, N., Grady, C., Hagelberg, J., Lagrange, A-M, Lannier, J., Ligi, R., Maire, A-L, Mawet, D., Menard, F., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Schmidt, T., Sissa, E., Thalmann, C., Vigan, A., Abe, L., Feautrier, P., Le Mignant, D., Moulin, T., Pavlov, A., Rabou, P., Rousset, G., and Roux, A.
Abstract: Context. Debris disks are the intrinsic by-products of the star and planet formation processes. Most likely due to instrumental limitations and their natural faintness, little is known about debris disks around low mass stars, especially when it comes to spatially resolved observations. Aims. We present new VLT/SPHERE IRDIS dual-polarization imaging (DPI) observations in which we detect the dust ring around the M2 spectral type star TWA 7. Combined with additional angular differential imaging observations we aim at a fine characterization of the debris disk and setting constraints on the presence of low-mass planets. Methods. We modeled the SPHERE DPI observations and constrain the location of the small dust grains, as well as the spectral energy distribution of the debris disk, using the results inferred from the observations, and performed simple N-body simulations. Results. We find that the dust density distribution peaks at similar to 0.72 '' (25 au), with a very shallow outer power-law slope, and that the disk has an inclination of similar to 13 degrees with a position angle of similar to 91 degrees east of north. We also report low signal-to-noise ratio detections of an outer belt at a distance of similar to 1.5 '' (similar to 52 au) from the star, of a spiral arm in the southern side of the star, and of a possible dusty clump at 0.11 ''. These findings seem to persist over timescales of at least a year. Using the intensity images, we do not detect any planets in the close vicinity of the star, but the sensitivity reaches Jovian planet mass upper limits. We find that the SED is best reproduced with an inner disk at similar to 0.2 '' (similar to 7 au) and another belt at 0.72 '' (25 au). Conclusions. We report the detections of several unexpected features in the disk around TWA 7. A yet undetected 100 M-circle plus planet with a semi-major axis at 20-30 au could possibly explain the outer belt as well as the spiral arm. We conclude that stellar winds are unlike
Published: 2018
Full Text: View/download PDF

32. Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70

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

33. Discovery of a brown dwarf companion to the star HIP 64892

Author: Cheetham, A., primary, Bonnefoy, M., additional, Desidera, S., additional, Langlois, M., additional, Vigan, A., additional, Schmidt, T., additional, Olofsson, J., additional, Chauvin, G., additional, Klahr, H., additional, Gratton, R., additional, D’Orazi, V., additional, Henning, T., additional, Janson, M., additional, Biller, B., additional, Peretti, S., additional, Hagelberg, J., additional, Ségransan, D., additional, Udry, S., additional, Mesa, D., additional, Sissa, E., additional, Kral, Q., additional, Schlieder, J., additional, Maire, A.-L., additional, Mordasini, C., additional, Menard, F., additional, Zurlo, A., additional, Beuzit, J.-L., additional, Feldt, M., additional, Mouillet, D., additional, Meyer, M., additional, Lagrange, A.-M., additional, Boccaletti, A., additional, Keppler, M., additional, Kopytova, T., additional, Ligi, R., additional, Rouan, D., additional, Le Coroller, H., additional, Dominik, C., additional, Lagadec, E., additional, Turatto, M., additional, Abe, L., additional, Antichi, J., additional, Baruffolo, A., additional, Baudoz, P., additional, Blanchard, P., additional, Buey, T., additional, Carbillet, M., additional, Carle, M., additional, Cascone, E., additional, Claudi, R., additional, Costille, A., additional, Delboulbé, A., additional, De Caprio, V., additional, Dohlen, K., additional, Fantinel, D., additional, Feautrier, P., additional, Fusco, T., additional, Giro, E., additional, Gluck, L., additional, Hubin, N., additional, Hugot, E., additional, Jaquet, M., additional, Kasper, M., additional, Llored, M., additional, Madec, F., additional, Magnard, Y., additional, Martinez, P., additional, Maurel, D., additional, Le Mignant, D., additional, Möller-Nilsson, O., additional, Moulin, T., additional, Origné, A., additional, Pavlov, A., additional, Perret, D., additional, Petit, C., additional, Pragt, J., additional, Puget, P., additional, Rabou, P., additional, Ramos, J., additional, Rigal, F., additional, Rochat, S., additional, Roelfsema, R., additional, Rousset, G., additional, Roux, A., additional, Salasnich, B., additional, Sauvage, J.-F., additional, Sevin, A., additional, Soenke, C., additional, Stadler, E., additional, Suarez, M., additional, Weber, L., additional, and Wildi, F., additional
Published: 2018
Full Text: View/download PDF

34. Discovery of a warm, dusty giant planet around HIP 65426

Author: Chauvin, G., Desidera, S., Lagrange, A. -M., Vigan, A., 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., Mollière, P., Mordasini, C., Müller, 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., De, Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le, Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, 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., Szulágyi, J., Thalmann, C., Wahhaj, Z., Chauvin, G., Desidera, S., Lagrange, A. -M., Vigan, A., 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., Mollière, P., Mordasini, C., Müller, 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., De, Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le, Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, 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., Szulágyi, J., Thalmann, C., and Wahhaj, Z.
Abstract: Aims. The SHINE program is a high-contrast near-infrared survey of 600 young, nearby stars aimed at searching for and characterizing new planetary systems using VLT/SPHERE's unprecedented high-contrast and high-angular-resolution imaging capabilities. It is also intended to place statistical constraints on the rate, mass and orbital distributions of the giant planet population at large orbits as a function of the stellar host mass and age to test planet-formation theories. Methods. We used the IRDIS dual-band imager and the IFS integral field spectrograph of SPHERE to acquire high-contrast coronagraphic differential near-infrared images and spectra of the young A2 star HIP 65426. It is a member of the ~17 Myr old Lower Centaurus-Crux association. Results. At a separation of 830 mas (92 au projected) from the star, we detect a faint red companion. Multi-epoch observations confirm that it shares common proper motion with HIP 65426. Spectro-photometric measurements extracted with IFS and IRDIS between 0.95 and 2.2 μm indicate a warm, dusty atmosphere characteristic of young low-surface-gravity L5-L7 dwarfs. Hot-start evolutionary models predict a luminosity consistent with a 6-12 MJup, Teff = 1300-1600 K and R = 1.5 ± 0.1 RJup giant planet. Finally, the comparison with Exo-REM and PHOENIX BT-Settl synthetic atmosphere models gives consistent effective temperatures but with slightly higher surface gravity solutions of log (g) = 4.0-5.0 with smaller radii (1.0-1.3 RJup). Conclusions. Given its physical and spectral properties, HIP 65426 b occupies a rather unique placement in terms of age, mass, and spectral-type among the currently known imaged planets. It represents a particularly interesting case to study the presence of clouds as a function of particle size, composition, and location in the atmosphere, to search for signatures of non-equilibrium chemistry, and finally to test the theory of planet formation and evolution. © ESO, 2017.
Published: 2017

35. The Circumstellar Disk HD 169142 : Gas, Dust, and Planets Acting in Concert?

Author: Pohl, A., Benisty, M., Pinilla, P., Ginski, C., de Boer, J., Avenhaus, H., Henning, Th., Zurlo, A., Boccaletti, A., Augereau, J. -C., Birnstiel, T., Dominik, C., Facchini, S., Fedele, D., Janson, Markus, Keppler, M., Kral, Q., Langlois, M., Ligi, R., Maire, A. -L., Menard, F., Meyer, M., Pinte, C., Quanz, S. P., Sauvage, J. -F., Sezestre, E., Stolker, T., Szulagyi, J., van Boekel, R., van der Plas, G., Villenave, M., Baruffolo, A., Baudoz, P., Le Mignant, D., Maurel, D., Ramos, J., Weber, L., Pohl, A., Benisty, M., Pinilla, P., Ginski, C., de Boer, J., Avenhaus, H., Henning, Th., Zurlo, A., Boccaletti, A., Augereau, J. -C., Birnstiel, T., Dominik, C., Facchini, S., Fedele, D., Janson, Markus, Keppler, M., Kral, Q., Langlois, M., Ligi, R., Maire, A. -L., Menard, F., Meyer, M., Pinte, C., Quanz, S. P., Sauvage, J. -F., Sezestre, E., Stolker, T., Szulagyi, J., van Boekel, R., van der Plas, G., Villenave, M., Baruffolo, A., Baudoz, P., Le Mignant, D., Maurel, D., Ramos, J., and Weber, L.
Abstract: HD 169142 is an excellent target for investigating signs of planet-disk interaction due to previous evidence of gap structures. We perform J-band (similar to 1.2 mu m) polarized intensity imaging of HD 169142 with VLT/SPHERE. We observe polarized scattered light down to 0 ''.16 (similar to 19 au) and find an inner gap with a significantly reduced scattered-light flux. We confirm the previously detected double-ring structure peaking at 0 ''.18 (similar to 21 au) and 0 ''.56 (similar to 66 au) and marginally detect a faint third gap at 0 ''.70-0 ''.73 (similar to 82-85 au). We explore dust evolution models in a disk perturbed by two giant planets, as well as models with a parameterized dust size distribution. The dust evolution model is able to reproduce the ring locations and gap widths in polarized intensity but fails to reproduce their depths. However, it gives a good match with the ALMA dust continuum image at 1.3 mm. Models with a parameterized dust size distribution better reproduce the gap depth in scattered light, suggesting that dust filtration at the outer edges of the gaps is less effective. The pileup of millimeter grains in a dust trap and the continuous distribution of small grains throughout the gap likely require more efficient dust fragmentation and dust diffusion in the dust trap. Alternatively, turbulence or charging effects might lead to a reservoir of small grains at the surface layer that is not affected by the dust growth and fragmentation cycle dominating the dense disk midplane. The exploration of models shows that extracting planet properties such as mass from observed gap profiles is highly degenerate.
Published: 2017
Full Text: View/download PDF

36. Stop-less Lyot coronagraph for exoplanet characterization: first on-sky validation in VLT/SPHERE

Author: Vigan, Arthur, N'Diaye, M., Dohlen, K., Beuzit, J.-L., Costille, A., Caillat, A., Baruffolo, A., Blanchard, P., Carle, M., Ferrari, M., Fusco, T., Gluck, L., Hugot, E., Jaquet, M., Langlois, M., Le Mignant, D., Llored, M., Madec, F., Mouillet, D., Origné, A., Puget, P., Salasnich, B., Sauvage, J.-F., Navarro, Ramon, Burge, James, Sauvage, F., 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), Space Telescope Science Institute (STSci), 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), Chimie, Ingénierie Moléculaire et Matériaux d'Angers (CIMMA), Université d'Angers (UA)-Centre National de la Recherche Scientifique (CNRS), Caratterizzazione e Sviluppo di Materiali per la Fotonica e l'Optoelecttronica (CSMFO), CNR Istituto di Fotonica e Nanotecnologie [Trento] (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR)-Consiglio Nazionale delle Ricerche [Roma] (CNR), Netherlands Institute for Radio Astronomy (ASTRON), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)-National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'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), Laboratoire de Chimie, Ingénierie Moléculaire et Matériaux d'Angers (CIMMA), Centre National de la Recherche Scientifique (CNRS)-Université d'Angers (UA), 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), ITA, USA, and FRA
Subjects: Physics, Lyot stop, business.industry, media_common.quotation_subject, Phase (waves), 01 natural sciences, Exoplanet, law.invention, 010309 optics, Speckle pattern, Optics, Apodization, law, Sky, 0103 physical sciences, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Coronagraph, Long-slit spectroscopy, media_common
Abstract: International audience; The VLT/SPHERE instrument includes a unique long-slit spectroscopy (LSS) mode coupled with Lyot coronagraphy dedicated to the spectral characterization of directly imaged giant exoplanets. The performance of this mode is limited by its non-optimal coronagraph, but in a previous work we demonstrated that it could be significantly improved at small inner-working angles using the stop-less Lyot coronagraph (SLLC). A prototype of the SLLC was installed in VLT/SPHERE in 2014 during the reintegration of the instrument in Paranal, and it was extensively tested in 2015 to characterize its performance. The performance is tested in both imaging and spectroscopy using data acquired on the internal source of SPHERE. In imaging, we obtain a raw contrast gain of a factor 10 at 0.3" with the SLLC. We also demonstrate that no Lyot stop is required to reach the full performance, which validates the SLLC concept. Comparison with a realistic simulation model shows that we are currently limited by the internal phase aberrations of SPHERE. In spectroscopy, we obtain a gain of 1 mag in a limited range of angular separations. Simulations show that although the main limitation comes from phase errors, the performance in the non-SLLC case is very close to the ultimate limit of the LSS mode. We present the very first on-sky data with the SLLC, which appear extremely promising for the future scientific exploitation of an apodized LSS mode in SPHERE. Finally, we explore a new possibility for the speckle subtraction in the LSS mode that could significantly improve the data analysis with respect to methods based on spectral differences.
Published: 2016

37. Discovery of a warm, dusty giant planet around HIP 65426

Author: Chauvin, G., primary, Desidera, S., additional, Lagrange, A.-M., additional, Vigan, A., additional, Gratton, R., additional, Langlois, M., additional, Bonnefoy, M., additional, Beuzit, J.-L., additional, Feldt, M., additional, Mouillet, D., additional, Meyer, M., additional, Cheetham, A., additional, Biller, B., additional, Boccaletti, A., additional, D’Orazi, V., additional, Galicher, R., additional, Hagelberg, J., additional, Maire, A.-L., additional, Mesa, D., additional, Olofsson, J., additional, Samland, M., additional, Schmidt, T. O. B., additional, Sissa, E., additional, Bonavita, M., additional, Charnay, B., additional, Cudel, M., additional, Daemgen, S., additional, Delorme, P., additional, Janin-Potiron, P., additional, Janson, M., additional, Keppler, M., additional, Le Coroller, H., additional, Ligi, R., additional, Marleau, G. D., additional, Messina, S., additional, Mollière, P., additional, Mordasini, C., additional, Müller, A., additional, Peretti, S., additional, Perrot, C., additional, Rodet, L., additional, Rouan, D., additional, Zurlo, A., additional, Dominik, C., additional, Henning, T., additional, Menard, F., additional, Schmid, H.-M., additional, Turatto, M., additional, Udry, S., additional, Vakili, F., additional, Abe, L., additional, Antichi, J., additional, Baruffolo, A., additional, Baudoz, P., additional, Baudrand, J., additional, Blanchard, P., additional, Bazzon, A., additional, Buey, T., additional, Carbillet, M., additional, Carle, M., additional, Charton, J., additional, Cascone, E., additional, Claudi, R., additional, Costille, A., additional, Deboulbe, A., additional, De Caprio, V., additional, Dohlen, K., additional, Fantinel, D., additional, Feautrier, P., additional, Fusco, T., additional, Gigan, P., additional, Giro, E., additional, Gisler, D., additional, Gluck, L., additional, Hubin, N., additional, Hugot, E., additional, Jaquet, M., additional, Kasper, M., additional, Madec, F., additional, Magnard, Y., additional, Martinez, P., additional, Maurel, D., additional, Le Mignant, D., additional, Möller-Nilsson, O., additional, Llored, M., additional, Moulin, T., additional, Origné, A., additional, Pavlov, A., additional, Perret, D., additional, Petit, C., additional, Pragt, J., additional, Puget, P., additional, Rabou, P., additional, Ramos, J., additional, Rigal, R., additional, Rochat, S., additional, Roelfsema, R., additional, Rousset, G., additional, Roux, A., additional, Salasnich, B., additional, Sauvage, J.-F., additional, Sevin, A., additional, Soenke, C., additional, Stadler, E., additional, Suarez, M., additional, Weber, L., additional, Wildi, F., additional, Antoniucci, S., additional, Augereau, J.-C., additional, Baudino, J.-L., additional, Brandner, W., additional, Engler, N., additional, Girard, J., additional, Gry, C., additional, Kral, Q., additional, Kopytova, T., additional, Lagadec, E., additional, Milli, J., additional, Moutou, C., additional, Schlieder, J., additional, Szulágyi, J., additional, Thalmann, C., additional, and Wahhaj, Z., additional
Published: 2017
Full Text: View/download PDF

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

Author: Maire, A.-L., primary, Stolker, T., additional, Messina, S., additional, Müller, A., additional, Biller, B. A., additional, Currie, T., additional, Dominik, C., additional, Grady, C. A., additional, Boccaletti, A., additional, Bonnefoy, M., additional, Chauvin, G., additional, Galicher, R., additional, Millward, M., additional, Pohl, A., additional, Brandner, W., additional, Henning, T., additional, Lagrange, A.-M., additional, Langlois, M., additional, Meyer, M. R., additional, Quanz, S. P., additional, Vigan, A., additional, Zurlo, A., additional, van Boekel, R., additional, Buenzli, E., additional, Buey, T., additional, Desidera, S., additional, Feldt, M., additional, Fusco, T., additional, Ginski, C., additional, Giro, E., additional, Gratton, R., additional, Hubin, N., additional, Lannier, J., additional, Le Mignant, D., additional, Mesa, D., additional, Peretti, S., additional, Perrot, C., additional, Ramos, J. R., additional, Salter, G., additional, Samland, M., additional, Sissa, E., additional, Stadler, E., additional, Thalmann, C., additional, Udry, S., additional, and Weber, L., additional
Published: 2017
Full Text: View/download PDF

39. First light of the VLT planet finder SPHERE I. Detection and characterization of the substellar companion GJ 758 B

Author: Vigan, A., Bonnefoy, M., Ginski, C., Beust, H., Galicher, R., Janson, Markus, Baudino, J. -L., Buenzli, E., Hagelberg, J., D'Orazi, V., Desidera, S., Maire, A. -L., Gratton, R., Sauvage, J. -F., Chauvin, G., Thalmann, C., Malo, L., Salter, G., Zurlo, A., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Boccaletti, A., Beuzit, J. -L., Carle, M., Claudi, R., Costille, A., Delboulbe, A., Dohlen, K., Dominik, C., Feldt, M., Fusco, T., Gluck, L., Girard, J., Giro, E., Gry, C., Henning, T., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Lagrange, A. -M., Langlois, M., Le Mignant, D., Llored, M., Madec, F., Martinez, P., Mawet, D., Mesa, D., Milli, J., Mouillet, D., Moulin, T., Moutou, C., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Rochat, S., Roelfsema, R., Salasnich, B., Schmid, H. -M., Sevin, A., Siebenmorgen, R., Smette, A., Stadler, E., Suarez, M., Turatto, M., Udry, S., Vakili, F., Wahhaj, Z., Weber, L., Wildi, F., Vigan, A., Bonnefoy, M., Ginski, C., Beust, H., Galicher, R., Janson, Markus, Baudino, J. -L., Buenzli, E., Hagelberg, J., D'Orazi, V., Desidera, S., Maire, A. -L., Gratton, R., Sauvage, J. -F., Chauvin, G., Thalmann, C., Malo, L., Salter, G., Zurlo, A., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Boccaletti, A., Beuzit, J. -L., Carle, M., Claudi, R., Costille, A., Delboulbe, A., Dohlen, K., Dominik, C., Feldt, M., Fusco, T., Gluck, L., Girard, J., Giro, E., Gry, C., Henning, T., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Lagrange, A. -M., Langlois, M., Le Mignant, D., Llored, M., Madec, F., Martinez, P., Mawet, D., Mesa, D., Milli, J., Mouillet, D., Moulin, T., Moutou, C., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Rochat, S., Roelfsema, R., Salasnich, B., Schmid, H. -M., Sevin, A., Siebenmorgen, R., Smette, A., Stadler, E., Suarez, M., Turatto, M., Udry, S., Vakili, F., Wahhaj, Z., Weber, L., and Wildi, F.
Abstract: GJ 758 B is a brown dwarf companion to a nearby (15.76%) solar-type, metal-rich (M/H = +0.2 dex) main-sequence star (G9V) that was discovered with Subaru/HiCIAO in 2009. From previous studies, it has drawn attention as being the coldest (similar to 600 K) companion ever directly imaged around a neighboring star. We present new high-contrast data obtained during the commissioning of the SPHERE instrument at the Very Large Telescope (VLT). The data was obtained in Y-, J-, H-, and K-s-bands with the dual-band imaging (DBI) mode of IRDIS, thus providing a broad coverage of the full near-infrared (near-IR) range at higher contrast and better spectral sampling than previously reported. In this new set of high-quality data, we report the re-detection of the companion, as well as the first detection of a new candidate closer-in to the star. We use the new eight photometric points for an extended comparison of GJ 758 B with empirical objects and four families of atmospheric models. From comparison to empirical object, we estimate a T8 spectral type, but none of the comparison objects can accurately represent the observed near-IR fluxes of GJ 758 B. From comparison to atmospheric models, we attribute a T-eff = 600 +/- 100 K, but we find that no atmospheric model can adequately fit all the fluxes of GJ 758 B. The lack of exploration of metal enrichment in model grids appears as a major limitation that prevents an accurate estimation of the companion physical parameters. The photometry of the new candidate companion is broadly consistent with L-type objects, but a second epoch with improved photometry is necessary to clarify its status. The new astrometry of GJ 758 B shows a significant proper motion since the last epoch. We use this result to improve the determination of the orbital characteristics using two fitting approaches: Least-Squares Monte Carlo and Markov chain Monte Carlo. We confirm the high-eccentricity of the orbit (peak at 0.5), and find a most likely semi-major
Published: 2016
Full Text: View/download PDF

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

Author: N’Diaye, M., primary, Vigan, A., additional, Dohlen, K., additional, Sauvage, J.-F., additional, Caillat, A., additional, Costille, A., additional, Girard, J. H. V., additional, Beuzit, J.-L., additional, Fusco, T., additional, Blanchard, P., additional, Le Merrer, J., additional, Le Mignant, D., additional, Madec, F., additional, Moreaux, G., additional, Mouillet, D., additional, Puget, P., additional, and Zins, G., additional
Published: 2016
Full Text: View/download PDF

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

Author: Khorrami, Z., primary, Lanz, T., additional, Vakili, F., additional, Lagadec, E., additional, Langlois, M., additional, Brandner, W., additional, Chesneau, O., additional, Meyer, M. R., additional, Carbillet, M., additional, Abe, L., additional, Mouillet, D., additional, Beuzit, J. L., additional, Boccaletti, A., additional, Perrot, C., additional, Thalmann, C., additional, Schmid, H.-M., additional, Pavlov, A., additional, Costille, A., additional, Dohlen, K., additional, Le Mignant, D., additional, Petit, C., additional, and Sauvage, J. F., additional
Published: 2016
Full Text: View/download PDF

42. First light of the VLT planet finder SPHERE

Author: Maire, A.-L., primary, Bonnefoy, M., additional, Ginski, C., additional, Vigan, A., additional, Messina, S., additional, Mesa, D., additional, Galicher, R., additional, Gratton, R., additional, Desidera, S., additional, Kopytova, T. G., additional, Millward, M., additional, Thalmann, C., additional, Claudi, R. U., additional, Ehrenreich, D., additional, Zurlo, A., additional, Chauvin, G., additional, Antichi, J., additional, Baruffolo, A., additional, Bazzon, A., additional, Beuzit, J.-L., additional, Blanchard, P., additional, Boccaletti, A., additional, de Boer, J., additional, Carle, M., additional, Cascone, E., additional, Costille, A., additional, De Caprio, V., additional, Delboulbé, A., additional, Dohlen, K., additional, Dominik, C., additional, Feldt, M., additional, Fusco, T., additional, Girard, J. H., additional, Giro, E., additional, Gisler, D., additional, Gluck, L., additional, Gry, C., additional, Henning, T., additional, Hubin, N., additional, Hugot, E., additional, Jaquet, M., additional, Kasper, M., additional, Lagrange, A.-M., additional, Langlois, M., additional, Le Mignant, D., additional, Llored, M., additional, Madec, F., additional, Martinez, P., additional, Mawet, D., additional, Milli, J., additional, Möller-Nilsson, O., additional, Mouillet, D., additional, Moulin, T., additional, Moutou, C., additional, Origné, A., additional, Pavlov, A., additional, Petit, C., additional, Pragt, J., additional, Puget, P., additional, Ramos, J., additional, Rochat, S., additional, Roelfsema, R., additional, Salasnich, B., additional, Sauvage, J.-F., additional, Schmid, H. M., additional, Turatto, M., additional, Udry, S., additional, Vakili, F., additional, Wahhaj, Z., additional, Weber, L., additional, and Wildi, F., additional
Published: 2016
Full Text: View/download PDF

43. First light of the VLT planet finder SPHERE

Author: Vigan, A., primary, Bonnefoy, M., additional, Ginski, C., additional, Beust, H., additional, Galicher, R., additional, Janson, M., additional, Baudino, J.-L., additional, Buenzli, E., additional, Hagelberg, J., additional, D’Orazi, V., additional, Desidera, S., additional, Maire, A.-L., additional, Gratton, R., additional, Sauvage, J.-F., additional, Chauvin, G., additional, Thalmann, C., additional, Malo, L., additional, Salter, G., additional, Zurlo, A., additional, Antichi, J., additional, Baruffolo, A., additional, Baudoz, P., additional, Blanchard, P., additional, Boccaletti, A., additional, Beuzit, J.-L., additional, Carle, M., additional, Claudi, R., additional, Costille, A., additional, Delboulbé, A., additional, Dohlen, K., additional, Dominik, C., additional, Feldt, M., additional, Fusco, T., additional, Gluck, L., additional, Girard, J., additional, Giro, E., additional, Gry, C., additional, Henning, T., additional, Hubin, N., additional, Hugot, E., additional, Jaquet, M., additional, Kasper, M., additional, Lagrange, A.-M., additional, Langlois, M., additional, Le Mignant, D., additional, Llored, M., additional, Madec, F., additional, Martinez, P., additional, Mawet, D., additional, Mesa, D., additional, Milli, J., additional, Mouillet, D., additional, Moulin, T., additional, Moutou, C., additional, Origné, A., additional, Pavlov, A., additional, Perret, D., additional, Petit, C., additional, Pragt, J., additional, Puget, P., additional, Rabou, P., additional, Rochat, S., additional, Roelfsema, R., additional, Salasnich, B., additional, Schmid, H.-M., additional, Sevin, A., additional, Siebenmorgen, R., additional, Smette, A., additional, Stadler, E., additional, Suarez, M., additional, Turatto, M., additional, Udry, S., additional, Vakili, F., additional, Wahhaj, Z., additional, Weber, L., additional, and Wildi, F., additional
Published: 2016
Full Text: View/download PDF

44. Apodization in high-contrast long-slit spectroscopy

Author: Vigan, A., primary, N’Diaye, M., additional, Dohlen, K., additional, Beuzit, J.-L., additional, Costille, A., additional, Caillat, A., additional, Baruffolo, A., additional, Blanchard, P., additional, Carle, M., additional, Ferrari, M., additional, Fusco, T., additional, Gluck, L., additional, Hugot, E., additional, Jaquet, M., additional, Langlois, M., additional, Le Mignant, D., additional, Llored, M., additional, Madec, F., additional, Mouillet, D., additional, Origné, A., additional, Puget, P., additional, Salasnich, B., additional, and Sauvage, J.-F., additional
Published: 2016
Full Text: View/download PDF

45. Superresolving Distant Galaxies with Gravitational Telescopes: Keck Laser Guide Star Adaptive Optics and Imaging of the Lens System SDSS J0737+3216

Author: Marshall, P, Treu, T, Melbourne, J, Gavazzi, R, Bundy, K, Ammons, S, Bolton, A, Burles, S, Larkin, J, Le Mignant, D, Koo, D, Koopmans, L, Max, C, Moustakas, L, Steinbring, E, and Wright, SA
Published: 2007

46. The science case for the Next Generation AO system at W. M. Keck Observatory

Author: Hubin, Norbert, Max, Claire E., Wizinowich, Peter L., Max, C., McGrath, E., Gavel, D., Le Mignant, D., Wizinowich, P., Dekany, R., Hubin, Norbert, Max, Claire E., Wizinowich, Peter L., Max, C., McGrath, E., Gavel, D., Le Mignant, D., Wizinowich, P., and Dekany, R.
Abstract: The W. M. Keck Observatory is designing a new adaptive optics system providing precision AO correction in the near infrared, good correction at visible wavelengths, and multiplexed spatially resolved spectroscopy. We discuss science cases for this Next Generation AO (NGAO), and show how the system requirements were derived from these science cases. Key science drivers include asteroid companions, planets around low-mass stars, general relativistic effects around the Galactic Center black hole, nearby active galactic nuclei, and high-redshift galaxies (including galaxies lensed by intervening galaxies or clusters). The multi-object AO-corrected integral field spectrograph will be optimized for high-redshift galaxy science.
Published: 2008

47. Adaptive optics imaging of IRAS 18276-1431: A bipolar preplanetary nebula with circumstellar 'searchlight beams' and 'ARCS'

Author: European Commission, National Aeronautics and Space Administration (US), Ministerio de Ciencia y Tecnología (España), National Science Foundation (US), Sánchez Contreras, C., Le Mignant, D., Sahai, R., Gil de Paz, A., Morris, M., European Commission, National Aeronautics and Space Administration (US), Ministerio de Ciencia y Tecnología (España), National Science Foundation (US), Sánchez Contreras, C., Le Mignant, D., Sahai, R., Gil de Paz, A., and Morris, M.
Abstract: We present high angular resolution images of the post-AGB nebula IRAS 18276-1431 (also known as OH 17.7-2.0) obtained with the Keck II adaptive optics (AO) system in its natural guide star (NGS) mode in the Kp, L p, and Ms near-infrared bands. We also present supporting optical F606W and F814W HST images as well as interferometric observations of the 12CO J = 1-0, 13CO J = 1-0, and 2.6 mm continuum emission with OVRO. The envelope of IRAS 18276-1431 displays a clear bipolar morphology in our optical and NIR images with two lobes separated by a dark waist and surrounded by a faint 4.5″ × 3.4″ halo. Our K p-band image reveals two pairs of radial >searchlight beams> emerging from the nebula center and several intersecting, arclike features. From our CO data we derive a mass of M > 0.38(D/3 kpc)2 M⊙ and an expansion velocity Vexp = 17 kms-1 for the molecular envelope. The density in the halo follows a radial power law ∝r-3, which is consistent with a mass-loss rate increasing with time. Analysis of the NIR colors indicates the presence of a compact central source of ∼300-500 K dust illuminating the nebula in addition to the central star. Modeling of the thermal IR suggests a two-shell structure in the dust envelope: (1) an outer shell with inner and outer radius Rin ∼ 1.6 × 1016 and Rout ≳ 1.25 × 10 17 cm, dust temperature Tdust ∼ 105-50 K, and a mean mass-loss rate of M ≈ 10-3 M⊙ yr-1; and (2) an inner shell with Rin ∼ 6.3 × 1014 cm, Tdust ∼ 500-105 K, and Ṁ ∼ 3 × 10-5 M⊙ yr-1. An additional population of big dust grains (radius a ≳; 0.4 mm) with Tdust 150-20 K and mass M dust = (0.16-1.6) × 10-3 (D/3 kpc)2 M⊙can account for the observed submillimeter and millimeter flux excess. The mass of the envelope enclosed within Aout = 1.25 × 1017 cm derived from SED modeling is ∼1 (D/ 3 kpc)2 Ṁ. © 2007. The American Astronomical Society. All rights reserved.
Published: 2007

48. GRB 071003: Broadband Follow‐up Observations of a Very Bright Gamma‐Ray Burst in a Galactic Halo

Author: Perley, D. A., primary, Li, W., additional, Chornock, R., additional, Prochaska, J. X., additional, Butler, N. R., additional, Chandra, P., additional, Pollack, L. K., additional, Bloom, J. S., additional, Filippenko, A. V., additional, Swan, H., additional, Yuan, F., additional, Akerlof, C., additional, Auger, M. W., additional, Cenko, S. B., additional, Chen, H.‐W., additional, Fassnacht, C. D., additional, Fox, D., additional, Frail, D., additional, Johansson, E. M., additional, McKay, T., additional, Le Mignant, D., additional, Modjaz, M., additional, Rujopakarn, W., additional, Russel, R., additional, Skinner, M. A., additional, Smith, G. H., additional, Smith, I., additional, van Dam, M. A., additional, and Yost, S., additional
Published: 2008
Full Text: View/download PDF

49. Adaptive Optics Imaging of IRAS 18276−1431: A Bipolar Preplanetary Nebula with Circumstellar “Searchlight Beams” and “Arcs”

Author: Sanchez Contreras, C., primary, Le Mignant, D., additional, Sahai, R., additional, Gil de Paz, A., additional, and Morris, M., additional
Published: 2007
Full Text: View/download PDF

50. Keck Interferometer Observations of FU Orionis Objects

Author: Millan‐Gabet, R., primary, Monnier, J. D., additional, Akeson, R. L., additional, Hartmann, L., additional, Berger, J.‐P., additional, Tannirkulam, A., additional, Melnikov, S., additional, Billmeier, R., additional, Calvet, N., additional, D’Alessio, P., additional, Hillenbrand, L. A., additional, Kuchner, M., additional, Traub, W. A., additional, Tuthill, P. G., additional, Beichman, C., additional, Boden, A., additional, Booth, A., additional, Colavita, M., additional, Creech‐Eakman, M., additional, Gathright, J., additional, Hrynevych, M., additional, Koresko, C., additional, Le Mignant, D., additional, Ligon, R., additional, Mennesson, B., additional, Neyman, C., additional, Sargent, A., additional, Shao, M., additional, Swain, M., additional, Thompson, R., additional, Unwin, S., additional, van Belle, G., additional, Vasisht, G., additional, and Wizinowich, P., additional
Published: 2006
Full Text: View/download PDF

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

Language

Publication Type

Journal

Database

Publisher

93 results on '"Le Mignant, D."'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources