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Start Over Author "Malbet, Fabien" Topic fos: physical sciences
21 results on '"Malbet, Fabien"'

1. Sculpting the disk around T Cha: an interferometric view

Author

Olofsson, Johan, Benisty, Myriam, Bouquin, Jean-Baptiste Le, Berger, Jean-Philippe, Lacour, Sylvestre, M��nard, Fran��ois, Henning, Thomas, Crida, Aur��lien, Burtscher, Leonard, Meeus, Gwendolyn, Ratzka, Thorsten, Pinte, Christophe, Augereau, Jean-Charles, Malbet, Fabien, Lazareff, Bernard, and Traub, Wesley A.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), 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, Astrophysics - Earth and Planetary Astrophysics
Abstract

(Abridged) Circumstellar disks are believed to be the birthplace of planets and are expected to dissipate on a timescale of a few Myr. The processes responsible for the removal of the dust and gas will strongly modify the radial distribution of the dust and consequently the SED. In particular, a young planet will open a gap, resulting in an inner disk dominating the near-IR emission and an outer disk emitting mostly in the far-IR. We analyze a full set of data (including VLTI/Pionier, VLTI/Midi, and VLT/NaCo/Sam) to constrain the structure of the transition disk around TCha. We used the Mcfost radiative transfer code to simultaneously model the SED and the interferometric observations. We find that the dust responsible for the emission in excess in the near-IR must have a narrow temperature distribution with a maximum close to the silicate sublimation temperature. This translates into a narrow inner dusty disk (0.07-0.11 AU). We find that the outer disk starts at about 12 AU and is partially resolved by the Pionier, Sam, and Midi instruments. We show that the Sam closure phases, interpreted as the signature of a candidate companion, may actually trace the asymmetry generated by forward scattering by dust grains in the upper layers of the outer disk. These observations help constrain the inclination and position angle of the outer disk. The presence of matter inside the gap is difficult to assess with present-day observations. Our model suggests the outer disk contaminates the interferometric signature of any potential companion that could be responsible for the gap opening, and such a companion still has to be unambiguously detected. We stress the difficulty to observe point sources in bright massive disks, and the consequent need to account for disk asymmetries (e.g. anisotropic scattering) in model-dependent search for companions., Removed the word "first" in the abstract of the paper: "obtained with the first 4-telescope combiner (VLTI/Pionier)"

Published
2013

2. The binary Be star $��$ Scorpii at high spectral and spatial resolution : II The circumstellar disk evolution after the periastron

Author

Meilland, Anthony, Stee, Philippe, Spang, Alain, Malbet, Fabien, Massi, Fabrizio, and Schertl, Dieter

Subjects
Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Classical Be stars are hot non-supergiant stars surrounded by a gaseous circumstellar disk that is responsible for the observed infrared (IR) excess and emission lines. The influence of binarity on these phenomena remains controversial. We followed the evolution of the environment surrounding the binary Be star $��$ Scorpii one year before and one year after the 2011 periastron to check for any evidence of a strong interaction between its companion and the primary circumstellar disk. We used the VLTI/AMBER spectro-interferometric instrument operating in the K band in high (12000) spectral resolution to obtain information on both the disk geometry and kinematics. Observations were carried out in two emission lines: Br$��$ (2.172\,$��$m) and $\ion{He}{i}$ (2.056\,$��$m). We detected some important changes in $��$ Scorpii's circumstellar disk geometry between the first observation made in April 2010 and the new observation made in June 2012. During the last two years the disk has grown at a mean velocity of 0.2\,km\,s$^{-1}$. This is compatible with the expansion velocity previously found during the 2001-2007 period. The disk was also found to be asymmetric at both epochs, but with a different morphology in 2010 and 2012. Considering the available spectroscopic data showing that the main changes in the emission-line profiles occurred quickly during the periastron, it is probable that the differences between the 2010 and 2012 disk geometry seen in our interferometric data stem from a disk perturbation caused by the companion tidal effects. However, taking into account that no significant changes have occurred in the disk since the end of the 2011 observing season, it is difficult to understand how this induced inhomogeneity has been "frozen" in the disk for such a long period., Astronomy and Astrophysics (2013)

Published
2013
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3. NEAT: a space born astrometric mission for the detection and characterization of nearby habitable planetary systems

Author

Malbet, Fabien, Goullioud, Renaud, Lagage, Pierre-Olivier, Léger, Alain, Shao, Mike, Crouzier, Antoine, and Consortium, the NEAT

Subjects
Physics, Cosmic Vision, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy, Planetary system, Stellar classification, Earth mass, Space (mathematics), law.invention, Telescope, Stars, Astrophysics - Solar and Stellar Astrophysics, law, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Circumstellar habitable zone, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

The NEAT (Nearby Earth Astrometric Telescope) mission is a proposal submitted to ESA for its 2010 call for M-size mission within the Cosmic Vision 2015-2025 plan. The main scientific goal of the NEAT mission is to detect and characterize planetary systems in an exhaustive way down to 1 Earth mass in the habitable zone and further away, around nearby stars for F, G, and K spectral types. This survey would provide the actual planetary masses, the full characterization of the orbits including their inclination, for all the components of the planetary system down to that mass limit. NEAT will continue the work performed by Hipparcos and Gaia by reaching a precision that is improved by two orders of magnitude on pointed targets., 17 pages, in SPIE 2012 symposium in "Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave" SPIE Conference 8442, 16

Published
2012

4. The Formation and Evolution of Planetary Systems: The Search for and Characterization of Young Planets

Author

Beichman, Charles, Baraffe, Isabelle, Crockett, Christopher, Dodson-Robinson, Sarah, Fortney, Jonathan, Ghez, Andrea, Greene, Thomas P., Kraus, Adam, Lin, Doug, Mahmud, Naved, Malbet, Fabien, Marley, Mark, Millan-Gabet, Rafael, Prato, Lisa, Oppenheimer, Ben, Simon, Michal, Stauffer, John, Tanner, Angelle, and Velusamy, T.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Despite the revolution in our knowledge resulting from the detection of planets around mature stars, we know almost nothing about planets orbiting young stars because rapid rotation and active photospheres preclude detection by radial velocities or transits and because direct imaging has barely penetrated the requisite range of high contrast and angular resolution. Of the techniques presently under consideration for the coming decade, only space-based astrometry offers the prospect of discovering gas giants (100 to >> 300 Mearth), lower mass systems such as icy giants (10 to 100 Mearth), and even a few rocky, super-Earths 300 Mearth) orbiting stars ranging in age from 1 to 100 Myr. Astrometry will complement high contrast imaging which should be able to detect gas giants (1~10 MJup) in orbits from a few to a few hundred AU. An astrometric survey in combination with imaging data for a subsample of objects will allow a detailed physical understanding of the formation and evolution of young gas giant planets impossible to achieve by any one technique., White Paper Submission to Astro2010

Published
2009

5. Astrometric Detection of Earthlike Planets

Author

Shao, Michael, Marcy, Geoff, Catanzarite, Joseph H., Edberg, Stephen J., Leger, Alain, Malbet, Fabien, Queloz, Didier, Muterspaugh, Matthew W., Beichman, Charles, Fischer, Debra A., Ford, Eric, Olling, Robert, Kulkarni, Shrinivas, Unwin, Stephen C., and Traub, Wesley

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract

Astrometry can detect rocky planets in a broad range of masses and orbital distances and measure their masses and three-dimensional orbital parameters, including eccentricity and inclination, to provide the properties of terrestrial planets. The masses of both the new planets and the known gas giants can be measured unambiguously, allowing a direct calculation of the gravitational interactions, both past and future. Such dynamical interactions inform theories of the formation and evolution of planetary systems, including Earth-like planets. Astrometry is the only technique technologically ready to detect planets of Earth mass in the habitable zone (HZ) around solar-type stars within 20 pc. These Earth analogs are close enough for follow-up observations to characterize the planets by infrared imaging and spectroscopy with planned future missions such as the James Webb Space Telescope (JWST) and the Terrestrial Planet Finder/Darwin. Employing a demonstrated astrometric precision of 1 microarcsecond and a noise floor under 0.1 micro-arcseconds, SIM Lite can make multiple astrometric measurements of the nearest 60 F-, G-, and K-type stars during a five-year mission. SIM Lite directly tests theories of rocky planet formation and evolution around Sun-like stars and identifies the nearest potentially habitable planets for later spaceborne imaging, e.g., with Terrestrial Planet Finder and Darwin. SIM was endorsed by the two recent Decadal Surveys and it meets the highest-priority goal of the 2008 AAAC Exoplanet Task Force., Comment: Astro2010 White Paper, 8 pages

Published
2009
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6. First astrophysical results from AMBER/VLTI

Author

Malbet, Fabien, Petrov, Romain G., Weigelt, Gerd, Stee, Philippe, Tatulli, Eric, De Souza, Armando Domiciano, Millour, Florentin, Collaboration, the AMBER consortium, Laboratoire Hippolyte Fizeau (FIZEAU), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), 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)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), J.D. Monnier, M. Schöller, W.C. Danchi, and AMBER consortium

Subjects
stars, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], massive stars, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Very Large Telescope, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), Near-infrared spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, young stellar objects, evolved stars, Optical interferometry, infrared, Astrophysics::Earth and Planetary Astrophysics, hot stars
Abstract

The AMBER instrument installed at the Very Large Telescope (VLT) combines three beams from as many telescopes to produce spectrally dispersed fringes from milli-arcsecond angular scale in the near infrared. Two years after installation, first scientific observations have been carried out during the Science Demonstration Time and the Guaranteed Time mostly on bright sources due to some VLTI limitations. In this paper, we review these first astrophysical results and we show which types of completely new information is brought by AMBER. The first astrophysical results have been mainly focusing on stellar wind structure, kinematics, and its interaction with dust usually concentrated in a disk. Because AMBER has dramatically increased the number of measures per baseline, this instrument brings strong constraints on morphology and models despite a relatively poor (u, v) coverage for each object., Comment: SPIE 6268 proceedings

Published
2006

7. First direct detection of a Keplerian rotating disk around the Be star $��$ Arae using the VLTI/AMBER instrument

Author

Meilland, Anthony, Stee, Philippe, Vannier, Martin, Millour, Florentin, De Souza, Armando Domiciano, Malbet, Fabien, Martayan, Christophe, Paresce, Francesco, Petrov, Romain, Richichi, Andrea, Spang, Alain, and Collaboration, the AMBER Consortium

Subjects
Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Aims. We aim to study the geometry and kinematics of the disk around the Be star $��$ Arae as a function of wavelength, especially across the Br$��$ emission line. The main purpose of this paper is to answer the question about the nature of the disk rotation around Be stars. Methods. We use the VLTI/AMBER instrument operating in the K band which provides a gain by a factor 5 in spatial resolution compared to previous VLTI/MIDI observations. Moreover, it is possible to combine the high angular resolution provided with the (medium) spectral resolution of AMBER to study the kinematics of the inner part of the disk and to infer its rotation law. Results. We obtain for the first time the direct evidence that the disk is in keplerian rotation, answering a question that occurs since the discovery of the first Be star $��$ Cas by father Secchi in 1866. We also present the global geometry of the disk showing that it is compatible with a thin disk + polar enhanced winds modeled with the SIMECA code. We found that the disk around $��$ Arae is compatible with a dense equatorial matter confined in the central region whereas a polar wind is contributing along the rotational axis of the central star. Between these two regions the density must be low enough to reproduce the large visibility modulus (small extension) obtained for two of the four VLTI baselines. Moreover, we obtain that $��$ Arae is rotating very close to its critical rotation. This scenario is also compatible with the previous MIDI measurements., 15 pages

Published
2006
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8. Probing the close environment of young stellar objects with interferometry

Author

Malbet, Fabien, Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Interferometry, Pre-Main Sequence Stars, Star Formation, Astrophysics::Solar and Stellar Astrophysics, Young Stellar Objects, Astrophysics::Earth and Planetary Astrophysics, 95.75.Kk, 97.10.Bt, 97.21.+a , 95.85.Jq, 95.85.Kr, 95.85.Hp, Infrared, Optical, Astrophysics::Galaxy Astrophysics
Abstract

The study of Young Stellar Objects (YSOs) is one of the most exciting topics that can be undertaken by long baseline optical interferometry. The magnitudes of these objects are at the edge of capabilities of current optical interferometers, limiting the studies to a few dozen, but are well within the capability of coming large aperture interferometers like the VLT Interferometer, the Keck Interferometer, the Large Binocular Telescope or 'OHANA. The milli-arcsecond spatial resolution reached by interferometry probes the very close environment of young stars, down to a tenth of an astronomical unit. In this paper, I review the different aspects of star formation that can be tackled by interferometry: circumstellar disks, multiplicity, jets. I present recent observations performed with operational infrared interferometers, IOTA, PTI and ISI, and I show why in the next future one will extend these studies with large aperture interferometers., Comment: Review to be published in JENAM'2002 proceedings "The Very Large Telescope Interferometer Challenges for the future"

Published
2003
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9. Star Formation Studies at the VLT

Author

Bertout, Claude, Reipurth, Bo, and Malbet, Fabien

Subjects
Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present an overview of what can be done in the field of star formation using the VLT and its advanced instrumentation, and especially with the very high angular resolution provided by the VLT in the VLTI mode. Herbig-Haro objects and early stellar evolution, pre-main sequence binaries, circumstellar disks and surface properties of young stars are investigated. We show that the VLT and VISA will be not only very useful to better understand star formation processes, but indeed necessary in order to advance in certain subjects., 13 pages including 7 figures and tables, uuencoded postscript; Invited talk, Proceedings of the ESO Workshop ``Science with the VLT'', eds. Danziger \& J., Walsh, J., Garching, June 1994.

Published
1995

10. High angular resolution coronography for adaptive optics

Author

Malbet, Fabien

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

Recent adaptive optics systems in astronomy achieve high-angular resolution. With the extreme stability of the images, detection at very low fluxes can be reached using a coronograph at the diffraction limit of the telescopes. This paper is an overview of the issues of stellar coronography used at the diffraction limit. Image formation through such a system is illustrated by numerical simulations. The description of a coronograph implemented on the VLT adaptive optics prototype, COME-ON, is presented as well as the first observations., Comment: 23 pages including figures and tables, uuencoded gz-compressed postscript

Published
1995
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11. Active Optics and Coronography with the Hubble Space Telescope

Author

Malbet, Fabien, Shao, Michael, and Yu, Jeffrey

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics
Abstract

In the field of planet and proto-planetary disk detection, achieving high angular resolution and high dynamic range is a necessity. Coronography coupled with adaptive optics on Hubble Space Telescope is a way to get both good spatial resolution and high dynamic range. However, because of the residual figure errors on the primary and on the secondary, HST has a scattered light level that prevents it from detecting extra-solar planets. Our simulations show that by using an active mirror (400-1000 actuators) in the optical path of HST with adaptive optics, we can correct the mirror errors and decrease the scattering level by a factor $10^{2}$ (from $10^{-4}$ to $10^{-6}$ fainter than the star). Furthermore, by controlling the spatial frequencies of the active mirror with a {\em dark hole\/} algorithm we can decrease the scattering level in image zones where planet detection is likely. Using this technique, we have succeeded in decreasing the scattering level to $3\times 10^{-8}$ of the star intensity within 1 arcsec from the central star. This will allow the detection of a Jupiter-like planet $10^{-9}$ times dimmer than the central star located 10 pc away in 1 hour of integration time with a signal-to-noise ratio of 5. This paper describes the method used to determine the actuator strokes applied to a deformable mirror to achieve planet detection and the design of a coronograph which implements this novel technique., in Proc. of 1994's SPIE symposium on "Astronomical Telescopes & Instrumentation for the 21st Century",(10 pages, Postscript format, figures included) - contact: [malbet@huey.jpl.nasa.gov]

Published
1994

12. Theia: Faint objects in motion or the new astrometry frontier

Author

Boehm, Céline, Krone-Martins, Alberto, Amorim, António, Anglada-Escudé, Guillem, Brandeker, Alexis, Courbin, Frederic, Enßlin, Torsten, Falcão, António, Freese, Katherine, Holl, Berry, Labadie, Lucas, Leger, Alain, Malbet, Fabien, Mamon, Gary, Mcarthur, Barbara, Mora, Alcione, Shao, Michael, Sozzetti, Alessandro, Spolyar, Douglas, Villaver, Eva, Albertus, Conrado, Bertone, Stefano, Bouy, Hervé, Boylan-Kolchin, Michael, Brown, Anthony, Brown, Warren, Cardoso, Vitor, Chemin, Laurent, Claudi, Riccardo, Correia, Alexandre C. M., Crosta, Mariateresa, Crouzier, Antoine, Cyr-Racine, Francis-Yan, Damasso, Mario, Da Silva, António, Davies, Melvyn, Das, Payel, Dayal, Pratika, Val-Borro, Miguel, Diaferio, Antonaldo, Erickcek, Adrienne, Fairbairn, Malcolm, Fortin, Morgane, Fridlund, Malcolm, Garcia, Paulo, Gnedin, Oleg, Goobar, Ariel, Gordo, Paulo, Goullioud, Renaud, Hambly, Nigel, Hara, Nathan, Hobbs, David, Hog, Erik, Holland, Andrew, Ibata, Rodrigo, Jordi, Carme, Klioner, Sergei, Kopeikin, Sergei, Lacroix, Thomas, Laskar, Jacques, Le Poncin-Lafitte, Christophe, Luri, Xavier, Majumdar, Subhabrata, Makarov, Valeri, Massey, Richard, Mennesson, Bertrand, Michalik, Daniel, Almeida, André Moitinho, Mourão, Ana, Moustakas, Leonidas, Murray, Neil, Muterspaugh, Matthew, Oertel, Micaela, Ostorero, Luisa, Perez-Garcia, Angeles, Platais, Imants, I Portell I Mora, Jord, Quirrenbach, Andreas, Randall, Lisa, Read, Justin, Regos, Eniko, Rory, Barnes, Rybicki, Krzysztof, Scott, Pat, Schneider, Jean, Jakub Scholtz, Siebert, Arnaud, Tereno, Ismael, Tomsick, John, Traub, Wesley, Valluri, Monica, Walker, Matt, Walton, Nicholas, Watkins, Laura, White, Glenn, Evans, Dafydd Wyn, Wyrzykowski, Lukasz, Wyse, Rosemary, Abbas, Ummi, Alimi, Jean-Michel, Altmann, Martin, Alves, João, Anderson, Richard, Arenou, Frédéric, Bailer-Jones, Coryn, Carlton, Baugh, Biermann, Michael, Blanco-Cuaresma, Sergi, Bonomo, Aldo Stefano, Broderick, Avery, Busso, Giorgia, Cabrera, Juan, Carrasco, Josep Manel, Carvalho, Carla Sofia, Castellani, Marco, Cermeño-Gavilán, Marina, Chadwick, Paula, Darling, Jeremy, Davidson, Michael, Angeli, Francesca, Carvalho, Reinaldo, Desidera, Silvano, Done, Chris, Ducourant, Christine, Erkal, Denis, Eyer, Laurent, Famey, Benoit, Feltzing, Sofia, Garcia, Emilio Fraile, Gomez, Facundo Ariel, Frenk, Carlos, Gai, Mario, Galli, Phillip, Galluccio, Laurent, Gavras, Panagiotis, Giacobbe, Paolo, Gratton, Raffaele, Guglielmetti, Fabrizia, Gunther, Eike, Hall, David, Harrison, Diana, Hatzes, Artie, Hestroffer, Daniel, Ishida, Emille, Jablonka, Pascale, Jacobs, Christopher, Janson, Markus, Jasche, Jens, Jauzac, Mathilde, Jones, Hugh, Jonker, Peter, Julbe, Francesc, Kneib, Jean-Paul, Kordopatis, Georges, Lancon, Arianne, Lattanzi, Mario Gilberto, Leguidou, Jean-Michel, Lehnert, Matt, Lehto, Harry, Lopes, Ilidio, Maldonado, Jesus, Marconi, Marcella, Martin, Nicolas, Marie-Elisabeth, Maury, Mazumdar, Anupam, Michtchenko, Tatiana, Minardi, Stefano, Munoz, Carlos, Murante, Giuseppe, Musella, Ilaria, Gerhard, Ortwin, Pagano, Isabella, Pani, Paolo, Paetzold, Martin, Daniel, Pfenniger, Piotto, Giampaolo, Preis, Olivier, Produit, Nicolas, Prost, Jean-Pierre, Rauer, Heike, Raymond, Sean, Reinaldo, Rosa, Revaz, Yves, Rita, Ribeiro, Rimoldini, Lorenzo, Huguet, Arnau Rios, Ripepi, Vincenzo, Rocci, Pier-Francesco, Rodriguez Frias, Maria D., Rosa, Reinaldo R., Sahlmann, Johannes, Saltas, Ippocratis, E E Lemos, José Pizarro Sand, Sarro, Luis M., Schaefer, Bjoern Malte, Schewtschenko, Jascha, Segransan, Damien, Selsis, Franck, Silk, Joe, Silva, Manuel, Solitro, Filomena, Spagna, Alessandro, Springel, Volker, Süveges, Maria, Teixeira, Ramachrisna, Shindou, Tetsuo, Thebault, Philippe, Tian, Feng, Turon, Catherine, Valle, José W. F., Vasiliev, Eugene, Vladilo, Juan, Martin, Vollmann, Ward, Martin, Weller, Jochen, Wilkinson, Mark, Wolf, Sebastian, Xiaoting, Fu, Yamada, Yoshiyuki, Zschocke, Sven, Zucker, Shay, 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), Université Grenoble Alpes (UGA), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Laboratoire Univers et Théories (LUTH (UMR_8102)), 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), 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), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Blaise Pascal - Clermont-Ferrand 2 (UBP), Centre National d’Études Spatiales [Paris] (CNES), 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), Theia, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and HEP, INSPIRE

Subjects
[PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract

In the context of the ESA M5 (medium mission) call we proposed a new satellite mission, Theia, based on relative astrometry and extreme precision to study the motion of very faint objects in the Universe. Theia is primarily designed to study the local dark matter properties, the existence of Earth-like exoplanets in our nearest star systems and the physics of compact objects. Furthermore, about 15 $\%$ of the mission time was dedicated to an open observatory for the wider community to propose complementary science cases. With its unique metrology system and "point and stare" strategy, Theia's precision would have reached the sub micro-arcsecond level. This is about 1000 times better than ESA/Gaia's accuracy for the brightest objects and represents a factor 10-30 improvement for the faintest stars (depending on the exact observational program). In the version submitted to ESA, we proposed an optical (350-1000nm) on-axis TMA telescope. Due to ESA Technology readiness level, the camera's focal plane would have been made of CCD detectors but we anticipated an upgrade with CMOS detectors. Photometric measurements would have been performed during slew time and stabilisation phases needed for reaching the required astrometric precision., Comment: http://theia.phyip3.dur.ac.uk

13. Planet Formation Imager (PFI): science vision and key requirements

Author

Ridgway Steve, Regaly Zsolt, Kral Quentin, Gandhi Poshak, Packham Chris, Tristram Konrad R. W., Baruteau Clement, Tuthill Peter, Mordasini Chris, Matter Alexis, A. Pierens, Duchene Gaspard, Olofsson Johan, Ilee John, Bitsch Bertram, Wittkowski Markus, Pinte Christophe, Meru Farzana, Armitage Phil, Chiavassa Andrea, Berger Jean-Philippe, Millour Florentin, Buscher David, Rosotti Giovanni P., Zhao Ming, Pott Joerg-Uwe, Wolf Sebastian, ten Brummelaar Theo, Bayo Amelia, Labadie Lucas, Morlok Andreas, Millan-Gabet Rafael, Kishimoto Makoto, Gallenne Alexandre, Ciardi David, Turner Neal, Gonzalez Jean-Francois, Vasisht Gautam, Monnier John D., Zhu Zhaohuan, Weigelt Gerd, Quiroga-Nunez Luis Henry, Kratter Kaitlin, Ramos Almeida Cristina, Juhasz Attila, Kley Wilhelm, Smith Michael, Espaillat Catherine, Alonso Herrero Almudena, Paladini Claudia, Pope Benjamin, Bate Matthew R., de Wit Willem-Jan, Harries Tim J., Lacour Sylvestre, Boyajian Tabetha, Petrov Romain, Paardekooper Sijme-Jan, Laughlin Greg, Nelson Richard P., Hoenig Sebastian, Pepper Joshua, Stassun Keivan, Jensen Eric L. N., Bonsor Amy, Kraus Stefan, Haniff Chris, Reynold Mark, Panic Olja, Sean N. Raymond, Masset Frederic, van Belle Gerard, Morbidelli Alessandro, Kane Stephen R., Ireland Michael J., Surdej Jean, Oudmaijer Rene, Benisty Myriam, Micromotive GmbH, Mainz, Germany, Université Paris Diderot - Paris 7 (UPD7), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université libre de Bruxelles (ULB), The Breakthrough Breast Cancer Research Centre, Institute of cancer research, Institut de Biologie du Développement de Marseille (IBDM), Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), foreign laboratories (FL), CERN [Genève], Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, 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), Department of Materials Science and Engineering, Institute of Ceramics and Glass-Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Pontifical Catholic University of Paraná (PUCPR), Pontifical Catholic University of Paraná, UNESCO Chinese Center of Marine Biotechnology, Ocean University of China, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), École Supérieure Polytechnique de Dakar (ESP), Université Cheikh Anta Diop [Dakar, Sénégal] (UCAD), ECLIPSE 2016, 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), The Samuel Roberts Noble Foundation, Max-Planck-Institut für Radioastronomie (MPIFR), LT2C, Laboratoire Telecom Claude Chappe (LT2C), Université Jean Monnet [Saint-Étienne] (UJM)-Ecole d'ingenieurs Telecom Saint Etienne-Université Jean Monnet [Saint-Étienne] (UJM)-Ecole d'ingenieurs Telecom Saint Etienne, NASA ExoPlanet Science Institute (NExScI), California Institute of Technology (CALTECH), Universidad de Concepción [Chile], European Southern Observatory (ESO), Department of Physics, Durham University, Durham University, GRI-CEL, National Optical Astronomy Observatory (NOAO), Sydney Institute for Astronomy (SIfA), The University of Sydney, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Lund Observatory, Lund University [Lund], Malbet, Fabien, Creech-Eakman, Michelle J., Tuthill, Peter G., University of Exeter, Department of Astronomy, University of Michigan, Australian National University (ANU), University of California [Berkeley] (UC Berkeley), University of California (UC), Boston University [Boston] (BU), University of Southampton, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), University of Bern, Instituto de Fisica y Astronomia [Valparaiso], Universidad de Valparaiso [Chile], Vanderbilt University [Nashville], Jet Propulsion Laboratory, California Institute of Technology (JPL), 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), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Astrophysical Sciences, Princeton University, Konkoly Observatory, Research Center for Astronomy and Earth Sciences, University of Kiel, Pennsylvania State University, Department of Astronomy & Astrophysics, Institut für Planetologie [Münster], Westfälische Wilhelms-Universität Münster = University of Münster (WWU), San Francisco State University (SFSU), University of Arizona, Yale University [New Haven], Lehigh University [Bethlehem], Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln = University of Cologne, Queen Mary University of London (QMUL), Georgia State University, Atlanta, Georgia State University, University System of Georgia (USG)-University System of Georgia (USG), University of Leeds, University of Tübingen, University of Oxford, Swarthmore College, University of Kent, Sterrewacht Leiden, Universiteit Leiden, Joint Institute for VLBI ERIC, Dwingeloo (JIVE), European Southern Observatory [Santiago] (ESO), Instituto de Astrofisica de Canarias (IAC), University of Cantabria, Santander, University of Madrid, The University of Texas at San Antonio (UTSA), Kyoto Sangyo University, Max Planck Institute for Astronomy (MPIA), University of Liege, Liege, Belgium, Observatoire de Paris, Université Paris sciences et lettres (PSL), Lowell Observatory [Flagstaff], JILA, NIST, and Department of Physics, University of Colorado, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Institut de Mathématiques de Toulouse UMR5219 (IMT), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences Appliquées (INSA), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Université Libre de Bruxelles [Bruxelles] (ULB), Aix Marseille Université (AMU)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA), 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, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institute of Ceramics and Glass-Friedrich Alexander University [Erlangen-Nürnberg], 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), 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), École Supérieure Polytechnique - Université Cheikh Anta DIOP de Dakar (ESP - UCAD), 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), Samuel Roberts Noble Foundation, Inc., National Optical Astronomical Observatory (NOAO), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU)-Institute of Ceramics and Glass, Pontifícia Universidade Católica do Paraná (PUCPR), Université Jean Monnet - Saint-Étienne (UJM)-Ecole d'ingenieurs Telecom Saint Etienne-Université Jean Monnet - Saint-Étienne (UJM)-Ecole d'ingenieurs Telecom Saint Etienne, Universidad de Concepción - University of Concepcion [Chile], Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Computer science, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, 01 natural sciences, Astrobiology, 010309 optics, Planet, extrasolar planets, 0103 physical sciences, planet formation, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, high angular resolution imaging, Earth and Planetary Astrophysics (astro-ph.EP), protoplanetary disks, Planetary system, interferometry, Exoplanet, 13. Climate action, Hill sphere, Systems architecture, Key (cryptography), Astrophysics::Earth and Planetary Astrophysics, Protoplanet, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Planet Formation Imager (PFI) project aims to provide a strong scientific vision for ground-based optical astronomy beyond the upcoming generation of Extremely Large Telescopes. We make the case that a breakthrough in angular resolution imaging capabilities is required in order to unravel the processes involved in planet formation. PFI will be optimised to provide a complete census of the protoplanet population at all stellocentric radii and over the age range from 0.1 to about 100 Myr. Within this age period, planetary systems undergo dramatic changes and the final architecture of planetary systems is determined. Our goal is to study the planetary birth on the natural spatial scale where the material is assembled, which is the "Hill Sphere" of the forming planet, and to characterise the protoplanetary cores by measuring their masses and physical properties. Our science working group has investigated the observational characteristics of these young protoplanets as well as the migration mechanisms that might alter the system architecture. We simulated the imprints that the planets leave in the disk and study how PFI could revolutionise areas ranging from exoplanet to extragalactic science. In this contribution we outline the key science drivers of PFI and discuss the requirements that will guide the technology choices, the site selection, and potential science/technology tradeoffs., Comment: 13 pages, 5 figures, Proceedings of SPIE 2016

Published
2016
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14. Simultaneous Water Vapor and Dry Air Optical Path Length Measurements and Compensation with the Large Binocular Telescope Interferometer

Author

Jordan M. Stone, Denis Defrere, M. Montoya, O. Durney, Andy Skemer, E. Downey, William C. Danchi, Bertrand Mennesson, A. Vaz, Steve Ertel, Rafael Millan-Gabet, Eckhart Spalding, Philip M. Hinz, W. F. Hoffmann, John M. Hill, Michael C. Böhm, Jörg-Uwe Pott, Malbet, Fabien, Creech-Eakman, Michelle J., and Tuthill, Peter G.

Subjects
Physics, business.industry, Measure (physics), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Large Binocular Telescope, 01 natural sciences, 010309 optics, Interferometry, Optics, Path length, 0103 physical sciences, Astronomical interferometer, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Optical path length, Water vapor, Nuller, Physics::Atmospheric and Oceanic Physics
Abstract

The Large Binocular Telescope Interferometer uses a near-infrared camera to measure the optical path length variations between the two AO-corrected apertures and provide high-angular resolution observations for all its science channels (1.5-13 $\mu$m). There is however a wavelength dependent component to the atmospheric turbulence, which can introduce optical path length errors when observing at a wavelength different from that of the fringe sensing camera. Water vapor in particular is highly dispersive and its effect must be taken into account for high-precision infrared interferometric observations as described previously for VLTI/MIDI or the Keck Interferometer Nuller. In this paper, we describe the new sensing approach that has been developed at the LBT to measure and monitor the optical path length fluctuations due to dry air and water vapor separately. After reviewing the current performance of the system for dry air seeing compensation, we present simultaneous H-, K-, and N-band observations that illustrate the feasibility of our feedforward approach to stabilize the path length fluctuations seen by the LBTI nuller., Comment: SPIE conference proceedings

Published
2016

15. Co-phasing the Large Binocular Telescope: status and performance of LBTI/PHASECam

Author

Jarron Leisenring, Andy Skemer, Guido Brusa, P. Grenz, John M. Hill, T. J. McMahon, C. Veillet, Denis Defrere, Vanessa P. Bailey, Julien Lozi, E. Downey, Julian C. Christou, D. Ashby, Vidhya Vaitheeswaran, William F. Hoffmann, Keith Powell, A. Vaz, William C. Danchi, M. Montoya, Philip M. Hinz, Bertrand Mennesson, Rafael Millan-Gabet, Rajagopal, Jayadev K., Creech-Eakman, Michelle J., and Malbet, Fabien

Subjects
Physics, business.industry, Resolution (electron density), Phase (waves), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Large Binocular Telescope, Astrophysics::Cosmology and Extragalactic Astrophysics, Phaser, law.invention, Telescope, Interferometry, Optics, law, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Image resolution, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract

The Large Binocular Telescope Interferometer is a NASA-funded nulling and imaging instrument designed to coherently combine the two 8.4-m primary mirrors of the LBT for high-sensitivity, high-contrast, and high-resolution infrared imaging (1.5-13 um). PHASECam is LBTI's near-infrared camera used to measure tip-tilt and phase variations between the two AO-corrected apertures and provide high-angular resolution observations. We report on the status of the system and describe its on-sky performance measured during the first semester of 2014. With a spatial resolution equivalent to that of a 22.8-meter telescope and the light-gathering power of single 11.8-meter mirror, the co-phased LBT can be considered to be a forerunner of the next-generation extremely large telescopes (ELT)., Comment: 8 pages, 5 figures, SPIE Conference proceedings

Published
2015
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16. PIONIER: a status report

Author

Wesley A. Traub, Alain Roux, S. Rochat, T. Moulin, N. Blind, Karine Perraut, Pierre Haguenauer, P. Kern, Gerard Zins, Alain Delboulbé, Fabien Malbet, Myriam Benisty, P. Rabou, Jean-Charles Augereau, J. Knudstrup, M. Germain, Philippe Feautrier, Bernard Lazareff, Rafael Millan-Gabet, François Ménard, L. Michaud, Dan Popovic, Jean-Philippe Berger, J.-L. Lizon, F. Roussel, M. Micallef, D. Maurel, Eric Stadler, Mario Kiekebusch, Laurent Jocou, E. Tatulli, Olivier Absil, Yves Magnard, Philippe B. Gitton, J.-B. Le Bouquin, D. Gillier, Delplancke, Françoise, Rajagopal, Jayadev K., and Malbet, Fabien

Subjects
medicine.medical_specialty, Computer science, Visitor pattern, medicine, FOS: Physical sciences, Medical physics, Integrated optics, Technical committee, Astrophysics - Instrumentation and Methods for Astrophysics, Status report, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The visitor instrument PIONIER provides VLTI with improved imaging capabilities and sensitivity. The instrument started routinely delivering scientific data in November 2010, that is less than 12 months after being approved by the ESO Science and Technical Committee. We recall the challenges that had to be tackled to design, built and commission PIONIER. We summarize the typical performances and some astrophysical results obtained so far. We conclude this paper by summarizing lessons learned., Comment: To appear in the proceedings of the 2012 SPIE Conference "Astronomical Telescopes and Instrumentation"

Published
2012

17. Control interface concepts for CHARA 6-telescope fringe tracking with CHAMP+MIRC

Author

Xiao Che, John D. Monnier, Fabien Baron, Ettore Pedretti, Stefan Kraus, Rafael Millan-Gabet, Nathalie Thureau, Delplancke, Françoise, Rajagopal, Jayadev K., and Malbet, Fabien

Subjects
Observer (quantum physics), Computer science, Interface (computing), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Tracking (particle physics), law.invention, CHARA array, Telescope, Interferometry, Cophasing, law, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Remote sensing, Digital recording
Abstract

Cophasing six telescopes from the CHARA array, the CHARA-Michigan Phasetracker (CHAMP) and Michigan Infrared Combiner (MIRC) are pushing the frontiers of infrared long-baseline interferometric imaging in key scientific areas such as star- and planet-formation. Here we review our concepts and recent improvements on the CHAMP and MIRC control interfaces, which establish the communication to the real-time data recording & fringe tracking code, provide essential performance diagnostics, and assist the observer in the alignment and flux optimization procedure. For fringe detection and tracking with MIRC, we have developed a novel matrix approach, which provides predictions for the fringe positions based on cross-fringe information., 6 pages, 4 figures, published in SPIE conference proceedings (http://dx.doi.org/10.1117/12.926559)

Published
2012

18. Intricate visibility effects from resolved emission of young stellar objects: the case of MWC158 observed with the VLTI

Author

Jean-Philippe Berger, W. A. Traub, Jacques Kluska, Christophe Pinte, Rafael Millan-Gabet, Francois Menard, B. Lazareff, J.-B. Le Bouquin, Fabien Malbet, Myriam Benisty, Delplancke, Françoise, Rajagopal, Jayadev K., and Malbet, Fabien

Subjects
Physics, Channel (digital image), Young stellar object, Visibility (geometry), FOS: Physical sciences, Astrophysics, Iterative reconstruction, Star (graph theory), Stars, Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Chromatic scale, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Image restoration, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

In the course of our VLTI young stellar object PIONIER imaging program, we have identified a strong visibility chromatic dependency that appeared in certain sources. This effect, rising value of visibilities with decreasing wavelengths over one base, is also present in previous published and archival AMBER data. For Herbig AeBe stars, the H band is generally located at the transition between the star and the disk predominance in flux for Herbig AeBe stars. We believe that this phenomenon is responsible for the visibility rise effect. We present a method to correct the visibilities from this effect in order to allow "gray" image reconstruction software, like Mira, to be used. In parallel we probe the interest of carrying an image reconstruction in each spectral channel and then combine them to obtain the final broadband one. As an illustration we apply these imaging methods to MWC158, a (possibly Herbig) B[e] star intensively observed with PIONIER. Finally, we compare our result with a parametric model fitted onto the data., 14 pages, 7 figures

Published
2012

19. First faint dual-field phase-referenced observations on the Keck interferometer

Author

Sam Ragland, Rafael Millan-Gabet, K. Summers, E. Appleby, Julien Woillez, Andrew Cooper, Peter Wizinowich, Josh A. Eisner, Jörg-Uwe Pott, O. Martin, C. Felizardo, Kevin Tsubota, B. Smith, Drew Medeiros, John D. Monnier, T. Panteleeva, D. Morrison, Ed Wetherell, M. Mark Colavita, Rachel Akeson, C. Tyau, J. Herstein, Delplancke, Françoise, Rajagopal, Jayadev K., and Malbet, Fabien

Subjects
Physics, Time delay and integration, business.industry, Phase (waves), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Laser, law.invention, Interferometry, Optics, Laser guide star, law, Magnitude (astronomy), Astronomical interferometer, Astrophysics::Solar and Stellar Astrophysics, Guide star, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract

Ground-based long baseline interferometers have long been limited in sensitivity by the short integration periods imposed by atmospheric turbulence. The first observation fainter than this limit was performed on January 22, 2011 when the Keck Interferometer observed a K=11.5 target, about one magnitude fainter than its K=10.3 limit. This observation was made possible by the Dual Field Phase Referencing instrument of the ASTRA project: simultaneously measuring the real-time effects of the atmosphere on a nearby bright guide star, and correcting for it on the faint target, integration time longer than the turbulence time scale are made possible. As a prelude to this demonstration, we first present the implementation of Dual Field Phase Referencing on the interferometer. We then detail its on-sky performance focusing on the accuracy of the turbulence correction, and on the resulting fringe contrast stability. We conclude with a presentation of early results obtained with Laser Guide Star AO and the interferometer., 10 pages, 12 figures, Proc. SPIE 2012

Published
2012

20. A publication database for optical long baseline interferometry

Author

S. Lafrasse, Fabien Malbet, Peter R. Lawson, Guillaume Mella, Esther Taillifet, Malbet, Fabien, 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), Jet Propulsion Laboratory (JPL), and California Institute of Technology (CALTECH)-NASA

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Database, computer.internet_protocol, FOS: Physical sciences, computer.software_genre, 01 natural sciences, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010309 optics, Metadata, Interferometry, [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Bibcode, Scripting language, 0103 physical sciences, Instrumentation (computer programming), Baseline (configuration management), Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR.IM] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010303 astronomy & astrophysics, computer, Instrumentation and Methods for Astrophysics (astro-ph.IM), XML, Web site
Abstract

Optical long baseline interferometry is a technique that has generated almost 850 refereed papers to date. The targets span a large variety of objects from planetary systems to extragalactic studies and all branches of stellar physics. We have created a database hosted by the JMMC and connected to the Optical Long Baseline Interferometry Newsletter (OLBIN) web site using MySQL and a collection of XML or PHP scripts in order to store and classify these publications. Each entry is defined by its ADS bibcode, includes basic ADS informations and metadata. The metadata are specified by tags sorted in categories: interferometric facilities, instrumentation, wavelength of operation, spectral resolution, type of measurement, target type, and paper category, for example. The whole OLBIN publication list has been processed and we present how the database is organized and can be accessed. We use this tool to generate statistical plots of interest for the community in optical long baseline interferometry., Comment: To be published in the SPIE'2010 conference on "Optical and Infrared Interferometry II"

Published
2010

21. Tomorrow optical interferometry: astrophysical prospects and instrumental issues

Author

Fabien Malbet, Malbet, Fabien, Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, astronomical instruments, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics, optical interferometry
Abstract

Interferometry has brought many new constraints in optical astronomy in the recent years. A major leap in this field is the opening of large interferometric facilities like the Very Large Telescope Interferometer and the Keck Interferometer to the astronomical community. Planning for the future is both easy --most specialists know in which directions to develop interferometry-- and difficult because of the increasing complexity of the technique. I present a short status of interferometry today. Then I detail the possible astrophysical prospects. Finally I address some important instrumental issues that are decisive for the future of interferometry., Comment: 8 pages, invited review at the "Visions in IR astronomy" conference held in Paris, 21-23 March 2006

Published
2006
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