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1. Ultrafast laser processing of refractive index changes in bulk Ge15As15S70 chalcogenide glass for photonics applications in the mid-infrared

Author

Manoj Kumar Bhuyan, Etienne LeCoarer, B. Arezki, P. Kern, Jean-Philippe Colombier, Laurent Calvez, Celine Caillaud, Guillermo Martin, C. D'Amico, Praveen Kumar Velpula, Virginie Nazabal, J. Troles, Razvan Stoian, Laboratoire Hubert Curien (LHC), Institut d'Optique Graduate School (IOGS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences Chimiques de Rennes (ISCR), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-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]), Laboratoire Hubert Curien [Saint Etienne] (LHC), Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes-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), Institut d'Optique Graduate School (IOGS)-Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), and Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)

Subjects
Materials science, business.industry, Chalcogenide, Doping, Physics::Optics, Chalcogenide glass, 02 engineering and technology, 021001 nanoscience & nanotechnology, Condensed Matter::Disordered Systems and Neural Networks, 01 natural sciences, Waveguide (optics), chemistry.chemical_compound, Optics, chemistry, 0103 physical sciences, [CHIM]Chemical Sciences, Photonics, 0210 nano-technology, business, 010303 astronomy & astrophysics, Ultrashort pulse, Refractive index, Excitation, ComputingMilieux_MISCELLANEOUS
Abstract

We study the role of carrier excitation in driving either heat deposition or non-thermal molecular mobility via electronic relaxation in ultrafast laser-irradiated chalcogenide S-based glasses. We show the influence of doping and of the glass thermal history in determining permanent positive and negative refractive index change regimes (type I or type II) discussing the case of Ge 15 As 15 S 70 chalcogenide glass. We also point out material and index engineering approaches in defining large mode area light transport concepts in evanescently-coupled waveguide arrays and their application for building embedded detectors for astronomical measurements.

Published
2016

2. All integrated Lithium Niobate Standing Wave Fourier Transform Spectrometer to improve sampling resolution

Author

Fabrice Thomas, Samuel Heidmann, Mikhaël de Mengin, Nadège Courjal, Gwenn Ulliac, Alain Morand, Pierre Benech, Pierre Kern, Etienne Lecoarer, Resolution Spectra Systems, 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), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), Institut de Microélectronique, Electromagnétisme et Photonique - Laboratoire d'Hyperfréquences et Caractérisation (IMEP-LAHC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2015

3. AMBER: a near infrared focal instrument for the VLTI

Author

Michael Geng, Martin Vannier, G. Martinot-Lagarde, M. Dugué, Yves Rabbia, S. Rebattu, Djamel Mékarnia, T. Forveille, Bruno Lopez, Karl-Heinz Hofmann, Stephane Lagarde, Carlo Baffa, Gilles Duvert, Pascal Puget, Karine Rousselet-Perraut, Fabien Malbet, Albrecht Dreiss, Udo Beckmann, Andrea Richichi, Eric Aristidi, Romain Petrov, Frédéric Cassaing, Danielle LeContel, Markus Schoeller, Yves Bresson, S. Robbe-Dubois, A. Glentzlin, Alessandro Marconi, D. Kamm, Philippe Berio, Sandro Gennari, David Mouillet, François Reynaud, P. Antonelli, K. Agabi, Isabelle Tallon-Bosc, Piero Salinari, Jean-Louis Monin, Franco Lisi, G. Mars, Alain Chelli, Etienne LeCoarer, M. Sacchettini, Gerd Weigelt, Denis Mourard, Laboratoire Universitaire d'Astrophysique de Nice (LUAN), 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)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Radioastronomie (MPIFR), Département Fresnel (FRESNEL), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-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), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Division technique INSU/SDU (DTI), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche en Communications Optiques et Microondes (IRCOM), Université de Limoges (UNILIM)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), 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), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Limoges (UNILIM), 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
Active galactic nucleus, Young stellar object, FOS: Physical sciences, General Physics and Astronomy, Astrophysics, 01 natural sciences, 7. Clean energy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010309 optics, Optics, [CHIM.ANAL]Chemical Sciences/Analytical chemistry, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, optical interferometry, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, instrumentation, Physics, Very Large Telescope, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Spatial filter, business.industry, Astrophysics (astro-ph), Near-infrared spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, Single-mode optical fiber, Astronomy, [CHIM.MATE]Chemical Sciences/Material chemistry, Exoplanet, astronomy, very large telescope, Interferometry, Astrophysics::Earth and Planetary Astrophysics, business, high angular resolution
Abstract

AMBER is the General User near-infrared focal instrument of the Very Large Telescope interferometer. Its specifications are based on three key programs on Young Stellar Objects, Active Galactic Nuclei central regions, masses and spectra of hot Extra Solar Planets. It has an imaging capacity because it combines up to three beams and very high accuracy measurement are expected from the spatial filtering of beams by single mode fibers and the comparison of measurements made simultaneously in different spectral channels., 10 pages

Published
2001
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4. A compact SWIFTS spectrograph with a leaky loop structure

Author

Pierre Benech, Gilles Lerondel, Sylvain Blaize, B. Martin, Etienne Lecoarer, Gregory Leblond, and Alain Morand

Subjects
business.industry, Photonic integrated circuit, Bent molecular geometry, Physics::Optics, Near and far field, Effective radiated power, Discrete Fourier transform, law.invention, symbols.namesake, Fourier transform, Optics, law, symbols, business, Waveguide, Fourier series, Mathematics
Abstract

This paper deals with a new spectrograph on integrated optics. It is composed of an Y-junction where the two junction arms are guided in a loop structure in order to obtain an interference pattern. The measurement of this intensity distribution gives access to the optical spectrum source after a Inverse Fourier Transform. To measure it, we use the property of the loop composed of a bent waveguide which is a leaky structure. Depending on the radius of the bent waveguide, a part of the light leaks from the waveguide to outside. The radiated power, proportional to the intensity in the waveguide, is coupled into a plan waveguide set near the bent waveguide. Indeed the two structures are separated by a gap which changes along the periphery of the loop. This structure enables both to control the leaking light part and to confine in the plan waveguide the propagation of the radiated field. Thereby, the radiated intensity is measured at a peculiar distance of the loop on a perpendicular plan to the input waveguide. So, the interference pattern measured is magnified by the ratio of the plan waveguide length over the loop radius, allowing to use a commercial photodetectors array to sufficiently sample the interference pattern. The spectrum is finally obtained operating a Discrete Fourier Transform. The device modelization is divided in two parts. The first part describes the coupling between the bent and the plan waveguide modelised by a modal method based on a Fourier series expansion (RCWA) combined with an exponential conformal mapping in order to simulate the electromagnetic field near the loop. The second part describes the Helmholtz-Kirchhoff theorem to simulate the far-electromagnetic field. From the interference pattern modelized, the spectrum of the signal is then calculated. A demonstrator in integrated optics on glass is being developed.

Published
2008
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5. VITRUV - Imaging Close Environments of Stars and Galaxies with the VLTI at Milli-Arcsec Resolution

Author

Fabien Malbet, J. B. Lebouquin, Jean-Philippe Berger, Pierre Labeye, Etienne LeCoarer, Laurent Jocou, Paulo J. V. Garcia, Emilie Herwats, Karine Perraut, Eric Thi éebaut, Myriam Benisty, E. Tatulli, Olivier Preis, Pierre Kern, 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), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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), The European Southern Observatory (ESO), F. Paresce, A. Richichi, A. Chelli et al., Universidade do Porto, 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
Physics, Active galactic nucleus, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, Aperture synthesis, Astrophysics (astro-ph), Near-infrared spectroscopy, FOS: Physical sciences, Integrated optics, Astrophysics, 01 natural sciences, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010309 optics, Joint research, Interferometry, Stars, 0103 physical sciences, Large telescopes, 010303 astronomy & astrophysics
Abstract

The VITRUV project has the objective to deliver milli-arcsecond spectro-images of the environment of compact sources like young stars, active galaxies and evolved stars to the community. This instrument of the VLTI second generation based on the integrated optics technology is able to combine from 4 to 8 beams from the VLT telescopes. Working primarily in the near infrared, it will provide intermediate to high spectral resolutions and eventually polarization analysis. This paper summarizes the result from the concept study led within the Joint Research Activity advanced instruments of the OPTICON program., In "The Power of Optical/IR Interferometry: Recent Scientific Results and 2nd Generation VLTI Instrumentation", Allemagne (2005) in press

Published
2007
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6. A Laboratory Interferometer for VITRUV

Author

Etienne LeCoarer, A. Delboulbe, Fabien Malbet, Laurent Jocou, Jean-Philippe Berger, K. Perraut, P. Kern, Pierre Gratier, Yves Magnard, and Myriam Benisty

Subjects
Physics, Interferometry, Optics, business.industry, Binary star, business
Published
2007
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7. Recent Progress in Mid Infrared Integrated Optics for Nulling Interferometry

Author

Laetitia Abel-Tiberini, Annie Pradel, P. Labeye, Cyril Ruilier, Volker Kirschner, Etienne LeCoarer, Alain Delboulbé, Caroline Vigreux-Bercovici, Pierre Saguet, Pierre Kern, Marc Barillot, Jean-Emmanuel Broquin, Brahim Arezki, Lucas Labadie, 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), Institut Charles Gerhardt Montpellier - Institut de Chimie Moléculaire et des Matériaux de Montpellier (ICGM ICMMM), Université Montpellier 1 (UM1)-Université Montpellier 2 - Sciences et Techniques (UM2)-Ecole Nationale Supérieure de Chimie de Montpellier (ENSCM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de Microélectronique, Electromagnétisme et Photonique (IMEP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Ecole Nationale Supérieure de Chimie de Montpellier (ENSCM)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Université Montpellier 1 (UM1)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut de Chimie du CNRS (INC), Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG)-Université Joseph Fourier - Grenoble 1 (UJF), and European Space Agency (ESA)

Subjects
Wavefront, Physics, business.industry, Optical engineering, Near-infrared spectroscopy, 02 engineering and technology, 021001 nanoscience & nanotechnology, Polarization (waves), 01 natural sciences, 7. Clean energy, Starlight, law.invention, 010309 optics, Interferometry, Modal, Optics, law, 0103 physical sciences, [PHYS.COND.CM-MS]Physics [physics]/Condensed Matter [cond-mat]/Materials Science [cond-mat.mtrl-sci], 0210 nano-technology, business, Waveguide, ComputingMilieux_MISCELLANEOUS
Abstract

This paper presents the development and tests in the thermal infrared of Integrated Optics (IO) technology in preparation of ESA's space mission Darwin . This mission aims to detect and characterize earth-like planets orbiting solar-type stars, using nulling interferometry in the spectral range 6 - 20 μm. Since typically 1:1e6 rejection of starlight is required, wavefront modal filtering is mandatory. Thus, mid-infrared single-mode IO is being developed in the framework of the ESA-funded "Integrated Optics for Darwin" project. Beyond its wavefront filtering capabilities, an IO component may support various optical functions, and is thus likely to ease instrumental design. This paper addresses the manufacturing process and the characterization tests results of newly developed IO devices. Investigated solutions are dielectric waveguides based on Chalcogenide glasses and Hollow Metallic Waveguides. In a first phase, the pre-selected technological solutions were validated and modal behavior of the manufactured devices was demonstrated, both through polarization and spectral analysis. Preliminary nulling ratios up to 5000 have been obtained with an IO modal filter in the 6 - 20 μm range. In a second phase of the project, the development of more complex IO functions was attempted. The methods used to validate the waveguide behavior and interferometric capabilities are also discussed. After achieving 1:1e5 polychromatic extinctions with similar solutions in the near IR, the presented results further underline the credibility of a mid-infrared IO concept for Darwin.© (2006) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

Published
2006
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8. AMBER integration and laboratory performances

Author

Gerard Zins, E. Tatulli, Yves Magnard, Florentin Millour, J. Behrend, Karine Rousselet-Perraut, Matteo Accardo, P. Antonelli, Stephane Lagarde, Yves Bresson, Franco Lisi, Carla S. Gil, Fabien Malbet, Etienne LeCoarer, Udo Beckmann, S. Busoni, Pierre Kern, L. Gluck, Gilles Duvert, Alain Delboulbé, Brahim Arezki, Sylvie Robbe-Dubois, Alain Roussel, and Romain Petrov

Subjects
Physics, Accuracy and precision, Optics, Modal, business.industry, K band, media_common.quotation_subject, Contrast (vision), Spectral resolution, business, Throughput (business), Stability (probability), media_common
Abstract

AMBER is the focal near-infrared instrument of the VLTI combining 2 or 3 telescopes in the J, H and K bands with 3 spectral resolution modes. It uses single-mode fibers to ensure modal filtering and high measurement accuracies. AMBER has been integrated and tested in Grenoble during 2003. We report in this paper the lab performances of the instrument in terms of instrumental contrast, measurement accuracy and stability, and throughput.

Published
2004
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9. A laboratory interferometer simulator for integrated optics combiners qualification

Author

Laurent Jocou, Jean-Philippe Berger, Pierre Kern, Pierre Haguenauer, Etienne LeCoarer, Karine Rousselet-Perraut, Fabien Malbet, and Myriam Benisty

Subjects
Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Reconfigurable array, law.invention, Telescope, Interferometry, Optics, law, Binary star, Astronomical interferometer, Astrophysics::Solar and Stellar Astrophysics, Integrated optics, Astrophysics::Earth and Planetary Astrophysics, business, Simulation
Abstract

We present a laboratotry interferometer simulator specifically designed to characterize prototype integrated optics combiners. In the current configuration it allows to simulate a complex object made of luminous points and observe it with a reconfigurable array made of three telescopes. We used a three-way integrated optics similar to the one used at IOTA to combine the beams. We describe it in detail and present first validation measurements and the first measurements of a binary star. This work paves the way for an up-to eight telescope simulator capable of simulating the VLTI and the VITRUV focal instrument.

Published
2004
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10. The VLTI focal instrument Amber: results of the first phase of the alignment, integration, and verification in Paranal

Author

Gerd Weigelt, Florentin Millour, P. Stefanini, Martin Vannier, Gerard Zins, Franco Lisi, Andrea Richichi, Pedro Mardones, Gilles Duvert, Fredrik T. Rantakyrö, Etienne LeCoarer, Karine Rousselet-Perraut, Stephane Lagarde, Florence Puech, Markus Schoeller, Carla S. Gil, L. Gluck, P. Antonelli, N. Haddad, E. Tatulli, Fabien Malbet, Udo Beckmann, M. Heininger, Pierre Kern, Matteo Accardo, Nico Housen, Denis Mourard, Sylvie Robbe-Dubois, Romain Petrov, Mario Kiekebusch, Yves Bresson, Alain Delboulbé, and Alain Roussel

Subjects
Physics, Stars, Optics, business.industry, Instrumentation, Phase (waves), Multi beam, Spectral bands, business, Visibility, Differential phase, Remote sensing
Abstract

AMBER, Astronomical Multi BEam combineR, is the near-infrared focal instrument dedicated to the VLTI. It is designed to combine three of the VLTI Telescopes and to work simultaneously in the J, H and K spectral bands (1.0 to 2.4 μm). The project successfully passed the Preliminary Acceptance in Europe in November 2003, resulting in the validation of the instrument laboratory performance1, of the compliance with the initial scientific specifications, and of the acceptance of ESO for AMBER to be part of the VLTI. After the transportation of the instrument to Paranal, Chile in January 2004, the Assembly Integration and Verification phase occurred mid-March to succeed with the first fringes observing bright stars with the VLTI siderostats. This paper describes the different steps of the AIV and the first results in terms of instrumental stability, estimated visibility and differential phase.

Published
2004
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11. Design and tests for the correction of atmospheric and instrumental effects on color-differential phase with AMBER/VLTI

Author

Sebastien Morel, Sylvie Robbe-Dubois, Stephane Lagarde, Andreas Glindemann, Karine Rousselet-Perraut, Martin Vannier, Romain Petrov, Markus Schoeller, P. Antonelli, Gilles Duvert, Yves Bresson, Fabien Malbet, Etienne LeCoarer, Carla S. Gil, Florentin Millour, Bruno Lopez, and Fredrik T. Rantakyrö

Subjects
Physics, business.industry, Near-infrared spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, Phase (waves), Observable, Residual, Exoplanet, Differential phase, Interferometry, Optics, Astrophysics::Solar and Stellar Astrophysics, Chromatic scale, business
Abstract

The near-infrared instrument AMBER at the VLTI allows, among other interferometric observables, the simultaneous measurement of the phase between various spectral channels. Color-differential phase thus yields spatial and spectral information on unresolved sources, and could lead to such ambitious goals as the spectroscopy of nearby hot, giant exoplanets. This will require, though, an extreme stability on the measurement, which is likely to be affected by chromatic effects at the various stages of the light path. We present how AMBER has been designed to minimize and to calibrate such effects. We give estimates of their contributions from different origins, and present recent measurements of the instrumental stability. We discuss the possibility to supress the residual chromatic effects in post-data treatment in order to reach a precision limited by the photon noise on the differential phase.

Published
2004
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12. AMBER instrument control software

Author

Gilles Duvert, J. M. Clausse, C. Connot, Etienne LeCoarer, Florentin Millour, J. Behrend, Keiichi Ohnaka, Thomas Driebe, M. Dugué, L. Gluck, Gerard Zins, and M. Heininger

Subjects
Physics, Very Large Telescope, Instrument control, business.industry, Aperture, Instrumentation, Astrophysics::Instrumentation and Methods for Astrophysics, Interferometry, Software, Astronomical interferometer, Calibration, Astrophysics::Solar and Stellar Astrophysics, business, Computer hardware, Remote sensing
Abstract

AMBER (Astronomical Multiple BEam Recombiner) is a 3 aperture interferometric recombiner operating between 1 and 2.5 um, for the Very Large Telescope Interferometer (VLTI). The control software of the instrument, based on the VLT Common Software, has been written to comply with specific features of the AMBER hardware, such as the Infrared detector read out modes or piezo stage drivers, as well as with the very specific operation modes of an interferomtric instrument. In this respect, the AMBER control software was designed to insure that all operations, from the preparation of the observations to the control/command of the instrument during the observations, would be kept as simple as possible for the users and operators, opening the use of an interferometric instrument to the largest community of astronomers. Peculiar attention was given to internal checks and calibration procedures both to evaluate data quality in real time, and improve the successes of long term UV plane coverage observations.

Published
2004
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13. Using the near infrared VLTI instrument AMBER

Author

P. Antonelli, Gilles Duvert, Denis Mourard, Gerd Weigelt, Sylvie Robbe-Dubois, Sandro Gennari, M. Dugué, Etienne LeCoarer, Fabien Malbet, Udo Beckmann, Karine Rousselet-Perraut, Stephane Lagarde, Alain Chelli, Romain Petrov, Martin Vannier, Pascal Puget, and Franco Lisi

Subjects
Physics, Very Large Telescope, Young stellar object, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics, Exoplanet, Planet, Limiting magnitude, Closure phase, Astronomical interferometer, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Spectral resolution, Astrophysics::Galaxy Astrophysics
Abstract

AMBER is the General User near infrared focal instrument of the Very Large Telescope Interferometer. Its a single mode, dispersed fringes, three telescopes instrument. A limiting magnitude of the order of H=13 will allow to tackle a fair sample of extra galactic targets. A very high accuracy, in particular in color differential phase and closure phase modes gives good hope for very high dynamic range observation, possibly including hot extra solar planets. The relatively high maximum spectral resolution, up to 10000, will allow some stellar activity observations. Between this extreme goals, AMBER should have a wide range of applications including Young Stellar Objects, Evolved Stars, circumstellar material and many others. This paper tries to introduce AMBER to its future users with information on what it measures, how it is calibrated and hopes to give the readers ideas for applications.

Published
2003
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14. Large-mode-area infrared guiding in ultrafast laser written waveguides in Sulfur-based chalcogenide glasses

Author

Johann Troles, Etienne LeCoarer, Virginie Nazabal, Guillermo Martin, Brahim Arezki, Razvan Stoian, Guanghua Cheng, Celine Caillaud, Cyril Mauclair, C. D'Amico, P. Kern, Laurent Calvez, Laboratoire Hubert Curien [Saint Etienne] (LHC), Institut d'Optique Graduate School (IOGS)-Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS), State Key Laboratory of Transient Optics and Photonics (XIOPM), Xi'an Institute of Optics and Precision Mechanics, Institut des Sciences Chimiques de Rennes (ISCR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), ULTRA, Laboratoire Hubert Curien (LHC), Institut d'Optique Graduate School (IOGS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Materials science, business.industry, Infrared, Chalcogenide, (140.3390) Laser materials processing, (320.2250) Femtosecond phenomena, (230.7370) Waveguides, (130.3120) Integrated optics devices, (160.2750) Glass and other amorphous materials, (130.3060) Infrared, Physics::Optics, Chalcogenide glass, Laser, Atomic and Molecular Physics, and Optics, law.invention, chalcogenide glass, Interferometry, chemistry.chemical_compound, Optics, 3D photonics, chemistry, refractive index changes, law, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, Optoelectronics, ultrafast laser fabrication, business, Refractive index, Ultrashort pulse, Phase modulation
Abstract

International audience; Current demands in astrophotonics impose advancing optical functions in infrared domains within embedded refractive index designs. We demonstrate concepts for large-mode-area guiding in ultrafast laser photowritten waveguides in bulk Sulfur-based chalcogenide glasses. If positive index contrasts are weak in As2S3, Ge doping increases the matrix rigidity and allows for high contrast (10−3) positive refractive index changes. Guiding with variable mode diameter and large-mode-area light transport is demonstrated up to 10μm spectral domain using transverse slit-shaped and evanescently-coupled multicore traces.

Published
2014
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15. Combining and cophasing a telescope array in a single chip-integrated optics: a new solution for spaced based aperture synthesis interferometry

Author

Karine Perraut, P. Haguenauer, P. Kern, I. Schanen, Etienne LeCoarer, Jean-Emmanuel Broquin, M. Lacolle, Fabien Malbet, J. P. Berger, Pierre Benech, Sylvain Blaize, E. Ghibaudo, C. Sanchez-Perez, G. Fontaine, 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), Institut de Microélectronique, Electromagnétisme et Photonique (IMEP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Nanotechnologie et d'Instrumentation Optique (LNIO), Institut Charles Delaunay (ICD), Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG)-Université Joseph Fourier - Grenoble 1 (UJF), and Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)

Subjects
Active galactic nucleus, Aperture synthesis, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, law.invention, Telescope, Optics, interferometers, law, Astronomical interferometer, Astrophysics::Solar and Stellar Astrophysics, Angular resolution, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, telescopes, waveguides, Exoplanet, Cophasing, Interferometry, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, Astrophysics::Earth and Planetary Astrophysics, business
Abstract

Astrophysical key programs such as exoplanet detection, young stars accretion disk and active galactic nuclei imaging require high angular resolution capability. Today, optical long baseline interferometers are the only instruments to allow such resolutions.

Published
2000
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16. GriF: an infrared 3D spectroscopic mode for KIR/PUEO

Author

Patrick Rabou, Olivier Lai, Sylvain Pau, Yann Clénet, A. Chalabaev, Claude Delage, Robin Arsenault, Gilles Joncas, Daniel Rouan, David Le Mignant, Jean-Luc Beuzit, Etienne LeCoarer, and Francois Lacombe

Subjects
Physics, business.industry, Near-infrared spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Grism, Interferometry, Optics, Astronomical interferometer, Spectral resolution, business, Adaptive optics, Image resolution, Fabry–Pérot interferometer
Abstract

When combined with Adaptive Optics, integral field spectroscopy, i.e. observation of a sky field simultaneously in a number of spectral passbands, is the most efficient way to perform spectro-imaging at high angular resolution. GriF will provide the CFHT community with such a capability in the near infrared K-band. This extension will be completed by means of two simple optical devices to be installed in the KIR cryostat (the infrared camera of PUEO): a cooled grism in the filter-wheel and a cold aperture on an entrance focal plane wheel. They will be completed by a room-temperature Fabry- Perot (FP) interferometer in front of KIR. The FP selects narrow bandpass images while the grism spatially separates them, giving a 3-D spectroscopic capacity within a compact and light design. At each exposure, several (up to 9) monochromatic images of a rectangular field of about 36 arcseconds X 4 arc-seconds will be simultaneously acquired, allowing a precise subtraction of continuum and background. The cooled grism will guarantee a low background environment, thus a good sensitivity at K. The medium spectral resolution (about 2600) will fit to a number of programs and will represent a considerable improvement on imaging with narrow- band filters. Thus, combining high angular resolution with the spectroscopic diagnosis, GriF will allow the study of a large class of compact objects or structures, especially in the extragalactic domain where its sensitivity should be unique.

Published
2000
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17. PUMA: the first results of a nebular spectrograph for the study of the kinematics of interstellar medium

Author

Leonel Gutierrez, Etienne LeCoarer, Abel Bernal, Francisco J. Cobos Duenas, Silvio J. Tinoco, Carlos Tejada, Margarita Rosado, F. Garfias, and R. Langarica

Subjects
Physics, business.industry, Field of view, law.invention, Telescope, Interferometry, Optics, law, Observatory, Astronomical interferometer, Spectral resolution, business, Spectrograph, Free spectral range, Remote sensing
Abstract

The kinematics of the interstellar medium may be studied by means of a scanning Fabry-Perot interferometer (SFPI). This allows the coverage of a wider field of view with higher spatial and spectral resolution than when a high-dispersion classical spectrograph is used. The system called PUMA consists of a focal reducer and a SFPI installed in the 2.1 m telescope of the San Pedro Martir National Astronomical Observatory (SPM), Mexico, in its f/7.5 configuration. It covers a field of view of 10 arcmin providing direct images as well as interferograms which are focused on a 1024 X 1024 Tektronix CCD, covering a wide spectral range. It is considered the integration of other optical elements for further developments. The optomechanical system and the developed software allow exact, remote positioning of all movable parts and control the FPI scanning and data acquisition. The parallelism of the interferometer plates is automatically achieved by a custom method. The PUMA provides spectral resolutions of 0.414 Angstrom and a free spectral range of 19.8 Angstrom. Results of high quality that compete with those obtained by similar systems in bigger telescopes, are presented.

Published
1998
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18. Astronomical uses of integral field spectrography: present applications at CFHT and future developments

Author

Y. P. Georgelin, Guy Monnet, Christian Vanderriest, Etienne LeCoarer, and Roland Bacon

Subjects
Astronomical Objects, Physics, Galactic astronomy, Star formation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, law.invention, Telescope, law, Globular cluster, Astrophysics::Solar and Stellar Astrophysics, Spectral resolution, Adaptive optics, Image resolution, Astrophysics::Galaxy Astrophysics
Abstract

Since the digital detectors (like CCDs) presently available for astronomical instruments have two dimensions only, there is an obvious problem for obtaining detailed spectroscopic information on extended astronomical objects (e.g. active galaxies, regions of star formation, globular clusters, etc.); the classical long- slit spectrographic techniques are grossly inadequate. Several so-called integral field spectrographs (IFS) have been used at the Canada-France-Hawaii telescope during the past years to improve this situation. They typically provide hundreds of spectra in a small (approximately 10' by 10') field with a subarcsecond spatial resolution capability and hundreds of spectral elements, both simultaneously accessed. We describe these various instruments and their present performances, review a few illustrative results obtained with CFH telescope and discuss the expected developments: use of IFS in combination with adaptive optics systems for the study of individual objects at spatial resolution near the 0.1' level, as well as their potential capabilities on Very Large Telescopes, with or without adaptive optics.

Published
1994
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19. 2-D mask generation by YAG laser for multiobject spectroscopy at CFHT: LAMA

Author

Etienne LeCoarer, Bernard DiBiagio, and Gerard R. Lemaitre

Subjects
Curvilinear coordinates, Engineering, business.industry, Edge (geometry), Laser, law.invention, Telescope, Optics, law, Feature (computer vision), Optoelectronics, Rectangle, Spectroscopy, business, Punching
Abstract

New YAG lasers have been found as useful machines to generate 2D masks for multi-object spectroscopy. Compared to the punching technique presently under operation in some astrophysical observatories or to the C02 laser capability, the performances are higher in several ways. The cutting accuracy at the edge of slits is greatly increased and can be improved by selecting the number of loop paths. The size of conventional rectangle slits is easily controlled. Another feature of interest is that various type of curvilinear slits can be generated. Presented results have been obtained with the YAG laser machine commissioned by the Canada-France-Hawaii Telescope Corp.

Published
1990
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20. Qualification of IONIC (integrated optics near-infrared interferometric camera)

Author

Denis Mourard, Guillaume Huss, Fabien Malbet, Pierre Haguenauer, Etienne LeCoarer, Jean-Philippe Berger, Karine Perraut-Rousselet, Sam Ragland, François Reynaud, Pierre Kern, and Panayoti Petmezakis

Subjects
Physics, Optical fiber, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral bands, law.invention, Interferometry, chemistry.chemical_compound, Optics, Observational astronomy, chemistry, law, K band, Astronomical interferometer, Optoelectronics, Astrophysics::Earth and Planetary Astrophysics, Infrared detector, Mercury cadmium telluride, business
Abstract

We report the first technical results of the Integrated Optics Near-infrared Interferometric Camera developed and characterized at the Observatoire de Grenoble as well as the first tests carried out on the GI2T Interferometer (Observatoire de la Cote d'Azur, France). This near-infrared interferometric camera dedicated to astronomical observations is implemented in a single dewar, which hosts the planar integrated optics beam combiner and a cooled HgCdTe infrared detector, with optical interfaces reduced to optical fibers for signal injection in the component. Thanks to its versatility, this concept allows to combine any number of telescopes in the near infrared range (J, H and K bands). The compactness of the integrated optics components allows various combining schemes (co- and multi-axial ones) and observations in different spectral bands simultaneously. Finally, a camera upgrade with a PICNIC chip is also described. This new set-up under integration at the Observatoire de Grenoble would allow to reach limiting magnitudes of H equals 4 - 6 with the GI2T.

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