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51. GG Tauri A: gas properties and dynamics from the cavity to the outer disk

Author

Phuong, N. T., primary, Dutrey, A., additional, Diep, P. N., additional, Guilloteau, S., additional, Chapillon, E., additional, Di Folco, E., additional, Tang, Y.-W., additional, Piétu, V., additional, Bary, J., additional, Beck, T., additional, Hersant, F., additional, Hoai, D. T., additional, Huré, J. M., additional, Nhung, P. T., additional, Pierens, A., additional, and Tuan-Anh, P., additional

Published
2020
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52. A Precise Physical Orbit For The M-Dwarf Binary Gliese 268

Author

Barry, R. K, Demory, B. -O, Segransan, D, Forveille, T, Danchi, W. C, Di Folco, E, Queloz, D, Spooner, H. R, Torres, G, Traub, W. A, Delfosse, X, Mayor, M, Perrier, C, and Udry, S

Subjects
Astrophysics
Abstract

We report high-precision interferometric and radial velocity (RV) observations of the M-dwarf binary Gl 268. Combining measurements conducted using the IOTA interferometer and the ELODIE and Harvard Center for Astrophysics RV instruments leads to a mass of 0.22596 plus-minus 0.00084 Mass compared to the sun for component A and 0.19230 plus-minus 0.00071 Mass compared to the sun for component B. The system parallax as determined by these observations is 0.1560 plus-minus 0.0030 arcsec - a measurement with 1.9% uncertainty in excellent agreement with Hipparcos (0.1572 plus-minus 0.0033). The absolute H-band magnitudes of the component stars are not well constrained by these measurements; however, we can place an approximate upper limit of 7.95 and 8.1 for Gl 268A and B, respectively.We test these physical parameters against the predictions of theoretical models that combine stellar evolution with high fidelity, non-gray atmospheric models. Measured and predicted values are compatible within 2sigma. These results are among the most precise masses measured for visual binaries and compete with the best adaptive optics and eclipsing binary results.

Published
2012
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53. Reducing the Clinical and Public Health Burden of Familial Hypercholesterolemia: A Global Call to Action

Author

Wilemon, KA, Patel, J, Aguilar-Salinas, C, Ahmed, CD, Alkhnifsawi, M, Almahmeed, W, Alonso, R, Al-Rasadi, K, Badimon, L, Bernal, LM, Bogsrud, MP, Braun, LT, Brunham, L, Catapano, AL, Cillikova, K, Corral, P, Cuevas, R, Defesche, JC, Descamps, OS, de Ferranti, S, Eisele, JL, Elikir, G, Folco, E, Freiberger, T, Fuggetta, F, Gaspar, IM, Gesztes, AG, Groselj, U, Hamilton-Craig, I, Hanauer-Mader, G, Harada-Shiba, M, Hastings, G, Hovingh, GK, Izar, MC, Jamison, A, Karlsson, GN, Kayikcioglu, M, Koob, S, Koseki, M, Lane, S, Lima-Martinez, MM, Lopez, G, Martinez, TL, Marais, D, Marion, L, Mata, P, Maurina, I, Maxwell, D, Mehta, R, Mensah, GA, Miserez, AR, Neely, D, Nicholls, SJ, Nohara, A, Nordestgaard, BG, Ose, L, Pallidis, A, Pang, J, Payne, J, Peterson, AL, Popescu, MP, Puri, R, Ray, KK, Reda, A, Sampietro, T, Santos, RD, Schalkers, I, Schreier, L, Shapiro, MD, Sijbrands, E, Soffer, D, Stefanutti, C, Stoll, M, Sy, RG, Tamayo, ML, Tilney, MK, Tokgozoglu, L, Tomlinson, B, Vallejo-Vaz, AJ, Vazquez-Cardenas, A, de Luca, PV, Wald, DS, Watts, GF, Wenger, NK, Wolf, M, Wood, D, Zegerius, A, Gaziano, TA, Gidding, SS, and Global Familial

Abstract

ImportanceFamilial hypercholesterolemia (FH) is an underdiagnosed and undertreated genetic disorder that leads to premature morbidity and mortality due to atherosclerotic cardiovascular disease. Familial hypercholesterolemia affects 1 in 200 to 250 people around the world of every race and ethnicity. The lack of general awareness of FH among the public and medical community has resulted in only 10% of the FH population being diagnosed and adequately treated. The World Health Organization recognized FH as a public health priority in 1998 during a consultation meeting in Geneva, Switzerland. The World Health Organization report highlighted 11 recommendations to address FH worldwide, from diagnosis and treatment to family screening and education. Research since the 1998 report has increased understanding and awareness of FH, particularly in specialty areas, such as cardiology and lipidology. However, in the past 20 years, there has been little progress in implementing the 11 recommendations to prevent premature atherosclerotic cardiovascular disease in an entire generation of families with FH. ObservationsIn 2018, the Familial Hypercholesterolemia Foundation and the World Heart Federation convened the international FH community to update the 11 recommendations. Two meetings were held: one at the 2018 FH Foundation Global Summit and the other during the 2018 World Congress of Cardiology and Cardiovascular Health. Each meeting served as a platform for the FH community to examine the original recommendations, assess the gaps, and provide commentary on the revised recommendations. The Global Call to Action on Familial Hypercholesterolemia thus represents individuals with FH, advocacy leaders, scientific experts, policy makers, and the original authors of the 1998 World Health Organization report. Attendees from 40 countries brought perspectives on FH from low-, middle-, and high-income regions. Tables listing country-specific government support for FH care, existing country-specific and international FH scientific statements and guidelines, country-specific and international FH registries, and known FH advocacy organizations around the world were created. Conclusions and RelevanceBy adopting the 9 updated public policy recommendations created for this document, covering awareness; advocacy; screening, testing, and diagnosis; treatment; family-based care; registries; research; and cost and value, individual countries have the opportunity to prevent atherosclerotic heart disease in their citizens carrying a gene associated with FH and, likely, all those with severe hypercholesterolemia as well. This guideline presents updated recommendations for management of familial hypercholesterolemia. (c) 2020 American Medical Association. All rights reserved.

Published
2020

54. Reducing the clinical and public health Burden of Familial hypercholesterolemia

Author

Wilemon, KA, Patel, J, Aguilar-Salinas, C, Ahmed, CD, Alkhnifsawi, M, Almahmeed, W, Alonso, R, Al-Rasadi, K, Badimon, L, Bernal, LM, Bogsrud, MP, Braun, LT, Brunham, L, Catapano, AL, Cillíková, K, Corral, P, Cuevas, R, Defesche, JC, Descamps, OS, De Ferranti, S, Eiselé, J-L, Elikir, G, Folco, E, Freiberger, T, Fuggetta, F, Gaspar, IM, Gesztes, ÁG, Grošelj, U, Hamilton-Craig, I, Hanauer-Mader, G, Harada-Shiba, M, Hastings, G, Hovingh, GK, Izar, MC, Jamison, A, Karlsson, GN, Kayikçioglu, M, Koob, S, Koseki, M, Lane, S, Lima-Martinez, MM, López, G, Martinez, TL, Marais, D, Marion, L, Mata, P, Maurina, I, Maxwell, D, Mehta, R, Mensah, GA, Miserez, AR, Neely, D, Nicholls, SJ, Nohara, A, Nordestgaard, BG, Ose, L, Pallidis, A, Pang, J, Payne, J, Peterson, AL, Popescu, MP, Puri, R, Ray, KK, Reda, A, Sampietro, T, Santos, RD, Schalkers, I, Schreier, L, Shapiro, MD, Sijbrands, E, Soffer, D, Stefanutti, C, Stoll, M, Sy, RG, Tamayo, ML, Tilney, MK, Tokgözoglu, L, Tomlinson, B, Vallejo-Vaz, AJ, Vazquez-Cárdenas, A, De Luca, PV, Wald, DS, Watts, GF, Wenger, NK, Wolf, M, Wood, D, Zegerius, A, Gaziano, TA, and Gidding, SS

Subjects
Science & Technology, Cardiac & Cardiovascular Systems, GUIDANCE, STATEMENT, SOCIETY, CHILDREN, CARE, GUIDELINES, DIAGNOSIS, PANEL, COST-EFFECTIVENESS, Cardiovascular System & Cardiology, MANAGEMENT, Representatives of the Global Familial Hypercholesterolemia Community, Life Sciences & Biomedicine
Abstract

Importance Familial hypercholesterolemia (FH) is an underdiagnosed and undertreated genetic disorder that leads to premature morbidity and mortality due to atherosclerotic cardiovascular disease. Familial hypercholesterolemia affects 1 in 200 to 250 people around the world of every race and ethnicity. The lack of general awareness of FH among the public and medical community has resulted in only 10% of the FH population being diagnosed and adequately treated. The World Health Organization recognized FH as a public health priority in 1998 during a consultation meeting in Geneva, Switzerland. The World Health Organization report highlighted 11 recommendations to address FH worldwide, from diagnosis and treatment to family screening and education. Research since the 1998 report has increased understanding and awareness of FH, particularly in specialty areas, such as cardiology and lipidology. However, in the past 20 years, there has been little progress in implementing the 11 recommendations to prevent premature atherosclerotic cardiovascular disease in an entire generation of families with FH. Observations In 2018, the Familial Hypercholesterolemia Foundation and the World Heart Federation convened the international FH community to update the 11 recommendations. Two meetings were held: one at the 2018 FH Foundation Global Summit and the other during the 2018 World Congress of Cardiology and Cardiovascular Health. Each meeting served as a platform for the FH community to examine the original recommendations, assess the gaps, and provide commentary on the revised recommendations. The Global Call to Action on Familial Hypercholesterolemia thus represents individuals with FH, advocacy leaders, scientific experts, policy makers, and the original authors of the 1998 World Health Organization report. Attendees from 40 countries brought perspectives on FH from low-, middle-, and high-income regions. Tables listing country-specific government support for FH care, existing country-specific and international FH scientific statements and guidelines, country-specific and international FH registries, and known FH advocacy organizations around the world were created. Conclusions and Relevance By adopting the 9 updated public policy recommendations created for this document, covering awareness; advocacy; screening, testing, and diagnosis; treatment; family-based care; registries; research; and cost and value, individual countries have the opportunity to prevent atherosclerotic heart disease in their citizens carrying a gene associated with FH and, likely, all those with severe hypercholesterolemia as well.

Published
2019

55. High-fidelity Imaging of the Inner AU Mic Debris Disk: Evidence of Differential Wind Sculpting?

Author

Molaverdikhani, K., Trifonov, T., Mollière, P., Frankel, N., Messina, S., Biller, B. A., Roux, A., Damasso, M., Del Sordo, F., Brandner, W., Kervella, P., Mugnier, L., Romero, C., Sozzetti, A., Antichi, J., Huby, E., N’Diaye, M., Kitzmann, D., Tang, Y. W., Habart, E., Beck, T. L., Potier, A., Singh, G., Di Folco, E., Péricaud, J., Dutrey, A., Chapillon, E., Guilloteau, S., Piétu, V., Pawellek, N., Brown, S., Buey, T., Moeller-Nilsson, O., Stolker, T., Hunziker, S., Abe, L., Avenhaus, H., Baruffolo, A., Bazzon, A., Costille, A., Daban, J.-B., Downing, M., Engler, N., Gisler, D., Hubin, N., Puget, P., Quanz, S. P., Roelfsema, R., Salasnich, B., Siebenmorgen, R., Suarez, M., Szulágyi, J., Thalmann, Ch., Pohl, A., Fantinel, D., Maurel, D., Origné, A., Petit, C., Rigal, F., Girard, J. H., Mouillet, D., Dohlen, K., Snik, F., Keller, C. U., Ginski, C., Stam, D. M., Wahhaj, Z., Kasper, M., Schmid, H. M., Perret, D., Dominik, C., Turatto, M., Beuzit, J.-L., Keppler, M., Rodet, L., Charnay, B., Bae, J., De Boer, J., Müller, A., Pairet, B., Antoniucci, S., Brown Sevilla, S., Cascone, E., Claudi, R. U., Lagadec, E., Martinez, P., Meunier, N., Petrus, S., Pinte, C., Rochat, S., Sauvage, J.-F., Peretti, S., Ségransan, D., Lavie, B., Baudino, J.-L., Janson, M., Heng, Kevin, Udry, S., Daemgen, S., Le Coroller, H., Samland, M., Carbillet, M., Carle, M., Hugot, E., Magnard, Y., Moulin, T., Pavlov, A., Pragt, J., Rabou, P., Rousset, G., Sevin, A., Soenke, C., Stadler, E., Weber, L., Wildi, F., Bhowmik, T., Thébault, P., Kral, Q., Mazoyer, J., van Holstein, R. G., Baudoz, P., Galicher, R., Olofsson, J., Pantin, E., Perrot, C., Mesa, D., Langlois, M., Garufi, A., Gratton, R., Desidera, S., D'Orazi, V., Flasseur, O., Barbieri, M., Benisty, M., Henning, Th., Ligi, R., Sissa, E., Vigan, A., Zurlo, A., Bonnefoy, M., Cantalloube, F., Chauvin, G., Cheetham, A. C., De Caprio, V., Delorme, P., Feldt, M., Fusco, T., Gluck, L., Hagelberg, J., Lazzoni, C., Madec, F., Maire, A.-L., Ménard, F., Meyer, M. R., Ramos, J., Rickman, E. L., Rouan, D., Schmidt, T., van der Plas, G., D’Orazi, V., De Caprio, V, Van der Plas, G, Wisniewski, John P., Kowalski, Adam F., Davenport, James R. A., Schneider, Glenn, Grady, Carol A., Hebb, Leslie, Lawson, Kellen D., Augereau, Jean-Charles, Boccaletti, A., Brown, Alexander, Debes, John H., Gaspar, Andras, Henning, Thomas K., Hines, Dean C., Kuchner, Marc J., Lagrange, Anne-Marie, Milli, Julien, Sezestre, Elie, Stark, Christopher C., Thalmann, Christian, Wisniewski, John, Kowalski, Adam, Davenport, James, Grady, Carol, Lawson, Kellen, Debes, John, Henning, Thomas, Hines, Dean, Kuchner, Marc, Stark, Christopher, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
planets and satellites: detection, 010504 meteorology & atmospheric sciences, planets and satellites: dynamical evolution and stability, stars: individual: HD 117214, stars: individual: AB Aur, techniques: image processing, Astrophysics, M dwarf stars, 01 natural sciences, stars: individual: HD 19467, accretion, Debris disks, Astrophysics::Solar and Stellar Astrophysics, infrared: planetary systems, 010303 astronomy & astrophysics, instrumentation: spectrographs, Physics, Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: atmospheres, [PHYS]Physics [physics], planet-disk interactions, accretion disks, stars: individual: HD 32297, protoplanetary disks, stars: individual: Proxima, Exoplanet, Astrophysics - Solar and Stellar Astrophysics, binaries: general, techniques: imaging spectroscopy, techniques: interferometric, stars individual: HIP 65875, planets and satellites: individual: Proxima c, Astrophysics::Earth and Planetary Astrophysics, methods: observational, radio lines: stars, binaries: spectroscopic, brown dwarfs, (stars:) planetary systems, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Brown dwarf, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, stars: pre-main sequence, instrumentation: adaptive optics, planets and satellites: terrestrial planets, stars: individual: PDS70, instrumentation: high angular resolution, 0103 physical sciences, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Debris disk, polarization, HD 163296, Stellar rotation, Starspot, techniques: high angular resolution, Astronomy and Astrophysics, Planetary system, methods: data analysis, binaries: visual, Starspots, techniques: polarimetric, Polar wind, Space and Planetary Science, Circumstellar disks, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Heliosphere, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Astrophysical Journal Letters, 883 (1), ISSN:1967-2014, ISSN:2041-8213

Published
2019
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58. Defining severe familial hypercholesterolaemia and the implications for clinical management: a consensus statement from the International Atherosclerosis Society Severe Familial Hypercholesterolemia Panel

Author

Santos, RD, Gidding, SS, Hegele, RA, Cuchel, MA, Barter, PJ, Watts, GF, Baum, SJ, Catapano, AL, Chapman, MJ, Defesche, JC, Folco, E, Freiberger, T, Genest, J, Hovingh, GK, Harada-Shiba, M, Humphries, SE, Jackson, AS, Mata, P, Moriarty, PM, Raal, FJ, Al-Rasadi, K, Ray, KK, Reiner, Z, Sijbrands, EJ, Yamashita, S, International Atherosclerosis Society Severe Familial Hypercholesterolemia Panel, and Internal Medicine

Subjects
Male, medicine.medical_specialty, Pediatrics, Endocrinology, Diabetes and Metabolism, International Atherosclerosis Society Severe Familial Hypercholesterolemia Panel, Disease, Familial hypercholesterolemia, 030204 cardiovascular system & hematology, Hyperlipoproteinemia Type II, 03 medical and health sciences, 0302 clinical medicine, Endocrinology, Risk Factors, Internal Medicine, Humans, Medicine, 030212 general & internal medicine, Myocardial infarction, PCSK9 Inhibitors, Societies, Medical, Coronary atherosclerosis, Subclinical infection, Familial hypercholesterolaemia (FH), treatment, PCSK9 inhibitors, mipomersen, lomitapide, business.industry, nutritional and metabolic diseases, Cholesterol, LDL, medicine.disease, Response to treatment, 3. Good health, Young age, Cardiovascular Diseases, Practice Guidelines as Topic, Physical therapy, Female, lipids (amino acids, peptides, and proteins), business
Abstract

Familial hypercholesterolaemia is common in individuals who had a myocardial infarction at a young age. As many as one in 200 people could have heterozygous familial hypercholesterolaemia, and up to one in 300 000 individuals could be homozygous. The phenotypes of heterozygous and homozygous familial hypercholesterolaemia overlap considerably; the response to treatment is also heterogeneous. In this Review, we aim to define a phenotype for severe familial hypercholesterolaemia and identify people at highest risk for cardiovascular disease, based on the concentration of LDL cholesterol in blood and individuals' responsiveness to conventional lipid-lowering treatment. We assess the importance of molecular characterisation and define the role of other cardiovascular risk factors and advanced subclinical coronary atherosclerosis in risk stratification. Individuals with severe familial hypercholesterolaemia might benefit in particular from early and more aggressive cholesterol-lowering treatment (eg, with PCSK9 inhibitors). In addition to better tailored therapy, more precise characterisation of individuals with severe familial hypercholesterolaemia could improve resource use.

Published
2016
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59. Interferometric Constraints on Gravity Darkening with Application to the Modeling of Spica A & B

Author

Aufdenberg, J.P., Ireland, M. J., Mérand, A., du Foresto, V. Coudé, Absil, O., Folco, E. Di, Kervella, P., Bagnuolo, W. G., Gies, D. R., Ridgway, S. T., Berger, D. H., ten Brummelaar, T. A., McAlister, H. A., Sturmann, J., Sturmann, L., Turner, N. H., and Jacob, A. P.

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

In 2005 we obtained very precise interferometric measurements of the pole-on rapid rotator Vega (A0 V) with the longest baselines of the Center for High Angular Angular Resolution (CHARA) Array and the Fiber Linked Unit for Optical Recombination (FLUOR). For the analysis of these data, we developed a code for mapping sophisticated PHOENIX model atmospheres on to the surface of rotationally distorted stars described by a Roche-von Zeipel formalism. Given a set of input parameters for a star or binary pair, this code predicts the interferometric visibility, spectral energy distribution and high-resolution line spectrum expected for the system. For the gravity-darkened Vega, our model provides a very good match to the K-band interferometric data, a good match to the spectral energy distribution - except below 160 nm - and a rather poor match to weak lines in the high dispersion spectrum where the model appears overly gravity darkened. In 2006, we used the CHARA Array and FLUOR to obtain high precision measurements of the massive, non-eclipsing, double-line spectroscopic binary Spica, a 4-day period system where both components are gravity darkened rapid rotators. These data supplement recent data obtained with the Sydney University Stellar Interferometer (SUSI). Our study follows the classic 1971 study by Herbison-Evans et al. who resolved Spica as a binary with the Narrabri Stellar Intensity Interferometer (NSII). We will report on our progress modeling the new interferometric and archival spectroscopic data, with the goal towards better constraining the apsidal constant

Published
2017

61. Roles of PAD4 and netosis in experimental atherosclerosis and arterial injury: Implications for superficial erosion

Author

Franck, G., primary, Mawson, T., additional, Folco, E., additional, Molinaro, R., additional, Ruvkun, V., additional, Engelbertsen, D., additional, Liu, X., additional, Tesmenitsky, Y., additional, Shvartz, E., additional, Sukhova, G.K., additional, Michel, J.B., additional, Nicoletti, A., additional, Lichtman, A., additional, Wagner, D., additional, and Libby, K.J., additional

Published
2018
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65. Tau Ceti: our nearest cousin

Author

Di Folco, E., Pericaud, J., Augereau, J.-C., Marshall, J., Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Bordeaux (UB), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AMOR 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-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)-Université Joseph Fourier - Grenoble 1 (UJF)-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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of research, Proloque, 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), and 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)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

International audience; The 10 Gyr old G8V star τCeti is the closest Solar analogue. It harbors the less massive exo-Kuiper belt detected so far among debris disks stars. With a total disk mass only ten times larger than that of our Kuiper belt, it represents a case study of evolved debris disks. Whether its disk has been continuously eroded by steady-state collisions of planetesimals or recently regenerated by a dynamical instability remains a puzzling question. The detection of the dust points to the existence of (undetected) planetary bodies, which are expected to sculpt the belt and may scatter material inwards to the terrestrial planet region, where hot dust is also observed. Unfortunately, the disk morphology remains unknown. We report a recent Herschel PACS (70μ and 160μ)detection of a 15 au ring-like structure which is in conflict with the earlier SCUBA discovery. The disk is partly resolved by Herschel and we derive its morphology and the dust properties from the images and SED analysis with the GraTer modeling code. τCeti is a unique laboratory to highlight the long-term dynamical evolution of planetary systems and may represent an alternative outcome to the evolution of our Solar system.

Published
2014

66. Chemistry in disks

Author

Guilloteau, S., primary, Reboussin, L., additional, Dutrey, A., additional, Chapillon, E., additional, Wakelam, V., additional, Piétu, V., additional, Di Folco, E., additional, Semenov, D., additional, and Henning, Th., additional

Published
2016
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67. Discovery of concentric broken rings at sub-arcsec separations in the HD 141569A gas-rich, debris disk with VLT/SPHERE

Author

Perrot, C., primary, Boccaletti, A., additional, Pantin, E., additional, Augereau, J.-C., additional, Lagrange, A.-M., additional, Galicher, R., additional, Maire, A.-L., additional, Mazoyer, J., additional, Milli, J., additional, Rousset, G., additional, Gratton, R., additional, Bonnefoy, M., additional, Brandner, W., additional, Buenzli, E., additional, Langlois, M., additional, Lannier, J., additional, Mesa, D., additional, Peretti, S., additional, Salter, G., additional, Sissa, E., additional, Chauvin, G., additional, Desidera, S., additional, Feldt, M., additional, Vigan, A., additional, Di Folco, E., additional, Dutrey, A., additional, Péricaud, J., additional, Baudoz, P., additional, Benisty, M., additional, De Boer, J., additional, Garufi, A., additional, Girard, J. H., additional, Menard, F., additional, Olofsson, J., additional, Quanz, S. P., additional, Mouillet, D., additional, Christiaens, V., additional, Casassus, S., additional, Beuzit, J.-L., additional, Blanchard, P., additional, Carle, M., additional, Fusco, T., additional, Giro, E., additional, Hubin, N., additional, Maurel, D., additional, Moeller-Nilsson, O., additional, Sevin, A., additional, and Weber, L., additional

Published
2016
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68. Hearing loss and cognitive decline in older adults: Questions and answers

Author

Bernabei, R, Bonuccelli, U, Maggi, S, Marengoni, Alessandra, Martini, A, Memo, Maurizio, Pecorelli, Sergio, Peracino, A, Quaranta, N, Stella, R, Lin, F, Berrettini, S, Bertolotti, A, Canale, A, Castiglione, A, Cristofari, E, Cuda, D, De Caria, A, Folco, E, Gabelli, C, Genovese, E, Ghidoni, E, Leone, Ca, Mauri, Marta Rosa Maria, Padovani, Alessandro, Paludetti, G, Pirodda, A, Postiglione, A, REDAELLI DE ZINIS, Luca Oscar, Tortelli, R., Roberto Bernabei, Ubaldo Bonuccelli, Stefania Maggi, Alessandra Marengoni, Alessandro Martini, Maurizio Memo, Sergio Pecorelli, Andrea P. Peracino, Nicola Quaranta, Roberto Stella, Frank R. Lin, For the participants in the Workshop on Hearing Loss and Cognitive Decline in Older Adults [.., Antonio Pirodda, and ]

Subjects
Questions and answers, Gerontology, Age-related hearing loss, Cognitive decline, Dementia, Interdisciplinary collaboration, Sensory therapy, Animals, Cognition, Cognition Disorders, Hearing Loss, Humans, Aging, Geriatrics and Gerontology, Medicine (all), Hearing loss, media_common.quotation_subject, MEDLINE, Presentation, Cognition Disorder, otorhinolaryngologic diseases, Medicine, Association (psychology), Hearing Lo, cognitive impairment, media_common, business.industry, Animal, Settore MED/09 - MEDICINA INTERNA, medicine.disease, Age-related hearing lo, Settore MED/32 - AUDIOLOGIA, Settore MED/31 - OTORINOLARINGOIATRIA, medicine.symptom, business, Human
Abstract

The association between hearing impairment, the diagnosis of dementia, and the role of sensory therapy has been proposed for some time, but further research is needed. Current understanding of this association requires the commitment of those experts who can integrate experience and research from several fields to be able to understand the link from hearing to dementia. A workshop whose panelists included experts from many areas, ranging from ear, nose and throat (ENT) to dementia's specialists, was promoted and organized by the Giovanni Lorenzini Medical Science Foundation (Milan, Italy; Houston, TX, USA) to increase the awareness of the relationship between hearing loss and dementia, and included questions and comments following a presentation from the clinical researcher, Frank Lin, who has been evaluating the relationship between hearing loss and cognitive decline since 2009.

Published
2014

69. Planet formation in multiple stellar systems: GG Tau A

Author

Di Folco, E., Dutrey, A., Guilloteau, S., Le Bouquin, J. -B, Lacour, S., Jean-Philippe Berger, Köhler, R., Piétu, V., AMOR 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), 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)-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)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Bordeaux (UB), 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 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), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-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)-Université Joseph Fourier - Grenoble 1 (UJF)-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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

International audience; GG Tau is a hierarchical quadruple system of young, low-mass stars. Because of its well-studied bright circumbinary ring of dust and gas surrounding the main binary GG Tau A, it is a unique laboratory to study planet formation in the disturbed environment of binary/multiple stellar systems. We have started a large observing program of GG Tau A that combines several high-resolution instruments in a multi-wavelength approach. We have recently reported the detection of a new low-mass companion in GG Tau A that turns out to itself be a triple system. This discovery was possible thanks to the very high angular resolution of the near-IR instrument PIONIER on the VLT interferometer, and was confirmed with sub-aperture masking techniques on VLT/NaCo. The detected close binary GG Tau Ab (ρ = 0.032'', or about 5 AU) provides a natural explanation for two enigmas: the discrepancy between the dynamical mass and the spectral type estimates in GG Tau A, and the absence of dust thermal emission in the vicinity of the Ab component. GRAVITY will provide the adequate angular resolution to complete the astrometric characterization of the close binary in the next 10 years. With now 5 coeval low-mass stars, GG Tau is an ideal laboratory to calibrate stellar evolution tracks at young ages (few Myr). Beyond this peculiar system, GRAVITY also has a strong potential to study the impact of multiplicity on the existence of disks, and in fine on planet formation mechanisms in multiple systems.

Published
2014

70. Star and planet formation in the E-ELT era - Physics of circumstellar disks

Author

Di Folco, E., AMOR 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2013

71. Hot circumstellar material resolved around β Pic with VLTI/PIONIER

Author

Defrère, D., Lebreton, J., Le Bouquin, J.-B., Lagrange, A.-M., Absil, O., Augereau, J.-C., Berger, J.-P., Di Folco, E., Ertel, S., Kluska, J., Montagnier, G., Millan-Gabet, R., Traub, W., and Zins, G.

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Aims. We aim at resolving the circumstellar environment around β Pic in the near-infrared in order to study the inner planetary system (

Published
2012

72. High-sensitivity search for clumps in the Vega Kuiper-belt

Author

DI FOLCO, E., GUILLOTEAU, S., GUETH, F., COX, P., PIÉTU, V., aMOR 2011, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-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)-Université Joseph Fourier - Grenoble 1 (UJF)-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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

International audience; We present new observations of the Vega system with the Plateau de Bure Interferometer. The debris disc around the prototypic Vega is known to extend up to > 800AU, with a very smooth far IR emission, and possible clumpiness at sub-mm wavelengths. Our observations of a three-field mosaic at 1.3mm have a factor of two higher sensitivity than previous works. The stellar photosphere is detected with the expected flux, but we find no evidence for the previously reported dust emission peaks that should have been detected at the > 6 level. We derive upper limits for the dust continuum emission that are compatible with observations at shorter wavelengths. All angularly resolved observations indicate that the disc emission around Vega is smooth and circularly symmetric, hence do not require the gravitational influence of a giant planet to sculpt asymmetries, at the current level of detection.

Published
2011

73. Imaging the inner regions of debris disks with near-infrared interferometry

Author

Defrère, D., Absil, O., Augereau, J. C., Di Folco, E., Coudé Du Foresto, V., Le Bouquin, J. B., Antoine Mérand, Mollier, B., Université de Liège, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-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)-Université Joseph Fourier - Grenoble 1 (UJF)-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)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), aMOR 2011, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), 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), European Southern Observatory (ESO), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), 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)-Observatoire aquitain des sciences de l'univers (OASU), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
Abstract

International audience; Most debris disks resolved so far show extended structures located at tens to hundreds AU from the host star, and are more analogous to our solar system's dusty Kuiper belt than to the AU-scale zodiacal disk inside our solar system's asteroid belt. Over the last few years however, a few hot debris disks have been detected around a handful of main sequence stars thanks to the advance of infrared interferometry. The grain populations derived from these observations are quite intriguing, as they point towards very high dust replenishment rates, high cometary activity or major collisional events. In this talk, we review the ongoing efforts to detect bright exozodiacal disks with precision near-infrared interferometry in both hemispheres with CHARA/FLUOR and VLTI/PIONIER. We discuss preliminary statistical trends on the occurrence of bright exozodi around nearby main sequence stars and show how this information could be used to constrain the global architecture and evolution of debris disks.

Published
2011

77. BD+20 1790 radial velocity curve (Figueira+, 2010)

Author

Figueira, P., Marmier, M., Bonfils, X., Di Folco, E., Udry, S., Santos, N. C., Lovis, C., Megevand, D., Melo, C. H. F., Pepe, F., Queloz, D., Segransan, D., Triaud, A. H. M. J., Viana Almeida, P., Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2010

79. VLTI/VINCI diameter constraints on the evolutionary status of delta Eri, xi Hya, eta Boo

Author

Thévenin, Frederic, Kervella, Pierre, Pichon, Bernard, Morel, Pierre, Di Folco, E., Lebreton, Yveline, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), 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, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), 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), 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), European Southern Observatory (ESO), Galaxies, Etoiles, Physique, Instrumentation (GEPI), and Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stellar characteristics and properties, 97.10., 97.10.Cv, 97.10.Nf, 97.10.Pg, 97.10.Ri, 97.10.Sj, stellar radii, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, stellar structure and evolution, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, stellar masses, Astrophysics::Galaxy Astrophysics
Abstract

Using VLTI/VINCI angular diameter measurements, we constrain the evolutionary status of three asteroseismic targets: the stars $\delta$ Eri, $\xi$ Hya, $\eta$ Boo. Our predictions of the mean large frequency spacing of these stars are in agreement with published observational estimations. Looking without success for a companion of $\delta$ Eri we doubt on its classification as an RS CVn star., Comment: other location: http://www.obs-nice.fr/pichon/science.html ; Accepted for publication in Astron. Astrophys

Published
2005
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80. VLTI near-IR interferometric observations of Vega-like stars: Radius and age of a PsA, b Leo, b Pic, e Eri and t Cet

Author

Di Folco, E., Thévénin, F., Kervella, P., Domiciano De Souza, A., Coudé Du Foresto, V., Ségransan, D., Morel, Pierre, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), 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, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and Laboratoire Hippolyte Fizeau (FIZEAU)

Abstract

Astron. and Astroph., 426, pp. 601-617 (2004); International audience

Published
2004

82. GG Tauri: the fifth element

Author

Di Folco, E., primary, Dutrey, A., additional, Le Bouquin, J.-B., additional, Lacour, S., additional, Berger, J.-P., additional, Köhler, R., additional, Guilloteau, S., additional, Piétu, V., additional, Bary, J., additional, Beck, T., additional, Beust, H., additional, and Pantin, E., additional

Published
2014
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84. First scientific results from the VLT interferometer

Author

Paresce, F., van Boekel, R.J.H.M., Correia, S., di Folco, E., Glindemann, A., Kervella, P., Richichi, A., Schoeller, M., Tarenghi, M., Wittkowski, M., Traub, W.A., and Low Energy Astrophysics (API, FNWI)

Published
2003

85. Report on VLTI/VINCI observations of the Be star Achernar

Author

Domiciano De Souza, A., Kervella, P., Jankov, S., Abe, L., Vakili, F., Di Folco, E., Paresce, F., Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Abstract

Conference on Scientific highlights 2003, eds. Combes and D. Barret, SF2A 217, (2003); International audience

Published
2003

86. The VLTI and Its Subsystems

Author

Glindemann, A., Algomedo, J., Amestica, R., Ballester, P., Bauvir, B., Bugueño, E., Correia, S., Delgado, F., Delplancke, F., Derie, F., Duhoux, Ph, Di Folco, E., Alberto Gennai, Gilli, B., Giordano, P., Gitton, Ph, Guisard, S., Housen, N., Huxley, A., Kervella, P., Kiekebusch, M., Koehler, B., Lévêque, S., Longinotti, A., Ménardi, S., Morel, S., Paresce, F., Phan Duc, T., Richichi, A., Schöller, M., Tarenghi, M., Wallander, A., Wittkowski, M., Wilhelm, R., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Astronomie du LESIA, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

Published
2002

87. Ultra-precise Masses and Magnitudes for the Gliese 268 M-dwarf Binary

Author

Stempels, Eric, Barry, R. K., Demory, B. O., Ségransan, D., Forveille, T., Danchi, W. C., Di Folco, E., Queloz, D., Torres, G., Traub, W. A., Delfosse, X., Mayor, M., Perrier, C., Udry, S., Stempels, Eric, Barry, R. K., Demory, B. O., Ségransan, D., Forveille, T., Danchi, W. C., Di Folco, E., Queloz, D., Torres, G., Traub, W. A., Delfosse, X., Mayor, M., Perrier, C., and Udry, S.

Abstract

Recent advances in astrometry using interferometry and precision radial velocity techniques combined allow for a significant improvement in the precision of masses of M‐dwarf stars in visual systems. We report recent astrometric observations of Gliese 268, an M‐dwarf binary with a 10.4 day orbital period, with the IOTA interferometer and radial velocity observations with the ELODIE instrument. Combining these measurements leads to preliminary masses of the constituent stars with uncertainties of 0.4%. The masses of the components are 0.22596±0.00084 M_⊙ for the primary and 0.19230±0.00071 M_⊙ for the secondary. The system parallax is determined by these observations to be 0.1560±.0030 arcsec (2.0% uncertainty) and is within Hipparcos error bars (0.1572±.0033). We tested these physical parameters, along with the near‐infrared luminosities of the stars, against stellar evolution models for low‐mass stars. Discrepancies between the measured and theoretical values point toward a low‐level departure from the predictions. These results are among the most precise masses measured for visual binaries.

Published
2009

88. TW Hydrae: Evidence of stellar spots instead of a hot Jupiter

Author

Fundação Calouste Gulbenkian, Ministerio de Educación y Ciencia (España), Fundação para a Ciência e a Tecnologia (Portugal), Huélamo, Nuria, Figueira, P., Bonfils, Xavier, Santos, N. C., Pepe, F., Gillon, M., Azevedo, R., Barman, T., Fernández, Matilde, Di Folco, E., Guenther, E. W., Lovis, C., Melo, C. H. F., Queloz, D., Udry, Stephane, Fundação Calouste Gulbenkian, Ministerio de Educación y Ciencia (España), Fundação para a Ciência e a Tecnologia (Portugal), Huélamo, Nuria, Figueira, P., Bonfils, Xavier, Santos, N. C., Pepe, F., Gillon, M., Azevedo, R., Barman, T., Fernández, Matilde, Di Folco, E., Guenther, E. W., Lovis, C., Melo, C. H. F., Queloz, D., and Udry, Stephane

Abstract

Context. TW Hya is a classical T Tauri star that shows significant radial-velocity variations in the optical regime. These variations have been attributed to a 10 planet orbiting the star at 0.04 AU. Aims. The aim of this letter is to confirm the presence of the giant planet around TW Hya by (i) testing whether the observed RV variations can be caused by stellar spots and (ii) analyzing new optical and infrared data to detect the signal of the planet companion. Methods. We fitted the RV variations of TW Hya using a cool spot model. In addition, we obtained new high-resolution optical & infrared spectra, together with optical photometry of TW Hya and compared them with previous data. Results. Our model shows that a cold spot covering 7% of the stellar surface and located at a latitude of 54°can reproduce the reported RV variations. The model also predicts a bisector semi-amplitude variation < 10 m s-1, which is less than the errors of the RV measurements discussed in Setiawan et al. (2008, Nature, 451, 38). The analysis of our new optical RV data, with typical errors of 10 m s-1, shows a larger RV amplitude that varies depending on the correlation mask used. A slight correlation between the RV variation and the bisector is also observed although not at a very significant level. The infrared -band RV curve is almost flat, showing a small variation (<35 m s-1) that is not consistent with the published optical orbit. All these results support the spot scenario rather than the presence of a hot Jupiter. Finally, the photometric data shows a 20% (peak to peak) variability, which is much larger than the 4% variation expected for the modeled cool spot. The fact that the optical data are correlated with the surface of the cross-correlation function points towards hot spots as being responsible for the photometric variability. Conclusions. We conclude that the best explanation for the RV signal observed in TW Hya is the presence of a cool stellar spot and not an orbiting hot

Published
2008

89. A near-infrared interferometric survey of debris-disc stars

Author

Absil, O., primary, Defrère, D., additional, Coudé du Foresto, V., additional, Di Folco, E., additional, Mérand, A., additional, Augereau, J.-C., additional, Ertel, S., additional, Hanot, C., additional, Kervella, P., additional, Mollier, B., additional, Scott, N., additional, Che, X., additional, Monnier, J. D., additional, Thureau, N., additional, Tuthill, P. G., additional, ten Brummelaar, T. A., additional, McAlister, H. A., additional, Sturmann, J., additional, Sturmann, L., additional, and Turner, N., additional

Published
2013
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90. Chemistry in disks X. The molecular content of protoplanetary disks in Taurus.

Author

Guilloteau, S., Reboussin, L., Dutrey, A., Chapillon, E., Wakelam, V., Piétu, V., Di Folco, E., Semenov, D., and Henning, Th.

Abstract

Aims. We attempt to determine the molecular composition of disks around young low-mass stars. Methods. We used the IRAM 30 m radio telescope to perform a sensitive wideband survey of 30 stars in the Taurus Auriga region known to be surrounded by gaseous circumstellar disks. We simultaneously observed HCO+ (3−2), HCN(3−2), C2H(3−2), CS(5−4), and two transitions of SO. We combined the results with a previous survey that observed 13CO (2−1), CN(2−1), two o-H2CO lines, and another transition of SO. We used available interferometric data to derive excitation temperatures of CN and C2H in several sources. We determined characteristic sizes of the gas disks and column densities of all molecules using a parametric power-law disk model. Our study is mostly sensitive to molecules at 200−400 au from the stars. We compared the derived column densities to the predictions of an extensive gas-grain chemical disk model under conditions representative of T Tauri disks. Results. This survey provides 20 new detections of HCO+ in disks, 18 in HCN, 11 in C2H, 8 in CS, and 4 in SO. HCO+ is detected in almost all sources and its J = 3−2 line is essentially optically thick, providing good estimates of the disk radii. The other transitions are (at least partially) optically thin. Large variations of the column density ratios are observed, but do not correlate with any specific property of the star or disk. Disks around Herbig Ae stars appear less rich in molecules than those around T Tauri stars, although the sample remains small. SO is only found in the (presumably younger) embedded objects, perhaps reflecting an evolution of the S chemistry due to increasing depletion with time. Overall, the molecular column densities, and in particular the CN/HCN and CN/C2H ratios, are well reproduced by gas-grain chemistry in cold disks. Conclusions. This study provides a comprehensive census of simple molecules in disks of radii >200−300 au. Extending that to smaller disks, or searching for less abundant or more complex molecules requires a much more sensitive facility, i.e., NOEMA and ALMA. [ABSTRACT FROM AUTHOR]

Published
2016
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92. Hot circumstellar material resolved aroundβ Pic with VLTI/PIONIER

Author

Defrère, D., primary, Lebreton, J., additional, Le Bouquin, J.-B., additional, Lagrange, A.-M., additional, Absil, O., additional, Augereau, J.-C., additional, Berger, J.-P., additional, di Folco, E., additional, Ertel, S., additional, Kluska, J., additional, Montagnier, G., additional, Millan-Gabet, R., additional, Traub, W., additional, and Zins, G., additional

Published
2012
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93. Hot exozodiacal dust resolved around Vega with IOTA/IONIC

Author

Defrère, D., primary, Absil, O., additional, Augereau, J.-C., additional, di Folco, E., additional, Berger, J.-P., additional, Coudé du Foresto, V., additional, Kervella, P., additional, Le Bouquin, J.-B., additional, Lebreton, J., additional, Millan-Gabet, R., additional, Monnier, J. D., additional, Olofsson, J., additional, and Traub, W., additional

Published
2011
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96. Evidence against the young hot-Jupiter around BD +20 1790

Author

Figueira, P., primary, Marmier, M., additional, Bonfils, X., additional, di Folco, E., additional, Udry, S., additional, Santos, N. C., additional, Lovis, C., additional, Mégevand, D., additional, Melo, C. H. F., additional, Pepe, F., additional, Queloz, D., additional, Ségransan, D., additional, Triaud, A. H. M. J., additional, and Viana Almeida, P., additional

Published
2010
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97. ALADDIN nulling instrument

Author

Barillot, M., primary, Coudé du Foresto, V., additional, Surdej, J., additional, Absil, O., additional, Jamar, C., additional, and Di Folco, E., additional

Published
2009
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99. Mass-radius relation of low and very low-mass stars revisited with the VLTI

Author

Demory, B.-O., primary, Ségransan, D., additional, Forveille, T., additional, Queloz, D., additional, Beuzit, J.-L., additional, Delfosse, X., additional, Di Folco, E., additional, Kervella, P., additional, Le Bouquin, J.-B., additional, Perrier, C., additional, Benisty, M., additional, Duvert, G., additional, Hofmann, K.-H., additional, Lopez, B., additional, and Petrov, R., additional

Published
2009
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