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1. VLTI status update: tapping into a powerful second-generation instrumentation

Author

Mario Tapia, Nicolas Schuhler, M. Riquelme, Bruno Lopez, Andres Pino, Lorena Faundez, Christophe Verinaud, Frank Eisenhauer, J. Beltran, A. Ramirez, Pierre van der Heyden, Lieselotte Jochum, Jean-Baptiste Le Bouquin, J. P. Kirchbauer, Fernando Salgado, Claudia Cid, Richard Tamblay, Thibaut Moulin, Alexander Meister, Andreas Glindemann, Pierre Haguenauer, Javier Reyes, F. Delplancke-Ströbele, Angela Cortes, P. Guajardo, Stefan Huber, Anthony Meilland, Jürgen Ott, Sylvestre Lacour, Steffen Mieske, Julien Leclercq, S. Rochat, Marcus Pavez, Diego Del Valle, S. Guieu, Konrad R. W. Tristram, Sebastien Egner, Pierre Bourget, Luca Pasquini, A. Delboulbe, Christian Stephan, Pascaline Darré, Roderick Dembet, Christian A. Hummel, Peter Krempl, Marcos Suarez, Alain Smette, Pavel Shchekaturov, Yves Magnard, Ralf Conzelmann, Emmanuel Aller-Carpentier, Norbert Hubin, Isabelle Percheron, Frédéric Gonté, Jean Louis Lizon, Claudia Paladini, Thibaut Guerlet, Pablo Gutierrez, Jean-Philippe Berger, Antoine Mérand, Juan Pablo Gil, Célia Pelluet, Luis Caniguante, Johan Kosmalski, Markus Schöller, Reinaldo Donoso, Christophe Dupuy, Lorenzo Pettazzi, Laurent Jocou, Jaime Gonzales, Guillermo Valdes, Markus Wittkowski, Julien Woillez, Daniel Gaytan, Jaime Alonso, Sébastien Poupar, Xavier Haubois, Roberto Abuter, Gérard Zins, Bruno Chazelas, Eloy Fuenteseca, Paul Bristow, Laurent Pallanca, R. Frahm, Thomas Rivinius, Johann Kolb, and Juan Osorio

Subjects
Interferometry, Upgrade, Computer science, Real-time computing, Tapping, Context (language use), Instrumentation (computer programming), Adaptive optics, Status report
Abstract

Following the arrival of MATISSE, the second-generation of VLTI instrumentation is now complete and was simultaneously enhanced by a major facility upgrade including the NAOMI Adaptive Optics on the Auxiliary Telescopes. On the Unit Telescopes, significant efforts were also made to improve the injection stability into VLTI instruments. On top of GRAVITY's own evolution, its fringe tracker is now being used to allow coherent integrations on MATISSE (the so-called GRA4MAT project). Meanwhile, operations also evolved to be more flexible and make the most of an extended observing parameter space. In this context, we present an overview of the current VLTI performances. Finally, we will report on on-going improvements such as the extension of the longest baselines.

Published
2020

2. NAOMI: the adaptive optics system of the Auxiliary Telescopes of the VLTI

Author

E. Cottalorda, C. Heritier, F. Delplancke-Ströbele, S. Zúñiga-Fernández, S. Guieu, Javier Reyes, M. Seidel, Alexander Meister, Laurent Jocou, Johan Kosmalski, G. Santos Tomás, Oliver Pfuhl, Pierre Bourget, Marcos Suarez, Christophe Verinaud, J. L. Beuzit, Anthony Meilland, Philippe B. Gitton, Andreas Haimerl, J.-B. Le Bouquin, Eric Stadler, C. Frank, Christophe Dupuy, Lorenzo Pettazzi, Pascaline Darré, Xavier Haubois, Gérard Zins, Frédéric Gonté, Jaime Alonso, Bruno Lopez, R. Donaldson, Peter Krempl, H. Bonnet, Pavel Shchekaturov, Johann Kolb, Frank Eisenhauer, Pablo Gutierrez, Thibaut Guerlet, Paul Lilley, Julien Woillez, J. P. Berger, Gerhard Fischer, M. Todorovic, Sebastien Egner, A. Mérand, Thibaut Moulin, Luis Caniguante, Christian Stephan, J. P. Kirchbauer, Luigi Andolfato, Guillermo Valdes, N. Hubin, D. Phan, Eloy Fuenteseca, Stewart McLay, M. Riedel, Isabelle Percheron, A. Delboulbe, Jerome Paufique, W. Pirani, Christian Schmid, Christian Soenke, J. Dupeyron, Jose Abad, Andrew Rakich, M. Le Louarn, Pablo Barriga, Stefan Huber, P. Haguenauer, Paul Jolley, G. Bourdarot, E. Aller Carpentier, R. Brast, Nicolas Schuhler, B. Delabre, Reinhold J. Dorn, Roderick Dembet, Sylvain Rochat, Roberto Abuter, Yves Magnard, J. Quentin, Luca Pasquini, R. Ridings, European Southern Observatory (ESO), 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]), Centre Spatial Universitaire de Grenoble ( CSUG), CRLCC Eugène Marquis (CRLCC), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Wavefront, Coupling, Very Large Telescope, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Tracking (particle physics), 01 natural sciences, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010309 optics, Interferometry, Optics, Space and Planetary Science, 0103 physical sciences, Astronomical seeing, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, business, Adaptive optics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics
Abstract

The tip-tilt stabilisation system of the 1.8 m Auxiliary Telescopes of the Very Large Telescope Interferometer was never dimensioned for robust fringe tracking, except when atmospheric seeing conditions are excellent. Increasing the level of wavefront correction at the telescopes is expected to improve the coupling into the single-mode fibres of the instruments, and enable robust fringe tracking even in degraded conditions. We deployed a new adaptive optics module for interferometry (NAOMI) on the Auxiliary Telescopes. We present its design, performance, and effect on the observations that are carried out with the interferometric instruments., Comment: 10 pages, 18 figures, 2 tables, A&A forthcoming

Published
2019

3. The AO in AOF

Author

Robin Arsenault, Johann Kolb, Joel Vernet, Norbert Hubin, Sylvain Oberti, Marcos Suarez Valles, Lorenzo Pettazzi, Pierre-Yves Madec, Jerome Paufique, Javier Argomedo, Mario Kiekebusch, Paolo La Penna, Andrés Guesalaga, Pierre Haguenauer, Christian Soenke, Miska Le Louarn, Robert Donaldson, and B. Jeram

Subjects
Wavefront, Very Large Telescope, business.industry, Computer science, media_common.quotation_subject, Strehl ratio, Optics, Limiting magnitude, Sky, Tomography, business, Adaptive optics, Secondary mirror, media_common
Abstract

The long commissioning of the Adaptive Optics Facility (AOF) project has been completed shortly after this conference, providing AO correction to two Very Large Telescope (VLT) foci supported by an adaptive secondary mirror and four laser guide stars. Four AO modes are delivered: a Single Conjugate AO (SCAO) system for commissioning purpose, wide field and medium field Ground Layer AO (GLAO) for seeing improvement and narrow field Laser Tomography AO (LTAO) for ultimate performance. This paper intends to describe the implemented AO baseline and to highlight the most relevant results and lessons learned. In particular, it will address the control and reconstruction strategy, the wavefront sensing baseline and the online telemetry used to optimize the system online, estimate the turbulence profile and calibrate the misregistrations. Focusing on the LTAO mode, we will describe the tomography optimization, by exploring the reconstruction parameter space. Finally, on sky performance results will be presented both in terms of strehl ratio and limiting magnitude.

Published
2018

4. VLTI status update: three years into the second generation

Author

Pierre van der Heyden, Roberto Abuter, Thibaut Guerlet, Andreas Glindemann, Yves Magnard, Frédéric Gonté, Andreas Haimerl, Andres Pino, Nicolas Schuhler, Richard Tamblay, Alexander Meister, Xavier Haubois, Pierre Haguenauer, Frederic Derie, Stefan Huber, Christian Stephan, Isabelle Percheron, Sébastien Poupar, Angela Cortes, Javier Reyes, F. Delplancke-Ströbele, J. Quentin, Roderick Dembet, Marcos Suarez, Julien Woillez, A. Ramirez, Christophe Verinaud, Mario Tapia, Luca Pasquini, Jean-Baptiste Le Bouquin, J. P. Kirchbauer, Emmanuel Aller-Carpentier, Pierre Bourget, R. Brast, José Antonio Abad, S. Rochat, Eloy Fuenteseca, Ralf Conzelmann, S. Guieu, A. Delboulbe, Pablo Barriga, Marcus Pavez, R. Frahm, Jean-Philippe Berger, Guillermo Valdes, Diego Del Valle, Sebastien Egner, Pascaline Darré, Antoine Mérand, R. Ridings, Christophe Dupuy, Lorenzo Pettazzi, Luigi Andolfato, Jerome Paufique, Lieselotte Jochum, Thomas Rivinius, Daniel Gaytan, Paul Bristow, Jean Francois Pirard, Pedro Mardones, Paul Jolley, Reinaldo Donoso, Fernando Salgado, Samuel Lévêque, Johann Kolb, Peter Krempl, Philippe Duhoux, Juan Osorio, Stephane Guisard, Gérard Zins, Willem-Jan de Wit, Jürgen Ott, Pavel Shchekaturov, Thibaut Moulin, Paul Lilley, Jean Louis Lizon, Laurent Pallanca, Andreas Förster, Norbert Hubin, Thanh Phan Duc, Johan Kosmalski, Markus Schöller, Luis Caniguante, Konrad R. W. Tristram, Jaime Alonso, Pablo Gutierrez, J. Beltran, Laurent Jocou, and Jaime Gonzales

Subjects
Interferometry, Upgrade, business.industry, Computer science, Astrometry, Telecommunications, business, Adaptive optics
Abstract

The near-infrared GRAVITY instrument has become a fully operational spectro-imager, while expanding its capability to support astrometry of the key Galactic Centre science. The mid-infrared MATISSE instrument has just arrived on Paranal and is starting its commissioning phase. NAOMI, the new adaptive optics for the Auxiliary Telescopes, is about to leave Europe for an installation in the fall of 2018. Meanwhile, the interferometer infrastructure has continuously improved in performance, in term of transmission and vibrations, when used with both the Unit Telescopes and Auxiliary Telescopes. These are the highlights of the last two years of the VLTI 2nd generation upgrade started in 2015.

Published
2018

5. First scattered light detection of a nearly edge-on transition disk around the T Tauri star RY Lupi

Author

A. Pohl, Alice Zurlo, Anne-Lise Maire, R. van Boekel, T. Kopytova, C. Petit, Mickael Bonnefoy, Marcos Suarez, Tristan Buey, Dino Mesa, Christian Ginski, Myriam Benisty, R. G. Gratton, R. Ligi, P. Blanchard, Anthony Cheetham, Enrico Cascone, Anthony Boccaletti, Yves Magnard, Th. Henning, Raphaël Galicher, Maud Langlois, Carsten Dominik, Hubert Klahr, L. Weber, J. de Boer, Arthur Vigan, Christophe Pinte, Quentin Kral, Francois Menard, M. Feldt, Anne-Marie Lagrange, S. Peretti, Markus Janson, S. Messina, Julien Girard, Henning Avenhaus, Gael Chauvin, L. Denneulin, O. Möller-Nilsson, J. Pragt, Silvano Desidera, Tomas Stolker, E. Sissa, 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), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Heidelberg University, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Instituto de Astronomia y ciencias Planetarias de Atacama (INCT), Universidad de Atacama, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Stockholm University, University of Cambridge [UK] (CAM), Geneva Observatory, University of Geneva [Switzerland], European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Capodimonte (OAC), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, NOVA Optical Infrared Instrumentation Group, Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Genève = University of Geneva (UNIGE), Universiteit Leiden, 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), and Low Energy Astrophysics (API, FNWI)

Subjects
INFRARED DEVICES, NUMERICAL [METHODS], Polarimetry, FOS: Physical sciences, Context (language use), DUST, POLARIMETERS, Astrophysics, 01 natural sciences, methods: numerical, 010309 optics, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, observational, techniques: polarimetric [protoplanetary disks, planet-disk interactions, methods], SILICATES, Adaptive optics, NUMERICAL METHODS, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), PLANET-DISK INTERACTIONS, POLARIMETRIC [TECHNIQUES], ADAPTIVE OPTICS, Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], protoplanetary disks, NUMERICALS [METHODS], Astronomy and Astrophysics, Wavelength, T Tauri star, techniques: polarimetric, LIGHT, 13. Climate action, Space and Planetary Science, OBSERVATIONAL [METHODS], Astrophysics::Earth and Planetary Astrophysics, LIGHT SCATTERING, methods: observational, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], PROTOPLANETARY DISKS, STARS, Astrophysics - Earth and Planetary Astrophysics, PLANETS
Abstract

Context. Transition disks are considered sites of ongoing planet formation, and their dust and gas distributions could be signposts of embedded planets. The transition disk around the T Tauri star RY Lup has an inner dust cavity and displays a strong silicate emission feature. Aims. Using high-resolution imaging we study the disk geometry, including non-axisymmetric features, and its surface dust grain, to gain a better understanding of the disk evolutionary process. Moreover, we search for companion candidates, possibly connected to the disk. Methods. We obtained high-contrast and high angular resolution data in the near-infrared with the VLT/SPHERE extreme adaptive optics instrument whose goal is to study the planet formation by detecting and characterizing these planets and their formation environments through direct imaging. We performed polarimetric imaging of the RY Lup disk with IRDIS (at 1.6 μm), and obtained intensity images with the IRDIS dual-band imaging camera simultaneously with the IFS spectro-imager (0.9-1.3 μm). Results. We resolved for the first time the scattered light from the nearly edge-on circumstellar disk around RY Lup, at projected separations in the 100 au range. The shape of the disk and its sharp features are clearly detectable at wavelengths ranging from 0.9 to 1.6 μm. We show that the observed morphology can be interpreted as spiral arms in the disk. This interpretation is supported by in-depth numerical simulations. We also demonstrate that these features can be produced by one planet interacting with the disk. We also detect several point sources which are classified as probable background objects. © 2018 ESO. Acknowledgements. We acknowledge our anonymous reviewers for the very careful reading and constructive suggestions that contributed to improving this paper. SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF–Osservatorio di Padova (Italy), Observatoire astronomique de l’universite de Geneve (Switzerland), ETH Zurich (Switzerland), NOVA (Netherlands), ONERA (France), and ASTRON (Netherlands) in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland), and NOVA (Netherlands). SPHERE also received funding from the European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (2004-2008), grant number 226604 for FP7 (2009-2012), and grant number 312430 for FP7 (2013-2016). This work was supported by the Programme National de Planétologie (PNP) and the Programme National de Physique Stellaire (PNPS) of CNRS-INSU co-funded by CNES. This work has also been supported by a grant from the French Labex OSUG2020 (Investisse-ments d’avenir - ANR10 LABX56) and by the ANR grant ANR-14-CE33-0018 (GIPSE). This work has made use of the SPHERE Data Centre, jointly operated by OSUG/IPAG (Grenoble), PYTHEAS /LAM/CeSAM (Marseille), OCA/Lagrange (Nice), and Observatoire de Paris/LESIA (Paris). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. Q. Kral also acknowledges support from STFC (consolidated grant) via the institute of Asronomy, Cambridge.

Published
2018

6. NAOMI: a low-order adaptive optics system for the VLT interferometer

Author

Pavel Shchkaturov, Julien Woillez, Angela Cortes, Javier Reyes, Jean-Baptiste Le Bouquin, Norbert Hubin, Paul Jolley, Rob Donaldson, Jean-Jacques Correia, Yves Magnard, F. Delplancke-Ströbele, Marcos Suarez, Laurence Michaud, Thanh Phan Duc, Sebastian Egner, Emmanuel Aller-Carpentier, Miska Le Louarn, J. Quentin, Stefan Huber, T. Moulin, Frédéric Gonté, Luca Pasquini, Luigi Andolfato, Jaime Alonso, Guillermo Valdes, R. Ridings, Reinhold J. Dorn, Didier Maurel, Jean-Philippe Berger, Paul Lilley, Sylvain Rochat, Christophe Dupuy, Alessandro Martis, Alain Roux, Jerome Paufique, J. P. Kirchbauer, Jean-Luc Beuzit, Christophe Verinaud, Alain Delboulbé, and Eric Stadler

Subjects
Physics, Wavefront, Interferometry, Optics, 010308 nuclear & particles physics, business.industry, 0103 physical sciences, Astronomical interferometer, Strehl ratio, business, Adaptive optics, 010303 astronomy & astrophysics, 01 natural sciences
Abstract

The New Adaptive Optics Module for Interferometry (NAOMI) will be developed for and installed at the 1.8-metre Auxiliary Telescopes (ATs) at ESO Paranal. The goal of the project is to equip all four ATs with a low-order Shack– Hartmann adaptive optics system operating in the visible. By improving the wavefront quality delivered by the ATs for guide stars brighter than R = 13 mag, NAOMI will make the existing interferometer performance less dependent on the seeing conditions. Fed with higher and more stable Strehl, the fringe tracker(s) will achieve the fringe stability necessary to reach the full performance of the second-generation instruments GRAVITY and MATISSE.

Published
2016

7. Laboratory results of the AOF system testing

Author

Mario Kiekebusch, Jerome Paufique, Miska Le Louarn, Stefan Ströbele, Pierre Haguenauer, Pierre-Yves Madec, J. Valenzuela, Christian Soenke, E. Vernet, Sylvain Oberti, Philippe Duhoux, Robin Arsenault, Marcos Suarez Valles, Emmanuel Aller-Carpentier, Juan Carlos Guerra, Paolo La Penna, Johann Kolb, Javier Argomedo, and Robert Donaldson

Subjects
Hexapod, Test bench, Computer science, System testing, 02 engineering and technology, 021001 nanoscience & nanotechnology, 01 natural sciences, law.invention, 010309 optics, Telescope, Cardinal point, law, 0103 physical sciences, 0210 nano-technology, Adaptive optics, Secondary mirror, Simulation
Abstract

For two years starting in February 2014, the AO modules GRAAL for HAWK-I and GALACSI for MUSE of the Adaptive Optics Facility project have undergone System Testing at ESO's Headquarters. They offer four different modes: NGS SCAO, LGS GLAO in the IR, LGS GLAO and LTAO in the visible. A detailed characterization of those modes was made possible by the existence of ASSIST, a test bench emulating an adaptive VLT including the Deformable Secondary Mirror, a star simulator and turbulence generator and a VLT focal plane re-imager. This phase aimed at validating all the possible components and loops of the AO modules before installation at the actual VLT that comprises the added complexity of real LGSs, a harsher non-reproducible environment and the adaptive telescope control. In this paper we present some of the major results obtained and challenges encountered during the phase of System Tests, like the preparation of the Acquisition sequence, the testing of the Jitter loop, the performance optimization in GLAO and the offload of low-order modes from the DSM to the telescope (restricted to the M2 hexapod). The System Tests concluded with the successful acceptance, shipping, installation and first commissioning of GRAAL in 2015 as well as the acceptance and shipping of GALACSI, ready for installation and commissioning early 2017.

Published
2016

8. Adaptive Optics Facility: control strategy and first on-sky results of the acquisition sequence

Author

Jerome Paufique, Wolfgang Hackenberg, Harald Kuntschner, Marcos Suarez, P. La Penna, Rob Donaldson, Robin Arsenault, Johann Kolb, Javier Argomedo, Mario Kiekebusch, P. Y. Madec, and Sylvain Oberti

Subjects
Wavefront, Physics, business.industry, Active optics, Frame rate, 01 natural sciences, Deformable mirror, law.invention, 010309 optics, Telescope, Laser guide star, law, 0103 physical sciences, Adaptive optics, business, Secondary mirror, 010303 astronomy & astrophysics, Simulation, Computer hardware
Abstract

The Adaptive Optics Facility is an ESO project aiming at converting Yepun, one of the four 8m telescopes in Paranal, into an adaptive telescope. This is done by replacing the current conventional secondary mirror of Yepun by a Deformable Secondary Mirror (DSM) and attaching four Laser Guide Star (LGS) Units to its centerpiece. In the meantime, two Adaptive Optics (AO) modules have been developed incorporating each four LGS WaveFront Sensors (WFS) and one tip-tilt sensor used to control the DSM at 1 kHz frame rate. The four LGS Units and one AO module (GRAAL) have already been assembled on Yepun. Besides the technological challenge itself, one critical area of AOF is the AO control strategy and its link with the telescope control, including Active Optics used to shape M1. Another challenge is the request to minimize the overhead due to AOF during the acquisition phase of the observation. This paper presents the control strategy of the AOF. The current control of the telescope is first recalled, and then the way the AO control makes the link with the Active Optics is detailed. Lab results are used to illustrate the expected performance. Finally, the overall AOF acquisition sequence is presented as well as first results obtained on sky with GRAAL.

Published
2016

9. AOF LTAO mode: reconstruction strategy and first test results

Author

Jean-François Sauvage, Pierre-Yves Madec, Robin Arsenault, Paolo La Penna, Johann Kolb, Miska Le Louarn, Thierry Fusco, Robert Donaldson, Sylvain Oberti, Marcos Suarez Valles, Benoit Neichel, and Christian Soenke

Subjects
Physics, Tomographic reconstruction, business.industry, 01 natural sciences, Projection (linear algebra), Deformable mirror, Matrix multiplication, 010309 optics, Optical axis, Laser guide star, Optics, 0103 physical sciences, Tomography, Adaptive optics, business, 010303 astronomy & astrophysics
Abstract

GALACSI is the Adaptive Optics (AO) system serving the instrument MUSE in the framework of the Adaptive Optics Facility (AOF) project. Its Narrow Field Mode (NFM) is a Laser Tomography AO (LTAO) mode delivering high resolution in the visible across a small Field of View (FoV) of 7.5" diameter around the optical axis. From a reconstruction standpoint, GALACSI NFM intends to optimize the correction on axis by estimating the turbulence in volume via a tomographic process, then projecting the turbulence profile onto one single Deformable Mirror (DM) located in the pupil, close to the ground. In this paper, the laser tomographic reconstruction process is described. Several methods (virtual DM, virtual layer projection) are studied, under the constraint of a single matrix vector multiplication. The pseudo-synthetic interaction matrix model and the LTAO reconstructor design are analysed. Moreover, the reconstruction parameter space is explored, in particular the regularization terms. Furthermore, we present here the strategy to define the modal control basis and split the reconstruction between the Low Order (LO) loop and the High Order (HO) loop. Finally, closed loop performance obtained with a 3D turbulence generator will be analysed with respect to the most relevant system parameters to be tuned.

Published
2016

10. CIAO: wavefront sensors for GRAVITY

Author

Frank Eisenhauer, M. Ebert, Ralf-Rainer Rohloff, Frédéric Gonté, Lieselotte Jochum, Gert Finger, J. Moreno-Ventas, Johann Kolb, Stefan Hippler, Sarah Kendrew, Michael Esselborn, Armin Huber, Marcos Suarez, Jose Ramos, Tobias Adler, Martin Kulas, M. Riquelme, Johana Panduro, Sylvain Oberti, Adrian M. Glauser, Jürgen Ott, Laurent Jocou, Gérard Zins, Yann Clénet, Fanny Chemla, E. Müller, Zoltan Hubert, Rainer Lenzen, G. Rousset, M. Mellein, Gerd Jakob, Nicolas Schuhler, Henri Bonnet, Wolfgang Brandner, Pierre Bourget, Werner Laun, Francoise Delplancke, Casey Deen, Udo Neumann, Eric Gendron, Thomas Henning, Silvia Scheithauer, Ralf Klein, Laurent Pallanca, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Orbital mechanics, 01 natural sciences, law.invention, Telescope, Optics, Observatory, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, Adaptive optics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Wavefront, Physics, business.industry, Galactic Center, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Wavefront sensor, Astrophysics::Earth and Planetary Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

GRAVITY is a second generation near-infrared VLTI instrument that will combine the light of the four unit or four auxiliary telescopes of the ESO Paranal observatory in Chile. The major science goals are the observation of objects in close orbit around, or spiraling into the black hole in the Galactic center with unrivaled sensitivity and angular resolution as well as studies of young stellar objects and evolved stars. In order to cancel out the effect of atmospheric turbulence and to be able to see beyond dusty layers, it needs infrared wave-front sensors when operating with the unit telescopes. Therefore GRAVITY consists of the Beam Combiner Instrument (BCI) located in the VLTI laboratory and a wave-front sensor in each unit telescope Coude room, thus aptly named Coude Infrared Adaptive Optics (CIAO). This paper describes the CIAO design, assembly, integration and verification at the Paranal observatory.

Published
2016

11. SAXO: the extreme adaptive optics system of SPHERE (I) system overview and global laboratory performance

Author

Denis Perret, Kjetil Dohlen, Cyril Petit, Mark Downing, Hans Martin Schmid, Philippe Feautrier, Jean-François Sauvage, Dimitri Mawet, Anne Costille, David Mouillet, Julien Girard, Marcos Suarez, Arnaud Sevin, Bernardo Salasnich, Francois Wildi, Arthur Vigan, Ronald Roelfsema, Pierre Baudoz, Markus Kasper, Pascal Puget, Sylvain Rochat, Christian Soenke, Enrico Fedrigo, Thierry Fusco, Jared O'Neal, Andrea Baruffolo, Jean-Luc Beuzit, Emmanuel Hugot, ONERA - The French Aerospace Lab [Châtillon], ONERA, 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), European Southern Observatory (ESO), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), 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), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institut de Planétologique et d'Astrophysique de Institut de Planétologique et d'Astrophysique de Grenoble, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), NOVA-ASTRON, ONERA-Université Paris Saclay (COmUE), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université 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), Université de Genève = University of Geneva (UNIGE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), ITA, FRA, DEU, NLD, and CHE

Subjects
IMAGERIE À HAUT CONTRASTE, OPTIQUE ADAPTATIVE, 7. Clean energy, 01 natural sciences, law.invention, 010309 optics, Telescope, law, Observatory, 0103 physical sciences, Adaptive optics, 010303 astronomy & astrophysics, Instrumentation, Coronagraph, Remote sensing, EXOPLANETE, Physics, Very Large Telescope, Mechanical Engineering, Strehl ratio, Astronomy and Astrophysics, H band, Exoplanet, Electronic, Optical and Magnetic Materials, Space and Planetary Science, Control and Systems Engineering, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic
Abstract

International audience; The direct imaging of exoplanet is a leading field of today’s astronomy. The photons coming from the planet carry precious information on the chemical composition of its atmosphere. The second-generation instrument, Spectro-Polarimetric High contrast Exoplanet Research (SPHERE), dedicated to detection, photometry and spectral characterization of Jovian-like planets, is now in operation on the European very large telescope. This instrument relies on an extreme adaptive optics (XAO) system to compensate for atmospheric turbulence as well as for internal errors with an unprecedented accuracy. We demonstrate the high level of performance reached by the SPHERE XAO system (SAXO) during the assembly integration and test (AIT) period. In order to fully characterize the instrument quality, two AIT periods have been mandatory. In the first phase at Observatoire de Paris, the performance of SAXO itself was assessed. In the second phase at IPAG Grenoble Observatory, the operation of SAXO in interaction with the overall instrument has been optimized. In addition to the first two phases, a final check has been performed after the reintegration of the instrument at Paranal Observatory, in the New Integration Hall before integration at the telescope focus. The final performance aimed by the SPHERE instrument with the help of SAXO is among the highest Strehl ratio pretended for an operational instrument (90% in H band, 43% in V band in a realistic turbulence r0, and wind speed condition), a limit R magnitude for loop closure at 15, and a robustness to high wind speeds. The full-width at half-maximum reached by the instrument is 40 mas for infrared in H band and unprecedented 18.5 mas in V band.; L'imagerie directe d'exoplanètes est un domaine phare de l'astronomie actuelle. Les photons issus de la planète sont porteurs d'une information précieuse sur la composition chimique de son atmosphère. L'instrument de seconde génération SPHERE, Spectro-Polarimetri High-contrast Exoplanet Research, dédié à la détection la photométrie et la caractérisation spectrale de planètes joviennes, est maintenant en opération sur le très grand télescope Européen (VLT). Cet instrument repose sur une optique adaptative à très hautes performances (XAO) pour compenser les turbulences atmosphériques, comme les défauts optiques internes de l'instrument lui-même. Nous démontrons les très hauts niveaux de performance atteint par l'instrument SPHERE et son système de XAO SAXO, pendant la phase d'intégration (AIT). Pour pleinement caractériser les performances de l'instrument, deux périodes d'AIT ont été obligatoires. Dans la première phase à l'Observatoire de Paris, les performances de l'optique adaptative seule ont été obtenues. Dans la seconde phase à l'observatoire de Grenoble, l'opération de SAXO en interaction avec le reste de l'instrument ont été optimisées. En sus, une vérification finale a été faite au foyer du télescope. Les performances atteintes par SPHERE avec l'aide de SAXO sont parmi les plus hauts rapports de Strehl jamais atteint pour un instrument opérationnel (90% en bande H, 43% en bande V, sous hypothèse de turbulence et de vent classiques), et surtout une magnitude limite de R=15. La FHWM (largeur à mi-hauteur, la résolution de l'instrument) atteinte en bande H est de 40mas, et atteint une valeur sans précédent de 18.5mas en bande V.

Published
2016

12. Wave-front sensor strategies for SPHERE: first on-sky results and future improvements

Author

Anne Costille, Jean-François Sauvage, Cyril Petit, Thierry Fusco, Mark Downing, Pierre Baudoz, Laurent M. Mugnier, David Mouillet, Marcos Suarez Valles, Andrea Baruffolo, Kjetil Dohlen, Jean-Luc Beuzit, Markus Kasper, and Philippe Feautrier

Subjects
Wavefront, Physics, Spatial filter, business.industry, Noise reduction, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Speckle pattern, Optics, Robustness (computer science), Electronic engineering, Guide star, business, Adaptive optics
Abstract

SPHERE instrument [1] (Spectro-Polarimetry High-contrast Exoplanet Research) is a second generation ESO instrument dedicated to high contrast imaging, and exoplanet direct detection and characterisation. The overall performance of XAO system of SPHERE, as well as the optimal control law for turbulence correction, are presented in dedicated papers [5,6]. The global performance of the instrument and of all observing modes of SPHERE is done in [4]. The strategy of Wave-front Sensing [WFS] in SPHERE relies on two faces, and is thoroughly discussed in this paper. Firstly, extreme adaptive optics (XAO) is required for both turbulence and quasi-static pattern compensation. Particularly, the high frame rate and large subaperture numbers of the Shack-Hartmann WFS allows SAXO to optimally measure and compensate for atmospherical turbulence. Moreover, the spatial filtering [7,8] allows one to deepen the contrast curve, and is automatically adjusted on turbulence level to provide the best performance. Finally, a dedicated calibration procedure based on focal-plane wave-front sensing is optimized for NCPA compensation on the coronagraphic device, ensuring the best compensation of quasi-static speckle. Secondly, a high robustness to faint magnitude guide star allows SAXO to address a large panel of targets for exoplanet detection and characterization. This is only made possible by the joint use of a dedicated Wave- Front Sensing for turbulence, EMCCD detector capability, and adaptation of the system to the star magnitude. The noise propagation has been carefully monitored and optimized. The weighted center of gravity gives an optimal trade-off between performance with respect to noise, and complexity of implementation. The use of an EMCCD detector allows a powerful noise reduction on the wave-front sensor detector. And finaly, 5 SAXO observing modes are defined in order to cover all star magnitudes up to 16, with systematic optimal performance. During the whole assembly integrations and test period, choices have been done to optimise the trade-off between performance, robustness, and simplicity of use. The self-adaptation and auto-calibration of the instrument has been a strong investment, as well as developing a great simplicity of use. We describe here the actions taken to reach this level of operation for SPHERE. Finally, perspective are withdrawn for improving the strategy of WFS in the framework of future XAO instrumentations in E-ELT.

Published
2014

13. NAOMI: a new adaptive optics module for interferometry

Author

Enrico Marchetti, Andrew Rakich, Christian Schmid, Javier Reyes, Jean-Philippe Berger, Miska Le Louarn, J. Quentin, Than Phan Duc, Jerome Paufique, Christophe Dupuy, Luca Pasquini, Norbert Hubin, Stewart McLay, B. Delabre, Reinhold J. Dorn, R. Ridings, Luigi Andolfato, Marcos Suarez Valles, Emmanuel Aller-Carpentier, Paul Lilley, Enrico Fedrigo, Francoise Delplancke-Stroebele, Philippe B. Gitton, Julien Woillez, and Paul Jolley

Subjects
Physics, Interferometry, Tilt (optics), Optics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Single-mode optical fiber, Sensitivity (control systems), Avalanche photodiode, business, Adaptive optics, Encircled energy, Energy (signal processing)
Abstract

The New Adaptive Optics Module for Interferometry (NAOMI)1 is the future low order adaptive optics system to be developed for and installed at the ESO 1.8 m Auxiliary Telescopes (ATs). The four ATs2 are designed for interferometry which they are essentially dedicated for. Currently the AT’s are equipped with a fast, visible tip-tilt sensor called STRAP3 (System for Tip/tilt Removal with Avalanche Photodiodes), and the corrections are applied through a tip-tilt mirror. The goal is to equip all four ATs with a low-order Shack-Hartmann system operating in the visible for the VLTI dual feed light beams in place of the current tip-tilt correction. Because of the limited size of the ATs (1.8m diameter), a low-order system will be sufficient. The goal is to concentrate the energy into a coherent core and to make the encircled energy (into the single mode fibers) stable and less dependent on the atmospheric conditions in order to increase the sensitivity of the interferometric instruments. The system will use the ESO real time computer platform Sparta-light as the baseline. This paper presents the preliminary design concept and outlines the benefits to current and future VLTI instruments.

Published
2014

14. Sphere extreme AO control scheme: final performance assessment and on sky validation of the first auto-tuned LQG based operational system (Orale)

Author

Caroline Kulcsár, Denis Perret, J. L. Beuzit, Arnaud Sevin, David Mouillet, Thierry Fusco, Sylvain Rochat, Arthur Vigan, M. Kasper, Jean-François Sauvage, Jean-Marc Conan, Francois Wildi, A. Barrufolo, Pascal Puget, Kjetil Dohlen, Henri-François Raynaud, Bernardo Salasnich, Anne Costille, Christian Soenke, Cyril Petit, Marcos Suarez, ONERA - The French Aerospace Lab [Châtillon], ONERA, 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), Observatoire de Paris - Site de Paris (OP), 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), ESO, Physics Department [Garching], Technical University of Munich (TUM)-Technical University of Munich (TUM), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), University of Geneva, Genève, Laboratoire Charles Fabry / Spim, Laboratoire Charles Fabry (LCF), Université Paris-Sud - Paris 11 (UP11)-Institut d'Optique Graduate School (IOGS)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut d'Optique Graduate School (IOGS)-Centre National de la Recherche Scientifique (CNRS), ONERA-Université Paris Saclay (COmUE), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut 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), Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM)-Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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), and Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])

Subjects
Physics, ADAPTIVE OPTICS, CONTROL, [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], Operability, HIGH CONTRAST IMAGING, Optimal estimation, business.industry, Kalman filter, Linear-quadratic-Gaussian control, 01 natural sciences, Deformable mirror, 010309 optics, Optics, 13. Climate action, Robustness (computer science), Control theory, Integrator, 0103 physical sciences, Adaptive optics, business, 010303 astronomy & astrophysics
Abstract

International audience; The SPHERE (Spectro-Polarimetry High-contrast Exoplanet Research) instrument is an ESO project aiming at the direct detection of extra-solar planets. SPHERE has been successfully integrated and tested in Europe end 2013 and has been re-integrated at Paranal in Chile early 2014 for a first light at the beginning of May. The heart of the SPHERE instrument is its eXtreme Adaptive Optics (XAO) SAXO (SPHERE AO for eXoplanet Observation) subsystem that provides extremely high correction of turbulence and very accurate stabilization of images for coronagraphic purpose. However, SAXO, as well as the overall instrument, must also provide constant operability overnights, ensuring robustness and autonomy. An original control scheme has been developed to satisfy this challenging dichotomy. It includes in particular both an Optimized Modal Gain Integrator (OMGI) to control the Deformable Mirror (DM) and a Linear Quadratic Gaussian (LQG) control law to manage the tip-tilt (TT) mirror. LQG allows optimal estimation and prediction of turbulent angle of arrival but also of possible vibrations. A specific and unprecedented control scheme has been developed to continuously adapt and optimize LQG control ensuring a constant match to turbulence and vibrations characteristics. SPHERE is thus the first operational system implementing LQG, with automatic adjustment of its models. SAXO has demonstrated performance beyond expectations during tests in Europe, in spite of internal limitations. Very first results have been obtained on sky last May. We thus come back to SAXO control scheme, focusing in particular on the LQG based TT control and the various upgrades that have been made to enhance further the performance ensuring constant operability and robustness. We finally propose performance assessment based on in lab performance and first on sky results and discuss further possible improvements.

Published
2014

16. The SPHERE XAO system SAXO: integration, test, and laboratory performance

Author

J. L. Beuzit, Marcos Suarez, Arnaud Sevin, Pierre Baudoz, D. Perret, T. Fusco, Philippe Feautrier, David Mouillet, Jean Luc Gach, C. Petit, M. Kasper, Norbert Hubin, J.-F. Sauvage, Christian Soenke, Enrico Fedrigo, Emmanuel Hugot, Kjetil Dohlen, Jean-Christophe Sinquin, Tristan Buey, Anne Costille, Francois Wildi, Pascal Puget, Julien Charton, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Scientific instrument, Physics, Wavefront, Integration testing, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimetry, 01 natural sciences, 7. Clean energy, Exoplanet, 010309 optics, 13. Climate action, Planet, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Aerospace engineering, Adaptive optics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Host (network), Remote sensing
Abstract

Direct detection and spectral characterization of extra-solar planets is one of the most exciting and challenging areas in modern astronomy due to the very large contrast between the host star and the planet at very small angular separations. SPHERE (Spectro-Polarimetric High-contrast Exoplanet Research in Europe) is a second-generation instrument for the ESO VLT dedicated to this scientific objective. It combines an extreme adaptive optics system, various coronagraphic devices and a suite of focal instruments providing imaging, integral field spectroscopy and polarimetry capabilities in the visible and near-infrared spectral ranges. The extreme Adaptive Optics (AO) system, SAXO, is the heart of the SPHERE system, providing to the scientific instruments a flat wavefront corrected from all the atmospheric turbulence and internal defects. We present an updated analysis of SAXO assembly, integration and performance. This integration has been defined in a two step process. While first step is now over and second one is ongoing, we propose a global overview of integration results. The main requirements and system characteristics are briefly recalled, then each sub system is presented and characterized. Finally the full AO loop first performance is assessed. First results demonstrate that SAXO shall meet its challenging requirements.

Published
2012
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