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Author: Huélamo, N., Chauvin, G., Schmid-Hempel, Paul, Quanz, S.P., Whelan, Emma, Lillo-Box, J., Barrado, D., Montesinos, B., Alcalá, J.M., Benisty, M., de Gregorio-Monsalvo, I., Mendigutía, I., Bouy, H., Merin, B., de Boer, J., Garufi, A., Pantin, E., Huélamo, N., Chauvin, G., Schmid-Hempel, Paul, Quanz, S.P., Whelan, Emma, Lillo-Box, J., Barrado, D., Montesinos, B., Alcalá, J.M., Benisty, M., de Gregorio-Monsalvo, I., Mendigutía, I., Bouy, H., Merin, B., de Boer, J., Garufi, A., and Pantin, E.
Abstract: Context. MWC 758 is a young star surrounded by a transitional disk. The disk shows an inner cavity and spiral arms that could be caused by the presence of protoplanets. Recently, a protoplanet candidate has been detected around MWC758 through high-resolution L0-band observations. The candidate is located inside the disk cavity at a separation of _111 mas from the central star, and at an average position angle of _165.5_. Aims. We aim at detecting accreting protoplanet candidates within the disk of MWC 758 through angular spectral differential imaging (ASDI) observations in the optical regime. In particular, we explore the emission at the position of the detected planet candidate. Methods. We have performed simultaneous adaptive optics observations in the H_ line and the adjacent continuum using SPHERE/ZIMPOL at the Very Large Telescope (VLT). Results. The data analysis does not reveal any H_ signal around the target. The derived contrast curve in the B_Ha filter allows us to derive a 5_ upper limit of _7.6 mag at 111 mas, the separation of the previously detected planet candidate. This contrast translates into a H_ line luminosity of LH_ . 5_10
Published: 2018

152. The spatial extent of polycyclic aromatic hydrocarbons emission in the Herbig star HD 179218

Author: Taha, A. S., Labadie, L., Pantin, E., Matter, A., Alvarez, C., Esquej, P., Grellmann, R., Rebolo, R., Telesco, C., Wolf, S., Taha, A. S., Labadie, L., Pantin, E., Matter, A., Alvarez, C., Esquej, P., Grellmann, R., Rebolo, R., Telesco, C., and Wolf, S.
Abstract: Aims. We investigate, in the mid-infrared, the spatial properties of the polycyclic aromatic hydrocarbons (PAHs) emission in the disk of HD 179218, an intermediate-mass Herbig star at similar to 300 pc. Methods. We obtained mid-infrared images in the PAH-1, PAH-2 and Si-6 filters centered at 8.6, 11.3, and 12.5 mu m, and N-band low-resolution spectra using CanariCam on the 10-m Gran Telescopio Canarias (GTC). We compared the point spread function (PSF) profiles measured in the PAH filters to the profile derived in the Si-6 filter, where the thermal continuum emission dominates. We performed radiative transfer modeling of the spectral energy distribution (SED) and produced synthetic images in the three filters to investigate different spatial scenarios. Results. Our data show that the disk emission is spatially resolved in the PAH-1 and PAH-2 filters, while unresolved in the Si-6 filter. Thanks to very good observing conditions, an average full width at half maximum (FWHM) of 0.232 '', 0.280 '' and 0.293 '' is measured in the three filters, respectively. Gaussian disk fitting and quadratic subtraction of the science and calibrator PSFs suggests a lower-limit characteristic angular diameter of the emission of similar to 100 mas, or similar to 30 au. The photometric and spectroscopic results are compatible with previous findings. Our radiative transfer (RT) modeling of the continuum suggests that the resolved emission should result from PAH molecules on the disk atmosphere being UV-excited by the central star. Simple geometrical models of the PAH component compared to the underlying continuum point to a PAH emission uniformly extended out to the physical limits of the disk model. Furthermore, our RT best model of the continuum requires a negative exponent of the surface density power-law, in contrast with earlier modeling pointing to a positive exponent. Conclusions. We have spatially resolved - for the first time to our knowledge - the PAHs emission in the disk of HD
Published: 2018

153. Dust depletion in the inner disk of beta Pictoris as a possible indicator of planets

Author: Lagage, P.O. and Pantin, E.
Subjects: Beta Pictoris (Star) -- Observations, Planets -- Orbits, Spectrum analysis -- Evaluation, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract: Spectral energy distributional studies of planets orbiting other stars indicate the presence of dust-free regions in the star beta Pictoris with the help of an infrared image of the inner dust disk of the star. The asymmetrical distribution and depletion of dust within the star imply the presence of planetary bodies that orbit beta Pictoris. Planets which orbit in these dust disks help clear the dust-free tracks.
Published: 1994

154. Observational calibration of the projection factor of Cepheids

Author: Belkacem, K., Marques, J., Goupil, M., Sonoi, T., Ouazzani, R., Dupret, M., Mathis, S., Mosser, B., Grosjean, M., Benisty, M., Juhasz, A., Boccaletti, A., Avenhaus, H., Milli, J., Thalmann, C., Dominik, C., Pinilla, P., Buenzli, E., Pohl, A., Beuzit, J.-L., Birnstiel, T., De Boer, J., Bonnefoy, M., Chauvin, G., Christiaens, V., Garufi, A., Grady, C., Henning, T., Huélamo, N., Isella, A., Langlois, M., Menard, F., Mouillet, D., Olofsson, J., Pantin, E., Pinte, C., Pueyo, L., Breitfelder, J., Kervella, P., Mérand, A., Gallenne, A., Szabados, L., Anderson, R., Willson, M., Le Bouquin, J.-B., 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'automatique et de génie des procédés (LAGEP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École Supérieure Chimie Physique Électronique de Lyon-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), 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), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institute of Astronomy [ETH Zürich], 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), Ludwig-Maximilians-Universität München (LMU), Cardiovasculaire, métabolisme, diabétologie et nutrition (CarMeN), Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Hospices Civils de Lyon (HCL), Departamento de Astronomía, Universidad de Chile, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), 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), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, School of Physics, University of Exeter, Space Telescope Science Institute (STSci), Laboratoire Franco-Chilien d'Astronomie (LFCA), Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Chile, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA)-Hungarian Academy of Sciences (MTA), 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), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Hospices Civils de Lyon (HCL)-Institut National de la Santé et de la Recherche Médicale (INSERM), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2015
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155. NEAR: : Low-mass Planets in α Cen with VISIR

Author: Kasper, M., Arsenault, R., Käufl, H. -U, Jakob, G., Fuenteseca, E., Riquelme, M., Siebenmorgen, R., Sterzik, M., Zins, G., Ageorges, N., Gutruf, S., Reutlinger, A., Kampf, D., Absil, O., Carlomagno, B., Guyon, O., Klupar, P., Mawet, D., Ruane, G., Karlsson, Mikael, Pantin, E., Dohlen, K., Kasper, M., Arsenault, R., Käufl, H. -U, Jakob, G., Fuenteseca, E., Riquelme, M., Siebenmorgen, R., Sterzik, M., Zins, G., Ageorges, N., Gutruf, S., Reutlinger, A., Kampf, D., Absil, O., Carlomagno, B., Guyon, O., Klupar, P., Mawet, D., Ruane, G., Karlsson, Mikael, Pantin, E., and Dohlen, K.
Abstract: ESO, in collaboration with the Breakthrough Initiatives, is working to modify the Very Large Telescope mid-IR imager (VISIR) to greatly enhance its ability to search for potentially habitable planets around both components of the binary Alpha Centauri, part of the closest stellar system to the Earth. Much of the funding for the NEAR (New Earths in the Alpha Cen Region) project is provided by the Breakthrough Initiatives, and ESO mostly provides staff and observing time. The concept combines adaptive optics using the deformable secondary mirror at Unit Telescope 4, a new annular groove phase mask (AGPM) coronagraph optimised for the most sensitive spectral bandpass in the N-band, and a novel internal chopper system for noise filtering based on a concept for longer wavelengths invented by the microwave pioneer Robert Dicke. The NEAR experiment is relevant to the mid-infrared METIS instrument on the Extremely Large Telescope, as the knowledge gained and proof of concept will be transferable., Periodical, Internet resourceInga ISSN funna i Worldcat
Published: 2017
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156. The multiple spirals in the disk of HD100546

Author: Boccaletti, A., Lagrange, A.-M, Pantin, E., Augereau, J.-C, Quanz, S. P., Meheut, H., Boccaletti, A., Lagrange, A.-M, Pantin, E., Augereau, J.-C, Quanz, S. P., and Meheut, H.
Abstract: We report the detection of multi-armed spirals in the environment of HD 100546 using NICI at Gemini South in the Ks band. These data feature a better angular resolution and higher contrast than previous HST images, which allows to resolve the former known spiral into a multiple pattern. An analytic model with a gravitational perturber is used to fit the spiral pattern. We derived limit of detections which set constraints on the discovered forming planet
Published: 2017

157. The Return of the Mid-infrared to the VLT: News from the VISIR Upgrade

Author: Käufl, H. U., Kerber, F., Asmus, D., Baksai, P., Di Lieto, N., Duhoux, P., Heikamp, S., Christian Hummel, Ives, D., Jakob, G., Kirchbauer, J. -P, Mehrgan, L., Momany, Y., Pantin, E., Pozna, E., Riquelme, M., Sandrock, S., Siebenmorgen, R., Smette, A., Stegmeier, J., Taylor, J., Tristram, K., Valdes, G., Den Ancker, M., Weilenmann, U., Wolff, B., ITA, USA, GBR, FRA, DEU, and ESP
Subjects: Physics::Instrumentation and Detectors, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The VLT mid-infrared imager and spectrometer VISIR returns to science operations following an extended upgrade period. Among the most important modifications are: the imaging and spectroscopic detectors have been replaced with larger AQUARIUS (1024 by 1024 pixel) detector arrays; the N-band low-resolution grating has been exchanged; and support is now provided for precipitable water vapour monitoring, in order to select the best observing conditions. The AQUARIUS detectors stem from a development for very low background applications which result in excess noise under ground-based conditions. A series of interventions was needed to find a scheme that effectively exploits these detectors for ground-based use, involving the implementation of faster chopping. VISIR has been returned to service at the VLT with enhanced capabilities.
Published: 2015

158. The EChO science case

Author: Tinetti, G., Drossart, P., Eccleston, P., Hartogh, P., Isaak, K., Linder, M., Lovis, C., Micela, G., Olliver, M., Puig, L., Ribas, I., De Sio, A., Frith, J., Justtanot, K., Showman, A., Alard, C., Yurchenko, S. N., Parviainen, H., Fouqué, P., Oliva, E., Bordé, P., Balado, A., Varley, R., Di Giorgio, A., Griffin, M., Maillard, J. P., Maggio, A., Lellouch, E., Strazzulla, G., Villaver, E., Griffith, C., Stamper, R., Amado, P. J., Rezac, L., Laken, B., Hargrave, P., Orton, G., Thompson, S., Morales, J. C., Wright, G., Massi, F., Lundgaard Rasmussen, I., Altieri, F., Covino, E., Coustenis, A., Moses, J., Lithgow Bertelloni, C., Demangeon, O., Fletcher, L., Morales Calderón, M., Lo Cicero, U., López Puertas, M., Capria, M. T., Danielski, C., Luntzer, A., Bulgarelli, A., González Hernández, J., Jacquemoud, S., MacTavish, C., Mall, U., Christian Jessen, N., Sanromá, E., Femenía Castella, B., Rocchetto, M., Miles Paez, P., Allard, F., Aylward, A., Leconte, J., Palla, F., White, G., Malaguti, G., Cavarroc, C., Lammer, H., Leto, G., Batista, V., Adybekian, V., Readorn, K., Polichtchouk, I., Petrov, R., García Piquer, A., Pancrazzi, M., Gómez Leal, I., Israelian, G., Rebolo López, R., Peralta, J., Giro, E., Tecsa, M., Haigh, J., Moro Martín, A., Pezzuto, S., Piskunov, N., Agnor, C., Hollis, M., Radioti, A., De Kok, R., Gear, W., Eymet, V., Achilleos, N., Koskinen, T., Maurin, A. S., Rank Lüftinger, T., Barlow, M., Figueira, P., Affer, L., Viti, S., Machado, P., Vakili, F., Burston, R., González Merino, B., Dominic, C., Dorfi, E., Smith, A., Sitek, P., Sánchez Lavega, A., Kerschbaum, F., Hoogeeven, R., Ballerini, P., Filacchione, G., Rodler, F., Stixrude, L., Parmentier, V., Del Val Borro, M., Vandenbussche, B., Tingley, B. W., Deeg, H. J., Tabernero, H. M., Shore, S., Fossey, S., Alonso Floriano, F. J., Santos, N., Tozzi, A., Kipping, D., Maruquette, J. B., Trifoglio, M., Scandaratio, G., Scuderi, S., Hébrard, E., Lodieu, N., Forget, F., Gustin, J., Poretti, E., Murgas Alcaino, F., Sicardy, B., Stiepen, A., Hubert, B., Grodent, D., Magnes, W., Tennyson, J., Temple, J., Galand, M., Barton, E. J., Winter, B., Valdivieso, M. L., Cordier, D., Heredero, R. L., Barrado, D., Mueller Wodarg, I., Giani, E., Correira, A., Widemann, T., Ward Thompson, D., Montañés Rodríguez, P., Moya Bedon, A., Venot, O., Prinja, R., Pinfield, D., Waldmann, I., Morello, G., Lim, T., Pallé, E., Waters, R., Wawer, P., Lognonné, P., Pietrzak, R., Fernández Hernández, Maite, Winek, W., Andersen, A., Monteiro, M., Liu, S. J., Rengel, M., Tanga, P., Yelle, R., Barstow, J. K., Maldonado, J., Irshad, R., Nelson, R., Colomé, J., De Witt, J., Lanza, N., Glasse, A., Coudé du Foresto, V., Branduardi Raymont, G., Beaulieu, J. P., Claudi, R., García López, Ramón, Eales, S., López Valverde, M. A., Turrini, D., Vinatier, S., Crook, J., Damasso, M., Ramos Zapata, G., Kovács, G., Banaszkiewicz, M., Focardi, M., Mauskopf, P., Guedel, M., Rebordao, J., Stolarski, M., Adriani, A., Norgaard Nielsen, H. U., Selig, A., Peña Ramírez, K. Y., Schmider, F. X., Baffa, C., Piccioni, G., Pantin, E., Bowles, N., Hornstrup, A., Pilat Lohinger, E., Buchhave, L. A., Soret, L., Börne, P., López Morales, M., Medvedev, A., Gesa, L., Jones, H., Pérez Hoyos, S., Gerard, J. C., Bellucci, G., Morais, H., Álvarez Iglesias, C. A., Abe, L., Pinsard, F., Tessenyi, M., Blecka, M., Wawrzaszk, A., Middleton, K., Martín Torres, J., Cho, J., Berry, D., Rataj, M., Schrader, J. R., Scholz, A., Watkins, C., Abreu, M., Testi, L., Decin, L., Sánz Forcada, J., Sozzetti, A., Lagage, P. O., Ade, P., Alcala, J., Sousa, S., Espinoza Contreras, M., Swinyard, B., Dobrijévic, M., Sánchez Béjar, V. J., Krupp, N., Bakos, G., Chamberlain, S., Chadney, J., Brown, L., Iro, N., Montalto, M., Sethenadh, J., Bouy, H., Ottensamer, R., Kehoe, T., Doel, P., Delgado Mena, E., Read, P., Coates, A., Cecchi Pestellini, C., Guillot, T., Budaj, J., Selsis, F., Jarchow, C., Del Vecchio, C., Cassan, A., Burleigh, M. R., Pagano, I., Ray, T., Gambicorti, L., Biondi, D., Cerulli, R., Ciaravella, A., Watson, D., Deroo, P., Collura, A., Graczyk, R., North, C., Ramos, A. A., Waltham, D., Montes, D., Gianotti, F., Thrastarson, H., Cockell, C., Pace, E., Bryson, I., Gómez, H., Esposito, M., Azzollini, R., Allende Prieto, C., Gillon, M., Fabrizio, N., Rickman, H., Rees, J. M., Pascale, E., Luzzi, D., Bonford, B., Cole, R., Gizon, L., Licandro Goldaracena, J., Agundez, M., Lahav, O., Zapatero Osorio, M. R., Gaulme, P., Encrenaz, T., Heyrovsky, D., Guàrdia, J., Prisinzano, L., Terenzi, L., Swain, M., Grassi, D., Eiroa, C., Maxted, P., Kerins, E., Yung, Y., Irwin, P., Herrero, E., Guio, P., Boisse, I., Claret, A., Kervella, P., Heiter, U., Bézard, B., Cabral, A., Michaut, C., Giuranna, M., Hersant, F., Hueso, R., Savini, G., Snellen, I. A., Charnoz, S., Jones, G., Belmonte Avilés, J. A., Barber, R. J., Wisniowski, T., Morgante, G., University College of London [London] (UCL), 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Laboratoire des technologies de la microélectronique (LTM), Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Dpto. de Organización de Empresas, Escuela Técnica Superior de Ingeniería Industrial de Barcelona, Universitat Politècnica de Catalunya [Barcelona] (UPC), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Leicester], University of Leicester, U.S. Army Research Laboratory [Adelphi, MD] (ARL), United States Army (U.S. Army), Royal Observatory Edinburgh (ROE), University of Edinburgh, Departamento de Fisica [Aveiro], Universidade de Aveiro, SRON Netherlands Institute for Space Research (SRON), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Planetary Sciences [Tucson], University of Arizona, 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), Lunar and Planetary Laboratory [Tucson] (LPL), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), The Samuel Roberts Noble Foundation, Center for Human-Computer Interaction (HCI), Virginia Tech [Blacksburg], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), ECLIPSE 2015, 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 national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [UCL London], Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Centro de Astronomia e Astrofísica da Universidade de Lisboa (CAAUL), Universidade de Lisboa = University of Lisbon (ULISBOA), Department of Physics and Astronomy [Uppsala], Uppsala University, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Institute for Control Engineering of Machine Tools and Manufacturing Units (ISW), University of Stuttgart, Institute for Control Engineering of Machine Tools and Manufacturing Units (ISW), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford, Mullard Space Science Laboratory (MSSL), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut Curie [Paris], Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Centre for Behaviour and Evolution, Institute of Neuroscience, Newcastle University [Newcastle], foreign laboratories (FL), CERN [Genève], STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Estrutura de Missão para a Extensão da Plataforma Continental, Estrutura de Missão para a Extensão para a Extensão da Plataforma Continental, Centre for Planetary Sciences [UCL/Birkbeck] (CPS), Queen Mary University of London (QMUL), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Computational Science and Engineering Department [Daresbury] (STFC), Science & Technologie Facilities Council, Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Calar Alto Observatory, Centro Astronómico Hispano-Alemán, Department of Geoscience, Nelson Mandela University [Port Elizabeth], African Earth Observatory Network - Earth Stewardship Science Research Institute (AEON-ESSRI), Animal Genetics, Teagasc - The Agriculture and Food Development Authority (Teagasc), 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 Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Instituto Nacional de Engenharia, Tecnologia e Inovacao (INETI), Université Pierre et Marie Curie - Paris 6 (UPMC), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Università di Salerno - Dipartimento di Matematica, Università degli Studi di Salerno = University of Salerno (UNISA), Department of Genetics, University of North Carolina [Chapel Hill] (UNC), University of North Carolina System (UNC)-University of North Carolina System (UNC)-Carolina Center for the Genome Sciences, Institut de Recerca i Tecnologia Agroalimentàries = Institute of Agrifood Research and Technology (IRTA), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Department of Molecular Medicine, Università degli Studi di Padova = University of Padua (Unipd), 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 National d’Études Spatiales [Paris] (CNES), ASP 2015, 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), Institute for Astronomy [Vienna], University of Vienna [Vienna], Institut de génétique et microbiologie [Orsay] (IGM), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH = German Research Center for Artificial Intelligence (DFKI), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Dipartimento di Matematica 'Ulisse Dini', Università degli Studi di Firenze = University of Florence (UniFI), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Université de Rennes (UR), Imperial College London, Laboratoire Hippolyte Fizeau (FIZEAU), School of Physics and Astronomy [Cardiff], Cardiff University, Institut d'Astrophysique et de Géophysique [Liège], Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Bradford, Instituto Universitario de Electroquimica, Universidad de Alicante, Centre de recherche en éducation de Nantes (CREN), Le Mans Université (UM)-Université de Nantes - UFR Lettres et Langages (UFRLL), Université de Nantes (UN)-Université de Nantes (UN), Departamento de Fisica Aplicada [Bilbao], Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), NASA Goddard Space Flight Center (GSFC), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], Los Alamos National Laboratory (LANL), Osserv Astrofis Catania, Ist Nazl Astrofis, Centre d'Etude de l'Energie Nucléaire (SCK-CEN), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Consejo Super Invest Cient, Inst Astrofis Andalucia, ES-18080 Granada, Spain, Department of Rheumatology (LEIDEN - Rhumato), Leiden University Medical Center (LUMC), Universiteit Leiden-Universiteit Leiden, Department of Rheumatology (COIMBRA - Rhumato), Universidade de Coimbra [Coimbra], Centre Scientifique et Technique du Bâtiment (CSTB), INAF - Osservatorio Astrofisico di Arcetri (OAA), Université de Bordeaux (UB), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique des gaz et des plasmas (LPGP), Pontificia Universidad Católica de Chile (UC), Department of Computer Science [Verona] (UNIVR | DI), Università degli studi di Verona = University of Verona (UNIVR), IEB-UNIVERSITY OF BARCELONA, Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Thüringer Landessternwarte Tautenburg (TLS), Bremer Institut für Produktion und Logistik GmbH (BIBA), Universität Bremen, INAF - Osservatorio Astrofisico di Catania (OACT), Plasmon Nano-optics, Institut de Ciencies Fotoniques [Castelldefels] (ICFO), Royal Holloway [University of London] (RHUL), Hong Kong Government Environmental Protection Department, Water Policy and Science Group, National Space Agencies, 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), Max Planck Institute for Solar System Research (MPS), European Space Agency (ESA), European Space Agency, Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'Énergie Atomique et aux Énergies Alternatives (CEA) - Grenoble-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), 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), Samuel Roberts Noble Foundation, Inc., Universidade de Lisboa (ULISBOA), Polska Akademia Nauk (PAN), University of Oxford [Oxford], Max-Planck-Institut für Sonnensystemforschung (MPS), Institut Curie, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Nelson Mandela Metropolitan University [Port Elizabeth, South Africa], AEON-ESSRI African Earth Observatory Network — Earth Stewardship Science Research Institute, 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), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Instituto Nacional de Engenharia, Tecnologia e Inovacco (INETI), Physiologie de la reproduction et des comportements [Nouzilly] (PRC), Centre National de la Recherche Scientifique (CNRS)-Université de Tours-Institut Français du Cheval et de l'Equitation [Saumur]-Institut National de la Recherche Agronomique (INRA), Université Francois Rabelais [Tours], Institut Français du Cheval et de l'Equitation, Università degli Studi di Salerno (UNISA), IRTA, Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), Universita degli Studi di Padova, Université Paris-Sud - Paris 11 (UP11)-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)-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), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH (DFKI), Universidade do Porto [Porto], Università degli Studi di Firenze [Firenze], Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Department of Earth Sciences, University College London, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre interdisciplinaire de recherche, culture, éducation, formation, travail (CIRCEFT), Université Paris 8 Vincennes-Saint-Denis (UP8)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Station biologique, Centre National de la Recherche Scientifique (CNRS), Dipartimento di Informatica [Verona], Università degli Studi di Verona, Departamento de Física e Astronomia [Porto], UMR5116, Centre Émile Durkheim (CED), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS), Clinica Neurologica, Università degli Studi di Perugia (UNIPG), Rebordao, J. [0000-0002-7418-0345], Kerschbaum, F. [0000-0001-6320-0980], Abreu, M. [0000-0002-0716-9568], Tabernero, H. [0000-0002-8087-4298], López Puertas, M. [0000-0003-2941-7734], Jacquemoud, S. [0000-0002-1500-5256], Tennyson, J. [0000-0002-4994-5238], Focardi, M. [0000-0002-3806-4283], Leto, G. [0000-0002-0040-5011], Lodieu, N. [0000-0002-3612-8968], Tinetti, G. [0000-0001-6058-6654], Sanroma, E. [0000-0001-8859-7937], Poretti, E. [0000-0003-1200-0473], Deeg, H. [0000-0003-0047-4241], Grassi, D. [0000-0003-1653-3066], Piccioni, G. [0000-0002-7893-6808], Ribas, I. [0000-0002-6689-0312], Coates, A. [0000-0002-6185-3125], García Ramón, J. [0000-0002-8204-6832], Bouy, H. [0000-0002-7084-487X[, Lognonne, P. [0000-0002-1014-920X], Demangeon, O. [0000-0001-7918-0355], Morales, J. C. [0000-0003-0061-518X], Ray, T. [0000-0002-2110-1068], Guio, P. [0000-0002-1607-5862], Tanga, P. [0000-0002-2718-997X], Prisinzano, L. [0000-0002-8893-2210], Barstow, J. [0000-0003-3726-5419], Balado, A. [0000-0003-4268-2516], Lithgow Bertelloni, C. [0000-0003-0924-6587], Barton, E. [0000-0001-5945-9244], Delgado, M. E. [0000-0003-4434-2195], Affer, L. [0000-0001-5600-3778], Ciaravella, A. [0000-0002-3127-8078], Barrado Navascues, D. [0000-0002-5971-9242], Figueira, P. [0000-0001-8504-283X], Covino, E. [0000-0002-6187-6685], Venot, O. [0000-0003-2854-765X], Cabral, A. [0000-0002-9433-871X], Watson, D. [0000-0002-4465-8264], Morales Calderon, M. [0000-0001-9526-9499], Ward Thompson, D. [0000-0003-1140-2761], Rebolo, R. [0000-0003-3767-7085], López Valverde, M. A. [0000-0002-7989-4267], Gillon, M. [0000-0003-1462-7739], Morgante, G. [0000-0001-9234-7412], Zapatero Osorio, M. R. [0000-0001-5664-2852], Bulgarelli, A. [0000-0001-6347-0649], Pena Ramírez, K. [0000-0002-5855-401X], Galand, M. [0000-0001-5797-914X], Pancrazzi, M. [0000-0002-3789-2482], Malaguti, G. [0000-0001-9872-3378], Sánchez Lavega, A. [0000-0001-7234-7634], Waldmann, I. [0000-0002-4205-5267], Kovacs, G. [0000-0002-2365-2330], Guillot, T. [0000-0002-7188-8428], Turrini, D. [0000-0002-1923-7740], Altieri, F. [0000-0002-6338-8300], Bellucci, G. [0000-0003-0867-8679], Baffa, C. [0000-0002-4935-100X], Olivia, E. [0000-0002-9123-0412], Selsis, F. [0000-0001-9619-5356], Scuderi, Salvatore [0000-0002-8637-2109], Hersant, F. [0000-0002-2687-7500], Gear, W. [0000-0001-6789-6196], Damasso, M. [0000-0001-9984-4278], Tizzi, A. [0000-0002-6725-3825], Pinfield, D. [0000-0002-7804-4260], Kipping, D. [0000-0002-4365-7366], Maldonado, J. [0000-0002-4282-1072], Pace, E. [0000-0001-5870-1772], Burleigh, M. [0000-0003-0684-7803], Monteiro, M. [0000-0001-5644-0898], Pilat Lohinger, E. [0000-0002-5292-1923], Chadney, J. [0000-0002-5174-2114], Moro Martín, A. [0000-0001-9504-8426], Claret, A. [0000-0002-4045-8134], Gómez, H. [0000-0003-3398-0052], Maldonado, J. [0000-0002-2218-5689], Michaut, C. [0000-0002-2578-0117], Hornstrup, A. [0000-0002-3363-0936], Scholz, A. [0000-0001-8993-5053], Irwin, P. [0000-0002-6772-384X], Bezard, B. [0000-0002-5433-5661], López Heredero, R. [0000-0002-2197-8388], Sanz Forcada, J. [0000-0002-1600-7835], Danielski, C. [0000-0002-3729-2663], Sousa, S. [0000-0001-9047-2965], Medved, A. [0000-0003-2713-8977], Bakos, G. [0000-0001-7204-6727], Ade, P. [0000-0002-5127-0401], Vandenbussche, B. [0000-0002-1368-3109], Martín Torres, J. [0000-0001-6479-2236], Correira, A. [0000-0002-8946-8579], Haigh, J. [0000-0001-5504-4754], Scandariato, G. [0000-0003-2029-0626], Guedel, M. [0000-0001-9818-0588], Sánchez Bejar, V. [0000-0002-5086-4232], Rodríguez, P. [0000-0002-6855-9682], Piskunov, N. [0000-0001-5742-7767], Adibekyan, V. [0000-0002-0601-6199], Pérez Hoyos, S. [0000-0001-9797-4917], Kervella, P. [0000-0003-0626-1749], Pascale, E. [0000-0002-3242-8154], Claudi, R. [0000-0001-7707-5105], Filacchione, G. [0000-0001-9567-0055], Rickman, H. [0000-0002-9603-6619], Amado, P. J. [0000-0002-8388-6040], Maggio, A. [0000-0001-5154-6108], Agundez, M. [0000-0003-3248-3564], Montes, D. [0000-0002-7779-238X], Fletcher, L. [0000-0001-5834-9588], Stixrude, L. [0000-0003-3778-2432], Morais, M. H. [0000-0001-5333-2736], Hueso, R. [0000-0003-0169-123X], Yurchenko, S. [0000-0001-9286-9501], Rataj, M. [0000-0002-2978-9629], Pérez Hoyos, S. [0000-0002-2587-4682], Santos, N. [0000-0003-4422-2919], Peralta, J. [0000-0002-6823-1695], Budaj, J. [0000-0002-9125-7340], Barlow, M. [0000-0002-3875-1171], Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidade do Porto, Università degli Studi di Firenze = University of Florence [Firenze] (UNIFI), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), University of Verona (UNIVR), Universidade do Porto-Universidade do Porto, Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université de Nantes - UFR Lettres et Langages (UFRLL), Université de Nantes (UN)-Université de Nantes (UN)-Le Mans Université (UM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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)-Centre National de la Recherche Scientifique (CNRS), Institut National de la Recherche Agronomique (INRA)-Institut Français du Cheval et de l'Equitation [Saumur]-Université de Tours-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Firenze = University of Florence [Firenze], 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, University College of London [London] ( UCL ), 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 Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Max Planck Institute for Solar System Research ( MPS ), School of Physics & Astronomy, European Space Agency ( ESA ), INAF - Osservatorio Astronomico di Palermo ( OAPa ), Istituto Nazionale di Astrofisica ( INAF ), Laboratoire des technologies de la microélectronique ( LTM ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Microélectronique, Electromagnétisme et Photonique - Laboratoire d'Hyperfréquences et Caractérisation ( IMEP-LAHC ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut polytechnique de Grenoble - Grenoble Institute of Technology ( Grenoble INP ) -Institut National Polytechnique de Grenoble ( INPG ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ), Universidad Politécnica de Cataluña, U.S. Army Research Laboratory [Adelphi, MD] ( ARL ), United States Army ( U.S. Army ), Royal Observatory Edinburgh ( ROE ), SRON Netherlands Institute for Space Research ( SRON ), Laboratoire de Météorologie Dynamique (UMR 8539) ( LMD ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -École polytechnique ( X ) -École des Ponts ParisTech ( ENPC ) -Centre National de la Recherche Scientifique ( CNRS ) -Département des Géosciences - ENS Paris, École normale supérieure - Paris ( ENS Paris ) -École normale supérieure - Paris ( ENS Paris ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( 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 ), Lunar and Planetary Laboratory [Tucson], Space Research Institute of Austrian Academy of Sciences ( IWF ), Austrian Academy of Sciences ( OeAW ), 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 ), Center for Human-Computer Interaction ( HCI ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), University of Hertfordshire [Hatfield] ( UH ), 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 national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Atmosphérique et Planétaire ( LPAP ), Centro de Astronomia e Astrofísica da Universidade de Lisboa ( CAAUL ), Universidade de Lisboa ( ULISBOA ), Space Research Centre [Warsaw] ( CBK ), Polska Akademia Nauk ( PAN ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), Mullard Space Science Laboratory ( MSSL ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Instituut voor Sterrenkunde, Katholieke Universiteit Leuven ( KU Leuven ), foreign laboratories ( FL ), STFC Rutherford Appleton Laboratory ( RAL ), Science and Technology Facilities Council ( STFC ), Centre for Planetary Sciences [UCL/Birkbeck] ( CPS ), Queen Mary University of London ( QMUL ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Dark Cosmology Center, Niels Bohr Institute, University of Copenhagen ( KU ), Computational Science and Engineering Department [Daresbury] ( STFC ), LAEX, Depto. Astrofísica, Centro de Astrobiología, Nelson Mandela Metropolitan University, Nelson Mandela Metropolitan University [Port Elizabeth, South Africa]-Nelson Mandela Metropolitan University [Port Elizabeth, South Africa], Teagasc, Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Fraunhofer-Institute for Applied Solid-State Physics (IAF), Centro de Astrobiologia [Madrid] ( CAB ), Instituto Nacional de Técnica Aeroespacial ( INTA ) -Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Instituto Nacional de Engenharia, Tecnologia e Inovacco ( INETI ), INETI, Université Pierre et Marie Curie - Paris 6 ( UPMC ), Physiologie de la reproduction et des comportements [Nouzilly] ( PRC ), Institut National de la Recherche Agronomique ( INRA ) -Institut Français du Cheval et de l'Equitation [Saumur]-Université de Tours-Centre National de la Recherche Scientifique ( CNRS ), Università degli Studi di Salerno ( UNISA ), The University of North Carolina at Chapel Hill-Carolina Center for the Genome Sciences, Laboratoire d'astrophysique de l'observatoire de Besançon ( LAOB ), Université de Franche-Comté ( UFC ), Universita degli Studi di Padova = University of Padua = Université de Padoue, 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'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 génétique et microbiologie [Orsay] ( IGM ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH ( DFKI ), Consejo Nacional de Investigaciones Científicas y Técnicas ( CONICET ), Centro de Astrofísica da Universidade do Porto ( CAUP ), Institut Universitaire de France ( IUF ), Ministère de l'Éducation nationale, de l’Enseignement supérieur et de la Recherche ( M.E.N.E.S.R. ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ), Laboratoire Hippolyte Fizeau ( FIZEAU ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Istituto di Fisica dello Spazio Interplanetario CNR (IFSI), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de recherche en éducation de Nantes ( CREN ), Université de Nantes ( UN ), Universidad del Pais Vasco / Euskal Herriko Unibertsitatea ( UPV/EHU ), NASA Goddard Space Flight Center ( GSFC ), Onsala Space Observatory ( OSO ), Los Alamos National Laboratory ( LANL ), Centre d'Etude de l'Energie Nucléaire ( SCK-CEN ), Institut de Physique du Globe de Paris ( IPGP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Department of Rheumatology ( LEIDEN - Rhumato ), Department of Rheumatology ( COIMBRA - Rhumato ), Centre Scientifique et Technique du Bâtiment ( CSTB ), INAF - Osservatorio Astrofisico di Arcetri ( OAA ), Centre interdisciplinaire de recherche, culture, éducation, formation, travail ( CIRCEFT ), Université Paris 8 Vincennes-Saint-Denis ( UP8 ) -Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ), Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de physique des gaz et des plasmas ( LPGP ), Pontificia Universidad Católica de Chile, Thüringer Landessternwarte Tautenburg ( TLS ), BIBA Bremer Institut für Produktion und Logistik GmbH, Centre Émile Durkheim ( CED ), Université de Bordeaux ( UB ) -Sciences Po-Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Sciences Po-Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astrofisico di Catania ( OACT ), Institut de Ciencies Fotoniques [Castelldefels] ( ICFO ), Università di Perugia, Royal Holloway [University of London] ( RHUL ), and Low Energy Astrophysics (API, FNWI)
Subjects: Astrofísica, Solar System, Computer science, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], HOT-JUPITER ATMOSPHERES, 7. Clean energy, Space missions, law.invention, Astronomi, astrofysik och kosmologi, Planet, law, Observatory, Astronomy, Astrophysics and Cosmology, Transit (astronomy), Atmospheric science, Exoplanets, IR astronomy, Spectroscopy, Astronomy and Astrophysics, Space and Planetary Science, QC, QB, Eclipse, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Exoplanet, GIANT PLANETS, Physical Sciences, ENERGY-BALANCE, Astrophysics::Earth and Planetary Astrophysics, Population, MU-M, FOS: Physical sciences, F500, Astronomy & Astrophysics, Telescope, INFRARED-EMISSION-SPECTRUM, education, [ SDU.ASTR ] Sciences of the Universe [physics]/Astrophysics [astro-ph], EXTRASOLAR PLANET ATMOSPHERE, Science & Technology, Astronomy, EXOPLANET HD 189733B, HUBBLE-SPACE-TELESCOPE, Astronomía, TRANSMISSION SPECTROSCOPY, 0201 Astronomical And Space Sciences, 13. Climate action, WATER-VAPOR, astro-ph.EP, Astrophysics - Earth and Planetary Astrophysics
Abstract: The discovery of almost 2000 exoplanets has revealed an unexpectedly diverse planet population. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? What causes the exceptional diversity observed as compared to the Solar System? EChO (Exoplanet Characterisation Observatory) has been designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large and diverse planet sample within its four-year mission lifetime. EChO can target the atmospheres of super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300K-3000K) of F to M-type host stars. Over the next ten years, several new ground- and space-based transit surveys will come on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on finding bright, nearby systems. The current rapid rate of discovery would allow the target list to be further optimised in the years prior to EChO's launch and enable the atmospheric characterisation of hundreds of planets. Placing the satellite at L2 provides a cold and stable thermal environment, as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. A 1m class telescope is sufficiently large to achieve the necessary spectro-photometric precision. The spectral coverage (0.5-11 micron, goal 16 micron) and SNR to be achieved by EChO, thanks to its high stability and dedicated design, would enable a very accurate measurement of the atmospheric composition and structure of hundreds of exoplanets., Comment: 50 pages, 30 figures. Experimental Astronomy
Published: 2015
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159. Extreme Conditions in a Close Analog to the Young Solar System: Herschel Observation is an element of Eridani

Author: Greaves, J. S., Sibthorpe, B., Acke, B., Pantin, E. E., Vandenbussche, B., Olofsson, G., Dominik, C., Barlow, M. J., Bendo, G. J., Blommaert, J. A. D. L., Brandeker, A., de Vries, B. L., Dent, W. R. F., Di Francesco, J., Fridlund, M., Gear, W. K., Harvey, P. M., Hogerheijde, M. R., Holland, W. S., Ivison, R. J., Liseau, R., Matthews, B. C., Pilbratt, G. L., Walker, H. J., Waelkens, C., Physics, Astrophysics, and Astronomy and Astrophysics Research Group
Subjects: planet-disk interactions, stars: individual (is an element of Eridani), circumstellar matter
Abstract: Far-infrared Herschel images of the epsilon Eridani system, seen at a fifth of the Sun's present age, resolve two belts of debris emission. Fits to the 160 ?m PACS image yield radial spans for these belts of 12-16 and 54-68 AU. The south end of the outer belt is ?10% brighter than the north end in the PACS+SPIRE images at 160, 250, and 350 ?m, indicating a pericenter glow attributable to a planet "c." From this asymmetry and an upper bound on the offset of the belt center, this second planet should be mildly eccentric (ec ? 0.03-0.3). Compared to the asteroid and Kuiper Belts of the young Sun, the epsilon Eri belts are intermediate in brightness and more similar to each other, with up to 20 km sized collisional fragments in the inner belt totaling ?5% of an Earth mass. This reservoir may feed the hot dust close to the star and could send many impactors through the Habitable Zone, especially if it is being perturbed by the suspected planet epsilon Eri b, at semi-major axis ?3 AU.
Published: 2014

160. Herschel detects oxygen in the beta Pictoris debris disk

Author: Brandeker, Alexis, Cataldi, Gianni, Olofsson, Göran, Vandenbussche, B., Acke, B., Barlow, M. J., Blommaert, J. A. D. L., Cohen, M., Dent, W. R. F., Dominik, C., Di Francesco, J., Fridlund, M., Gear, W. K., Glauser, A. M., Greaves, J. S., Harvey, P. M., Heras, A. M., Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Leeks, S. J., Lim, T. L., Liseau, R., Matthews, B. C., Pantin, E., Pilbratt, G. L., Royer, P., Sibthorpe, B., Waelkens, C., Walker, H. J., Brandeker, Alexis, Cataldi, Gianni, Olofsson, Göran, Vandenbussche, B., Acke, B., Barlow, M. J., Blommaert, J. A. D. L., Cohen, M., Dent, W. R. F., Dominik, C., Di Francesco, J., Fridlund, M., Gear, W. K., Glauser, A. M., Greaves, J. S., Harvey, P. M., Heras, A. M., Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Leeks, S. J., Lim, T. L., Liseau, R., Matthews, B. C., Pantin, E., Pilbratt, G. L., Royer, P., Sibthorpe, B., Waelkens, C., and Walker, H. J.
Abstract: The young star beta Pictoris is well known for its dusty debris disk produced through collisional grinding of planetesimals, kilometre-sized bodies in orbit around the star. In addition to dust, small amounts of gas are also known to orbit the star; this gas is likely the result of vaporisation of violently colliding dust grains. The disk is seen edge on and from previous absorption spectroscopy we know that the gas is very rich in carbon relative to other elements. The oxygen content has been more difficult to assess, however, with early estimates finding very little oxygen in the gas at a C/O ratio that is 20x higher than the cosmic value. A C/O ratio that high is difficult to explain and would have far-reaching consequences for planet formation. Here we report on observations by the far-infrared space telescope Herschel, using PACS, of emission lines from ionised carbon and neutral oxygen. The detected emission from C+ is consistent with that previously reported observed by the HIFI instrument on Herschel, while the emission from O is hard to explain without assuming a higher density region in the disk, perhaps in the shape of a clump or a dense torus required to sufficiently excite the O atoms. A possible scenario is that the C/O gas is produced by the same process responsible for the CO clump recently observed by the Atacama Large Millimeter/submillimeter Array in the disk and that the redistribution of the gas takes longer than previously assumed. A more detailed estimate of the C/O ratio and the mass of O will have to await better constraints on the C/O gas spatial distribution.
Published: 2016
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161. An overview of the mid-infrared spectro-interferometer MATISSE: science, concept, and current status

Author: Matter, A., additional, Lopez, B., additional, Antonelli, P., additional, Lehmitz, M., additional, Bettonvil, F., additional, Beckmann, U., additional, Lagarde, S., additional, Jaffe, W., additional, Petrov, R., additional, Berio, P., additional, Millour, F., additional, Robbe-Dubois, S., additional, Glindemann, A., additional, Bristow, P., additional, Schoeller, M., additional, Lanz, T., additional, Henning, T., additional, Weigelt, G., additional, Heininger, M., additional, Morel, S., additional, Cruzalebes, P., additional, Meisenheimer, K., additional, Hofferbert, R., additional, Wolf, S., additional, Bresson, Y., additional, Agocs, T., additional, Allouche, F., additional, Augereau, J.-C., additional, Avila, G., additional, Bailet, C., additional, Behrend, J., additional, van Belle, G., additional, Berger, J.-P., additional, van Boekel, R., additional, Bourget, P., additional, Brast, R., additional, Clausse, J.-M., additional, Connot, C., additional, Conzelmann, R., additional, Csepany, G., additional, Danchi, W. C., additional, Delbo, M., additional, Dominik, C., additional, van Duin, A., additional, Elswijk, E., additional, Fantei, Y., additional, Finger, G., additional, Gabasch, A., additional, Gonté, F., additional, Graser, U., additional, Guitton, F., additional, Guniat, S., additional, De Haan, M., additional, Haguenauer, P., additional, Hanenburg, H., additional, Hofmann, K.-H., additional, Hogerheijde, M., additional, ter Horst, R., additional, Hron, J., additional, Hummel, C, additional, Isderda, J., additional, Ives, D., additional, Jakob, G., additional, Jasko, A., additional, Jolley, P., additional, Kiraly, S., additional, Kragt, J., additional, Kroener, T., additional, Kroes, G., additional, Kuindersma, S., additional, Labadie, L., additional, Laun, W., additional, Leinert, C., additional, Lizon, J.-L., additional, Lucuix, C., additional, Marcotto, A., additional, Martinache, F., additional, Martinot-Lagarde, G., additional, Mauclert, N., additional, Mehrgan, L., additional, Meilland, A., additional, Mellein, M., additional, Menardi, S., additional, Merand, A., additional, Neumann, U., additional, Nussbaum, E., additional, Ottogalli, S., additional, Palsa, R., additional, Panduro, J., additional, Pantin, E., additional, Percheron, I., additional, Phan Duc, T., additional, Pott, J.-U., additional, Pozna, E., additional, Roelfsema, R., additional, Rupprecht, G., additional, Schertl, D., additional, Schmidt, C., additional, Schuil, M., additional, Spang, A., additional, Stegmeier, J., additional, Tromp, N., additional, Vakili, F., additional, Vannier, M., additional, Wagner, K., additional, Venema, L., additional, and Woillez, J., additional
Published: 2016
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162. Herscheldetects oxygen in theβPictoris debris disk

Author: Brandeker, A., primary, Cataldi, G., additional, Olofsson, G., additional, Vandenbussche, B., additional, Acke, B., additional, Barlow, M. J., additional, Blommaert, J. A. D. L., additional, Cohen, M., additional, Dent, W. R. F., additional, Dominik, C., additional, Di Francesco, J., additional, Fridlund, M., additional, Gear, W. K., additional, Glauser, A. M., additional, Greaves, J. S., additional, Harvey, P. M., additional, Heras, A. M., additional, Hogerheijde, M. R., additional, Holland, W. S., additional, Huygen, R., additional, Ivison, R. J., additional, Leeks, S. J., additional, Lim, T. L., additional, Liseau, R., additional, Matthews, B. C., additional, Pantin, E., additional, Pilbratt, G. L., additional, Royer, P., additional, Sibthorpe, B., additional, Waelkens, C., additional, and Walker, H. J., additional
Published: 2016
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163. 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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164. Trapping planets in an evolving protoplanetary disk: preferred time, locations, and planet mass

Author: Baillié, K., primary, Charnoz, S., additional, and Pantin, E., additional
Published: 2016
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165. Gas lines from the 5-Myr old optically thin disk around HD 141569A

Author: Thi, W.-F., Pinte, C., Pantin, E., Augereau, J. C., Meeus, G., Ménard, F., Martin-Zaïdi, C., Woitke, P., Riviere-Marichalar, P., Kamp, I., Carmona, A., Sandell, G., Eiroa, C., Dent, W., Montesinos, B., Aresu, G., Meijerink, R., Spaans, M., White, G.J., Ardila, D., Lebreton, J., Mendigutía, I., Brittain, 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), 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), 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 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), and 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)
Subjects: astrochemistry, protoplanetary disks, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, stars: pre-main sequence, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: Context. The gas- and dust dissipation processes in disks around young stars remain uncertain despite numerous studies. At the distance of ~99-116 pc, HD 141569A is one of the nearest HerbigAe stars that is surrounded by a tenuous disk, probably in transition between a massive primordial disk and a debris disk. Atomic and molecular gases have been found in the structured 5-Myr old HD 141569A disk, making HD 141569A the perfect object within which to directly study the gaseous atomic and molecular component. \ud Aims. We wish to constrain the gas and dust mass in the disk around HD 141569A. \ud Methods. We observed the fine-structure lines of OI at 63 and 145 μm and the CII line at 157 μm with the PACS instrument onboard the Herschel Space Telescope as part of the open-time large program GASPS. We complemented the atomic line observations with archival Spitzer spectroscopic and photometric continuum data, a ground-based VLT-VISIR image at 8.6 μm, and 12CO fundamental ro-vibrational and pure rotational J = 3-2 observations. We simultaneously modeled the continuum emission and the line fluxes with the Monte Carlo radiative transfer code MCFOST and the thermo-chemical code ProDiMo to derive the disk gas- and dust properties assuming no dust settling. \ud Results. The models suggest that the oxygen lines are emitted from the inner disk around HD 141569A, whereas the [CII] line emission is more extended. The CO submillimeter flux is emitted mostly by the outer disk. Simultaneous modeling of the photometric and line data using a realistic disk structure suggests a dust mass derived from grains with a radius smaller than 1 mm of ~2.1 × 10-7M⊙ and from grains with a radius of up to 1 cm of 4.9 × 10-6M⊙. We constrained the polycyclic aromatic hydrocarbons (PAH) mass to be between 2 × 10-11 and 1.4 × 10-10M⊙ assuming circumcircumcoronene (C150H30) as the representative PAH. The associated PAH abundance relative to hydrogen is lower than those found in the interstellar medium (3 × 10-7) by two to three orders of magnitude. The disk around HD 141569A is less massive in gas (2.5 to 4.9 × 10-4M⊙ or 67 to 164 M⊕) and has a flat opening angle (\ud Conclusions. We constrained simultaneously the silicate dust grain, PAH, and gas mass in a ~5-Myr old Herbig Ae disk. The disk-averaged gas-to-dust-mass is most likely around 100, which is the assumed value at the disk formation despite the uncertainties due to disagreements between the different gas tracers. If the disk was originally massive, the gas and the dust would have dissipated at the same rate.
Published: 2014
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166. GASPS—A Herschel Survey of Gas and Dust in Protoplanetary Disks: Summary and Initial Statistics: Summary and Initial Statistics

Author: Dent, W. R. F., Thi, W. F., Kamp, I., Williams, J. P., Menard, F., Andrews, S., Ardila, D., Aresu, G., Augereau, J. -C., Barrado y Navascues, D., Brittain, S., Carmona, A., Ciardi, D., Danchi, W., Donaldson, J., Duchene, G., Eiroa, C., Fedele, D., Grady, C., de Gregorio-Molsalvo, I., Howard, C., Huelamo, N., Krivov, A., Lebreton, J., Liseau, R., Martin-Zaidi, C., Mathews, G., Meeus, G., Mendigutia, I., Montesinos, B., Morales-Calderon, M., Mora, A., Nomura, H., Pantin, E., Pascucci, I., Phillips, N., Pinte, C., Podio, L., Ramsay, S. K., Riaz, B., Riviere-Marichalar, P., Roberge, A., Sandell, G., Solano, E., Tilling, I., Torrelles, J. M., Vandenbusche, B., Vicente, S., White, G. J., Woitke, P., Astronomy, and Kapteyn Astronomical Institute
Subjects: AURIGA MOLECULAR CLOUD, PICTORIS MOVING GROUP, TUCANA-HOROLOGIUM ASSOCIATION, X-RAY-EMISSION, HERBIG AE/BE SYSTEMS, LOW-MASS PROTOSTARS, SPITZER-MIPS OBSERVATIONS, TW-HYDRAE ASSOCIATION, MAIN-SEQUENCE STARS, ETA-CHAMAELEONTIS CLUSTER
Abstract: We describe a large-scale far-infrared line and continuum survey of protoplanetary disk through to young debris disk systems carried out using the ACS instrument on the Herschel Space Observatory. This Open Time Key program, known as GASPS (Gas Survey of Protoplanetary Systems), targeted ~250 young stars in narrow wavelength regions covering the [OI] fine structure line at 63 μm the brightest far-infrared line in such objects. A subset of the brightest targets were also surveyed in [OI]145 μm, [CII] at 157 μm, as well as several transitions of H2O and high-excitation CO lines at selected wavelengths between 78 and 180 μm. Additionally, GASPS included continuum photometry at 70, 100 and 160 μm, around the peak of the dust emission. The targets were SED Class II-III T Tauri stars and debris disks from seven nearby young associations, along with a comparable sample of isolated Herbig AeBe stars. The aim was to study the global gas and dust content in a wide sample of circumstellar disks, combining the results with models in a systematic way. In this overview paper we review the scientific aims, target selection and observing strategy of the program. We summarise some of the initial results, showing line identifications, listing the detections, and giving a first statistical study of line detectability. The [OI] line at 63 μm was the brightest line seen in almost all objects, by a factor of ~10. Overall [OI]63 μm detection rates were 49%, with 100% of HAeBe stars and 43% of T Tauri stars detected. A comparison with published disk dust masses (derived mainly from sub-mm continuum, assuming standard values of the mm mass opacity) shows a dust mass threshold for [OI]63 μm detection of ~10-5 Msolar. Normalising to a distance of 140 pc, 84% of objects with dust masses >=10-5 Msolar can be detected in this line in the present survey; 32% of those of mass 10-6-10-5 Msolar, and only a very small number of unusual objects with lower masses can be detected. This is consistent with models with a moderate UV excess and disk flaring. For a given disk mass, [OI] detectability is lower for M stars compared with earlier spectral types. Both the continuum and line emission was, in most systems, spatially and spectrally unresolved and centred on the star, suggesting that emission in most cases was from the disk. Approximately 10 objects showed resolved emission, most likely from outflows. In the GASPS sample, [OI] detection rates in T Tauri associations in the 0.3-4 Myr age range were ~50%. For each association in the 5-20 Myr age range, ~2 stars remain detectable in [OI]63 μm, and no systems were detected in associations with age >20 Myr. Comparing with the total number of young stars in each association, and assuming a ISM-like gas/dust ratio, this indicates that ~18% of stars retain a gas-rich disk of total mass ~1 MJupiter for 1-4 Myr, 1-7% keep such disks for 5-10 Myr, but none are detected beyond 10-20 Myr. The brightest [OI] objects from GASPS were also observed in [OI]145 μm, [CII]157 μm and CO J = 18 - 17, with detection rates of 20-40%. Detection of the [CII] line was not correlated with disk mass, suggesting it arises more commonly from a compact remnant envelope.
Published: 2013

167. Herschel HIFI observations of ionised carbon in the �� Pictoris debris disk

Author: Cataldi, G., Brandeker, A., Olofsson, G., Larsson, B., Liseau, R., Blommaert, J., Fridlund, M., Ivison, R., Pantin, E., Sibthorpe, B., Vandenbussche, B., and Wu, Y.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Context: The dusty debris disk around the $\sim$20 Myr old main-sequence A-star �� Pictoris is known to contain gas. Evidence points towards a secondary origin of the gas as opposed to being a direct remnant form the initial protoplanetary disk, although the dominant gas production mechanism is so far not identified. The origin of the observed overabundance of C and O compared to solar abundances of metallic elements, e.g. Na and Fe, is also unclear. Aims: Our goal is to constrain the spatial distribution of C in the disk, and thereby the gas origin and its abundance pattern. Methods: We used the HIFI instrument onboard Herschel to observe and spectrally resolve CII emission at 158 $��$m from the �� Pic debris disk. Assuming Keplerian rotation, we use the spectrally resolved line profile to constrain the spatial distribution of the gas. Results: We show that most of the gas is located around $\sim$100 AU or beyond. We estimate a total C gas mass of $1.3\times10^{-2}$ M$_\oplus$. The data suggest that more gas is located on the southwest side of the disk than on the northeast side. The data are consistent with the hypothesis of a well-mixed gas (constant C/Fe ratio throughout the disk). Assuming instead a spatial profile expected from a simplified accretion disk model, we found it to give a significantly worse fit to the observations. Conclusions: Since the bulk of the gas is found outside 30 AU, we argue that the cometary objects known as "falling evaporating bodies" are unlikely to be the dominant source of gas; production from grain-grain collisions or photodesorption seems more likely. The incompatibility of the observations with a simplified accretion disk model could favour a preferential depletion explanation for the overabundance of C and O. More stringent constraints on the spatial distribution will be available from ALMA observations of CI at 609 $��$m., 10 pages, 7 figures, published in A&A. v2: Revised section 5.4 and figure 6, results unchanged. Changed x- and y-axis of figure 5. Some other minor changes. Fixed typos v3, v4: Language correction, some typos
Published: 2013
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168. EChO

Author: Tinetti, G, Beaulieu, JP, Henning, T, Meyer, M, Micela, G, Ribas, I, Stam, D, Swain, M, Krause, O, Ollivier, M, Pace, E, Swinyard, B, Aylward, A, van Boekel, R, Coradini, A, Encrenaz, T, Snellen, I, Zapatero-Osorio, MR, Bouwman, J, Cho, JY-K, du Foresto, VC, Guillot, T, Lopez-Morales, M, Mueller-Wodarg, I, Palle, E, Selsis, F, Sozzetti, A, Ade, PAR, Achilleos, N, Adriani, A, Agnor, CB, Afonso, C, Allende Prieto, C, Bakos, G, Barber, RJ, Barlow, M, Batista, V, Bernath, P, Bezard, B, Borde, P, Brown, LR, Cassan, A, Cavarroc, C, Ciaravella, A, Cockell, C, Coustenis, A, Danielski, C, Decin, L, De Kok, R, Demangeon, O, Deroo, P, Doel, P, Drossart, P, Fletcher, LN, Focardi, M, Forget, F, Fossey, S, Fouque, P, Frith, J, Galand, M, Gaulme, P, Gonzalez Hernandez, JI, Grasset, O, Grassi, D, Grenfell, JL, Griffin, MJ, Griffith, CA, Groezinger, U, Guedel, M, Guio, P, Hainaut, O, Hargreaves, R, Hauschildt, PH, Heng, K, Heyrovsky, D, Hueso, R, Irwin, P, Kaltenegger, L, Kervella, P, Kipping, D, Koskinen, TT, Kovacs, G, La Barbera, A, Lammer, H, Lellouch, E, Leto, G, Lopez Valverde, MA, Lopez-Puertas, M, Lovis, C, Maggio, A, Maillard, JP, Maldonado Prado, J, Marquette, JB, Martin-Torres, FJ, Maxted, P, Miller, S, Molinari, S, Montes, D, Moro-Martin, A, Moses, JI, Mousis, O, Nguyen Tuong, N, Nelson, R, Orton, GS, Pantin, E, Pascale, E, Pezzuto, S, Pinfield, D, Poretti, E, Prinja, R, Prisinzano, L, Rees, JM, Reiners, A, Samuel, B, Sanchez-Lavega, A, Sanz Forcada, J, Sasselov, D, Savini, G, Sicardy, B, Smith, A, Stixrude, L, Strazzulla, G, Tennyson, J, Tessenyi, M, Vasisht, G, Vinatier, S, Viti, S, Waldmann, I, White, GJ, Widemann, T, Wordsworth, R, Yelle, R, Yung, Y, and Yurchenko, SN
Subjects: Science & Technology, Exoplanets, EARTH-LIKE PLANETS, MU-M, Astronomy & Astrophysics, M-DWARFS, ATMOSPHERE, Space mission, EXOPLANET HD 209458B, 0201 Astronomical And Space Sciences, Physical Sciences, astro-ph.EP, UPSILON ANDROMEDAE B, TRANSMISSION SPECTRUM, PHASE CURVE, 189733B, TRANSITING EXTRASOLAR PLANET, Planetary atmospheres, astro-ph.IM
Published: 2012

169. Herschel images of Fomalhaut

Author: Acke, B., Min, M., Dominik, C., Vandenbussche, B., Sibthorpe, B., Waelkens, C., Olofsson, G., Degroote, P., Smolders, K., Pantin, E., Barlow, M. J., Blommaert, J. A. D. L., Brandeker, A., De Meester, W., Dent, W. R. F., Exter, K., Di Francesco, J., Fridlund, M., Gear, W. K., Glauser, A. M., Greaves, J. S., Harvey, P. M., Henning, Th., Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Jean, C., Liseau, R., Naylor, D. A., Pilbratt, G. L., Polehampton, E. T., Regibo, S., Royer, P., Sicilia-Aguilar, A., and Swinyard, B. M.
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Context. Fomalhaut is a young (2 ± 1 × 10^8 years), nearby (7.7 pc), 2 M⊙ star that is suspected to harbor an infant planetary system, interspersed with one or more belts of dusty debris. Aims. We present far-infrared images obtained with the Herschel Space Observatory with an angular resolution between 5.7′′ and 36.7′′ at wavelengths between 70 μm and 500 μm. The images show the main debris belt in great detail. Even at high spatial resolution, the belt appears smooth. The region in between the belt and the central star is not devoid of material; thermal emission is observed here as well. Also at the location of the star, excess emission is detected. We aim to construct a consistent image of the Fomalhaut system. Methods. We use a dynamical model together with radiative-transfer tools to derive the parameters of the debris disk. We include detailed models of the interaction of the dust grains with radiation, for both the radiation pressure and the temperature determination. Comparing these models to the spatially resolved temperature information contained in the images allows us to place strong constraints on the presence of grains that will be blown out of the system by radiation pressure. We use this to derive the dynamical parameters of the system. Results. The appearance of the belt points toward a remarkably active system in which dust grains are produced at a very high rate by a collisional cascade in a narrow region filled with dynamically excited planetesimals. Dust particles with sizes below the blow-out size are abundantly present. The equivalent of 2000 one-km-sized comets are destroyed every day, out of a cometary reservoir amounting to 110 Earth masses. From comparison of their scattering and thermal properties, we find evidence that the dust grains are fluffy aggregates, which indicates a cometary origin. The excess emission at the location of the star may be produced by hot dust with a range of temperatures, but may also be due to gaseous free-free emission from a stellar wind.
Published: 2012

170. EChO

Author: Tinetti, G., Beaulieu, J. P., Henning, T., Meyer, M., Micela, G., Ribas, I., Stam, D., Swain, M., Krause, O., Ollivier, M., Pace, E., Swinyard, B., Aylward, A., van Boekel, R., Coradini, A., Encrenaz, T., Snellen, I., Zapatero-Osorio, M. R., Bouwman, J., Cho, J. Y-K., Coudé de Foresto, V., Guillot, T., Lopez-Morales, M., Mueller-Wodarg, I., Palle, E., Selsis, F., Sozzetti, A., Ade, P. A. R., Achilleos, N., Adriani, A., Agnor, C. B., Afonso, C., Prieto, C. Allende, Bakos, G., Barber, R. J., Barlow, M., Batista, V., Bernath, P., Bézard, B., Bordé, P., Brown, L. R., Cassan, A., Cavarroc, C., Ciaravella, A., Cockell, C., Coustenis, A., Danielski, C., Decin, L., Kok, R. De, Demangeon, O., Deroo, P., Doel, P., Drossart, P., Fletcher, L. N., Focardi, M., Forget, F., Fossey, S., Fouqué, P., Frith, J., Galand, M., Gaulme, P., Hernández, J. I. González, Grasset, O., Grassi, D., Grenfell, J. L., Griffin, M. J., Griffith, C. A., Grözinger, U., Guedel, M., Guio, P., Hainaut, O., Hargreaves, R., Hauschildt, P. H., Heng, Kevin, Heyrovsky, D., Hueso, R., Irwin, P., Kaltenegger, L., Kervella, P., Kipping, D., Koskinen, T. T., Kovács, G., La Barbera, A., Lammer, H., Lellouch, E., Leto, G., Lopez Morales, M., Lopez Valverde, M. A., Lopez-Puertas, M., Lovis, C., Maggio, A., Maillard, J. P., Maldonado Prado, J., Marquette, J. B., Martin-Torres, F. J., Maxted, P., Miller, S., Molinari, S., Montes, D., Moro-Martin, A., Moses, J. I., Mousis, O., Nguyen Tuong, N., Nelson, R., Orton, G. S., Pantin, E., Pascale, E., Pezzuto, S., Pinfield, D., Poretti, E., Prinja, R., Prisinzano, L., Rees, J. M., Reiners, A., Samuel, B., Sánchez-Lavega, A., Forcada, J. Sanz, Sasselov, D., Savini, G., Sicardy, B., Smith, A., Stixrude, L., Strazzulla, G., Tennyson, J., Tessenyi, M., Vasisht, G., Vinatier, S., Viti, S., Waldmann, I., White, G. J., Widemann, T., Wordsworth, R., Yelle, R., Yung, Y., and Yurchenko, S. N.
Subjects: 530 Physics, 520 Astronomy, Astrophysics::Earth and Planetary Astrophysics
Abstract: A dedicated mission to investigate exoplanetary atmospheres represents a major milestone in our quest to understand our place in the universe by placing our Solar System in context and by addressing the suitability of planets for the presence of life. EChO—the Exoplanet Characterisation Observatory—is a mission concept specifically geared for this purpose. EChO will provide simultaneous, multi-wavelength spectroscopic observations on a stable platform that will allow very long exposures. The use of passive cooling, few moving parts and well established technology gives a low-risk and potentially long-lived mission. EChO will build on observations by Hubble, Spitzer and ground-based telescopes, which discovered the first molecules and atoms in exoplanetary atmospheres. However, EChO’s configuration and specifications are designed to study a number of systems in a consistent manner that will eliminate the ambiguities affecting prior observations. EChO will simultaneously observe a broad enough spectral region—from the visible to the mid-infrared—to constrain from one single spectrum the temperature structure of the atmosphere, the abundances of the major carbon and oxygen bearing species, the expected photochemically-produced species and magnetospheric signatures. The spectral range and resolution are tailored to separate bands belonging to up to 30 molecules and retrieve the composition and temperature structure of planetary atmospheres. The target list for EChO includes planets ranging from Jupiter-sized with equilibrium temperatures T eq up to 2,000 K, to those of a few Earth masses, with T eq \u223c 300 K. The list will include planets with no Solar System analog, such as the recently discovered planets GJ1214b, whose density lies between that of terrestrial and gaseous planets, or the rocky-iron planet 55 Cnc e, with day-side temperature close to 3,000 K. As the number of detected exoplanets is growing rapidly each year, and the mass and radius of those detected steadily decreases, the target list will be constantly adjusted to include the most interesting systems. We have baselined a dispersive spectrograph design covering continuously the 0.4–16 μm spectral range in 6 channels (1 in the visible, 5 in the InfraRed), which allows the spectral resolution to be adapted from several tens to several hundreds, depending on the target brightness. The instrument will be mounted behind a 1.5 m class telescope, passively cooled to 50 K, with the instrument structure and optics passively cooled to \u223c45 K. EChO will be placed in a grand halo orbit around L2. This orbit, in combination with an optimised thermal shield design, provides a highly stable thermal environment and a high degree of visibility of the sky to observe repeatedly several tens of targets over the year. Both the baseline and alternative designs have been evaluated and no critical items with Technology Readiness Level (TRL) less than 4–5 have been identified. We have also undertaken a first-order cost and development plan analysis and find that EChO is easily compatible with the ESA M-class mission framework.
Published: 2012
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171. Magnetic field structures in star-forming regions: mid-infrared imaging polarimetry of K3-50

Author: Wright, Christopher, Barnes, P, Li, D, Telesco, C, Tanakul, N, Marinas, N, Wright, CM, Packham, C, Pantin, E, Roche, P, Hough, J, Wright, Christopher, Barnes, P, Li, D, Telesco, C, Tanakul, N, Marinas, N, Wright, CM, Packham, C, Pantin, E, Roche, P, and Hough, J
Published: 2015

172. The EChO science case

Author: Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Isaak, Kate, Linder, Martin, Lovis, Christophe, Micela, Giusi, Ollivier, Marc, Puig, Ludovic, Ribas, Ignasi, Snellen, Ignas, Swinyard, Bruce, Allard, France, Barstow, Joanna, Cho, James, Coustenis, Athena, Cockell, Charles, Correia, Alexandre, Decin, Leen, de Kok, Remco, Deroo, Pieter, Encrenaz, Therese, Forget, Francois, Glasse, Alistair, Griffith, Caitlin, Guillot, Tristan, Koskinen, Tommi, Lammer, Helmut, Leconte, Jeremy, Maxted, Pierre, Mueller-Wodarg, Ingo, Nelson, Richard, North, Chris, Palle, Enric, Pagano, Isabella, Piccioni, Guseppe, Pinfield, David, Selsis, Franck, Sozzetti, Alessandro, Stixrude, Lars, Tennyson, Jonathan, Turrini, Diego, Zapatero-Osorio, Mariarosa, Beaulieu, Jean-Philippe, Grodent, Denis, Guedel, Manuel, Luz, David, Norgaard-Nielsen, Hans Ulrik, Ray, Tom, Rickman, Hans, Selig, Avri, Swain, Mark, Banaszkiewicz, Marek, Barlow, Mike, Bowles, Neil, Branduardi-Raymont, Graziella, du Foresto, Vincent Coude, Gerard, Jean-Claude, Gizon, Laurent, Hornstrup, Allan, Jarchow, Christopher, Kerschbaum, Franz, Kovacs, Geza, Lagage, Pierre-Olivier, Lim, Tanya, Lopez-Morales, Mercedes, Malaguti, Giuseppe, Pace, Emanuele, Pascale, Enzo, Vandenbussche, Bart, Wright, Gillian, Ramos Zapata, Gonzalo, Adriani, Alberto, Azzollini, Ruyman, Balado, Ana, Bryson, Ian, Burston, Raymond, Colome, Josep, Crook, Martin, Di Giorgio, Anna, Griffin, Matt, Hoogeveen, Ruud, Ottensamer, Roland, Irshad, Ranah, Middleton, Kevin, Morgante, Gianluca, Pinsard, Frederic, Rataj, Mirek, Reess, Jean-Michel, Savini, Giorgio, Schrader, Jan-Rutger, Stamper, Richard, Winter, Berend, Abe, L., Abreu, M., Achilleos, N., Ade, P., Adybekian, V., Affer, L., Agnor, C., Agundez, M., Alard, C., Alcala, J., Allende Prieto, C., Alonso Floriano, F. J., Altieri, F., Alvarez Iglesias, C. A., Amado, P., Andersen, A., Aylward, A., Baffa, C., Bakos, G., Ballerini, P., Banaszkiewicz, M., Barber, R. J., Barrado, D., Barton, E. J., Batista, V., Bellucci, G., Belmonte Aviles, J. A., Berry, D., Bezard, B., Biondi, D., Blecka, M., Boisse, I., Bonfond, B., Borde, P., Boerner, P., Bouy, H., Brown, L., Buchhave, L., Budaj, J., Bulgarelli, A., Burleigh, M., Cabral, A., Capria, M. T., Cassan, A., Cavarroc, C., Cecchi-Pestellini, C., Cerulli, R., Chadney, J., Chamberlain, S., Charnoz, S., Jessen, N. Christian, Ciaravella, A., Claret, A., Claudi, R., Coates, A., Cole, R., Collura, A., Cordier, D., Covino, E., Danielski, C., Damasso, M., Deeg, H. J., Delgado-Mena, E., Del Vecchio, C., Demangeon, O., De Sio, A., De Wit, J., Dobrijevic, M., Doel, P., Dominic, C., Dorfi, E., Eales, S., Eiroa, C., Espinoza Contreras, M., Esposito, M., Eymet, V., Fabrizio, N., Fernandez, M., Femena Castella, B., Figueira, P., Filacchione, G., Fletcher, L., Focardi, M., Fossey, S., Fouque, P., Frith, J., Galand, M., Gambicorti, L., Gaulme, P., Garcia Lopez, R. J., Garcia-Piquer, A., Gear, W., Gerard, J. -C, Gesa, L., Giani, E., Gianotti, F., Gillon, M., Giro, E., Giuranna, M., Gomez, H., Gomez-Leal, I., Gonzalez Hernandez, J., Gonzalez Merino, B., Graczyk, R., Grassi, D., Guardia, J., Guio, P., Gustin, J., Hargrave, P., Haigh, J., Hebrard, E., Heiter, Ulrike, Heredero, R. L., Herrero, E., Hersant, F., Heyrovsky, D., Hollis, M., Hubert, B., Hueso, R., Israelian, G., Iro, N., Irwin, P., Jacquemoud, S., Jones, G., Jones, H., Justtanont, K., Kehoe, T., Kerschbaum, F., Kerins, E., Kervella, P., Kipping, D., Koskinen, T., Krupp, N., Lahav, O., Laken, B., Lanza, N., Lellouch, E., Leto, G., Licandro Goldaracena, J., Lithgow-Bertelloni, C., Liu, S. J., Lo Cicero, U., Lodieu, N., Lognonne, P., Lopez-Puertas, M., Lopez-Valverde, M. A., Rasmussen, I. Lundgaard, Luntzer, A., Machado, P., MacTavish, C., Maggio, A., Maillard, J. -P, Magnes, W., Maldonado, J., Mall, U., Marquette, J. -B, Mauskopf, P., Massi, F., Maurin, A. -S, Medvedev, A., Michaut, C., Miles-Paez, P., Montalto, M., Montanes Rodriguez, P., Monteiro, M., Montes, D., Morais, H., Morales, J. C., Morales-Calderon, M., Morello, G., Moro Martin, A., Moses, J., Moya Bedon, A., Murgas Alcaino, F., Oliva, E., Orton, G., Palla, F., Pancrazzi, M., Pantin, E., Parmentier, V., Parviainen, H., Pena Ramirez, K. Y., Peralta, J., Perez-Hoyos, S., Petrov, R., Pezzuto, S., Pietrzak, R., Pilat-Lohinger, E., Piskunov, Nikolai, Prinja, R., Prisinzano, L., Polichtchouk, I., Poretti, E., Radioti, A., Ramos, A. A., Rank-Lueftinger, T., Read, P., Readorn, K., Rebolo Lopez, R., Rebordao, J., Rengel, M., Rezac, L., Rocchetto, M., Rodler, F., Sanchez Bejar, V. J., Lavega, A. Sanchez, Sanroma, E., Santos, N., Sanz Forcada, J., Scandariato, G., Schmider, F. -X, Scholz, A., Scuderi, S., Sethenadh, J., Shore, S., Showman, A., Sicardy, B., Sitek, P., Smith, A., Soret, L., Sousa, S., Stiepen, A., Stolarski, M., Strazzulla, G., Tabernero, H. M., Tanga, P., Tecsa, M., Temple, J., Terenzi, L., Tessenyi, M., Testi, L., Thompson, S., Thrastarson, H., Tingley, B. W., Trifoglio, M., Martin Torres, J., Tozzi, A., Turrini, D., Varley, R., Vakili, F., de Val-Borro, M., Valdivieso, M. L., Venot, O., Villaver, E., Vinatier, S., Viti, S., Waldmann, I., Waltham, D., Ward-Thompson, D., Waters, R., Watkins, C., Watson, D., Wawer, P., Wawrzaszk, A., White, G., Widemann, T., Winek, W., Wisniowski, T., Yelle, R., Yung, Y., Yurchenko, S. N., Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Isaak, Kate, Linder, Martin, Lovis, Christophe, Micela, Giusi, Ollivier, Marc, Puig, Ludovic, Ribas, Ignasi, Snellen, Ignas, Swinyard, Bruce, Allard, France, Barstow, Joanna, Cho, James, Coustenis, Athena, Cockell, Charles, Correia, Alexandre, Decin, Leen, de Kok, Remco, Deroo, Pieter, Encrenaz, Therese, Forget, Francois, Glasse, Alistair, Griffith, Caitlin, Guillot, Tristan, Koskinen, Tommi, Lammer, Helmut, Leconte, Jeremy, Maxted, Pierre, Mueller-Wodarg, Ingo, Nelson, Richard, North, Chris, Palle, Enric, Pagano, Isabella, Piccioni, Guseppe, Pinfield, David, Selsis, Franck, Sozzetti, Alessandro, Stixrude, Lars, Tennyson, Jonathan, Turrini, Diego, Zapatero-Osorio, Mariarosa, Beaulieu, Jean-Philippe, Grodent, Denis, Guedel, Manuel, Luz, David, Norgaard-Nielsen, Hans Ulrik, Ray, Tom, Rickman, Hans, Selig, Avri, Swain, Mark, Banaszkiewicz, Marek, Barlow, Mike, Bowles, Neil, Branduardi-Raymont, Graziella, du Foresto, Vincent Coude, Gerard, Jean-Claude, Gizon, Laurent, Hornstrup, Allan, Jarchow, Christopher, Kerschbaum, Franz, Kovacs, Geza, Lagage, Pierre-Olivier, Lim, Tanya, Lopez-Morales, Mercedes, Malaguti, Giuseppe, Pace, Emanuele, Pascale, Enzo, Vandenbussche, Bart, Wright, Gillian, Ramos Zapata, Gonzalo, Adriani, Alberto, Azzollini, Ruyman, Balado, Ana, Bryson, Ian, Burston, Raymond, Colome, Josep, Crook, Martin, Di Giorgio, Anna, Griffin, Matt, Hoogeveen, Ruud, Ottensamer, Roland, Irshad, Ranah, Middleton, Kevin, Morgante, Gianluca, Pinsard, Frederic, Rataj, Mirek, Reess, Jean-Michel, Savini, Giorgio, Schrader, Jan-Rutger, Stamper, Richard, Winter, Berend, Abe, L., Abreu, M., Achilleos, N., Ade, P., Adybekian, V., Affer, L., Agnor, C., Agundez, M., Alard, C., Alcala, J., Allende Prieto, C., Alonso Floriano, F. J., Altieri, F., Alvarez Iglesias, C. A., Amado, P., Andersen, A., Aylward, A., Baffa, C., Bakos, G., Ballerini, P., Banaszkiewicz, M., Barber, R. J., Barrado, D., Barton, E. J., Batista, V., Bellucci, G., Belmonte Aviles, J. A., Berry, D., Bezard, B., Biondi, D., Blecka, M., Boisse, I., Bonfond, B., Borde, P., Boerner, P., Bouy, H., Brown, L., Buchhave, L., Budaj, J., Bulgarelli, A., Burleigh, M., Cabral, A., Capria, M. T., Cassan, A., Cavarroc, C., Cecchi-Pestellini, C., Cerulli, R., Chadney, J., Chamberlain, S., Charnoz, S., Jessen, N. Christian, Ciaravella, A., Claret, A., Claudi, R., Coates, A., Cole, R., Collura, A., Cordier, D., Covino, E., Danielski, C., Damasso, M., Deeg, H. J., Delgado-Mena, E., Del Vecchio, C., Demangeon, O., De Sio, A., De Wit, J., Dobrijevic, M., Doel, P., Dominic, C., Dorfi, E., Eales, S., Eiroa, C., Espinoza Contreras, M., Esposito, M., Eymet, V., Fabrizio, N., Fernandez, M., Femena Castella, B., Figueira, P., Filacchione, G., Fletcher, L., Focardi, M., Fossey, S., Fouque, P., Frith, J., Galand, M., Gambicorti, L., Gaulme, P., Garcia Lopez, R. J., Garcia-Piquer, A., Gear, W., Gerard, J. -C, Gesa, L., Giani, E., Gianotti, F., Gillon, M., Giro, E., Giuranna, M., Gomez, H., Gomez-Leal, I., Gonzalez Hernandez, J., Gonzalez Merino, B., Graczyk, R., Grassi, D., Guardia, J., Guio, P., Gustin, J., Hargrave, P., Haigh, J., Hebrard, E., Heiter, Ulrike, Heredero, R. L., Herrero, E., Hersant, F., Heyrovsky, D., Hollis, M., Hubert, B., Hueso, R., Israelian, G., Iro, N., Irwin, P., Jacquemoud, S., Jones, G., Jones, H., Justtanont, K., Kehoe, T., Kerschbaum, F., Kerins, E., Kervella, P., Kipping, D., Koskinen, T., Krupp, N., Lahav, O., Laken, B., Lanza, N., Lellouch, E., Leto, G., Licandro Goldaracena, J., Lithgow-Bertelloni, C., Liu, S. J., Lo Cicero, U., Lodieu, N., Lognonne, P., Lopez-Puertas, M., Lopez-Valverde, M. A., Rasmussen, I. Lundgaard, Luntzer, A., Machado, P., MacTavish, C., Maggio, A., Maillard, J. -P, Magnes, W., Maldonado, J., Mall, U., Marquette, J. -B, Mauskopf, P., Massi, F., Maurin, A. -S, Medvedev, A., Michaut, C., Miles-Paez, P., Montalto, M., Montanes Rodriguez, P., Monteiro, M., Montes, D., Morais, H., Morales, J. C., Morales-Calderon, M., Morello, G., Moro Martin, A., Moses, J., Moya Bedon, A., Murgas Alcaino, F., Oliva, E., Orton, G., Palla, F., Pancrazzi, M., Pantin, E., Parmentier, V., Parviainen, H., Pena Ramirez, K. Y., Peralta, J., Perez-Hoyos, S., Petrov, R., Pezzuto, S., Pietrzak, R., Pilat-Lohinger, E., Piskunov, Nikolai, Prinja, R., Prisinzano, L., Polichtchouk, I., Poretti, E., Radioti, A., Ramos, A. A., Rank-Lueftinger, T., Read, P., Readorn, K., Rebolo Lopez, R., Rebordao, J., Rengel, M., Rezac, L., Rocchetto, M., Rodler, F., Sanchez Bejar, V. J., Lavega, A. Sanchez, Sanroma, E., Santos, N., Sanz Forcada, J., Scandariato, G., Schmider, F. -X, Scholz, A., Scuderi, S., Sethenadh, J., Shore, S., Showman, A., Sicardy, B., Sitek, P., Smith, A., Soret, L., Sousa, S., Stiepen, A., Stolarski, M., Strazzulla, G., Tabernero, H. M., Tanga, P., Tecsa, M., Temple, J., Terenzi, L., Tessenyi, M., Testi, L., Thompson, S., Thrastarson, H., Tingley, B. W., Trifoglio, M., Martin Torres, J., Tozzi, A., Turrini, D., Varley, R., Vakili, F., de Val-Borro, M., Valdivieso, M. L., Venot, O., Villaver, E., Vinatier, S., Viti, S., Waldmann, I., Waltham, D., Ward-Thompson, D., Waters, R., Watkins, C., Watson, D., Wawer, P., Wawrzaszk, A., White, G., Widemann, T., Winek, W., Wisniowski, T., Yelle, R., Yung, Y., and Yurchenko, S. N.
Abstract: The discovery of almost two thousand exoplanets has revealed an unexpectedly diverse planet population. We see gas giants in few-day orbits, whole multi-planet systems within the orbit of Mercury, and new populations of planets with masses between that of the Earth and Neptune-all unknown in the Solar System. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? How do planetary systems work and what causes the exceptional diversity observed as compared to the Solar System? The EChO (Exoplanet Characterisation Observatory) space mission was conceived to take up the challenge to explain this diversity in terms of formation, evolution, internal structure and planet and atmospheric composition. This requires in-depth spectroscopic knowledge of the atmospheres of a large and well-defined planet sample for which precise physical, chemical and dynamical information can be obtained. In order to fulfil this ambitious scientific program, EChO was designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large, diverse and well-defined planet sample within its 4-year mission lifetime. The transit and eclipse spectroscopy method, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allows us to measure atmospheric signals from the planet at levels of at least 10(-4) relative to the star. This can only be achieved in conjunction with a carefully designed stable payload and satellite platform. It is also necessary to provide broad instantaneous wavelength coverage to detect as many molecular species as possible, to probe the thermal structure of the planetary atmospheres and to correct for the contaminating effects of the stellar photosphere. This requires wavelength cove
Published: 2015
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173. The vortex coronagraph:from laboratory characterizationto on-sky operation

Author: Huby, Elsa, Absil, Olivier, Serabyn, E, Baudoz, Pierre, Delacroix, Christian, Jolivet, Aïssa, Piron, Pierre, Vargas Catalan, Ernesto, Forsberg, Pontus, Karlsson, Mikael, Carlomagno, Brunella, Ruane, G, Habraken, Serge, Gomez Gonzales, Carlos, Wertz, Olivier, Surdej, Jean, Absil, Pierre-Antoine, Christiaens, Valentin, Defrère, Denis, Girard, J, Hinz, P, Milli, Julien, Pantin, E, Van Droogenbroeck, Marc, Huby, Elsa, Absil, Olivier, Serabyn, E, Baudoz, Pierre, Delacroix, Christian, Jolivet, Aïssa, Piron, Pierre, Vargas Catalan, Ernesto, Forsberg, Pontus, Karlsson, Mikael, Carlomagno, Brunella, Ruane, G, Habraken, Serge, Gomez Gonzales, Carlos, Wertz, Olivier, Surdej, Jean, Absil, Pierre-Antoine, Christiaens, Valentin, Defrère, Denis, Girard, J, Hinz, P, Milli, Julien, Pantin, E, and Van Droogenbroeck, Marc
Published: 2015

174. Asymmetric features in the protoplanetary disk MWC758

Author: Benisty, M., Juhasz, A., Boccaletti, A., Avenhaus, H., Milli, J., Thalmann, C., Dominik, C., Pinilla, P., Buenzli, E., Pohl, A., Beuzit, J. -L., Birnstiel, T., de Boer, J., Bonnefoy, M., Chauvin, G., Christiaens, V., Garufi, A., Grady, C., Henning, T., Huelamo, N., Isella, A., Langlois, M., Menard, F., Mouillet, D., Olofsson, J., Pantin, E., Pinte, C., Pueyo, L., Benisty, M., Juhasz, A., Boccaletti, A., Avenhaus, H., Milli, J., Thalmann, C., Dominik, C., Pinilla, P., Buenzli, E., Pohl, A., Beuzit, J. -L., Birnstiel, T., de Boer, J., Bonnefoy, M., Chauvin, G., Christiaens, V., Garufi, A., Grady, C., Henning, T., Huelamo, N., Isella, A., Langlois, M., Menard, F., Mouillet, D., Olofsson, J., Pantin, E., Pinte, C., and Pueyo, L.
Abstract: The study of dynamical processes in protoplanetary disks is essential to understand planet formation. In this context, transition disks are prime targets because they are at an advanced stage of disk clearing and may harbor direct signatures of disk evolution. In this paper, we aim to derive new constraints on the structure of the transition disk MWC 758, to detect non-axisymmetric features and understand their origin. We obtained infrared polarized intensity observations of the protoplanetary disk MWC 758 with SPHERE/VLT at 1.04 microns to resolve scattered light at a smaller inner working angle (0.093") and a higher angular resolution (0.027") than previously achieved. We observe polarized scattered light within 0.53" (148 au) down to the inner working angle (26 au) and detect distinct non-axisymmetric features but no fully depleted cavity. The two small-scale spiral features that were previously detected with HiCIAO are resolved more clearly, and new features are identified, including two that are located at previously inaccessible radii close to the star. We present a model based on the spiral density wave theory with two planetary companions in circular orbits. The best model requires a high disk aspect ratio (H/r~0.20 at the planet locations) to account for the large pitch angles which implies a very warm disk. Our observations reveal the complex morphology of the disk MWC758. To understand the origin of the detected features, the combination of high-resolution observations in the submillimeter with ALMA and detailed modeling is needed., Comment: Accepted by A&A Letters
Published: 2015
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175. Very Large Telescope observations of Gomez's Hamburger: Insights into a young protoplanet candidate

Author: Berne, O., Fuente, A., Pantin, E., Bujarrabal, V., Baruteau, C., Pilleri, P., Habart, E., Menard, F., Cernicharo, J., Tielens, A., Joblin, C., Berne, O., Fuente, A., Pantin, E., Bujarrabal, V., Baruteau, C., Pilleri, P., Habart, E., Menard, F., Cernicharo, J., Tielens, A., and Joblin, C.
Abstract: Planets are thought to form in the gas and dust disks around young stars. In particular, it has been proposed that giant planets can form through the gravitational instability of massive extended disks around intermediate-mass stars. However, we still lack direct observations to constrain this mechanism. We have spatially resolved the 8.6 and 11.2 $\mu$m emission of a massive protoplanetary disk seen edge on around an A star, Gomez's Hamburger (GoHam), using VISIR at the Very Large Telescope. A compact region situated at a projected distance of $350\pm50$ AU south of the central star is found to have a reduced emission.This asymmetry is fully consistent with the presence of a cold density structure, or clump, identified in earlier CO observations, and we derive physical characteristics consistent with those observations: a mass of 0.8-11.4 Jupiter masses (for a dust-to-gas mass ratio of 0.01), a radius of about 10$^2$ astronomical units, and a local density of about $10^{7}$ cm$^{-3}$. Based on this evidence, we argue that this clump, which we call GoHam b, is a promising candidate for a young protoplanet formed by gravitational instability that might be representative of the precursors of massive planets observed around A stars, such as HR 8799 or Beta pictoris. More detailed studies at high angular resolution are needed to better constrain the physical properties of this object to confirm this proposal., Comment: 7 Pages, accepted for publication as a Letter in A&A
Published: 2015
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176. Asymmetric features in the protoplanetary disk MWC 758

Author: Benisty, M., primary, Juhasz, A., additional, Boccaletti, A., additional, Avenhaus, H., additional, Milli, J., additional, Thalmann, C., additional, Dominik, C., additional, Pinilla, P., additional, Buenzli, E., additional, Pohl, A., additional, Beuzit, J.-L., additional, Birnstiel, T., additional, de Boer, J., additional, Bonnefoy, M., additional, Chauvin, G., additional, Christiaens, V., additional, Garufi, A., additional, Grady, C., additional, Henning, T., additional, Huelamo, N., additional, Isella, A., additional, Langlois, M., additional, Ménard, F., additional, Mouillet, D., additional, Olofsson, J., additional, Pantin, E., additional, Pinte, C., additional, and Pueyo, L., additional
Published: 2015
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177. Very Large Telescope observations of Gomez’s Hamburger: Insights into a young protoplanet candidate

Author: Berné, O., primary, Fuente, A., additional, Pantin, E., additional, Bujarrabal, V., additional, Baruteau, C., additional, Pilleri, P., additional, Habart, E., additional, Ménard, F., additional, Cernicharo, J., additional, Tielens, A. G. G. M., additional, and Joblin, C., additional
Published: 2015
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178. The {\beta} Pictoris disk imaged by Herschel PACS and SPIRE

Author: Vandenbussche, B., Sibthorpe, B., Acke, B., Pantin, E., Olofsson, G., Waelkens, C., Dominik, C., Barlow, M. J., Blommaert, J. A. D. L., Bouwman, J., Brandeker, A., Cohen, M., DeMeester, W., Dent, W. R. F., Exter, K., Di Francesco, J., Fridlund, M., Gear, W. K., Glauser, A. M., Gomez, H. L., Greaves, J. S., Hargrave, P. C., Harvey, P. M., Henning, Th., Heras, A. M., Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Jean, C., Leeks, S. J., Lim, T. L., Liseau, R., Matthews, B. C., Naylor, D. A., Pilbratt, G. L., Polehampton, E. T., Regibo, S., Royer, P., Sicilia-Aguilar, A., Swinyard, B. M., Walker, H. J., and Wesson, R.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We obtained Herschel PACS and SPIRE images of the thermal emission of the debris disk around the A5V star {\beta} Pic. The disk is well resolved in the PACS filters at 70, 100, and 160 {\mu}m. The surface brightness profiles between 70 and 160 {\mu}m show no significant asymmetries along the disk, and are compatible with 90% of the emission between 70 and 160 {\mu}m originating in a region closer than 200 AU to the star. Although only marginally resolving the debris disk, the maps obtained in the SPIRE 250 - 500 {\mu}m filters provide full-disk photometry, completing the SED over a few octaves in wavelength that had been previously inaccessible. The small far-infrared spectral index ({\beta} = 0.34) indicates that the grain size distribution in the inner disk (, Comment: Accepted for publication in Astronomy&Astrophysics, Herschel First Results special issue
Published: 2010

179. Gas in Protoplanetary Discs (GASPS) 1. First results

Author: Mathews, G. S., Dent, W. R. F., Williams, J. P., Howard, C. D., Meeus, G., Riaz, B., Roberge, A., Sandell, G., Vandenbussche, B., Duch��ne, G., Kamp, I., M��nard, F., Montesinos, B., Pinte, C., Thi, W. F., Woitke, P., Alacid, J. M., Andrews, S. M., Ardila, D. R., Aresu, G., Augereau, J. C., Barrado, D., Brittain, S., Ciardi, D. R., Danchi, W., Eiroa, C., Fedele, D., Grady, C. A., de Gregorio-Monsalvo, I., Heras, A., Huelamo, N., Krivov, A., Lebreton, J., Liseau, R., Martin-Zaidi, C., Mendigut��a, I., Mora, A., Morales-Calderon, M., Nomura, H., Pantin, E., Pascucci, I., Phillips, N., Podio, L., Poelman, D. R., Ramsay, S., Rice, K., Riviere-Marichalar, P., Solano, E., Tilling, I., Walker, H., White, G. J., Wright, G., and Collaboration, the GASPS
Subjects: Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract: Context - Circumstellar discs are ubiquitous around young stars, but rapidly dissipate their gas and dust on timescales of a few Myr. The Herschel space observatory allows for the study of the warm disc atmosphere, using far-infrared spectroscopy to measure gas content and excitation conditions, and far-IR photometry to constrain the dust distribution. Aims - We aim to detect and characterize the gas content of circumstellar discs in four targets as part of the Herschel science demonstration phase. Methods - We carried out sensitive medium resolution spectroscopy and high sensitivity photometry at lambda ~60-190 micron using the Photodetector Array Camera and Spectrometer instrument on the Herschel space observatory. Results - We detect [OI] 63 micron emission from the young stars HD 169142, TW Hydrae, and RECX 15, but not HD 181327. No other lines, including [CII] 158 and [OI] 145, are significantly detected. All four stars are detected in photometry at 70 and 160 micron. Extensive models are presented in associated papers., Comments: 5 pages, 2 Postscript figures, accepted for publication in the A&A Herschel special issue
Published: 2010

180. Time evolution of snow regions and planet traps in an evolving protoplanetary disk

Author: Baillié, K., primary, Charnoz, S., additional, and Pantin, E., additional
Published: 2015
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181. The β Pictoris disk imaged by Herschel PACS and SPIRE [Letter]

Author: Vandenbussche, B., Sibthorpe, B., Acke, B., Pantin, E., Olofsson, G., Waelkens, C., Dominik, C., Barlow, M. J., Blommaert, J. A. D. L., Bouwman, J., Brandeker, A., Cohen, M., De Meester, W., Dent, W. R. F., Exter, K., Di Francesco, J., Fridlund, M., Gear, Walter Kieran, Glauser, A. M., Gomez, Haley Louise, Greaves, J. S., Hargrave, Peter Charles, Harvey, P. M., Henning, Th., Heras, A. M., Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Jean, C., Leeks, S. J., Lim, T. L., Liseau, R., Matthews, B. C., Naylor, D. A., Pilbratt, G. L., Polehampton, E. T., Regibo, S., Royer, P., Sicilia-Aguilar, A., Swinyard, B. M., Walker, H. J., and Wesson, R.
Subjects: QB
Abstract: We obtained Herschel PACS and SPIRE images of the thermal emission of the debris disk around the A5V star β Pic. The disk is well resolved in the PACS filters at 70, 100, and 160 μm. The surface brightness profiles between 70 and 160 μm show no significant asymmetries along the disk, and are compatible with 90% of the emission between 70 and 160 μm originating in a region closer than 200 AU to the star. Although only marginally resolving the debris disk, the maps obtained in the SPIRE 250–500 μm filters provide full-disk photometry, completing the SED over a few octaves in wavelength that had been previously inaccessible. The small far-infrared spectral index (β = 0.34) indicates that the grain size distribution in the inner disk (
Published: 2010

182. The �� Pictoris disk imaged by Herschel PACS and SPIRE

Author: Vandenbussche, B., Sibthorpe, B., Acke, B., Pantin, E., Olofsson, G., Waelkens, C., Dominik, C., Barlow, M. J., Blommaert, J. A. D. L., Bouwman, J., Brandeker, A., Cohen, M., DeMeester, W., Dent, W. R. F., Exter, K., Di Francesco, J., Fridlund, M., Gear, W. K., Glauser, A. M., Gomez, H. L., Greaves, J. S., Hargrave, P. C., Harvey, P. M., Henning, Th., Heras, A. M., Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Jean, C., Leeks, S. J., Lim, T. L., Liseau, R., Matthews, B. C., Naylor, D. A., Pilbratt, G. L., Polehampton, E. T., Regibo, S., Royer, P., Sicilia-Aguilar, A., Swinyard, B. M., Walker, H. J., and Wesson, R.
Subjects: FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We obtained Herschel PACS and SPIRE images of the thermal emission of the debris disk around the A5V star �� Pic. The disk is well resolved in the PACS filters at 70, 100, and 160 ��m. The surface brightness profiles between 70 and 160 ��m show no significant asymmetries along the disk, and are compatible with 90% of the emission between 70 and 160 ��m originating in a region closer than 200 AU to the star. Although only marginally resolving the debris disk, the maps obtained in the SPIRE 250 - 500 ��m filters provide full-disk photometry, completing the SED over a few octaves in wavelength that had been previously inaccessible. The small far-infrared spectral index (�� = 0.34) indicates that the grain size distribution in the inner disk (, Accepted for publication in Astronomy&Astrophysics, Herschel First Results special issue
Published: 2010
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183. Structure and composition of disks surrounding Herbig Be stars

Author: Ancker, M. van den, Acke, B., Bik, A., Bouwman, J., Dominik, C., Dullemond, K., Henning, T., Min, M., Pantin, E., Tielens, A.G.G.M., Verhoeff, A., Waelkens, C., Waters, L., and Boekel, R. van
Subjects: Research Programm of Institute for Mathematics, Astrophysics and Particle Physics, Spitzer Proposal, Astronomy
Abstract: Item does not contain fulltext
Published: 2008

184. E-ELT/METIS

Author: Brandl, B., primary, Quanz, S., additional, Feldt, M., additional, Glasse, A., additional, Guedel, M., additional, Meyer, M., additional, Pantin, E., additional, Waelkens, C., additional, Pontoppidan, K., additional, van Dishoeck, E., additional, Absil, O., additional, van Boekel, R., additional, Ratzka, T., additional, and Henning, T., additional
Published: 2015
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185. EXTREME CONDITIONS IN A CLOSE ANALOG TO THE YOUNG SOLAR SYSTEM : HERSCHEL OBSERVATIONS OF is an element of ERIDANI

Author: Greaves, J. S., Sibthorpe, B., Acke, B., Pantin, E. E., Vandenbussche, B., Olofsson, Göran, Dominik, C., Barlow, M. J., Bendo, G. J., Blommaert, J. A. D. L., Brandeker, Alexis, de Vries, Bernard L., Dent, W. R. F., Di Francesco, J., Fridlund, M., Gear, W. K., Harvey, P. M., Hogerheijde, M. R., Holland, W. S., Ivison, R. J., Liseau, R., Matthews, B. C., Pilbratt, G. L., Walker, H. J., Waelkens, C., Greaves, J. S., Sibthorpe, B., Acke, B., Pantin, E. E., Vandenbussche, B., Olofsson, Göran, Dominik, C., Barlow, M. J., Bendo, G. J., Blommaert, J. A. D. L., Brandeker, Alexis, de Vries, Bernard L., Dent, W. R. F., Di Francesco, J., Fridlund, M., Gear, W. K., Harvey, P. M., Hogerheijde, M. R., Holland, W. S., Ivison, R. J., Liseau, R., Matthews, B. C., Pilbratt, G. L., Walker, H. J., and Waelkens, C.
Abstract: Far-infrared Herschel images of the is an element of Eridani system, seen at a fifth of the Sun's present age, resolve two belts of debris emission. Fits to the 160 mu m PACS image yield radial spans for these belts of 12-16 and 54-68 AU. The south end of the outer belt is approximate to 10% brighter than the north end in the PACS+SPIRE images at 160, 250, and 350 mu m, indicating a pericenter glow attributable to a planet c From this asymmetry and an upper bound on the offset of the belt center, this second planet should be mildly eccentric (e(c) approximate to 0.03-0.3). Compared to the asteroid and Kuiper Belts of the young Sun, the is an element of Eri belts are intermediate in brightness and more similar to each other, with up to 20 km sized collisional fragments in the inner belt totaling approximate to 5% of an Earth mass. This reservoir may feed the hot dust close to the star and could send many impactors through the Habitable Zone, especially if it is being perturbed by the suspected planet is an element of Eri b, at semi-major axis approximate to 3 AU., AuthorCount:25
Published: 2014
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186. Herschel/HIFI observations of ionised carbon in the beta Pictoris debris disk

Author: Cataldi, Gianni, Brandeker, Alexis, Olofsson, Göran, Larsson, Bengt, Liseau, R., Blommaert, J., Fridlund, M., Ivison, R., Pantin, E., Sibthorpe, B., Vandenbussche, B., Wu, Y., Cataldi, Gianni, Brandeker, Alexis, Olofsson, Göran, Larsson, Bengt, Liseau, R., Blommaert, J., Fridlund, M., Ivison, R., Pantin, E., Sibthorpe, B., Vandenbussche, B., and Wu, Y.
Abstract: Context. The dusty debris disk around the similar to 20 Myr old main-sequence A-star beta Pictoris is known to contain gas. Evidence points towards a secondary origin of the gas as opposed to being a direct remnant from the initial protoplanetary disk, although the dominant gas production mechanism is so far not identified. The origin of the observed overabundance of C and O compared with solar abundances of metallic elements such as Na and Fe is also unclear. Aims. Our goal is to constrain the spatial distribution of C in the disk, and thereby the gas origin and its abundance pattern. Methods. We used the HIFI instrument on board the Herschel Space Observatory to observe and spectrally resolve C II emission at 158 mu m from the beta Pic debris disk. Assuming a disk in Keplerian rotation and a model for the line emission from the disk, we used the spectrally resolved line profile to constrain the spatial distribution of the gas. Results. We detect the C II 158 mu m emission. Modelling the shape of the emission line shows that most of the gas is located at about similar to 100 AU or beyond. We estimate a total C gas mass of 1.3(-0.5)(+1.3) x 10(2) M-circle plus (central 90% confidence interval). The data suggest that more gas is located on the south-west side of the disk than on the north-east side. The shape of the emission line is consistent with the hypothesis of a well mixed gas (constant C/Fe ratio throughout the disk). Assuming instead a spatial profile expected from a simplified accretion disk model, we found it to give a significantly poorer fit to the observations. Conclusions. Since the bulk of the gas is found outside 30 AU, we argue that the cometary objects known as falling evaporating bodies are probably not the dominant source of gas; production from grain-grain collisions or photodesorption seems more likely. The incompatibility of the observations with a simplified accretion disk model might favour a preferential depletion explanation for the overabu, AuthorCount:12
Published: 2014
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187. GG Tau: the fifth element

Author: Di Folco, E., Dutrey, A., Bouquin, J. -B. Le, Lacour, S., Berger, J. -P., Köhler, R., Guilloteau, S., Piétu, V., Bary, J., Beck, T., Beust, H., Pantin, E., Di Folco, E., Dutrey, A., Bouquin, J. -B. Le, Lacour, S., Berger, J. -P., Köhler, R., Guilloteau, S., Piétu, V., Bary, J., Beck, T., Beust, H., and Pantin, E.
Abstract: We aim at unveiling the observational imprint of physical mechanisms that govern planetary formation in young, multiple systems. In particular, we investigate the impact of tidal truncation on the inner circumstellar disks. We observed the emblematic system GG Tau at high-angular resolution: a hierarchical quadruple system composed of low-mass T Tauri binary stars surrounded by a well-studied, massive circumbinary disk in Keplerian rotation. We used the near-IR 4-telescope combiner PIONIER on the VLTI and sparse-aperture-masking techniques on VLT/NaCo to probe this proto-planetary system at sub-AU scales. We report the discovery of a significant closure-phase signal in H and Ks bands that can be reproduced with an additional low-mass companion orbiting GG Tau Ab, at a (projected) separation rho = 31.7 +/- 0.2mas (4.4 au) and PA = 219.6 +/- 0.3deg. This finding offers a simple explanation for several key questions in this system, including the missing-stellar-mass problem and the asymmetry of continuum emission from the inner dust disks observed at millimeter wavelengths. Composed of now five co-eval stars with 0.02 <= Mstar <= 0.7 Msun, the quintuple system GG Tau has become an ideal test case to constrain stellar evolution models at young ages (few 10^6yr)., Comment: 5pages, 3 figures, 1 appendix (online material)
Published: 2014
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188. Some (Little) Thing(s) about VISIR

Author: Pantin, E., primary, Vanzi, L., additional, and Weilenmann, U., additional
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189. Dynamical Modeling of the Deep Impact Dust Ejecta Cloud

Author: Bonev, T., primary, Ageorges, N., additional, Bagnulo, S., additional, Barrera, L., additional, Böhnhardt, H., additional, Hainaut, O., additional, Jehin, E., additional, Käufl, H. U., additional, Kerber, F., additional, LoCurto, G., additional, Manfroid, J., additional, Marco, O., additional, Pantin, E., additional, Pompei, E., additional, Saviane, I., additional, Selman, F., additional, Sterken, C., additional, Rauer, H., additional, Tozzi, G. P., additional, and Weiler, M., additional
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190. EXTREME CONDITIONS IN A CLOSE ANALOG TO THE YOUNG SOLAR SYSTEM: HERSCHEL OBSERVATIONS OF ϵ ERIDANI

Author: Greaves, J. S., primary, Sibthorpe, B., additional, Acke, B., additional, Pantin, E. E., additional, Vandenbussche, B., additional, Olofsson, G., additional, Dominik, C., additional, Barlow, M. J., additional, Bendo, G. J., additional, Blommaert, J. A. D. L., additional, Brandeker, A., additional, de Vries, B. L., additional, Dent, W. R. F., additional, Di Francesco, J., additional, Fridlund, M., additional, Gear, W. K., additional, Harvey, P. M., additional, Hogerheijde, M. R., additional, Holland, W. S., additional, Ivison, R. J., additional, Liseau, R., additional, Matthews, B. C., additional, Pilbratt, G. L., additional, Walker, H. J., additional, and Waelkens, C., additional
Published: 2014
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191. MATISSE status report and science forecast

Author: Lopez, B., additional, Lagarde, S., additional, Jaffe, W., additional, Petrov, R., additional, Schöller, M., additional, Antonelli, P., additional, Beckman, U., additional, Bério, Ph., additional, Bettonvil, F., additional, Graser, U., additional, Millour, F., additional, Robbe-Dubois, S., additional, Venema, L., additional, Wolf, S., additional, Bristow, P., additional, Glindemann, A., additional, Gonzalez, J.-C., additional, Lanz, Th., additional, Henning, T., additional, Weigelt, G., additional, Agócs, T., additional, Augereau, J.-C., additional, Ávila, G., additional, Bailet, C., additional, Behrend, J., additional, Berger, J.-P., additional, von Boekel, Roy, additional, Bonhomme, S., additional, Bourget, P., additional, Brast, R., additional, Bresson, Y., additional, Clausse, J. M., additional, Chesneau, O., additional, Csépány, G., additional, Connot, C., additional, Crida, A., additional, Danchi, W. C., additional, Delbo, M., additional, Delplancke, F., additional, Dominik, C., additional, Dugué, M., additional, Elswijk, E., additional, Fanteï, Y., additional, Finger, G., additional, Gabasch, A., additional, Girard, P., additional, Girault, V., additional, Gitton, P., additional, Glazenborg, A., additional, Gonté, F., additional, Guitton, F., additional, Guniat, S., additional, De Haan, M., additional, Haguenauer, P., additional, Hanenburg, H., additional, Heininger, M., additional, Hofmann, K.-H., additional, Hogerheijde, M., additional, ter Horst, R., additional, Hron, J., additional, Hughes, Y., additional, Ives, D., additional, Jakob, G., additional, Jaskó, A., additional, Jolley, P., additional, Kragt, J., additional, Köhler, R., additional, Kroener, T., additional, Kroes, G., additional, Labadie, L., additional, Laun, W., additional, Lehmitz, M., additional, Leinert, Ch., additional, Lizon, J. L., additional, Lucuix, Ch., additional, Marcotto, A., additional, Martinache, F., additional, Matter, A., additional, Martinot-Lagarde, G., additional, Mauclert, N., additional, Mehrgan, L., additional, Meilland, A., additional, Mellein, M., additional, Ménardi, S., additional, Menut, J. L., additional, Meisenheimer, K., additional, Morel, S., additional, Mosoni, L., additional, Navarro, R., additional, Neumann, U., additional, Nussbaum, E., additional, Ottogalli, S., additional, Palsa, R., additional, Panduro, J., additional, Pantin, E., additional, Percheron, I., additional, Duc, T. Phan, additional, Pott, J.-U., additional, Pozna, Eszter, additional, Przygodda, F., additional, Richichi, A., additional, Rigal, F., additional, Rupprecht, G., additional, Schertl, D., additional, Stegmeier, J., additional, Thiam, L., additional, Tromp, N., additional, Vannier, M., additional, Vakili, F., additional, van Belle, G., additional, Wagner, K., additional, and Woillez, J., additional
Published: 2014
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192. A multidisciplinary network to tackle childhood obesity in Upper Normandy (France). 5Years after!

Author: GEHANNO, B., primary, CHANONI, E., additional, CASTRES, I., additional, PANTIN, E., additional, CARLIOZ, C., additional, GROUT, B., additional, TOURANCHEAU, E., additional, SENGIER, A., additional, and LECOINTRE, C., additional
Published: 2014
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193. 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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194. The installation and ongoing commissioning of the MATISSE mid-infrared interferometer at the ESO Very Large Telescope Observatory

Author: Creech-Eakman, Michelle J., Tuthill, Peter G., Mérand, Antoine, Lopez, B., Lagarde, S., Matter, A., Agocs, T., Allouche, F., Antonelli, P., Augereau, J.-C., Bailet, C., Berio, P., Bettonvil, F., Beckmann, U., van Boekel, R., Bresson, Y., Bristow, P., Cruzalebes, P., Delbo, M., Dominik, C., Elswijk, E., Fantei, Y., Glindemann, A., Heininger, M., Hofmann, K.-H., Hogerheijde, M., Hron, J., Jaffe, W., Kroes, G., Laun, W., Lehmitz, M., Meilland, A., Meisenheimer, K., Millour, F., Morel, S., Neumann, U., Pantin, E., Petrov, R. G., Robbe-Dubois, S., Schertl, D., Schoeller, M., Wolf, S., Zins, G., Henning, T., Stee, Ph., and Weigelt, G.
Published: 2018
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195. Multiple spiral patterns in the transitional disk of HD 100546

Author: Boccaletti, A., Pantin, E., Lagrange, A. -M., Augereau, J. -C., Meheut, H., Quanz, S. P., Boccaletti, A., Pantin, E., Lagrange, A. -M., Augereau, J. -C., Meheut, H., and Quanz, S. P.
Abstract: Protoplanetary disks around young stars harbor many structures related to planetary formation. Of particular interest, spiral patterns were discovered among several of these disks and are expected to be the sign of gravitational instabilities leading to giant planets formation or gravitational perturbations caused by already existing planets. In this context, the star HD100546 presents some specific characteristics with a complex gas and dusty disk including spirals as well as a possible planet in formation. The objective of this study is to analyze high contrast and high angular resolution images of this emblematic system to shed light on critical steps of the planet formation. We retrieved archival images obtained at Gemini in the near IR (Ks band) with the instrument NICI and processed the data using advanced high contrast imaging technique taking advantage of the angular differential imaging. These new images reveal the spiral pattern previously identified with HST with an unprecedented resolution, while the large-scale structure of the disk is mostly erased by the data processing. The single pattern at the southeast in HST images is now resolved into a multi-armed spiral pattern. Using two models of a gravitational perturber orbiting in a gaseous disk we attempted to bring constraints on the characteristics of this perturber assuming each spiral being independent and we derived qualitative conclusions. The non-detection of the northeast spiral pattern observed in HST allows to put a lower limit on the intensity ratio between the two sides of the disk, which if interpreted as forward scattering yields a larger anisotropic scattering than derived in the visible. Also, we found that the spirals are likely spatially resolved with a thickness of about 5-10AU. Finally, we did not detect the candidate forming planet recently discovered in the Lp band, with a mass upper limit of 16-18 MJ., Comment: Accepted for publication in Astronomy and Astrophysics, 10 pages, 8 figures
Published: 2013
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196. GASPS - a Herschel survey of gas and dust in Protoplanetary Disks: Summary and Initial Statistics

Author: Dent, W. R. F., Thi, W. F., Kamp, I., Williams, J. P., Menard, F., Andrews, S., Ardila, D., Aresu, G., Augereau, J-C., Navascues, D. Barrado y, Brittain, S., Carmona, A., Ciardi, D., Danchi, W., Donaldson, J., Duchene, G., Eiroa, C., Fedele, D., Grady, C., de Gregorio-Molsalvo, I., Howard, C., Huelamo, N., Krivov, A., Lebreton, J., Liseau, R., Martin-Zaidi, C., Mathews, G., Meeus, G., Mendigutia, I., Montesinos, B., Morales-Calderon, M., Mora, A., Nomura, H., Pantin, E., Pascucci, I., Phillips, N., Pinte, C., Podio, L., Ramsay, S. K., Riaz, B., Riviere-Marichalar, P., Roberge, A., Sandell, G., Solano, E., Tilling, I., Torrelles, J. M., Vandenbusche, B., Vicente, S., White, G. J., Woitke, P., Dent, W. R. F., Thi, W. F., Kamp, I., Williams, J. P., Menard, F., Andrews, S., Ardila, D., Aresu, G., Augereau, J-C., Navascues, D. Barrado y, Brittain, S., Carmona, A., Ciardi, D., Danchi, W., Donaldson, J., Duchene, G., Eiroa, C., Fedele, D., Grady, C., de Gregorio-Molsalvo, I., Howard, C., Huelamo, N., Krivov, A., Lebreton, J., Liseau, R., Martin-Zaidi, C., Mathews, G., Meeus, G., Mendigutia, I., Montesinos, B., Morales-Calderon, M., Mora, A., Nomura, H., Pantin, E., Pascucci, I., Phillips, N., Pinte, C., Podio, L., Ramsay, S. K., Riaz, B., Riviere-Marichalar, P., Roberge, A., Sandell, G., Solano, E., Tilling, I., Torrelles, J. M., Vandenbusche, B., Vicente, S., White, G. J., and Woitke, P.
Abstract: GASPS is a far-infrared line and continuum survey of protoplanetary and young debris disks using PACS on the Herschel Space Observatory. The survey includes [OI] at 63 microns, as well as 70, 100 and 160um continuum, with the brightest objects also studied in [OI]145um, [CII]157um, H2O and CO. Targets included T Tauri stars and debris disks in 7 nearby young associations, and a sample of isolated Herbig AeBe stars. The aim was to study the global gas and dust content in a wide disk sample, systemically comparing the results with models. In this paper we review the main aims, target selection and observing strategy. We show initial results, including line identifications, sources detected, and a first statistical study. [OI]63um was the brightest line in most objects, by a factor of ~10. Detection rates were 49%, including 100% of HAeBe stars and 43% of T Tauri stars. Comparison with published dust masses show a dust threshold for [OI]63um detection of ~1e-5 M_solar. Normalising to 140pc distance, 32% with mass 1e-6 - 1e-5 M_solar, and a small number with lower mass were also detected. This is consistent with moderate UV excess and disk flaring. In most cases, continuum and line emission is spatially and spectrally unresolved, suggesting disk emission. ~10 objects were resolved, likely from outflows. Detection rates in [OI]145um, [CII]157um and CO J=18-17 were 20-40%, but [CII] was not correlated with disk mass, suggesting it arises instead from a compact envelope. [OI] detection rates in T Tauri associations of ages 0.3-4Myr were ~50%. ~2 stars were detectable in associations of 5-20Myr, with no detections in associations of age >20Myr. Comparing with the total number of young stars, and assuming a ISM-like gas/dust ratio, this indicates that ~18% of stars retain a gas-rich disk of total mass >1M_Jupiter for 1-4Myr, 1-7% keep such disks for 5-10Myr, and none remain beyond 10-20Myr., Comment: Accepted for PASP
Published: 2013
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197. A diamond AGPM coronagraph for VISIR

Author: Delacroix, C., Absil, O., Mawet, D., Hanot, C., Karlsson, Mikael, Forsberg, Pontus, Pantin, E., Surdej, J., Habraken, S., Delacroix, C., Absil, O., Mawet, D., Hanot, C., Karlsson, Mikael, Forsberg, Pontus, Pantin, E., Surdej, J., and Habraken, S.
Abstract: In recent years, phase mask coronagraphy has become increasingly efficient in imaging the close environment of stars, enabling the search for exoplanets and circumstellar disks. Coronagraphs are ideally suited instruments, characterized by high dynamic range imaging capabilities, while preserving a small inner working angle. The AGPM (Annular Groove Phase Mask, Mawet et al. 20051) consists of a vector vortex induced by a rotationally symmetric subwavelength grating. This technique constitutes an almost unique solution to the achromatization at longer wavelengths (mid-infrared). For this reason, we have specially conceived a mid-infrared AGPM coronagraph for the forthcoming upgrade of VISIR, the mid-IR imager and spectrograph on the VLT at ESO (Paranal), in collaboration with members of the VISIR consortium. The implementation phase of the VISIR Upgrade Project is foreseen for May-August 2012, and the AGPM installed will cover the 11-13.2 μm spectral range. In this paper, we present the entire fabrication process of our AGPM imprinted on a diamond substrate. Diamond is an ideal material for mid-infrared wavelengths owing to its high transparency, small dispersion, extremely low thermal expansion and outstanding mechanical and chemical properties. The design process has been performed with an algorithm based on the rigorous coupled wave analysis (RCWA), and the micro-fabrication has been carried out using nano-imprint lithography and reactive ion etching. A precise grating profile metrology has also been conducted using cleaving techniques. Finally, we show the deposit of fiducials (i.e. centering marks) with Aerosol Jet Printing (AJP). We conclude with the ultimate coronagraph expected performances.
Published: 2012
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198. Herschel images of Fomalhaut An extrasolar Kuiper belt at the height of its dynamical activity

Author: Acke, B., Min, M., Dominik, C., Vandenbussche, B., Sibthorpe, B., Waelkens, C., Olofsson, Göran, Degroote, P., Smolders, K., Pantin, E., Barlow, M. J., Blommaert, J. A. D. L., Brandeker, Alexis, De Meester, W., Dent, W. R. F., Exter, K., Di Francesco, J., Fridlund, M., Gear, W. K., Glauser, A. M., Greaves, J. S., Harvey, P. M., Henning, Th, Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Jean, C., Liseau, R., Naylor, D. A., Pilbratt, G. L., Polehampton, E. T., Regibo, S., Royer, P., Sicilia-Aguilar, A., Swinyard, B. M., Acke, B., Min, M., Dominik, C., Vandenbussche, B., Sibthorpe, B., Waelkens, C., Olofsson, Göran, Degroote, P., Smolders, K., Pantin, E., Barlow, M. J., Blommaert, J. A. D. L., Brandeker, Alexis, De Meester, W., Dent, W. R. F., Exter, K., Di Francesco, J., Fridlund, M., Gear, W. K., Glauser, A. M., Greaves, J. S., Harvey, P. M., Henning, Th, Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Jean, C., Liseau, R., Naylor, D. A., Pilbratt, G. L., Polehampton, E. T., Regibo, S., Royer, P., Sicilia-Aguilar, A., and Swinyard, B. M.
Abstract: Context. Fomalhaut is a young (2 +/- 1 x 10(8) years), nearby (7.7 pc), 2 M-circle dot star that is suspected to harbor an infant planetary system, interspersed with one or more belts of dusty debris. Aims. We present far-infrared images obtained with the Herschel Space Observatory with an angular resolution between 5.7 '' and 36.7 '' at wavelengths between 70 mu m and 500 mu m. The images show the main debris belt in great detail. Even at high spatial resolution, the belt appears smooth. The region in between the belt and the central star is not devoid of material; thermal emission is observed here as well. Also at the location of the star, excess emission is detected. We aim to construct a consistent image of the Fomalhaut system. Methods. We use a dynamical model together with radiative-transfer tools to derive the parameters of the debris disk. We include detailed models of the interaction of the dust grains with radiation, for both the radiation pressure and the temperature determination. Comparing these models to the spatially resolved temperature information contained in the images allows us to place strong constraints on the presence of grains that will be blown out of the system by radiation pressure. We use this to derive the dynamical parameters of the system. Results. The appearance of the belt points toward a remarkably active system in which dust grains are produced at a very high rate by a collisional cascade in a narrow region filled with dynamically excited planetesimals. Dust particles with sizes below the blow-out size are abundantly present. The equivalent of 2000 one-km-sized comets are destroyed every day, out of a cometary reservoir amounting to 110 Earth masses. From comparison of their scattering and thermal properties, we find evidence that the dust grains are fluffy aggregates, which indicates a cometary origin. The excess emission at the location of the star may be produced by hot dust with a range of temperatures, but may also be due to, AuthorCount:36;[SUBOlofsson, G.]Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden;[SUBBrandeker, A.]Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden
Published: 2012
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199. Comet-like mineralogy of olivine crystals in an extrasolar proto-Kuiper belt

Author: de Vries, B. L., Acke, B., Blommaert, J. A. D. L., Waelkens, C., Waters, L. B. F. M., Vandenbussche, B., Min, M., Olofsson, Göran, Dominik, C., Decin, L., Barlow, M. J., Brandeker, Alexis, Di Francesco, J., Glauser, A. M., Greaves, J., Harvey, P. M., Holland, W. S., Ivison, R. J., Liseau, R., Pantin, E. E., Pilbratt, G. L., Royer, P., Sibthorpe, B., de Vries, B. L., Acke, B., Blommaert, J. A. D. L., Waelkens, C., Waters, L. B. F. M., Vandenbussche, B., Min, M., Olofsson, Göran, Dominik, C., Decin, L., Barlow, M. J., Brandeker, Alexis, Di Francesco, J., Glauser, A. M., Greaves, J., Harvey, P. M., Holland, W. S., Ivison, R. J., Liseau, R., Pantin, E. E., Pilbratt, G. L., Royer, P., and Sibthorpe, B.
Abstract: Some planetary systems harbour debris disks containing planetesimals such as asteroids and comets(1). Collisions between such bodies produce small dust particles(2), the spectral features of which reveal their composition and, hence, that of their parent bodies. A measurement of the composition of olivine crystals (Mg2-2xFe2xSiO4) has been done for the protoplanetary disk HD 100546 (refs 3, 4) and for olivine crystals in the warm inner parts of planetary systems. The latter compares well with the iron-rich olivine in asteroids(5,6) (x approximate to 0.29). In the cold outskirts of the beta Pictoris system, an analogue to the young Solar System, olivine crystals were detected(7) but their composition remained undetermined, leaving unknown how the composition of the bulk of Solar System cometary olivine grains compares with that of extrasolar comets(8,9). Here we report the detection of the 69-micrometre-wavelength band of olivine crystals in the spectrum of beta Pictoris. Because the disk is optically thin, we can associate the crystals with an extrasolar proto-Kuiper belt a distance of 15-45 astronomical units from the star (one astronomical unit is the Sun-Earth distance), determine their magnesium-rich composition (x = 0.01 +/- 0.001) and show that they make up 3.6 +/- 1.0 per cent of the total dust mass. These values are strikingly similar to those for the dust emitted by the most primitive comets in the Solar System(8-10), even though beta Pictoris is more massive and more luminous and has a different planetary system architecture., AuthorCount:23
Published: 2012
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200. The complex circumstellar environment of HD 142527

Author: Verhoeff, A. P., Min, M., Pantin, E., Waters, L.B.F.M., Tielens, A. G. G. M., Honda, M., Fujiwara, H., Bouwman, J., Van Boekel, R., Dougherty, S.M., de Koter, A., Dominik, C., Mulders, G. D., Verhoeff, A. P., Min, M., Pantin, E., Waters, L.B.F.M., Tielens, A. G. G. M., Honda, M., Fujiwara, H., Bouwman, J., Van Boekel, R., Dougherty, S.M., de Koter, A., Dominik, C., and Mulders, G. D.
Abstract: Context. The recent findings of gas giant planets around young A-type stars suggest that disks surrounding Herbig Ae/Be stars will develop planetary systems. An interesting case is HD142527, for which previous observations revealed a complex circumstellar environment and an unusually high ratio of infrared to stellar luminosity. Its properties differ considerably from other Herbig Ae/Be stars. This suggests that the disk surrounding HD142527 is in an uncommon evolutionary stage. Aims. We aim for a better understanding of the geometry and evolutionary status of the circumstellar material around the Herbig Ae/Be star HD142527. Methods. We map the composition and spatial distribution of the dust around HD142527. We analyze SEST and ATCA millimeter data, VISIR N and Q-band imaging and spectroscopy. We gather additional relevant data from the literature. We use the radiative transfer code MCMax to construct a model of the geometry and density structure of the circumstellar matter, which fits all of the observables satisfactorily. Results. We find that the disk of HD142527 has three geometrically distinct components separated by a disk gap running from 30 to 130AU. There is a geometrically flat inner disk running from 0.3AU up to 30AU; an optically thin halo-like component of dust in the inner disk regions; and a massive self-shadowed outer disk running from 130AU up to 200AU. We derived a total dust mass in small grains of 1.0 × 10−3 M and a vertical height of the inner wall of the outer disk of h = 60AU. Owing to the gray extinction of the “halo” we obtained new stellar parameters, including a stellar luminosity of 20 ± 2 L and age of 106.7 ± 0.4 yr. Conclusions. We find that the disk surrounding HD142527 is highly evolved despite the relatively young age of the star. The peculiar disk geometry can explain the extreme IR reprocessing efficiency of the disk. Furthermore, the geometry, the large disk mass, and the highly processed dust composition are indicative of on-goi
Published: 2011

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