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1. The crossed-sine wavefront sensor: first tests and results

Author: Laura Schreiber, Yan Feng, Alain Spang, François B. Hénault, Jean-Jacques Correia, Eric Stadler, and David Mouillet
Subjects: crossed-sine wavefront sensor, gradient transmission filter, mini-lens array, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Optics (physics.optics), Physics - Optics
Abstract: The crossed-sine wavefront sensor (WFS) is a pupil plane wavefront sensor that measures the first derivatives of the wavefront. It is made by three main components: a gradient transmission filter (GTF) built from a product of sine functions rotated by 45 degrees around the optical axis, a 2x2 mini-lens array (MLA) at the focus of the tested optical system and a detector array located on a plane conjugated to the pupil. The basic principle consists in acquiring four pupil images simultaneously, each image being observed from different points located behind the GTF. After the simulation work which demonstrated the wavefront reconstruction capability, we are now in the phase of implementation of the prototype in the lab. The crossed-sine WFS could achieve a simultaneous high spatial resolution at the pupil of the tested optics and absolute measurement accuracy comparable to that attained by laser-interferometers. In this paper we introduce seven customized phase masks and make measurements of them.First tests and resultsare demonstrated, based on which we explore the performance of our crossed-sine WFS and make comparisons with that of the laser-interferomete
Published: 2022

2. Impact of local turbulence on high-order adaptive optics

Author: Hugo Nowacki, Jean-Baptiste Le Bouquin, Carole Gouvret, Aurélie Marcotto, Sylvie Robbe Dubois, Karine Perraut, Yves Magnard, Alain Delboulbé, Eric Stadler, Sylvain Guieu, Sylvain Rochat, and Didier Maurel
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: We present an experiment set to address a standard specification aiming at avoiding local turbulence inside the Coud\'e train of telescopes. Namely, every optical surface should be kept within a 1.5$^\circ$ range around ambient temperature. Such a specification represents an important concern and constraint when developing optical systems for astronomy. Our aim was to test its criticality in the context of the development of the VLTI/NAOMI and VLTI/GRAVITY+ adaptive optics. This experiment has been conducted using the hardware of the future Corrective Optics (CO) of GRAVITY+. Optical measurements were performed in order to observe the evolution of turbulence in front of a flat mirror for which the surface temperature was controlled in a range of $22^\circ$ above ambient temperature. A time-dependent analysis of the turbulence was led along with a spatial analysis. This experiment shows no influence of temperature on local turbulence. It should be noted however that this result is only applicable to the very specific geometry described in this paper, which is representative of an adaptive optics (AO) system located inside the Coud\'e train (facing-down mirror heated on its backface).
Published: 2022

3. SAXO+, a second-stage adaptive optics for SPHERE on VLT: optical and mechanical design concept

Author: Eric Stadler, Emiliano Diolaiti, Laura Schreiber, Fausto Cortecchia, Matteo Lombini, Magali Loupias, Yves Magnard, Adriano De Rosa, Giuseppe Malaguti, Didier Maurel, Gianluca Morgante, Patrick Rabou, Sylvain Rochat, Filomena Schiavone, Luca Terenzi, Fabrice Vidal, Faustine Cantalloube, Éric Gendron, Raffaele Gratton, Julien Milli, David Mouillet, Gaël Chauvin, François Wildi, Jean-Luc Beuzit, and Anthony Boccaletti
Published: 2022

4. HARMONI at ELT: overview of the capabilities and expected performance of the ELT's first light, adaptive optics assisted integral field spectrograph

Author: Niranjan . Thatte, Dave Melotte, Benoit Neichel, David Le Mignant, Ian Bryson, Fraser Clarke, Vanessa Ferraro-Wood, Thierry Fusco, Oscar Gonzalez, Hermine Schnetler, Matthias Tecza, Sandi Wilson, Alonso Álvarez Urueña, Heribert A. Vilaseca, Santiago Arribas Mocoroa, Gonzalo José Carracedo Carballale, Alejandro Crespo, Alberto Estrada Piqueras, Miriam García García, Cecilia Martínez Martín, Miguel Pereira Santaella, Michele Perna, Javier Piqueras López, Niolas Bouché, Didier Boudon, Eric Daguisé, Karen Disseau, Jérémy J. Fensch, Adrien Girardot, Matthieu Guibert, Aurélien Jarno, Alexandre Jeanneau, Jens-Kristian Krogager, Florence Laurent, Magali Loupias, Jean-Emmanuel Migniau, Laure Piqueras, Alban Remillieux, Johan Richard, Arlette Pecontal, Lisa F. Bardou, David Barr, Sylvain Cetre, Rishi Deshmukh, Sofia Dimoudi, Marc Dubbledam, Andrew Dunn, Dimitra Gadotti, Joss J. Guy, David L. King, David J. Little, Anna McLeod, Simon Morris, Tim Morris, Kieran S. O'Brien, Emily Ronson, Russell Smith, Lazar Staykov, Mark Swinbank, Matthew Townson, Matteo Accardo, Domingo Alvarez Mendez, Elizabeth George, Joshua Hopgood, Derek Ives, Leander Mehrgan, Eric Mueller, Javier Reyes-Moreno, Ralf Conzelmann, Pablo Gutierrez Cheetham, Ángel Alonso-Sánchez, Giuseppina Battaglia, Miguel Angel Cagigas Garcia, Haresh M. Chulani, Graciela C. Delgado García, Patricia Fernández-Izquierdo, Ana Belén Fragoso López, Begoña García-Lorenzo, Alberto Hernández González, Elvio Hernández Suárez, Jose Miguel Herreros Linares, Enrique Joven, Roberto López López, Alejandro Antonio Lujan Gonzalez, Yolanda Martín, Evencio Mediavilla, Saúl Menéndez Mendoza, Luz Maria Montoya Martínez, José Peñate Castro, Álvaro Pérez, José Luis Rasilla, Rafael Rebolo-López, Luis Fernando Rodríguez-Ramos, Afrodisio Vega Moreno, Teodora Viera-Curbelo, Natacha Zanon Dametto, Alexis Carlotti, Jean-Jacques Correia, Stéphane Curaba, Alain Delboulbé, Sylvain Guieu, Adrien Hours, Zoltan Hubert, Laurent Jocou, Yves Magnard, Thibaut Moulin, Fabrice Pancher, Patrick Rabou, Eric Stadler, Maxime Vérove, Thierry Contini, Marie Larrieu, Olivier Boebion, Yan Fantéï-Caujolle, Daniel Lecron, Sylvain Rousseau, Philippe Amram, Olivier Beltramo-Martin, William Bon, Anne Bonnefoi, William Ceria, Zalpha Challita, Yannick Charles, Elodie Choquet, Carlos Correia, Anne Costille, Kjetil Dohlen, Franck Ducret, Kacem El Hadi, Jean-Luc Gach, Jean-Luc Gimenez, Olivier Groussin, Marc Jaquet, Pierre Jouve, Fabrice Madec, Felipe Pedreros Bustos, Edgard Renault, Patrice Sanchez, Arthur Vigan, Pascal Vola, Annie Zavago, Romain Fétick, Caroline Lim, Cyril Petit, Jean-Francois Sauvage, Nicolas Védrenne, Fehim Taha Bagci, Martin E. Caldwell, Ellis Elliott, Peter Hiscock, Emma Johnson, Murali Nalagatla, Aristea Seitis, Mark Wells, Martin Black, Charlotte Z. Bond, Saskia Brierley, Kenneth Campbell, Neil Campbell, James Carruthers, William Cochrane, Chris Evans, Joel Harman, William Humphreys, Thomas Louth, Chris Miller, David Montgomery, Meenu Murali, John Murray, Norman O'Malley, Ruben Sanchez-Janssen, Noah Schwartz, Patrick Smith, Jonathan Strachan, Stephen Todd, Stuart Watt, Martyn Wells, Asim Yaqoob, Eric Bell, Oleg O. Gnedin, Kayhan Gultekin, Mario Mateo, Michael Meyer, Munadi Ahmad, Jayne Birkby, Michael Booth, Michele Cappellari, Edgar Castillo Dominguez, Jorge Chao Ortiz, David Gooding, Kearn Grisdale, Andrea Hidalgo Valadez, Laurence Hogan, James Kariuki, Ian Lewis, Adam Lowe, Zeynep Ozer, Laurence Routledge, Dimitra Rigopoulou, Alec York, 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), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, DOTA, ONERA, Université Paris Saclay [Châtillon], DOTA, ONERA [Salon], and ONERA
Subjects: ELT, [PHYS]Physics [physics], [SPI]Engineering Sciences [physics], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], OPTIQUE ADAPTATIVE, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; HARMONI is the first light, adaptive optics assisted, integral field spectrograph for the European Southern Observatory’s Extremely Large Telescope (ELT). A work-horse instrument, it provides the ELT’s diffraction limited spectroscopic capability across the near-infrared wavelength range. HARMONI will exploit the ELT’s unique combination of exquisite spatial resolution and enormous collecting area, enabling transformational science. The design of the instrument is being finalized, and the plans for assembly, integration and testing are being detailed. We present an overview of the instrument’s capabilities from a user perspective, and provide a summary of the instrument’s design. We also include recent changes to the project, both technical and programmatic, that have resulted from red-flag actions. Finally, we outline some of the simulated HARMONI observations currently being analyzed.
Published: 2022

5. C-RED 2 ER: high speed extended range InGaAs cameras

Author: Isaure De Kernier, Yann Wanwanscappel, David Boutolleau, Thomas Carmignani, Fabien Clop, Philippe Feautrier, Jean-Luc Gach, Stephane Lemarchand, and Eric Stadler
Published: 2022

6. HARMONI at ELT: development of the high-contrast module

Author: Laurent Jocou, Patrick Rabou, Thibaut Moulin, Yves Magnard, Adrien Hours, Fabrice Pancher, Sylvain Guieu, Alexis Carlotti, Alain Delboulbé, Maxime Vérove, Eric Stadler, Didier Maurel, Sylvain Rochat, François Hénault, Kjetil Dohlen, Niranjan Thatte, Benoit Neichel, Pascal Vola, Fraser Clarke, Dave Melotte, Matthias Tecza, Hermine Schnetler, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience
Published: 2022

7. C-RED 2 ER: an extended range SWIR camera with applications in hyperspectral imaging

Author: Isaure De Kernier, Yann Wanwanscappel, David Boutolleau, Thomas Carmignani, Fabien Clop, Philippe Feautrier, Jean-Luc Gach, Stéphane Lemarchand, and Eric Stadler
Published: 2022

8. C-BLUE One : A family of CMOS high speed cameras for wavefront sensing

Author: Jean-Luc Gach, David Boutolleau, Thomas Carmignani, Fabien Clop, Isaure De Kernier, Philippe Feautrier, Matthieu Florentin, Stéphane Lemarchand, Jordan Pettigiani, Theo Romano, Eric Stadler, Julien Tugnoli, and Yann Wanwanscappel
Subjects: Physics - Instrumentation and Detectors, FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: We present the evolutions of the C-BLUE One family of cameras (formerly introduced as C-MORE), a laser guide star oriented wavefront sensor camera family. Within the Opticon WP2 european funded project, which has been set to develop LGS cameras, fast path solutions based on existing sensors had to be explored to provide working-proven cameras to ELT projects ready for the first light schedule. Result of this study, C-BLUE One is a CMOS based camera with 1600x1100 pixels (9um pitch) and 481 FPS refresh rate. It has been developed to answer most of the needs of future laser based adaptive optics systems (LGS) to be deployed on 20-40m-class telescopes as well as on smaller ones. We present the main features of the camera and measured performance in terms of noise, dark current, quantum efficiency and image quality which are the key parameters for the application. The camera has been declined also in fast smaller format (800x600x1500FPS) and large format (3200X2200x250FPS) to cover most of the AO applications., Comment: arXiv admin note: substantial text overlap with arXiv:1910.00374
Published: 2022
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9. TOI-269 b: an eccentric sub-Neptune transiting a M2 dwarf revisited with ExTrA

Author: Sara Seager, Eric B. Ting, Felipe Murgas, Nicholas M. Law, D. Maurel, S. Curaba, Tianjun Gan, S. Rochat, Richard G. West, George R. Ricker, Francesco Pepe, René Doyon, P. Kern, Coel Hellier, Jon M. Jenkins, Thibaut Moulin, I. C. Leão, G. Gaisne, Caroline Dorn, Xavier Bonfils, Laurent Jocou, Yves Magnard, J.-J. Correia, Eric Stadler, P. Rabou, C. Melo, Joshua N. Winn, C. Ziegler, J. D. Twicken, C. Lovis, Karen A. Collins, Nicola Astudillo-Defru, B. L. Canto Martins, Aurélien Wyttenbach, X. Delfosse, Alain Roux, Kevin I. Collins, Alain Delboulbé, J. F. Otegi, David R. Anderson, Jose-Manuel Almenara, William Waalkes, Ravit Helled, Marion Cointepas, François Bouchy, J. R. De Medeiros, Roland Vanderspek, Étienne Artigau, David Charbonneau, Pedro Figueira, T. Forveille, David W. Latham, L. Gluck, David R. Rodriguez, Andrew W. Mann, A. Wunsche, S. Lafrasse, Nuno C. Santos, Damien Ségransan, Rodrigo F. Díaz, Stéphane Udry, Philippe Feautrier, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Departamento de Matemática y Fı́sica Aplicadas [Concepcion] (DMFA), Universidad Católica de la Santísima Concepción (UCSC), 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]), and Université de Montréal (UdeM)
Subjects: 010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, 01 natural sciences, Transmission spectroscopy, Photometry (optics), Neptune, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Eccentricity (behavior), Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Radius, Orbital period, Exoplanet, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the confirmation of a new sub-Neptune close to the transition between super-Earths and sub-Neptunes transiting the M2 dwarf TOI- 269 (TIC 220479565, V = 14.4 mag, J = 10.9 mag, Rstar = 0.40 Rsun, Mstar = 0.39 Msun, d = 57 pc). The exoplanet candidate has been identified in multiple TESS sectors, and validated with high-precision spectroscopy from HARPS and ground-based photometric follow-up from ExTrA and LCO-CTIO. We determined mass, radius, and bulk density of the exoplanet by jointly modeling both photometry and radial velocities with juliet. The transiting exoplanet has an orbital period of P = 3.6977104 +- 0.0000037 days, a radius of 2.77 +- 0.12 Rearth, and a mass of 8.8 +- 1.4 Mearth. Since TOI-269 b lies among the best targets of its category for atmospheric characterization, it would be interesting to probe the atmosphere of this exoplanet with transmission spectroscopy in order to compare it to other sub-Neptunes. With an eccentricity e = 0.425+0.082-0.086, TOI-269 b has one of the highest eccentricities of the exoplanets with periods less than 10 days. The star being likely a few Gyr old, this system does not appear to be dynamically young. We surmise TOI-269 b may have acquired its high eccentricity as it migrated inward through planet-planet interactions., Comment: 23 pages, 16 figures, Accepted for publication in A&A
Published: 2021

10. NanoCarb spaceborne miniaturized GHG sensor: first experimental results

Author: J. Boussey, Christophe Coudrain, Roland Domel, Yann Ferrec, Silvère Gousset, Yves Magnard, Etienne Le Coarer, Juana Rodrigo, Philippe Perrault, Remi Gouyon, Laurence Croizé, Florence de la Barrière, Mathieu Chambon, Cécile Gourgon, Eric Stadler, Marie Panabière, Nadine Gerges, Z. Hubert, Hélène Ehrhardt, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Laboratoire des technologies de la microélectronique (LTM ), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, ANR-11-LABX-0013,FOCUS,Des détecteurs pour Observer l'Univers(2011), and European Project: 769032,SCARBO
Subjects: Operability, Power station, Imaging spectrometer, 02 engineering and technology, 7. Clean energy, 01 natural sciences, 010309 optics, [SPI]Engineering Sciences [physics], Fourier Spectrometry, Observatory, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Atmospheric Remote Sensing, [SPI.NANO]Engineering Sciences [physics]/Micro and nanotechnologies/Microelectronics, Reliability (statistics), ComputingMilieux_MISCELLANEOUS, Green House Gas Monitoring, Constellation, [PHYS]Physics [physics], [SDE.IE]Environmental Sciences/Environmental Engineering, Airborne Demonstration, Hyperspectral Sensor, 13. Climate action, Greenhouse gas, Data quality, Systems engineering, Environmental science, 020201 artificial intelligence & image processing
Abstract: International audience; The Space CARBon Observatory (SCARBO) European program aims at assessing the monitoring of anthropogenic emissions of Green House Gas (GHG) with the uncovered goal of a sub-daily revisit of the Earth at an affordable cost. One of the main project scopes is the feasibility study of a hybrid constellation including both high accuracy reference missions (Copernicus CO2M or CNES MicroCarb mission) and 24 small-satellites onboarding innovative miniaturized payloads. The key GHG-sensor of the smallsat constellation is the NanoCarb concept, an unprecedently kilogram-class Fourier Transform imaging spectrometer. We are reporting here some preliminary experimental results from a demonstration airborne campaign. A low cost, 2-bands prototype designed for CO2 and CH4 measurement has been developed then integrated over a Falcon-20 from SAFIRE, jointly to SPEX aerosol sensor from SRON. During October 2020, we flew over Spain, Italy, and towards Poland from Francazal airport in Toulouse, France. Even if we did not have the opportunity to flight over a powerplant, a lot of data has been acquired and are being processed. After presented the instrument, mission and data products, we assess the data quality and the reliability of the model. We derive finally an expected sensitivity over CO2 and CH4 columns according to the background respectively about 1.5-2.5% and 5%. We finally demonstrate the operability of this first TRL5 prototype of NanoCarb.
Published: 2021

11. The SPHERE infrared survey for exoplanets (SHINE). I. Sample definition and target characterization

Author: E. L. Rickman, Julien Charton, Stéphane Udry, A. Roux, S. Rochat, Alice Zurlo, O. Möller-Nilsson, Riccardo Claudi, D. Fantinel, A. Pavlov, E. Covino, Christian Soenke, M. Kasper, Valentina D'Orazi, Anne-Lise Maire, Joshua E. Schlieder, J. Pragt, Enrico Cascone, Markus Janson, Mariangela Bonavita, T. Kopytova, C. Petit, P. Martinez, Mickael Bonnefoy, A. Deboulbe, Joany Andreina Manjarres Ramos, Franz-Josef Hambsch, L. Weber, Francois Menard, Thibaut Moulin, A. Bazzon, Yves Magnard, Norbert Hubin, F. Rigal, Thiam-Guan Tan, Eric Stadler, J.-F. Sauvage, T. O. B. Schmidt, Emmanuel Hugot, L. Gluck, Th. Henning, S. Benatti, Michael Meyer, Raphaël Galicher, Anne-Marie Lagrange, M. Feldt, M. Carle, Carsten Dominik, G. Rousset, Matthias Samland, Tristan Buey, Janis Hagelberg, H. M. Schmid, Philippe Feautrier, D. Le Mignant, Arnaud Sevin, H. LeCoroller, Pierre Baudoz, J. Antichi, Arthur Vigan, Wolfgang Brandner, Massimo Turatto, Gael Chauvin, Alain Origne, R. Ligi, P. Gigan, Bernardo Salasnich, C. Lazzoni, V. De Caprio, M. Jaquet, D. Gisler, Pascal Puget, Philippe Delorme, D. Perret, T. Fusco, Dino Mesa, E. Sissa, Francois Wildi, Silvano Desidera, D. Maurel, F. Madec, Joseph C. Carson, J. M. Alcalá, E. Rigliaco, S. Messina, J. Baudrand, Anne Costille, R. G. Gratton, M. Millward, André Müller, Beth Biller, Enrico Giro, Andrea Baruffolo, Faustine Cantalloube, Jean-Luc Beuzit, Ronald Roelfsema, Marcel Carbillet, Eric Lagadec, Kjetil Dohlen, R. Asensio-Torres, Anthony Cheetham, P. Rabou, M. Llored, Maud Langlois, P. Blanchard, Anthony Boccaletti, C. Fontanive, Marcos Suarez, L. Abe, and Low Energy Astrophysics (API, FNWI)
Subjects: PRE-MAIN SEQUENCE [STARS], HIGH CONTRAST IMAGING, STATISTICAL CONSTRAINTS, PLANET DETECTION, FOS: Physical sciences, Sample (statistics), Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ROTATION [STARS], ROTATION PERIOD, 01 natural sciences, 7. Clean energy, FUNDAMENTAL PARAMETERS [STARS], Planet, 0103 physical sciences, GENERAL [PLANETS AND SATELLITES], DETECTION LIMITS, Astrophysics::Solar and Stellar Astrophysics, KINEMATICS AND DYNAMICS [STARS], ACTIVITY [STARS], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astronomy and Astrophysics, TARGET CHARACTERIZATION, Light curve, Exoplanet, Characterization (materials science), SPHERES, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, ORIGINAL SAMPLE, STATISTICAL SAMPLES, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Rotation (mathematics), SURVEYS, STARS, EXTRASOLAR PLANETS, Astrophysics - Earth and Planetary Astrophysics
Abstract: Large surveys with new-generation high-contrast imaging instruments are needed to derive the frequency and properties of exoplanet populations with separations from ~5 to 300 au. A careful assessment of the stellar properties is crucial for a proper understanding of when, where, and how frequently planets form, and how they evolve. The sensitivity of detection limits to stellar age makes this a key parameter for direct imaging surveys. Aims. We describe the SpHere INfrared survey for Exoplanets (SHINE), the largest direct imaging planet-search campaign initiated at the VLT in 2015 in the context of the SPHERE Guaranteed Time Observations of the SPHERE consortium. In this first paper we present the selection and the properties of the complete sample of stars surveyed with SHINE, focusing on the targets observed during the first phase of the survey (from February 2015 to February 2017). This early sample composed of 150 stars is used to perform a preliminary statistical analysis of the SHINE data, deferred to two companion papers presenting the survey performance, main discoveries, and the preliminary statistical constraints set by SHINE. Methods. Based on a large database collecting the stellar properties of all young nearby stars in the solar vicinity (including kinematics, membership to moving groups, isochrones, lithium abundance, rotation, and activity), we selected the original sample of 800 stars that were ranked in order of priority according to their sensitivity for planet detection in direct imaging with SPHERE. The properties of the stars that are part of the early statistical sample wererevisited, including for instance measurements from the Gaia Data Release 2. Rotation periods were derived for the vast majority of the late-type objects exploiting TESS light curves and dedicated photometric observations. Results. The properties of individual targets and of the sample as a whole are presented. © ESO 2021. SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF – Osservatorio di Padova (Italy), Observatoire de Genève (Switzerland), ETH Zürich (Switzerland), NOVA (Netherlands), ONERA (France) and ASTRON (Netherlands) in collaboration with ESO. SPHERE was funded by ESO, with additional contributions from CNRS (France), MPIA (Germany), INAF (Italy), FINES (Switzerland) and NOVA (Netherlands). SPHERE also received funding from the European 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 226 604 for FP7 (2009–2012) and grant number 312430 for FP7 (2013–2016). This research has made use of the SIMBAD database and Vizier services, operated at CDS, Strasbourg, France and of the Washington Double Star Catalog maintained at the US Naval Observatory. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. This paper has made use of data products available in ESO archive. Program ID: 60.A-9036(A); 072.C-0488(E) (PI Mayor), 074.C-0364(A) (PI Robichon), 074.C-0037(A) (PI Gunther), 075.C-0202(A) (PI Gunther), 075.C-0689(A) (PI Galland), 076.C-0010(A) (PI Gunther), 077.C-0012(A) (PI Gunther), 077.C-0295(D) (PI Galland), 078.D-0245(C) (PI Dall), 079.C-0046(A) (PI Gunther), 080.D-0151(A) (PI Hatzes), 080.C-0712(A) (PI Desort), 180.C-0886(A) (PI Bonfils), 082.C-0718(B) (PI Bonfils), 082.C-0427(A) (PI Doellinger), 082.C-0390(A) (PI Weise), 183.C-0437(A) (PI Bonfils), 083.C-0794(A) (PI Chauvin), 084.C-1039(A) (PI Chauvin), 184.C-0815(B) (PI Desort), 089.C-0732(A) (PI Lo Curto), 191.C-0873(D) (PI Bonfils), 192.C-0224(A) (PI Lagrange), 097.C-0864(B) (PI Lannier), 098.C-0739(A) (PI Lagrange), 099.C-0205(A) (PI Lagrange), 099.C-0458(A) (PI Lo Curto), 1101.C-0557(A) (PI Lagrange). We have used data from the WASP public archive in this research. The WASP consortium comprises of the University of Cambridge, Keele University, University of Leicester, The Open University, The Queen’s University Belfast, St. Andrews University and the Isaac Newton Group. Funding for WASP comes from the consortium universities and from the UK’s Science and Technology Facilities Council. Based on data retrieved from the SOPHIE archive at Observatoire de Haute-Provence (OHP), available at http://atlas.obs-hp.fr/sophie/. We thank the anonymous referee for useful comments. S.D., V.D., D.M. and R.G. acknowledge the support by INAF/Frontiera through the “Progetti Premiali” funding scheme of the Italian Ministry of Education, University, and Research, the PRIN-INAF 2019 “Planetary systems at young ages” (PLATEA) and the ASI-INAF agreement n.2018-16-HH.0. AV acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 757561). A.M.L. acknowledges funding from Agence Nationale de la Recherche (France) under contract number ANR-14-CE33-0018. J.C. was supported by SC Space Grant and Fulbright Colombia. M.B. acknowledges funding by the UK Science and Technology Facilities Council (STFC) grant no. ST/M001229.
Published: 2021

12. HARMONI: first light spectroscopy for the ELT: instrument final design and quantitative performance predictions

Author: Sofia Dimoudi, Jorge Chao Ortiz, Alexandre Jeanneau, Joel Vernet, Eric Daguisé, Adrien Hours, William Bon, Laurence Routledge, Ian Tosh, Eric Stadler, Ana Monreal, Kearn Grisdale, Ruben Sanchez-Janssen, Luis Fernando Rodriguez-Ramos, Jim Lynn, Alvaro Menduina, Angel Alonso Sanchez, Javier Piqueras López, Sylvain Guieu, Aurélien Jarno, Lazar Staykov, Teodora Viera, Joshua Hopgood, Chris Miller, David King, Vanessa Ferraro-Wood, Edgard Renault, Sandi Wilson, Matteo Accardo, James Carruthers, Alberto Estrada Piqueras, Matthieu Guibert, Cyril Petit, Angus Gallie, Zoltan Hubert, William Cochrane, Patricia Fernández Izquierdo, Kenny Campbell, Afrodisio Vega Moreno, Thierry Fusco, David Gooding, Patrice Sanchez, Madeline Close, Mark Swinbank, Jose Luis Rasilla, Arthur Vigan, Andrea Melissa Hidalgo, Romain Fétick, Miguel Pereira Santaella, Adam Lowe, Hermine Schnetler, Michael Meyer, E. Joven, Jean-Luc Gach, Yves Magnard, Josh Anderson, Benoit Neichel, Andy Born, José Peñate Castro, Simon L. Morris, José Linares, Kayhan Gültekin, Nicholas Bouché, Naomi Dobson, Chris Evans, John Capone, Jean-François Sauvage, Yolanda Martín Hernando, Miguel A. Cagigas, Jean-Emmanuel Migniau, Lynn Ritchie, Noah Schwartz, Didier Boudon, Ian Bryson, Alejandro Crespo, Neil Campbell, Jose Miguel Delgado, Alexis Carlotti, Johan Richard, Benoit Epinat, Matthew J. Townson, Stuart Watt, Charlotte Bond, Monica Valluri, Martin Black, Ellis Elliott, Pascal Vola, Elvio Hernandez Suarez, Miriam García García, Magali Loupias, Kacem El-Hadi, Fraser Clarke, John Murray, Matthias Tecza, Patrick Smith, Domingo Avarez Mendez, Leander Mehrgan, Nick Cann, Kjetil Dohlen, Frédéric Gonté, Karen Disseau, Lisa Bardou, Michael J. Booth, David Montgomery, Dave Melotte, Laurent Jocou, Nicola Vedrenne, Florence Laurent, Ana Belén. Fragoso López, Carlos Correia, Tom Louth, William Humphreys, Felipe Pedreros, David Henry, James Kariuki, David Le Mignant, Patrick Rabou, Elizabeth George, Olivier Beltramo-Martin, Sebastian Egner, Olivier Groussin, C. B. Lim, S. Rousseau, Myriam Rodrigues, Jean-Jacques Correia, Martyn Wells, Marc Llored, Thierry Contini, Ralf Conzelmann, Thibaut Moulin, Tea Seitis, Taha Bagci, Joel Le Merrer, Jeremy Blaizot, Oscar A. Gonzalez, Anne Bonnefoi, A. Remillieux, Diane Chapuis, Tim Morris, Derek Ives, Niranjan Thatte, Dimitra Rigopoulou, Roy Preece, Elodie Choquet, Laure Piqueras, Maria Begoña. Garcia-Lorenzo, Fabrice Pancher, Alain Delboulbe, Marie Larrieu, Battaglia Giuseppina, William Ceria, Mario Mateo, Michele Cappellari, Celine Peroux, Rishi Deshmukh, Arlette Pécontal-Rousset, Santiago Arribas, Roberto López, Joel Harman, Norman O'Malley, E. Mueller, Issa Jaafar, Zeynep Ozer, Kieran O'Brien, Anne Costille, Franck Ducret, Yan Fantei-Caujolle, Eddy Younger, Ian Lewis, Marc Dubbledam, Rafael Rebolo, Munadi Ahmad, Evencio Mediavilla, Daniel Lecron, DOTA, ONERA, Université Paris Saclay [Châtillon], and ONERA-Université Paris-Saclay
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Computer science, Integration testing, First light, 01 natural sciences, 010309 optics, Integral field spectrograph, 0103 physical sciences, Systems engineering, Milestone (project management), Extremely Large Telescope, Adaptive optics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Design review
Abstract: HARMONI is the adaptive optics assisted, near-infrared and visible light integral field spectrograph for the Extremely Large Telescope (ELT). A first light instrument, it provides the work-horse spectroscopic capability for the ELT. As the project approaches its Final Design Review milestone, the design of the instrument is being finalized, and the plans for assembly, integration and testing are being detailed. We present an overview of the instrument's capabilities from a user perspective, provide a summary of the instrument's design, including plans for operations and calibrations, and provide a brief glimpse of the predicted performance for a specific observing scenario. The paper also provides some details of the consortium composition and its evolution since the project commenced in 2015.
Published: 2020

13. Ongoing flyby in the young multiple system UX Tauri

Author: S. Rochat, Myriam Benisty, Yann Boehler, Christian Ginski, Norbert Hubin, Antonio Garufi, Alice Zurlo, R. G. van Holstein, Janis Hagelberg, Nicolás Cuello, M. Villenave, Daniel J. Price, Raffaele Gratton, Anne-Lise Maire, G. van der Plas, Garreth Ruane, S. Chripko, Arthur Vigan, P. Pinilla, H. M. Schmid, François Ménard, Eric Stadler, A. Boccaletti, Th. Henning, J. de Boer, Carsten Dominik, Jean-François Sauvage, Jean-François Gonzalez, Christophe Pinte, Maud Langlois, A. Pavlov, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Leiden Observatory [Leiden], Universiteit Leiden, 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), University of Arizona, Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Bulgarian Academy of Sciences (BAS), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016), Low Energy Astrophysics (API, FNWI), Faculty of Science, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Universiteit Leiden [Leiden], École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Semi-major axis, FOS: Physical sciences, stars: pre-main sequence, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, circumstellar matter, 01 natural sciences, 0103 physical sciences, Coming out, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, protoplanetary disks, Astronomy and Astrophysics, Polarization (waves), Position angle, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Circumstellar disk, Stars, Astrophysics - Solar and Stellar Astrophysics, binaries: general, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Scattered light, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present observations of the young multiple system UX Tauri to look for circumstellar disks and for signs of dynamical interactions. We obtained SPHERE/IRDIS deep differential polarization images in the J and H bands. We also used ALMA archival CO data. Large extended spirals are well detected in scattered light coming out of the disk of UX Tau A. The southern spiral forms a bridge between UX Tau A and C. These spirals, including the bridge connecting the two stars, all have a CO (3-2) counterpart seen by ALMA. The disk of UX Tau C is detected in scattered light. It is much smaller than the disk of UX Tau A and has a major axis along a different position angle, suggesting a misalignment. We performed PHANTOM SPH hydrodynamical models to interpret the data. The scattered light spirals, CO emission spirals and velocity patterns of the rotating disks, and the compactness of the disk of UX Tau C all point to a scenario in which UX Tau A has been perturbed very recently (about 1000 years) by the close passage of UX Tau C., Comment: Accepted for publication in Astronomy & Astrophysics Letters. (8pages, 8 figures). 2 movies will be available on-line
Published: 2020

14. HD 117214 debris disk: scattered-light images and constraints on the presence of planets

Author: Arthur Vigan, H. M. Schmid, N. Pawellek, Th. Henning, Anthony Cheetham, D. Gisler, Gael Chauvin, Mickael Bonnefoy, A-M. Lagrange, Q. Kral, Faustine Cantalloube, E. L. Rickman, Alice Zurlo, Julien Milli, S. Hunziker, N. Engler, S. Petrus, A. Boccaletti, O. Moeller-Nilsson, Philippe Thébault, M. Carle, C. Lazzoni, Silvano Desidera, Sascha P. Quanz, Markus Feldt, Maud Langlois, Michael R. Meyer, Raffaele Gratton, Francois Wildi, Johan Olofsson, Cyril Petit, Eric Stadler, Samantha Brown, Dino Mesa, Tomas Stolker, Christian Ginski, T. Buey, FRAMATOME, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, European Southern Observatory (ESO), 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Leiden Observatory [Leiden], Universiteit Leiden, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Biochemistry and Molecular Biology, Mayo Clinic, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Institute of Astronomy [ETH Zürich], Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université de Genève (UNIGE), Universiteit Leiden [Leiden], École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), 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), 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), 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)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Institut d’Électronique, de Microélectronique et de Nanotechnologie (IEMN) - UMR 8520 (IEMN), and Ecole Centrale de Lille-Institut supérieur de l'électronique et du numérique (ISEN)-Université de Valenciennes et du Hainaut-Cambrésis (UVHC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Polytechnique Hauts-de-France (UPHF)
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Debris disk, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Radius, Planetary system, Debris, Exoplanet, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We performed observations of the Sco-Cen F star HD 117214 aiming at a search for planetary companions and the characterization of the debris disk structure. HD 117214 was observed with the SPHERE subsystems IRDIS, IFS and ZIMPOL at optical and near-IR wavelengths using angular and polarimetric differential imaging techniques. This provided the first images of scattered light from the debris disk with a spatial resolution reaching 25 mas and an inner working angle $< 0.1''$. With the observations with IRDIS and IFS we derive detection limits for substellar companions. The geometrical parameters of the detected disk are constrained by fitting 3D models for the scattering of an optically thin dust disk. Investigating the possible origin of the disk gap, we introduced putative planets therein and modeled the planet-disk and planet-planet dynamical interactions. The obtained planetary architectures are compared with the detection limit curves. The debris disk has an axisymmetric ring structure with a radius of $0.42(\pm 0.01)''$ or $\sim45$ au and an inclination of $71(\pm 2.5)^\circ$ and exhibits a $0.4''$ ($\sim40$ au) wide inner cavity. From the polarimetric data, we derive a polarized flux contrast for the disk of $(F_{\rm pol})_{\rm disk}/F_{\rm \ast}> (3.1 \pm 1.2)\cdot 10^{-4}$ in the RI band. The fractional scattered polarized flux of the disk is eight times smaller than the fractional infrared flux excess. This ratio is similar to the one obtained for the debris disk HIP 79977 indicating that dust radiation properties are not very different between these two disks. Inside the disk cavity we achieve the high sensitivity limits on planetary companions with a mass down to $\sim 4 M_{\rm J}$ at projected radial separations between $0.2''$ and $0.4''$. We can exclude the stellar companions at a radial separation larger than 75 mas from the star., 20 pages
Published: 2020

15. Searching for the near-infrared counterpart of Proxima c using multi-epoch high-contrast SPHERE data at VLT

Author: Thomas Henning, Mickael Bonnefoy, Arthur Vigan, Janis Hagelberg, Gael Chauvin, Philippe Delorme, Thierry Fusco, Markus Feldt, A. Potier, A-M. Lagrange, Mario Damasso, Julien Milli, E. Sissa, Valentina D'Orazi, R. Galicher, Alessandro Sozzetti, C. Lazzoni, T. O. B. Schmidt, L. Rodet, E. Lagadec, Samantha Brown, Michael R. Meyer, Jacopo Antichi, E. L. Rickman, H. Le Coroller, Laurent M. Mugnier, F. Del Sordo, Dino Mesa, Pierre Kervella, Alice Zurlo, Faustine Cantalloube, Anthony Boccaletti, Zahed Wahhaj, Francois Wildi, Roxanne Ligi, Maud Langlois, Raffaele Gratton, Wolfgang Brandner, Marcos Suarez, Markus Janson, C. Romero, François Ménard, Judit Szulágyi, Eric Stadler, Silvano Desidera, Anne-Lise Maire, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), 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), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Biochemistry and Molecular Biology, Mayo Clinic, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, European Southern Observatory (ESO), 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), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Astronomy, Stockholm University, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Departamento de Biologia de la Reproduccion, Universidad Autonoma Metropolitana, Unidad Iztapalapa (UAM), INAF - Osservatorio Astrofisico di Torino (OATo), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), INAF - Osservatorio Astrofisico di Arcetri (OAA), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université de Genève (UNIGE), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)
Subjects: planets and satellites: detection, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Context (language use), techniques: image processing, Astrophysics, 01 natural sciences, planets and satellites: terrestrial planets, Planet, instrumentation: high angular resolution, 0103 physical sciences, Circular orbit, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, stars: individual: Proxima, Quadrature (astronomy), Orbit, Fomalhaut, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Orbital motion, planets and satellites: individual: Proxima c, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract: Proxima Centauri is known to host an earth-like planet in its habitable zone; very recently a second candidate planet was proposed based on radial velocities. At quadrature, the expected projected separation of this new candidate is larger than 1 arcsec, making it a potentially interesting target for direct imaging. While difficult, identification of the optical counterpart of this planet would allow detailed characterization of the closest planetary system. We searched for a counterpart in SPHERE images acquired during four years through the SHINE survey. In order to account for the large orbital motion of the planet, we used a method that assumes the circular orbit obtained from radial velocities and exploits the sequence of observations acquired close to quadrature in the orbit. We checked this with a more general approach that considers keplerian motion, K-stacker. We did not obtain a clear detection. The best candidate has S/N=6.1 in the combined image. A statistical test suggests that the probability that this detection is due to random fluctuation of noise is < 1% but this result depends on the assumption that distribution of noise is uniform over the image. The position of this candidate and the orientation of its orbital plane fit well with observations in the ALMA 12m array image. However, the astrometric signal expected from the orbit of the candidate we detected is 3-sigma away from the astrometric motion of Proxima as measured from early Gaia data. This, together with the unexpectedly high flux associated with our direct imaging detection, means we cannot confirm that our candidate is indeed Proxima c. On the other hand, if confirmed, this would be the first observation in imaging of a planet discovered from radial velocities and the second one (after Fomalhaut b) of reflecting circumplanetary material. Further confirmation observations should be done as soon as possible., 14 pages, 5 figures. Accepted for publication on Astronomy and Astrophysics
Published: 2020

16. The SPHERE infrared survey for exoplanets (SHINE)

Author: Kjetil Dohlen, André Müller, C. Petit, A. Pavlov, Valentina D'Orazi, Alexandre Emsenhuber, Alice Zurlo, E. Sissa, Ronald Roelfsema, Norbert Hubin, Marc Jaquet, Gabriel-Dominique Marleau, Gérard Rousset, Anthony Cheetham, H. Le Coroller, Alain Roux, S. Brown Sevilla, Enrico Giro, Faustine Cantalloube, Anne Costille, Janis Hagelberg, Jean-Luc Beuzit, Thierry Fusco, P. Gigan, Julien Charton, Markus Feldt, A. Bazzon, Ruben Asensio-Torres, C. Fontanive, Zahed Wahhaj, Anne-Lise Maire, Th. Henning, M. Carle, Marcel Carbillet, J. Ramos, Matthias Samland, Alain Origne, Raffaele Gratton, Arthur Vigan, Stéphane Udry, H. M. Schmid, Pierre Baudoz, Patrice Martinez, Markus Janson, O. Möller-Nilsson, L. Weber, Marcos Suarez, Cecile Gry, Michael Meyer, Sergio Messina, N. Engler, Emmanuel Hugot, Arnaud Sevin, A. Boccaletti, Alexander J. Bohn, P. Rabou, Julien Girard, T. Moulin, Jacopo Antichi, Beth Biller, F. Rigal, David Mouillet, C. Soenke, F. Madec, Riccardo Claudi, Silvano Desidera, M. Llored, E. Cascone, Daniela Fantinel, D. Gisler, R. Galicher, J. Baudrand, T. O. B. Schmidt, J. Pragt, Mickael Bonnefoy, D. Le Mignant, Mariangela Bonavita, Philippe Delorme, Jean-François Sauvage, Francois Wildi, Duncan Forgan, C. Mordasini, L. Gluck, Denis Perret, E. L. Rickman, Carsten Dominik, C. Lazzoni, E. Lagadec, Roxanne Ligi, Andrea Baruffolo, Lyu Abe, Gael Chauvin, A-M. Lagrange, Massimo Turatto, Pascal Puget, Philippe Feautrier, Yves Magnard, Bernardo Salasnich, Maud Langlois, V. De Caprio, D. Maurel, M. Kasper, Ken Rice, Dino Mesa, S. Rochat, C. Moutou, C. Perrot, Alain Delboulbé, P. Blanchard, François Ménard, Eric Stadler, Low Energy Astrophysics (API, FNWI), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Center for Space and Habitability (CSH), University of Bern, University of Edinburgh, Max Planck Institute for Radio Astronomy, Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, 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), Scottish Universities Physics Alliance (SUPA), Max Planck Institute for Astronomy (MPIA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Department of Biochemistry and Molecular Biology, Mayo Clinic, INAF - Osservatorio Astrofisico di Catania (OACT), Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), 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), 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), Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), CHU Tenon [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), CHU Pitié-Salpêtrière [AP-HP], Laboratoire des biomolécules (LBM UMR 7203), Chimie Moléculaire de Paris Centre (FR 2769), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Institut de Chimie du CNRS (INC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Hippolyte Fizeau (FIZEAU), INAF - Osservatorio Astronomico di Capodimonte (OAC), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen], European Southern Observatory (ESO), Environnements et Paléoenvironnements OCéaniques (EPOC), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Institut de Recherche pour le Développement (IRD), Centre Hospitalier Henri Duffaut (Avignon), ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016), University of Michigan [Ann Arbor], University of Michigan System, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre for Exoplanet Science, Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Laboratoire Franco-Chilien d'Astronomie (LFCA), Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Chile, University of Geneva [Switzerland], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Anton Pannekoek Institute for Astronomy, University of Amsterdam [Amsterdam] (UvA), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Universidad Diego Portales [Santiago] (UDP), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Radboud university [Nijmegen], DAAA, ONERA, Université Paris Saclay [Meudon], Eberhard Karls Universität Tübingen, 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), Laboratoire Lagrange, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS., Laboratoire de Biomécanique et Mécanique des Chocs (LBMC UMR T9406 ), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Université Gustave Eiffel, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université 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, 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), CHU Tenon [APHP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université, Département Médico-Universitaire APPROCHES, Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université-Sorbonne Université (SU), Sorbonne Université-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Institut National de la Santé et de la Recherche Médicale (INSERM)-Chimie Moléculaire de Paris Centre (FR 2769), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-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)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, ARCHEORIENT - Environnements et sociétés de l'Orient ancien (Archéorient), Université Lumière - Lyon 2 (UL2)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Institut des sciences analytiques et de physico-chimie pour l'environnement et les materiaux (IPREM), Université de Pau et des Pays de l'Adour (UPPA)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidad de Chile = University of Chile [Santiago] (UCHILE)-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción - University of Concepcion [Chile], Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université 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), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Chimie Moléculaire de Paris Centre (FR 2769), Institut de Chimie du CNRS (INC)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Chimie de Paris - Chimie ParisTech-PSL (ENSCP), Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM), and Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: astro-ph.SR, astro-ph.GA, Brown dwarf, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, planets and satellites: formation, 10. No inequality, infrared: planetary systems, 010303 astronomy & astrophysics, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Very Large Telescope, methods: statistical, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, techniques: high angular resolution, Astronomy and Astrophysics, Planetary system, Astrophysics - Astrophysics of Galaxies, Exoplanet, Accretion (astrophysics), Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: The SHINE project is a 500-star survey performed with SPHERE on the VLT for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. Here we present an initial statistical analysis for a subsample of 150 stars that are representative of the full SHINE sample. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 MJup and semimajor axes between 5 and 300 au. We adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Based on the results obtained for each star and on the 13 detections in the sample, we use a MCMC tool to compare our observations to two different types of models. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are $23.0_{-9.7}^{+13.5}\%$, $5.8_{-2.8}^{+4.7}\%$, and $12.6_{-7.1}^{+12.9}\%$ for BA, FGK, and M stars, respectively. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1-75 MJup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using our population model and restricting our sample to FGK stars, we derive a frequency of $5.7_{-2.8}^{+3.8}\%$, consistent with predictions from the parametric model. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies., Comment: 24 pages, 14 figures, 3 tables. Accepted for publication in A&A
Published: 2020

17. 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

18. Spatial segregation of dust grains in transition disks : SPHERE observations of 2MASS J16083070-3828268 and RXJ1852.3-3700

Author: M. Villenave, L. Weber, Mario Flock, J. F. Sauvage, P. Pinilla, J. Pragt, M. Carle, Thomas Henning, Alice Zurlo, Misato Fukagawa, G. van der Plas, G. A. Muro-Arena, Christophe Pinte, Christian Ginski, Eric Stadler, Attila Juhasz, Myriam Benisty, A. Pavlov, Antonio Garufi, Jonathan P. Williams, M. Keppler, Johan Olofsson, Laura M. Pérez, J. de Boer, Joany Andreina Manjarres Ramos, William R. F. Dent, François Ménard, Philippe Feautrier, Carsten Dominik, Jun-Ichi Morino, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-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)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Universidad de Chile, Joint ALMA Observatory (JAO), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), University of Arizona, Monash University [Clayton], University of Hawai'i [Honolulu] (UH), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], National Astronomical Observatory of Japan (NAOJ), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Universidad de Valparaiso [Chile], Universidad Diego Portales [Santiago] (UDP), 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), NOVA Opticla Infrared Instrumentation group at ASTRON, DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), 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]), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), National Radio Astronomy Observatory (NRAO)-European Southern Observatory (ESO), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Low Energy Astrophysics (API, FNWI), Universidad de Chile = University of Chile [Santiago] (UCHILE), Universiteit Leiden, Université de Genève = University of Geneva (UNIGE), and ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016)
Subjects: FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Jupiter, [SPI]Engineering Sciences [physics], Atmospheric radiative transfer codes, Settling, Planet, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Astronomy and Astrophysics, Radius, Astrophysics - Astrophysics of Galaxies, Wavelength, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Millimeter, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. The mechanisms governing the opening of cavities in transition disks are not fully understood. Several processes have been proposed but their occurrence rate is still unknown. Aims. We present spatially resolved observations of two transition disks and aim at constraining their vertical and radial structure using multiwavelength observations. Methods. We have obtained near-IR scattered light observations with VLT/SPHERE of the transition disks J1608 and J1852. We complement our datasets with ALMA observations and with unresolved photometric observations covering a wide range of wavelengths. We performed radiative transfer modeling to analyze the morphology of the disks and compare the results with a sample of 20 other transition disks observed with both SPHERE and ALMA. Results. The scattered light image of J1608 reveals a very inclined disk, with two bright lobes and a large cavity. J1852 shows an inner ring extending beyond the coronagraphic radius up to 15au, a gap and a second ring at 42au. Our radiative transfer model of J1608 indicates that the millimeter-sized grains are less extended vertically and radially than the micron-sized grains, indicating advanced settling and radial drift. We find good agreement with the observations of J1852 with a similar model, but due to the low inclination of the system, the model remains partly degenerate. The analysis of 22 transition disks shows that, in general, the cavities observed in scattered light are smaller than the ones detected at millimeter wavelengths. Conclusions. The analysis of a sample of transition disks indicates that the small grains can flow inward of the region where millimeter grains are trapped. While 15 out of the 22 cavities in our sample could be explained by a planet of less than 13 Jupiter masses, the others either require the presence of a more massive companion or of several low-mass planets., Accepted in Astronomy and Astrophysics
Published: 2019

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

Author: Jean-Loup Baudino, Janis Hagelberg, Christophe Pinte, Cyril Petit, Quentin Kral, A. Delboulbe, A. Pohl, Pierre Baudoz, Anne-Lise Maire, Eric Stadler, T. O. B. Schmidt, Alain Origne, F. Madec, Laura M. Pérez, N. Hubin, Enrico Giro, Marcos Suarez, Andrea Baruffolo, Anne-Marie Lagrange, Mario Flock, A. Pavlov, Jonathan Williams, P. Martinez, L. Abe, L. Gluck, Raffaele Gratton, G. Rousset, Jean-Luc Beuzit, Zahed Wahhaj, Esther Buenzli, Paul Mollière, S. S. Brems, Michael Meyer, P. Pinilla, Markus Janson, Tomas Stolker, M. Feldt, Pascal Puget, Christian Ginski, R. van Boekel, Myriam Benisty, Christoph Mordasini, D. Perret, Christian Soenke, R. G. van Holstein, D. Le Mignant, Francois Menard, F. Rigal, Patrick Rabou, Thierry Fusco, Massimo Turatto, Raphaël Galicher, J. de Boer, Th. Henning, N. Pawellek, J. Antichi, André Müller, Julien Milli, J. Lannier, Kjetil Dohlen, Ronald Roelfsema, Attila Juhasz, Yves Magnard, J. Pragt, Jean-Charles Augereau, M. Carle, Emmanuel Hugot, Miriam Keppler, Marcel Carbillet, Anthony Cheetham, Alice Zurlo, P. Blanchard, Andrea Isella, Tilman Birnstiel, S. Peretti, G. Salter, M. Bonnefoy, Juan-Luis Ramos, M. Llored, Laurent M. Mugnier, G.-D. Marleau, L. Weber, Anthony Boccaletti, Tristan Buey, Philippe Feautrier, Julien Girard, M. Kasper, Carsten Dominik, Faustine Cantalloube, Alexis Matter, Dino Mesa, Silvano Desidera, Stéphane Udry, Enrico Cascone, Arthur Vigan, Gael Chauvin, David Mouillet, C. Lazzoni, Andreas Bazzon, Riccardo Claudi, Jean-François Sauvage, Thibaut Moulin, E. Sissa, M. Cudel, Wolfgang Brandner, D. Gisler, Sascha P. Quanz, O. Moeller-Nilsson, Ralf Launhardt, Francois Wildi, M. Samland, Henning Avenhaus, Sylvain Rochat, Arnaud Sevin, Bernardo Salasnich, Maud Langlois, V. De Caprio, M. Jaquet, D. Maurel, Anne Costille, J. Kemmer, A. Roux, C. Perrot, D. Fantinel, Johan Olofsson, Cecile Gry, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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]), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), DOTA, ONERA, Université Paris Saclay (COmUE) [Palaiseau], ONERA-Université Paris Saclay (COmUE), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Oxford [Oxford], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), 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), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Physikalisches Institut [Bern], Universität Bern [Bern], Hungarian Academy of Sciences (MTA), Ludwig-Maximilians-Universität München (LMU), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Kavli Institute for Theoretical Physics [Santa Barbara] (KITP), University of California [Santa Barbara] (UCSB), University of California-University of California, INAF - Osservatorio Astrofisico di Arcetri (OAA), Stockholm University, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Department of Physical Geography and Ecosystem Science [Lund], Lund University [Lund], Universidad de Chile, University of Arizona, Monash Centre for Astrophysics (MoCA), Monash University [Clayton], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institute for Astronomy (IfA), University of Hawai‘i [Mānoa] (UHM), Geneva Observatory, University of Geneva [Switzerland], Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg], INAF - Osservatorio Astronomico di Capodimonte (OAC), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], Department of Mathematics - University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, NOVA Optical Infrared Instrumentation Group, Universidade de Lisboa (ULISBOA), Anton Pannekoek Institute for Astronomy, 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), DOTA, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Eberhard Karls Universität Tübingen, 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), 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), DOTA, ONERA, Université Paris Saclay [Châtillon], 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), 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), Universiteit Leiden, University of Oxford, Universität Bern [Bern] (UNIBE), University of California [Santa Barbara] (UC Santa Barbara), University of California (UC)-University of California (UC), 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), Universidad de Chile = University of Chile [Santiago] (UCHILE), Université de Genève = University of Geneva (UNIGE), Universität Heidelberg [Heidelberg] = Heidelberg University, Universidade de Lisboa = University of Lisbon (ULISBOA), ANR-10-LABX-0056,OSUG@2020,Innovative strategies for observing and modelling natural systems(2010), European Project: 226604,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2008-1,OPTICON(2009), European Project: 312430,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2012-1-RTD,OPTICON(2013), and Low Energy Astrophysics (API, FNWI)
Subjects: Brightness, planets and satellites: detection, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Point source, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, symbols.namesake, stars: individual: PDS 70, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Rayleigh scattering, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, scattering, protoplanetary disks, techniques: high angular resolution, Astronomy and Astrophysics, Radius, Astrometry, Space and Planetary Science, radiative transfer, symbols, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: Young circumstellar disks are of prime interest to understand the physical and chemical conditions under which planet formation takes place. Only very few detections of planet candidates within these disks exist, and most of them are currently suspected to be disk features. In this context, the transition disk around the young star PDS 70 is of particular interest, due to its large gap identified in previous observations, indicative of ongoing planet formation. We aim to search for the presence of planets and search for disk structures indicative for disk-planet interactions and other evolutionary processes. We analyse new and archival near-infrared (NIR) images of the transition disk PDS 70 obtained with the VLT/SPHERE, VLT/NaCo and Gemini/NICI instruments in polarimetric differential imaging (PDI) and angular differential imaging (ADI) modes. We detect a point source within the gap of the disk at about 195 mas (about 22 au) projected separation. The detection is confirmed at five different epochs, in three filter bands and using different instruments. The astrometry results in an object of bound nature, with high significance. The comparison of the measured magnitudes and colours to evolutionary tracks suggests that the detection is a companion of planetary mass. We confirm the detection of a large gap of about 54 au in size within the disk in our scattered light images, and detect a signal from an inner disk component. We find that its spatial extent is very likely smaller than about 17 au in radius. The images of the outer disk show evidence of a complex azimuthal brightness distribution which may in part be explained by Rayleigh scattering from very small grains. Future observations of this system at different wavelengths and continuing astrometry will allow us to test theoretical predictions regarding planet-disk interactions, planetary atmospheres and evolutionary models., Comment: 23 pages, accepted by A&A
Published: 2018

20. MAORY for ELT: preliminary design overview

Author: Angelo Valentini, Luca Terenzi, Edoardo Redaelli, Giorgio Pariani, Estelle Moraux, Demetrio Magrin, Mauro Dolci, Simone Zaggia, Christophe Vérinaud, Noël Ventura, Marie-Hélène Sztefek, Eric Stadler, Marilena Spavone, Laura Schreiber, Paolo Saracco, Bernardo Salasnich, Alain Roux, Frédéric Roussel, Sylvain Rochat, Matteo Aliverti, Marco Riva, Roberto Ragazzoni, Patrick Rabou, Alfio T. Puglisi, Linda Podio, Cédric Plantet, Mauro Patti, Sylvain Oberti, Thibaut Moulin, Gianluca Morgante, Didier Maurel, Enrico Marchetti, Filippo Mannucci, Yves Magnard, Matteo Lombini, Miska Le Louarn, Etienne P. Le Coarer, Mimma Lauria, Sylvain Lafrasse, Paolo La Penna, Laurent Jocou, Francois B. Hénault, Laurence Gluck, Enrico Giro, Italo Foppiani, Giuliana Fiorentino, Daniela Fantinel, Simone Esposito, Gianluca Di Rico, Alain Delboulbe, Adriano De Rosa, Vincenzo De Caprio, Massimo Dall'Ora, Valentina D'Orazi, Giuseppe Cosentino, Fausto Cortecchia, Jean-Jacques Correia, Enrico Cascone, Alexis Carlotti, Davide Greggio, Paolo Grani, Ivan Di Antonio, Andrea Balestra, Natalia Auricchio, Laurence Michaud, Elisabetta Maiorano, Philippe Feautrier, Lorenzo Busoni, Olivier Brissaud, Giovanni Bregoli, Marco Bonaglia, Michele Bellazzini, Andrea Baruffolo, Carmelo Arcidiacono, Guido Agapito, Renata Abicca, Paolo Ciliegi, Emiliano Diolaiti, and ITA
Subjects: Wavefront, Computer science, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, 01 natural sciences, Compensation (engineering), law.invention, 010309 optics, Telescope, law, 0103 physical sciences, Extremely Large Telescope, Astrophysics::Solar and Stellar Astrophysics, Atmospheric turbulence, Astrophysics::Earth and Planetary Astrophysics, Aerospace engineering, business, Adaptive optics, Instrument design, 010303 astronomy & astrophysics
Abstract: MAORY is one of the approved instruments for the European Extremely Large Telescope. It is an adaptive optics module, enabling high-angular resolution observations in the near infrared by real-time compensation of the wavefront distortions due to atmospheric turbulence and other disturbances such as wind action on the telescope. An overview of the instrument design is given in this paper.
Published: 2018

21. MAORY for ELT: preliminary mechanical design of the support structure

Author: Marco Riva, Marco Bonaglia, Enrico Cascone, Edoardo Maria Alberto Redaelli, Roberto Ragazzoni, Fausto Cortecchia, Adriano De Rosa, Matteo Lombini, Simone Esposito, Luca Terenzi, Vincenzo De Caprio, Michele Bellazzini, Philippe Feautrier, Paolo Ciliegi, Enrico Giro, Eric Stadler, Emiliano Diolaiti, Mauro Patti, and Carmelo Arcidiacono
Subjects: Wavefront, Computer science, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Strehl ratio, Port (circuit theory), 01 natural sciences, law.invention, 010309 optics, Telescope, Cardinal point, Relay, law, 0103 physical sciences, Extremely Large Telescope, Aerospace engineering, business, Adaptive optics, 010303 astronomy & astrophysics
Abstract: MAORY (Multi Conjugate Adaptive Optics RelaY) is one of the four instruments for the ELT (Extremely Large Telescope) approved for construction. It is an adaptive optics module able to compensate the wavefront disturbances affecting the scientific observations, achieving high strehl ratio and high sky coverage. MAORY will be located on the straight-through port of the telescope Nasmyth platform and shall re-image the telescope focal plane to a wide field camera (MICADO) and a possible future second instrument. A trade-off study among different mechanical design options for the main mechanical structure has been carried out. This paper outlines an overview of the mechanical design that gives a better result in terms of stability, vibrations and manufacturing.
Published: 2018

22. C-RED 2 InGaAs 640x512 600-fps infrared camera for low order wavefront sensing

Author: Jean-Luc Gach, Eric Stadler, Philippe Feautrier, Stephane Lemarchand, David Boutolleau, Carine Doucouré, Yann Wanwanscappel, Thomas Carmignani, and Fabien Clop
Subjects: Wavefront, Infrared, business.industry, Computer science, Frame (networking), Detector, First light, 01 natural sciences, Low noise, 010309 optics, Optics, 0103 physical sciences, Noise (video), business, 010303 astronomy & astrophysics
Abstract: Infrared wavefront sensors are now implemented in MCAO systems as reference (or truth sensors). After the successful development of C-RED One, the only commercial 320×256 3500 fps e-APD sub-e noise infrared camera, First Light Imaging developed the C-RED 2 InGaAs 640×512 fast camera with unprecedented performances in terms of noise, dark and readout speed based on the SNAKE SWIR detector from Sofradir. The C-RED 2 characteristics and performances at 600 fps are fully described in this paper. The C-RED2 development is supported by the "Investments in the future" program and the Provence Alpes Cote d'Azur Region, in the frame of the CPER.
Published: 2018

23. The MAORY laser guide star wavefront sensor: design status

Author: Christophe Verinaud, Roberto Ragazzoni, Sylvain Oberti, Sylvain Rochat, Fausto Cortecchia, L. Gluck, Jean-Jacques Correia, Michele Bellazzini, Carmelo Arcidiacono, Sylvain Douté, Eric Stadler, Simone Esposito, Estelle Moraux, Lorenzo Busoni, T. Moulin, Paolo Ciliegi, Emiliano Diolaiti, Alain Delboulbé, Philippe Feautrier, Laurent Jocou, Yves Magnard, Laura Schreiber, Gael Chauvin, Patrick Rabou, ITA, and FRA
Subjects: Wavefront, business.industry, Computer science, Field of view, Wavefront sensor, First light, Laser, law.invention, Optics, Laser guide star, law, Extremely Large Telescope, business, Spectrograph
Abstract: MAORY will be the multi-adaptive optics module feeding the high resolution camera and spectrograph MICADO at the Extremely Large Telescope (ELT) first light. In order to ensure high and homogeneous image quality over the MICADO field of view and high sky coverage, the baseline is to operate wavefront sensing using six Sodium Laser Guide Stars. The Laser Guide Star Wavefront Sensor (LGS WFS) is the MAORY sub-system devoted to real-time measurement of the high order wavefront distortions. In this paper we describe the MAORY LGS WFS current design, including opto-mechanics, trade-offs and possible future improvements.
Published: 2018

24. Organization, management and risk analysis of the MAORY project

Author: Roberto Ragazzoni, Emiliano Diolaiti, Paolo Ciliegi, Enrico Giro, Fausto Cortecchia, Simone Esposito, Michele Bellazzini, Renata Abicca, P. Feautrier, Eric Stadler, and Matteo Lombini
Subjects: Telescope, Risk analysis, Risk analysis (engineering), Computer science, business.industry, law, ComputingMethodologies_SYMBOLICANDALGEBRAICMANIPULATION, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Project management, business, Risk management, law.invention
Abstract: In this paper we present the structure, organization and risk management of the MAORY Consortium, an Italian-French collaboration for the design and construction of the adaptive optics module for the European Large Telescope.
Published: 2018

25. NAOMI: the adaptive optics for the auxiliary telescopes of VLTI

Author: Johan Kosmalski, Jean-Baptiste Le Bouquin, Javier Reyes, J. P. Kirchbauer, Alain Delboulbé, Sebastien Egner, Luigi Andolfato, Yves Magnard, Alexander Meister, Christophe Dupuy, Pascaline Darré, Jean-Philippe Berger, Luca Pasquini, Norbert Hubin, Johann Kolb, Roderick Dembet, Frédéric Gonté, Eric Stadler, T. Moulin, Nicolas Schuhler, Julien Woillez, Pierre Bourget, S. Guieu, Guillermo Valdes, Christian Stephan, S. Rochat, Jaime Alonso, Stefan Huber, Peter Krempl, Laurent Jocou, Pavel Shchekaturov, Pablo Gutierrez, Pierre Haguenauer, Christophe Verinaud, and Emmanuel Aller-Carpentier
Subjects: Interferometry, Optics, Computer science, business.industry, Strehl ratio, System testing, Adaptive optics, business, Deformable mirror
Abstract: The New Adaptive Optics Module for Interferometry (NAOMI) is ready to be installed at the 1.8-metre Auxiliary Telescopes (ATs) at ESO Paranal. NAOMI will make the existing interferometer performance less dependent on the seeing conditions. Fed with higher and more stable Strehl, the fringe tracker will achieve the fringe stability necessary to reach the full performance of the second-generation instruments GRAVITY and MATISSE. All four ATs will be equipped between September and November 2018 with a Deformable mirror (ALPAO DM-241), a 4*4 Shack– Hartmann adaptive optics system operating in the visible and an RTC based on SPARTA Light. During the last 6 months thorough system test has been made in laboratory to demonstrate the Adaptive Optics and chopping capability of NAOMI.
Published: 2018

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

Author: Jacopo Antichi, L. Weber, E. Sissa, Johan Olofsson, H. Le Coroller, Markus Kasper, Damien Ségransan, Alain Roux, T. Buey, Alice Zurlo, Cyril Petit, Alain Delboulbé, Andrea Baruffolo, Thomas Henning, Arnaud Sevin, P. Blanchard, Ronald Roelfsema, Daniela Fantinel, Alain Origne, R. Ligi, Anne Costille, M. Carle, Kjetil Dohlen, François Ménard, Bernardo Salasnich, Maud Langlois, Pierre Baudoz, V. De Caprio, Enrico Giro, D. Maurel, Lyu Abe, Markus Janson, O. Möller-Nilsson, Raffaele Gratton, Jean-Luc Beuzit, Riccardo Claudi, Beth Biller, Eric Stadler, Valentina D'Orazi, Massimo Turatto, Marc Jaquet, Joshua E. Schlieder, Pascal Puget, Taisiya Kopytova, Yves Magnard, Arthur Vigan, C. Soenke, Anthony Cheetham, Anne-Lise Maire, Patrice Martinez, D. Le Mignant, Gérard Rousset, A. Pavlov, Norbert Hubin, M. Keppler, Anne-Marie Lagrange, Emmanuel Hugot, Eric Lagadec, Hubert Klahr, Daniel Rouan, Dino Mesa, Michael Meyer, Thierry Fusco, Janis Hagelberg, Markus Feldt, Philippe Feautrier, Joany Andreina Manjarres Ramos, Quentin Kral, M. Llored, E. Cascone, Marcel Carbillet, S. Rochat, T. O. B. Schmidt, Mickael Bonnefoy, T. Moulin, S. Peretti, P. Rabou, David Mouillet, L. Gluck, J. Pragt, Gael Chauvin, F. Madec, Jean-François Sauvage, Francois Wildi, C. Mordasini, Denis Perret, Carsten Dominik, Anthony Boccaletti, F. Rigal, Marcos Suarez, Stéphane Udry, Silvano Desidera, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Universidad de Chile, Universidad de Valparaiso [Chile], Stockholm University, University of Edinburgh, Instituto de Astronomia y ciencias Planetarias de Atacama (INCT), Universidad de Atacama, University of Cambridge [UK] (CAM), NASA Goddard Space Flight Center (GSFC), University of Bern, Universidad Diego Portales [Santiago] (UDP), Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Mathematics - University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Arizona State University [Tempe] (ASU), Ural Federal University [Ekaterinburg] (UrFU), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), INAF - Osservatorio Astronomico di Capodimonte (OAC), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), European Southern Observatory (ESO), NOVA Optical Infrared Instrumentation Group, European Southern Observatory [Santiago] (ESO), Université de Genève = University of Geneva (UNIGE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidad de Chile = University of Chile [Santiago] (UCHILE), 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), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), 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), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, 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), Low Energy Astrophysics (API, FNWI), Department of Physical Geography and Ecosystem Science [Lund], Lund University [Lund], Institute for Astronomy [Edinburgh] (IfA), Geneva Observatory, Department of Biochemistry and Molecular Biology, Mayo Clinic, Observatoire de Paris, Université Paris sciences et lettres (PSL), 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: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], INDIVIDUAL: HIP 64892 [STARS], HIGH ANGULAR RESOLUTIONS [TECHNIQUES], 530 Physics, Astrophysics::High Energy Astrophysical Phenomena, BROWN DWARFS, FOS: Physical sciences, Library science, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, DETECTIONS [PLANETS AND SATELLITES], OPTIQUE ADAPTATIVE, 01 natural sciences, Techniques: high angular resolution, VLT, 0103 physical sciences, DETECTION [PLANETS AND SATELLITES], Astrophysics::Solar and Stellar Astrophysics, European commission, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Stars: brown dwarfs individual: HIP 64892, HIGH ANGULAR RESOLUTION [TECHNIQUES], Earth and Planetary Astrophysics (astro-ph.EP), Physics, ASTRONOMIE, INDIVIDUAL [STARS], 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 520 Astronomy, EFFECTIVE TEMPERATURE, Astronomy and Astrophysics, Planets and satellites: detection, 500 Science, 620 Engineering, EVOLUTIONARY MODELS, Astrophysics - Solar and Stellar Astrophysics, FORMATION AND EVOLUTIONS, Space and Planetary Science, ATMOSPHERES [SATELLITES], SPECTRAL ENERGY DISTRIBUTION, Christian ministry, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SATELLITES, STARS, Astrophysics - Earth and Planetary Astrophysics, PLANETS
Abstract: We report the discovery of a bright, brown dwarf companion to the star HIP 64892, imaged with VLT/SPHERE during the SHINE exoplanet survey. The host is a B9.5V member of the Lower-Centaurus-Crux subgroup of the Scorpius Centaurus OB association. The measured angular separation of the companion ($1.2705\pm0.0023$") corresponds to a projected distance of $159\pm12$ AU. We observed the target with the dual-band imaging and long-slit spectroscopy modes of the IRDIS imager to obtain its SED and astrometry. In addition, we reprocessed archival NACO L-band data, from which we also recover the companion. Its SED is consistent with a young (, Comment: 12 pages, 11 figures, accepted for publication in A&A
Published: 2018

27. Orbital and spectral analysis of the benchmark brown dwarf HD 4747B

Author: Anthony Boccaletti, Dino Mesa, Baptiste Lavie, Yves Magnard, Maud Langlois, Jean-Loup Baudino, Janis Hagelberg, Gael Chauvin, A-M. Lagrange, L. Weber, Sebastian Daemgen, Emmanuel Hugot, Arnaud Sevin, Michael R. Meyer, Stéphane Udry, Damien Ségransan, V. De Caprio, Alice Zurlo, Anthony Cheetham, Joany Andreina Manjarres Ramos, M. Carle, Raffaele Gratton, Francois Wildi, J. Pragt, Kevin Heng, Mickael Bonnefoy, Marcel Carbillet, C. Soenke, Matthias Samland, L. Gluck, François Ménard, T. Moulin, S. Peretti, T. O. B. Schmidt, P. Rabou, Arthur Vigan, Eric Stadler, H. Le Coroller, Valentina D'Orazi, Gérard Rousset, Silvano Desidera, Markus Janson, Markus Feldt, A. Pavlov, Anne-Lise Maire, Daniel Rouan, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Physikalisches Institut [Bern], Universität Bern [Bern], INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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), University of Oxford [Oxford], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy, Stockholm University, 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]), Center for Space and Habitability (CSH), University of Bern, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Department of Biochemistry and Molecular Biology, Mayo Clinic, Department of Geriatric Medicine, Centre Hospitalier Lyon Sud [CHU - HCL] (CHLS), Hospices Civils de Lyon (HCL)-Hospices Civils de Lyon (HCL), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (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), INAF - Osservatorio Astronomico di Capodimonte (OAC), Bulgarian Academy of Sciences (BAS), NOVA Optical Infrared Instrumentation Group, University of Copenhagen = Københavns Universitet (KU), ESO, Physics Department [Garching], Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM)-Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), Université de Genève = University of Geneva (UNIGE), Universität Bern [Bern] (UNIBE), 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), University of Oxford, Stockholm Observatory Department of Astronomy, Geneva Observatory, Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), 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), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), University of Copenhagen = Københavns Universitet (UCPH), and Université Nice Sophia Antipolis (... - 2019) (UNS)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Brown dwarf, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, Photometry (optics), Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Substellar object, 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [PHYS]Physics [physics], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Effective temperature, Exoplanet, Radial velocity, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: Context. The study of high-contrast imaged brown dwarfs and exoplanets depends strongly on evolutionary models. To estimate the mass of a directly imaged substellar object, its extracted photometry or spectrum is used and adjusted with model spectra together with the estimated age of the system. These models still need to be properly tested and constrained. HD 4747B is a brown dwarf close to the H burning mass limit, orbiting a nearby (d = 19.25 ± 0.58 pc), solar-type star (G9V); it has been observed with the radial velocity method for over almost two decades. Its companion was also recently detected by direct imaging, allowing a complete study of this particular object. Aims. We aim to fully characterize HD 4747B by combining a well-constrained dynamical mass and a study of its observed spectral features in order to test evolutionary models for substellar objects and to characterize its atmosphere. Methods. We combined the radial velocity measurements of High Resolution Echelle Spectrometer (HIRES) and CORALIE taken over two decades and high-contrast imaging of several epochs from NACO, NIRC2, and SPHERE to obtain a dynamical mass. From the SPHERE data we obtained a low-resolution spectrum of the companion from Y to H band, and two narrow band-width photometric measurements in the K band. A study of the primary star also allowed us to constrain the age of the system and its distance. Results. Thanks to the new SPHERE epoch and NACO archival data combined with previous imaging data and high-precision radial velocity measurements, we were able to derive a well-constrained orbit. The high eccentricity (e = 0.7362 ± 0.0025) of HD 4747B is confirmed, and the inclination and the semi-major axis are derived (i = 47.3 ± 1.6°, a = 10.01 ± 0.21 au). We derive a dynamical mass of mB = 70.0 ± 1.6 MJup, which is higher than a previous study but in better agreement with the models. By comparing the object with known brown dwarfs spectra, we derive a spectral type of L9 and an effective temperature of 1350 ± 50 K. With a retrieval analysis we constrain the oxygen and carbon abundances and compare them with the values from the HR 8799 planets.
Published: 2018

28. C-RED One and C-RED2: SWIR high-performance cameras using Saphira e-APD and Snake InGaAs detectors

Author: Yann Wanwanscappel, Philippe Feautrier, David Boutolleau, Thomas Carmignani, Eric Stadler, Jean-Luc Gach, Stephane Lemarchand, and Fabien Clop
Subjects: Wavefront, Computer science, business.industry, Detector, First light, Frame rate, media_common.cataloged_instance, Computer vision, Noise (video), Artificial intelligence, European union, Adaptive optics, business, Field-programmable gate array, media_common
Abstract: After the development of the OCAM2 EMCCD fast visible camera dedicated to advanced adaptive optics wavefront sensing, First Light Imaging moved to the SWIR fast cameras with the development of the C-RED One and the C-RED 2 cameras. First Light Imaging’s C-RED One infrared camera is capable of capturing up to 3500 full frames per second with a subelectron readout noise and very low background. C-RED One is based on the last version of the SAPHIRA detector developed by Leonardo UK. This breakthrough has been made possible thanks to the use of an e-APD infrared focal plane array which is a real disruptive technology in imagery. C-RED One is an autonomous system with an integrated cooling system and a vacuum regeneration system. It operates its sensor with a wide variety of read out techniques and processes video on-board thanks to an FPGA. We will show its performances and expose its main features. In addition to this project, First Light Imaging developed an InGaAs 640x512 fast camera with unprecedented performances in terms of noise, dark and readout speed based on the SNAKE SWIR detector from Sofradir. The camera was called C-RED 2. The C-RED 2 characteristics and performances will be described. The C-RED One project has received funding from the European Union’s Horizon 2020 research and innovation program under grant agreement N° 673944. The C-RED 2 development is supported by the "Investments for the future" program and the Provence Alpes Cote d'Azur Region, in the frame of the CPER.
Published: 2018

29. Dynamical masses of M-dwarf binaries in young moving groups. I. The case of TWA 22 and GJ 2060

Author: Stephen Durkan, Thomas Henning, Derek Homeier, T. Schmidt, Markus Janson, Eric Stadler, Julien Girard, Jean-Philippe Berger, F. Allard, Sylvestre Lacour, Jean-Louis Monin, J.-B. Le Bouquin, Silvano Desidera, Raffaele Gratton, Dino Mesa, A. Pavlov, C. Bergfors, Joany Andreina Manjarres Ramos, Joshua E. Schlieder, Roxanne Ligi, Mickael Bonnefoy, L. Rodet, A. Bazzon, P. Delorme, Wolfgang Brandner, Sergio Messina, Matthias Samland, R. Rigal, A. Grandjean, A. Delboulbé, Stéphane Udry, Damien Ségransan, A. Boccaletti, Anne-Lise Maire, Markus Feldt, H. Beust, Janis Hagelberg, Gael Chauvin, Anne-Marie Lagrange, Maud Langlois, J.-L. Beuzit, Michael Meyer, D. Maurel, François Ménard, J. Lannier, Ronald Roelfsema, Arthur Vigan, Beth Biller, Graeme Salter, L. Weber, and S. Peretti
Subjects: Brown dwarf, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, visual [Binaries], 01 natural sciences, Spectral line, 010309 optics, low-mass [Stars], Planet, pre-main sequence [Stars], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Beta Pictoris, 010303 astronomy & astrophysics, individual: TWA 22 [Stars], Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Earth and Planetary Astrophysics (astro-ph.EP), Orbital elements, Physics, Astronomy and Astrophysics, Astrometry, high angular resolution [Techniques], Stars, Astrophysics - Solar and Stellar Astrophysics, individual: GJ 2060 [Stars], Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Evolutionary models are widely used to infer the mass of stars, brown dwarfs, and giant planets. Their predictions are thought to be less reliable at young ages ($, Comment: Accepted for publication in A&A. 26 pages, 22 figures, 12 tables
Published: 2018

30. MAORY requirements flow down and technical budgets

Author: Emiliano Diolaiti, Laura Schreiber, Mauro Patti, Lorenzo Busoni, Philippe Feautrier, Carmelo Arcidiacono, Eric Stadler, Roberto Ragazzoni, Paolo Ciliegi, Matteo Lombini, Simone Esposito, Marco Riva, and Fausto Cortecchia
Subjects: Design phase, Procurement, Flow (mathematics), Traceability, Computer science, Process (engineering), System level, Systems engineering, Task (project management)
Abstract: MAORY is the ELT-MCAO system providing first-light wide-field correction for the near infrared imager and spectrograph MICADO. This paper provides an overview of the systems engineering processes and tools implemented to MAORY project during preliminary design phase and it illustrates, with some practical examples, the role of MAORY technical budgets to derive requirements on subsystems. One of the critical activities in systems engineering is the requirements managing. In line with this, the MAORY team devotes a significant effort to this activity, which follows a well-established process. This involves the MAORY requirements break-down to subsystems level and from here down to subsystems procurements specifications. This paper also presents an overview of the MAORY Technical Budgets. One task of the System Engineering is to manage the technical budgets at system level combining the contributors at subsystems level to meet the overall requirements.
Published: 2018

31. Experimental test of a 40 cm-long R=100 000 spectrometer for exoplanet characterisation

Author: Jean-Jacques Correia, Guillaume Bourdarot, Étienne Artigau, P. Rabou, David Mouillet, Yves Magnard, Laurent Jocou, Philippe Vallée, René Doyon, Etienne Le Coarer, Eric Stadler, Xavier Bonfils, Thierry Forveille, Alexis Carlotti, Arthur Vigan, 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), Gemini Observatory [Southern Operations Center], Association of Universities for Research in Astronomy (AURA), 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), Departement de physique and Observatoire du Mont Megantic, Université de Montréal [Montréal], Laboratoire d'optique des solides (LOS), Université Pierre et Marie Curie - Paris 6 (UPMC)-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 de Montréal (UdeM), 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), 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]), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Spectrometer, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Phased array, business.industry, Single-mode optical fiber, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Context (language use), 7. Clean energy, 01 natural sciences, Exoplanet, 010309 optics, Interferometry, Optics, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Spectral resolution, Adaptive optics, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: High-resolution spectroscopy is a key element for present and future astronomical instrumentation. In particular, coupled to high contrast imagers and coronagraphs, high spectral resolution enables higher contrast and has been identified as a very powerful combination to characterise exoplanets, starting from giant planets now, up to Earth-like planet eventually for the future instruments. In this context, we propose the implementation of an innovative echelle spectrometer based on the use of VIPA (Virtually Imaged Phased Array, Shirasaki 1996). The VIPA itself is a particular kind of Fabry-Perot interferometer, used as an angular disperser with much greater dispersive power than common diffraction grating. The VIPA is an efficient, small component (3 cm x 2.4 cm), that takes the very advantage of single mode injection in a versatile design. The overall instrument presented here is a proof-of-concept of a compact, high-resolution (R > 80 000) spectrometer, dedicated to the H and K bands, in the context of the project High-Dispersion Coronagrahy developed at IPAG. The optical bench has a foot-print of 40 cm x 26 cm ; it is fed by two Single-Mode Fibers (SMF), one dedicated to the companion, and one to the star and/or to a calibration channel, and is cooled down to 80 K. This communication first presents the scientific and instrumental context of the project, and the principal merit of single-mode operations in high-resolution spectrometry. After recalling the physical structure of the VIPA and its implementation in an echelle-spectrometer design, it then details the optical design of the spectrometer. In conclusion, further steps (integration, calibration, coupling with adaptive optics) and possible optimization are briefly presented. Keywords: Echelle Spectrometer, High Spectral Resolution, Exoplanets, High-Dispersion Coronography, Infrared, Adaptive Optics, SPHERE
Published: 2018
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32. Orbital and atmospheric characterization of the planet within the gap of the PDS 70 transition disk

Author: Anne-Lise Maire, Hervé Beust, Th. Henning, Daniel Rouan, Anthony Boccaletti, Alice Zurlo, Jean-Loup Baudino, Janis Hagelberg, Francois Menard, N. Pawellek, Benjamin Charnay, Karan Molaverdikhani, P. Mollière, Faustine Cantalloube, Maud Langlois, Gael Chauvin, L. Weber, Myriam Benisty, Zahed Wahhaj, Eric Stadler, E. Sissa, Anthony Cheetham, Michael Meyer, Matthias Samland, M. Feldt, André Müller, R. van Boekel, Miriam Keppler, Z. C. Long, Dino Mesa, M. Bonnefoy, R. Ligi, Christoph Mordasini, C. Lazzoni, Joany Andreina Manjarres Ramos, R. G. Gratton, Julien Girard, Thierry Fusco, Arthur Vigan, A. Pavlov, Sascha P. Quanz, Anne-Marie Lagrange, Thibaut Moulin, M. Gennaro, Silvano Desidera, Markus Janson, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, 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]), Universidad de Santiago de Chile [Santiago] (USACH), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Oxford [Oxford], Space Telescope Science Institute (STSci), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), 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), Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Stockholm University, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Instituto de Astronomia y ciencias Planetarias de Atacama (INCT), Universidad de Atacama, University of Michigan [Ann Arbor], University of Michigan System, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Universität Bern [Bern], Research Centre for Astronomy and Earth Sciences [Budapest], Hungarian Academy of Sciences (MTA), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Universidad Diego Portales [Santiago] (UDP), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, 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), 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), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Pawellek, Nicole [0000-0002-9385-9820], Apollo - University of Cambridge Repository, University of Oxford, Université de Genève = University of Geneva (UNIGE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Universiteit Leiden, Universität Bern [Bern] (UNIBE), ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire Franco-Chilien d'Astronomie, UMI 3386, Pôle Planétologie du LESIA, 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, 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), Department of Physics, University of Oxford, Oxford, UK, Space Telescope Science Institute (STScI), Geneva Observatory, University of Geneva, Chemin des Mailettes 51, 1290, Versoix, Switzerland, INAF-Osservatorio Astronomico di Padova, ONERA, Institute for Astronomy, Department of Physics, ETH Zürich, INAF-Osservatorio Astronomico di Brera (INAF-OAB), Leiden Observatory, Physikalisches Institut, Universitat Bern, Gesellschaftsstrasse 6, 3012, Bern, Switzerland, European Southern Observatory, and Nucleo de Astronomia, Facultad de Ingenieria y Ciencias, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile
Subjects: 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, planets and satellites: individual: PDS 70, Astrophysics::Solar and Stellar Astrophysics, Circular orbit, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, planets and satellites: atmospheres, Earth and Planetary Astrophysics (astro-ph.EP), Atmospheric models, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Astrometry, Orbit, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Orbital motion, Spectral energy distribution, astrometry, Astrophysics::Earth and Planetary Astrophysics, methods: observational, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract: Aims: We aim to characterize the orbital and atmospheric properties of PDS 70 b, which was first identified on May 2015 in the course of the SHINE survey with SPHERE, the extreme adaptive-optics instrument at the VLT. Methods: We obtained new deep SPHERE/IRDIS imaging and SPHERE/IFS spectroscopic observations of PDS 70 b. The astrometric baseline now covers 6 years which allows us to perform an orbital analysis. For the first time, we present spectrophotometry of the young planet which covers almost the entire near-infrared range (0.96 to 3.8 micrometer). We use different atmospheric models covering a large parameter space in temperature, log(g), chemical composition, and cloud properties to characterize the properties of the atmosphere of PDS 70 b. Results: PDS 70 b is most likely orbiting the star on a circular and disk coplanar orbit at ~22 au inside the gap of the disk. We find a range of models that can describe the spectrophotometric data reasonably well in the temperature range between 1000-1600 K and log(g) no larger than 3.5 dex. The planet radius covers a relatively large range between 1.4 and 3.7 R_jupiter with the larger radii being higher than expected from planet evolution models for the age of the planet of 5.4 Myr. Conclusions: This study provides a comprehensive dataset on the orbital motion of PDS 70 b, indicating a circular orbit and a motion coplanar with the disk. The first detailed spectral energy distribution of PDS 70 b indicates a temperature typical for young giant planets. The detailed atmospheric analysis indicates that a circumplanetary disk may contribute to the total planet flux., Comment: accepted for publication in A&A (10 pages, 8 figures)
Published: 2018
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33. Testing giant planet formation in the transitional disk of SAO 206462 using deep VLT/SPHERE imaging

Author: Christian Thalmann, Gael Chauvin, Dino Mesa, M. Millward, J. Lannier, T. Buey, Alice Zurlo, C. Perrot, S. Messina, Arthur Vigan, Carsten Dominik, Anne-Lise Maire, Silvano Desidera, R. Galicher, Anne-Marie Lagrange, Adriana Pohl, Matthias Samland, Thayne Currie, Anthony Boccaletti, Enrico Giro, Mickael Bonnefoy, André Müller, E. Sissa, Norbert Hubin, Thierry Fusco, Markus Feldt, Michael Meyer, Maud Langlois, Tomas Stolker, Raffaele Gratton, Wolfgang Brandner, Jose Ramos, D. Le Mignant, Esther Buenzli, Stéphane Udry, Carol A. Grady, Christian Ginski, R. van Boekel, Graeme Salter, L. Weber, Beth Biller, Thomas Henning, S. Peretti, Eric Stadler, Sascha P. Quanz, Low Energy Astrophysics (API, FNWI), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, National Astronomical Observatory of Japan (NAOJ), GSFC Exoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center (GSFC), 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]), York Creek Observatory, Heidelberg University, International Max Planck Research School on Astrophysics (IMPRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), 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), Department of Astronomy University of Michigan, University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Universidad Diego Portales [Santiago] (UDP), Universidad de Santiago de Chile [Santiago] (USACH), INAF - Osservatorio Astronomico di Padova (OAPD), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), 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), 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), Universiteit Leiden, Université de Genève = University of Geneva (UNIGE), Exoplanets and Stellar Astrophysics Lab, 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), 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), ONERA, Astronomical Institute Anton Pannekoek, University of Amsterdam, INAF-Osservatorio Astrofisico di Catania (INAF-OACt), Institute for Astronomy, The University of Edinburgh, Royal Observatory, Blackford Hill View, Edinburgh, EH9 3HJ, UK, National Astronomical Observatory of Japan, Subaru Telescope, Hilo, HI, 96720, USA, Exoplanets and Stellar Astrophysics Laboratory, NASA Goddard Space Flight Center, Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, York Creek Observatory, Georgetown, Tasmania, Australia, Department of Astronomy, University of Michigan, 1085 S. University Ave, Ann Arbor, MI, 48109-1107, USA, Institute for Astronomy, Department of Physics, ETH Zürich, Nucleo de Astronomia, Facultad de Ingenieria, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile, INAF-Osservatorio Astronomico di Padova, Leiden Observatory, and ISDC, Geneva Observatory, University of Geneva
Subjects: IMAGE PROCESSING, INDIVIDUAL, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, OPTIQUE ADAPTATIVE, 01 natural sciences, Density wave theory, Jupiter, VLT, DATA ANALYSIS, SPHERE, Planet, TECHNIQUES, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Spiral, Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, SAO 206462 (HD 135344B), Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Giant planet, HIGH ANGULAR RESOLUTION, Astronomy and Astrophysics, SPECTROSCOPIC, 13. Climate action, Space and Planetary Science, METHODS, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Protoplanet, STARS, Astrophysics - Earth and Planetary Astrophysics, PLANETARY DISKS
Abstract: Context. The SAO 206462 (HD 135344B) disk is one of the few known transitional disks showing asymmetric features in scattered light and thermal emission. Near-infrared scattered-light images revealed two bright outer spiral arms and an inner cavity depleted in dust. Giant protoplanets have been proposed to account for the disk morphology. Aims. We aim to search for giant planets responsible for the disk features and, in the case of non-detection, to constrain recent planet predictions using the data detection limits. Methods. We obtained new high-contrast and high-resolution total intensity images of the target spanning the Y to the K bands (0.95-2.3 mic) using the VLT/SPHERE near-infrared camera and integral field spectrometer. Results. The spiral arms and the outer cavity edge are revealed at high resolutions and sensitivities without the need for image post-processing techniques, which introduce photometric biases. We do not detect any close-in companions. For the derivation of the detection limits on putative giant planets embedded in the disk, we show that the knowledge of the disk aspect ratio and viscosity is critical for the estimation of the attenuation of a planet signal by the protoplanetary dust because of the gaps that these putative planets may open. Given assumptions on these parameters, the mass limits can vary from ~2-5 to ~4-7 Jupiter masses at separations beyond the disk spiral arms. The SPHERE detection limits are more stringent than those derived from archival NaCo/L' data and provide new constraints on a few recent predictions of massive planets (4-15 MJ) based on the spiral density wave theory. The SPHERE and ALMA data do not favor the hypotheses on massive giant planets in the outer disk (beyond 0.6). There could still be low-mass planets in the outer disk and/or planets inside the cavity., A&A, in press. 16 pages, 17 figures. Updated to match proofs
Published: 2017

34. C-RED One and C-RED 2: SWIR advanced cameras using Saphira e-APD and Snake InGaAs detectors

Author: Eric Stadler, Timothée Greffe, Jean-Luc Gach, Fabien Clop, Carine Doucouré, Thomas Carmignani, Stephane Lemarchand, Philippe Feautrier, and David Boutolleau
Subjects: Wavefront, Physics, business.industry, Detector, First light, Frame rate, 01 natural sciences, 010309 optics, Optics, 0103 physical sciences, media_common.cataloged_instance, Computer vision, Artificial intelligence, Noise (video), European union, business, Adaptive optics, Field-programmable gate array, 010303 astronomy & astrophysics, media_common
Abstract: After the development of the OCAM2 EMCCD fast visible camera [1] dedicated to advanced adaptive optics wavefront sensing, First Light Imaging moved to the SWIR fast cameras with the C-RED One and the C-RED 2 cameras. These cameras and their performances are described extensively in this paper. First Light Imaging C-RED One infrared camera is capable of capturing up to 3500 full frames per second with subelectron readout noise and very low background. C-RED One is based on the last version of the SAPHIRA detector developed by Leonardo UK. This breakthrough has been made possible thanks to the use of an e-APD infrared focal plane array which is a real disruptive technology in imagery. C-RED One is an autonomous system with an integrated cooling system and a vacuum regeneration system. It operates its sensor with a wide variety of read out techniques and processes video on-board thanks to a Xlinks embedded FPGA. In addition to this project, First Light Imaging developed an InGaAs 640x512 fast camera with unprecedented performances in terms of noise, dark and readout speed for equivalent products. This camera is based on the SNAKE SWIR detector from Sofradir and was called C-RED 2. The C-RED 2 characteristics and performances are also fully described in this paper. The C-RED One project has received funding from the European Union’s Horizon 2020 research and innovation program under grant agreement N° 673944. C-RED2 development is supported by the "Investments for the future" program and the Provence Alpes Cote d'Azur Region, in the frame of the CPER.
Published: 2017

35. Infrared detectors for wavefront sensing

Author: Thomas Carmignani, Eric Stadler, Jean-Luc Gach, Stephane Lemarchand, Carine Doucouré, Philippe Feautrier, David Boutolleau, Fabien Clop, and Yann Wanwanscappel
Subjects: Physics, Wavefront, Optics, business.industry, Infrared, Detector, business
Published: 2017

36. A detector interferometric calibration experiment for high precision astrometry

Author: Mike Shao, François Hénault, M. Donati, A. Léger, Eric Stadler, C. Ketchazo, Renaud Goullioud, P. O. Lagage, J. M. LeDuigou, Alain Delboulbé, Christophe Cara, P. Kern, Fabien Malbet, E. Doumayrou, E. Behar, M. Saint-Pe, Olivier Preis, Bijan Nemati, J. Dupont, S. Rochat, Guillermo Martin, Philippe Feautrier, S. Lafrasse, Chengxing Zhai, S. Potin, and Antoine Crouzier
Subjects: Point spread function, Computer science, Physics::Instrumentation and Detectors, FOS: Physical sciences, Context (language use), 01 natural sciences, 010309 optics, Planet, 0103 physical sciences, Calibration, Computer vision, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Signal processing, Pixel, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrometry, Interferometry, Space and Planetary Science, Artificial intelligence, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Context: Exoplanet science has made staggering progress in the last two decades, due to the relentless exploration of new detection methods and refinement of existing ones. Yet astrometry offers a unique and untapped potential of discovery of habitable-zone low-mass planets around all the solar-like stars of the solar neighborhood. To fulfill this goal, astrometry must be paired with high precision calibration of the detector. Aims: We present a way to calibrate a detector for high accuracy astrometry. An experimental testbed combining an astrometric simulator and an interferometric calibration system is used to validate both the hardware needed for the calibration and the signal processing methods. The objective is an accuracy of 5e-6 pixel on the location of a Nyquist sampled polychromatic point spread function. Methods: The interferometric calibration system produced modulated Young fringes on the detector. The Young fringes were parametrized as products of time and space dependent functions, based on various pixel parameters. The minimization of func- tion parameters was done iteratively, until convergence was obtained, revealing the pixel information needed for the calibration of astrometric measurements. Results: The calibration system yielded the pixel positions to an accuracy estimated at 4e-4 pixel. After including the pixel position information, an astrometric accuracy of 6e-5 pixel was obtained, for a PSF motion over more than five pixels. In the static mode (small jitter motion of less than 1e-3 pixel), a photon noise limited precision of 3e-5 pixel was reached.
Published: 2016

37. LGSD/NGSD: high speed visible CMOS imagers for E-ELT adaptive optics

Author: Mark Downing, Paul Jerram, Nick Swift, Javier Reyes, Manfred Meyer, Jean-Luc Gach, Eric Stadler, Martin Fryer, Paul Jorden, Johann Kolb, Bart Dierickx, Andy Pike, Arnaud Defernez, and Philippe Feautrier
Subjects: Physics, Laser guide star, Optics, CMOS, business.industry, Detector, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, Large format, Guide star, Wavefront sensor, business, Adaptive optics, Noise (electronics)
Abstract: The success of the next generation of instruments for ELT class telescopes will depend upon improving the image quality by exploiting sophisticated Adaptive Optics (AO) systems. One of the critical components of the AO systems for the E-ELT has been identified as the optical Laser/Natural Guide Star WFS detector. The combination of large format, 1760×1680 pixels to finely sample the wavefront and the spot elongation of laser guide stars, fast frame rate of 700 frames per second (fps), low read noise ( 90%) makes the development of this device extremely challenging. Design studies concluded that a highly integrated Backside Illuminated CMOS Imager built on High Resistivity silicon as the most likely technology to succeed. Two generations of the CMOS Imager are being developed: a) the already designed and manufactured NGSD (Natural Guide Star Detector), a quarter-sized pioneering device of 880×840 pixels capable of meeting first light needs of the E-ELT; b) the LGSD (Laser Guide Star Detector), the larger full size device. The detailed design is presented including the approach of using massive parallelism (70,400 ADCs) to achieve the low read noise at high pixel rates of ~3 Gpixel/s and the 88 channel LVDS 220Mbps serial interface to get the data off-chip. To enable read noise closer to the goal of 1e- to be achieved, a split wafer run has allowed the NGSD to be manufactured in the more speculative, but much lower read noise, Ultra Low Threshold Transistors in the unit cell. The NGSD has come out of production, it has been thinned to 12μm, backside processed and packaged in a custom 370pin Ceramic PGA (Pin Grid Array). First results of tests performed both at e2v and ESO are presented.
Published: 2016

38. 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

39. C-RED one: ultra-high speed wavefront sensing in the infrared made possible

Author: Philippe Feautrier, Stephane Lemarchand, Ian Baker, Fabien Clop, Thomas Carmignani, Jean Luc Gach, David Boutolleau, Eric Stadler, and Timothée Greffe
Subjects: Ultra high speed, Wavefront, Physics, Infrared, business.industry, Wavefront sensor, First light, Frame rate, 01 natural sciences, 010309 optics, Optics, 0103 physical sciences, media_common.cataloged_instance, Noise (video), European union, business, 010303 astronomy & astrophysics, Remote sensing, media_common
Abstract: First Light Imaging's CRED-ONE infrared camera is capable of capturing up to 3500 full frames per second with a subelectron readout noise. This breakthrough has been made possible thanks to the use of an e-APD infrared focal plane array which is a real disruptive technology in imagery. We will show the performances of the camera, its main features and compare them to other high performance wavefront sensing cameras like OCAM2 in the visible and in the infrared. The project leading to this application has received funding from the European Union’s Horizon 2020 research and innovation program under grant agreement N° 673944.
Published: 2016

40. Getting ready for the first on sky experiment using an ELT-scaled elongated sodium laser guide star

Author: Tristan Buey, Alastair Basden, James Osborn, Domenico Bonaccini Calia, Richard M. Myers, Damien Gratadour, Eric Stadler, R. G. Talbot, Tim Morris, Fanny Chemla, Andrew P. Reeves, Eric Gendron, Jean-Luc Gach, Thomas Pfrommer, Mauro Centrone, Gérard Rousset, Lisa Bardou, Fabrice Vidal, Philippe Feautrier, 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: Physics, business.industry, media_common.quotation_subject, 01 natural sciences, 010309 optics, Laser guide star, Optics, Sky, Fiber laser, 0103 physical sciences, William Herschel Telescope, Extremely Large Telescope, Adaptive optics, Adaptive optics systems, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, media_common
Abstract: The use of sodium laser guide star for Extremely Large Telescopes (ELT) adaptive optics systems is a key concern due to the perspective effect that produces elongated images in the Shack-Hartmann pattern. In order to assess the feasibility of using an elongated sodium beacon on an ELT, an on-sky experiment reproducing the extreme off-axis launch conditions of the European ELT is scheduled for summer and autumn 2016. The experiment will use the demonstrator CANARY installed on the William Herschel Telescope and the ESO transportable 20W CW fiber laser, embedded in the Wendelstein LGS unit. We will discuss here the challenges this experiment addresses as well as the details of its implementation and the derivation of the error budget.
Published: 2016

41. Final two-stage MOAO on-sky demonstration with CANARY

Author: Eric Stadler, Arnaud Sevin, James Osborn, D. Perret, David Henry, Andrew P. Reeves, Nigel Dipper, J. M. Huet, Urban Bitenc, Richard M. Myers, Damien Gratadour, Stephen Todd, Gérard Rousset, Colin Dickson, G. Talbot, Carine Morel, Alastair Basden, Eric Gendron, Tristan Buey, Tim Morris, Philippe Feautrier, Simon L. Morris, M. Cohen, David Atkinson, Jean-Luc Gach, E. Younger, Fanny Chemla, Fabrice Vidal, 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, 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), and Technique
Subjects: Physics, media_common.quotation_subject, 01 natural sciences, Woofer, Tweeter, Deformable mirror, law.invention, 010309 optics, Stars, Laser guide star, law, Sky, 0103 physical sciences, William Herschel Telescope, Adaptive optics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Remote sensing, media_common
Abstract: CANARY is an on-sky Laser Guide Star (LGS) tomographic AO demonstrator in operation at the 4.2m William Herschel Telescope (WHT) in La Palma. From the early demonstration of open-loop tomography on a single deformable mirror using natural guide stars in 2010, CANARY has been progressively upgraded each year to reach its final goal in July 2015. It is now a two-stage system that mimics the future E-ELT: a GLAO-driven woofer based on 4 laser guide stars delivers a ground-layer compensated field to a figure sensor locked tweeter DM, that achieves the final on-axis tomographic compensation. We present the overall system, the control strategy and an overview of its on-sky performance.
Published: 2016

42. Experience with wavefront sensor and deformable mirror interfaces for wide-field adaptive optics systems

Author: C. N. Dunlop, Nigel Dipper, Serge Meimon, Philippe Laporte, Carine Morel, Tim Morris, J. M. Huet, B. Le Roux, Alastair Basden, Andrew P. Reeves, C. Petit, Alan H. Greenaway, Timothy Butterley, O. Martin, Henri-François Raynaud, M. L. Sánchez Rodríguez, Urban Bitenc, Fabrice Vidal, M. Cohen, Brian Stobie, Jesús Daniel Santos, A. Guesalaga, Tristan Buey, Z. Hubert, Andy Longmore, N. Looker, Philippe Feautrier, Diego Cano, Paul Clark, M. Brangier, Eric Gendron, C. D. Guzman, Arnaud Sevin, Fanny Chemla, Deli Geng, Aglae Kellerer, Jean-Luc Gach, Stephen J. Goodsell, Nazim Ali Bharmal, Caroline Kulcsár, M. Marteaud, James Osborn, David Henry, Daniel Hölck, Gaetano Sivo, Colin Dickson, Richard M. Myers, Damien Gratadour, Eric Stadler, F. J. de Cos, E. Younger, Gérard Rousset, Jean-Marc Conan, D. Perret, F. Sánchez Lasheras, G. Talbot, Stephen Todd, David Atkinson, T. Fusco, Department of Physics, Centre for Advanced Instrumentation, Durham University, Royal Observatory (UKATC), 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), Issac Newton Group, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Universidad de Oviedo [Oviedo], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire d'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), Herriot watt university, Pontificia Universidad Católica de Chile (UC), Cambridge University, 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), Institut d'Optique Graduate School (IOGS), 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), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), ONERA, Oviedo University, Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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)-Université Paris-Sud - Paris 11 (UP11), and Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)
Subjects: Physics - Instrumentation and Detectors, ASTRONOMICAL INSTRUMENTATION, FOS: Physical sciences, 02 engineering and technology, 01 natural sciences, Deformable mirror, Optics, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, Electronic engineering, Instrumentation (computer programming), METHOD, Adaptive optics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), DETECTOR, Physics, Wavefront, ADAPTIVE OPTICS, business.industry, Detector, Astronomy and Astrophysics, Wavefront sensor, Instrumentation and Detectors (physics.ins-det), Space and Planetary Science, Control system, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, 020201 artificial intelligence & image processing, Adaptive optics systems, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Recent advances in adaptive optics (AO) have led to the implementation of wide field-of-view AO systems. A number of wide-field AO systems are also planned for the forthcoming Extremely Large Telescopes. Such systems have multiple wavefront sensors of different types, and usually multiple deformable mirrors (DMs). Here, we report on our experience integrating cameras and DMs with the real-time control systems of two wide-field AO systems. These are CANARY, which has been operating on-sky since 2010, and DRAGON, which is a laboratory adaptive optics real-time demonstrator instrument. We detail the issues and difficulties that arose, along with the solutions we developed. We also provide recommendations for consideration when developing future wide-field AO systems., Accepted for publication in MNRAS
Published: 2016

43. Tomography for Astronomical Adaptive Optics using the CANARY On-Sky Demonstrator

Author: Andy Longmore, Richard Wilson, Timothy Butterley, Simon L. Morris, Colin Dickson, Eric Stadler, David Atkinson, Fabrice Vidal, Carine Morel, G. Talbot, Tim Morris, J-M. Huet, Urban Bitenc, Nigel Dipper, Stephen Todd, D. Perret, Gérard Rousset, Eric Gendron, Arnaud Sevin, P. Feautrier, F. Chemlac, M. Cohen, James Osborn, David Henry, Andrew P. Reeves, Richard M. Myers, Damien Gratadour, Tristan Buey, J-L. Gach, Alastair Basden, and E. Younger
Subjects: Wavefront, business.industry, Deformable mirror, law.invention, Telescope, Optics, Geography, Laser guide star, law, Extremely Large Telescope, William Herschel Telescope, Guide star, business, Adaptive optics, Remote sensing
Abstract: CANARY is an on-sky demonstrator instrument for the investigation of novel forms of tomographic Adaptive Optics (AO) which are required by the prospective European Extremely Large Telescope (E-ELT). CANARY is deployed on the 4.2m William Herschel Telescope in the Canary Islands, Spain. In its most evolved variant (Phase C2), CANARY employs four Laser Guide Star (LGS) Wavefront Sensors (WFS) and three Natural Guide Star (NGS) WFS to perform tomography on the turbulent atmospheric volume above the telescope. The projected wavefront phase error for a particular line of sight is then corrected by two Deformable Mirrors (DMs), and the resultant residual wavefront error is monitored by a further NGS WFS and an image recording camera. We outline the CANARY design, and present the most recent results obtained with a novel open/closed loop control approach designed to mimic the E-ELT.
Published: 2016

44. MAORY: adaptive optics module for the E-ELT

Author: Guido Agapito, E. Le Coarer, G. Cosentino, Christophe Verinaud, Matteo Lombini, F. Henault, Roberto Ragazzoni, Armando Riccardi, Laurent Jocou, L. Gluck, Laura Schreiber, Luca Fini, A. Roux, A. de Rosa, Sylvain Oberti, G. Di Rico, P. La Penna, Luca Carbonaro, O. Brissaud, Thibaut Moulin, Patrick Rabou, L. Michaud, S. Lafrasse, Marie-Helene Sztefek, Renata Abicca, Christophe Giordano, Suzanne Ramsay, Philippe Feautrier, Yves Magnard, Jean-Jacques Correia, Giovanni Bregoli, C. Del Vecchio, Giuliana Fiorentino, Paolo Saracco, Filippo Maria Zerbi, F. Mannucci, Carmelo Arcidiacono, Eric Stadler, D. Ferruzzi, M. Le Louarn, Marilena Spavone, Enrico Cascone, M. Mapelli, Sylvain Rochat, Alexis Carlotti, Fausto Cortecchia, Elisabetta Maiorano, Alfio Puglisi, Marco Bonaglia, Runa Briguglio, Marco Xompero, Daniela Fantinel, A. Delboulbe, Emiliano Diolaiti, G. Pareschi, Adriano Fontana, M. De Pascale, S. Ricciardi, Enrico Giro, Simone Esposito, N. Ventura, Andrea Baruffolo, Gianluca Morgante, Valdemaro Biliotti, Corrado Felini, Bernardo Salasnich, V. De Caprio, D. Maurel, Marco Riva, Enrico Marchetti, Italo Foppiani, M. Lauria, F. Roussel, Florian Kerber, Mauro Patti, Lorenzo Busoni, Michele Bellazzini, Mauro Ghigo, Paolo Ciliegi, ITA, FRA, and DEU
Subjects: Physics, Extremely Large Telescopes, Laser Guide Stars, business.industry, Phase (waves), Active optics, E-ELT, 01 natural sciences, Multi-Conjugate Adaptive Optics, Compensation (engineering), 010309 optics, Optics, 0103 physical sciences, Electronic engineering, Current (fluid), Adaptive optics, business, 010303 astronomy & astrophysics
Abstract: MAORY is one of the four instruments for the E-ELT approved for construction. It is an adaptive optics module offering two compensation modes: multi-conjugate and single-conjugate adaptive optics. The project has recently entered its phase B. A system-level overview of the current status of the project is given in this paper.
Published: 2016

45. The latest results from DICE (Detector Interferometric Calibration Experiment)

Author: A. Léger, E. Behar, S. Potin, P. O. Lagage, P. Kern, Christophe Cara, J. M. Le Duigou, Eric Stadler, M. Saint-Pe, A. Delboulbe, Bijan Nemati, Sylvain Rochat, G. Martin, Chengxing Zhai, C. Ketchazo, Renaud Goullioud, M. Shao, Olivier Preis, Antoine Crouzier, François Hénault, M. Donati, Philippe Feautrier, Eric Doumayrou, S. Lafrasse, Fabien Malbet, and J. Dupont
Subjects: Physics, Pixel, business.industry, Physics::Instrumentation and Detectors, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Centroid, FOS: Physical sciences, Astrometry, Metrology, Interferometry, Optics, Pixelation, Calibration, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: Theia is an astrometric mission proposed to ESA in 2014 for which one of the scientific objectives is detecting Earth-like exoplanets in the habitable zone of nearby solar-type stars. This objective requires the capability to measure stellar centroids at the precision of 1x10-5 pixel. Current state-of-the-art methods for centroid estimation have reached a precision of about 3x10-5 pixel at two times Nyquist sampling, this was shown at the JPL by the VESTA experiment. A metrology system was used to calibrate intra and inter pixel quantum efficiency variations in order to correct pixelation errors. The Theia consortium is operating a testbed in vacuum in order to achieve 1x10-5 pixel precision for the centroid estimation. The goal is to provide a proof of concept for the precision requirement of the Theia spacecraft. The testbed consists of two main sub-systems. The first one produces pseudo stars: a blackbody source is fed into a large core fiber and lights-up a pinhole mask in the object plane, which is imaged by a mirror on the CCD. The second sub-system is the metrology, it projects young fringes on the CCD. The fringes are created by two single mode fibers facing the CCD and fixed on the mirror. In this paper we present the latest experiments conducted and the results obtained after a series of upgrades on the testbed was completed. The calibration system yielded the pixel positions to an accuracy estimated at 4x10-4 pixel. After including the pixel position information, an astrometric accuracy of 6 x 10-5 pixel was obtained, for a PSF motion over more than 5 pixels. In the static mode (small jitter motion of less than 1 x 10-3 pixel), a photon noise limited precision of 3x10-5 pixel was reached.
Published: 2016
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46. ExTrA: Exoplanets in transit and their atmospheres

Author: Thierry Forveille, A. Roux, Alain Delboulbé, A. Wunsche, Jose-Manuel Almenara, Eric Stadler, P. Kern, D. Maurel, S. Lafrasse, L. Gluck, Laurent Jocou, S. Rochat, X. Delfosse, Xavier Bonfils, P. Rabou, Philippe Feautrier, Yves Magnard, Felipe Murgas, and T. Moulin
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), Planet, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Spectrograph, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, James Webb Space Telescope, Near-infrared spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Exoplanet, 13. Climate action, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract: The ExTrA facility, located at La Silla observatory, will consist of a near-infrared multi-object spectrograph fed by three 60-cm telescopes. ExTrA will add the spectroscopic resolution to the traditional differential photometry method. This shall enable the fine correction of color-dependent systematics that would otherwise hinder ground-based observations. With both this novel method and an infrared-enabled efficiency, ExTrA aims to find transiting telluric planets orbiting in the habitable zone of bright nearby M dwarfs. It shall have the versatility to do so by running its own independent survey and also by concurrently following-up on the space candidates unveiled by K2 and TESS. The exoplanets detected by ExTrA will be amenable to atmospheric characterisation with VLTs, JWST, and ELTs and could give our first peek into an exo-life laboratory., Comment: 15 pages, 11 figures, SPIE 2015
Published: 2015

47. Metrology calibration and very high accuracy centroiding with the NEAT testbed

Author: S. Potin, Olivier Preis, A. Delboulbe, E. Doumayrou, J. M. Le Duigou, J. Dupont, François Hénault, Eric Stadler, M. Donati, Philippe Feautrier, P. Lagage, P. Kern, Fabien Malbet, M. Shao, Antoine Crouzier, M. Saint-Pe, Renaud Goullioud, S. Lafrasse, A. Léger, Guillermo Martin, E. Behar, and Christophe Cara
Subjects: Physics, Pixel, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Centroid, Astrometry, First light, Metrology, Interferometry, Optics, Physics::Space Physics, Calibration, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, business, Instrumentation and Methods for Astrophysics (astro-ph.IM), Data reduction
Abstract: NEAT is an astrometric mission proposed to ESA with the objectives of detecting Earth-like exoplanets in the habitable zone of nearby solar-type stars. NEAT requires the capability to measure stellar centroids at the precision of 5 x 10 -6 pixel. Current state-of-the-art methods for centroid estimation have reached a precision of about 2 x 10 -5 pixel at two times Nyquist sampling, this was shown at the JPL by the VESTA experiment. A metrology system was used to calibrate intra and inter pixel quantum efficiency variations in order to correct pixelation errors. The European part of the NEAT consortium is building a testbed in vacuum in order to achieve 5 x 10 -6 pixel precision for the centroid estimation. The goal is to provide a proof of concept for the precision requirement of the NEAT spacecraft. The testbed consists of two main sub-systems. The first one produces pseudo stars: a blackbody source is fed into a large core fiber and lights-up a pinhole mask in the object plane, which is imaged by a mirror on the CCD. The second sub-system is the metrology, it projects young fringes on the CCD. The fringes are created by two single mode fibers facing the CCD and fixed on the mirror. In this paper we present the experiments conducted and the results obtained since July 2013 when we had the first light on both the metrology and pseudo stars. We explain the data reduction procedures we used.
Published: 2014

48. RAPID, a revolutionary fast optical to NIR camera applied to interferometry

Author: Antoine Mérand, E. De Borniol, Clélia Robert, P. Kern, Thibaut Moulin, Michel Vuillermet, Jérôme Coussement, Gérard Zins, Johan Rothman, J.-B. Le Bouquin, Sylvain Rochat, M. Tauvy, Jean-Luc Gach, Pierre Bourget, A. Delboulb, M. Jacquard, Philippe Feautrier, Eric Stadler, S. Derelle, and S. Guieu
Subjects: Physics, business.industry, media_common.quotation_subject, Near-infrared spectroscopy, Avalanche photodiode, Low noise, Interferometry, Optics, Sky, Astronomical interferometer, Instrument design, business, Focus (optics), media_common, Remote sensing
Abstract: The RAPID camera is an Avalanche Photo Diode array allowing very fast observation from the optical to the infrared with still a low noise per read. The camera born from a large collaboration within the FUI/FOCUS is intensively tested at IPAG (Grenoble) on an interferometric bench and will soon replace the actual camera of the PIONIER interferometer mounted on the visitor focus of the VLTi. We shortly present here the PIONIER instrument design and success to then focus on the RAPID tested performances. We will then resume the performance tests made on sky with the PIONIER. The RAPID camera is the first IR APD matrix ever mounted on an on-sky astronomical instrument. We show here how this fast, low-noise, large-band and sensitive camera improves PIONIER and the optical interferometry in general.
Published: 2014

49. LGSD/NGSD: high speed optical CMOS imagers for E-ELT adaptive optics

Author: Mark Downing, Johann Kolb, Philippe Balard, Bart Dierickx, Arnaud Defernez, Philippe Feautrier, Gert Finger, Martin Fryer, Jean-Luc Gach, Christian Guillaume, Norbert Hubin, Paul Jerram, Paul Jorden, Manfred Meyer, Andrew Payne, Andrew Pike, Javier Reyes, Robert Simpson, Eric Stadler, Jeremy Stent, and Nick Swift
Published: 2014

50. Very low noise Shack-Hartmann wavefront sensor for adaptive optics in the near-IR

Author: Johan Rothman, Thierry Fusco, Vincent Michau, Philippe Feautrier, Joël Deschamps, Jérôme Coussement, Eric De Borniol, Cyril Petit, Eric Stadler, Sophie Derelle, Clélia Robert, and Silvère Gousset
Subjects: Wavefront, Physics, Pixel, Physics::Instrumentation and Detectors, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Wavefront sensor, Avalanche photodiode, Residual, chemistry.chemical_compound, Optics, chemistry, Mercury cadmium telluride, Adaptive optics, business, Shack–Hartmann wavefront sensor
Abstract: Near-Infrared wave front sensing allows to enhance sky coverage with adaptive optics. The recently developed HgCdTe avalanche photodiode arrays are promising, but still present an unperfect cosmetic. After the fine characterization of such a HgCdTe array, we propose a statistical model of the pixel response. Assuming the cosmetic is partially corrected, we simulate the impact of the residual error on a Shack-Hartmann wavefront sensor measurement. The study shows the operability of such a real time correction, and of the HgCdTe APD array characterized in this framework: the RAPID camera.
Published: 2014

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