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13 results on '"Alberto Gennai"'

1. interTwin D7.2 Report on requirements and thematic modules definition for the physics domain first version

Author

Kalliopi Tsolaki, Sofia Vallecorsa, David Rousseau, Isabel Campos, Yurii Pidopryhora, Sara Vallero, Alberto Gennai, and Massimiliano Razzano

Subjects
Particle detector simulation, Gravitational Waves, Digital Twin, Lattice QCD, Radio Astronomy, High Energy Physics
Abstract

interTwin co-designs and implements the prototype of an interdisciplinary Digital Twin Engine (DTE). The developed DTE will be an open source platform that includes software components for modelling and simulation to integrate application-specific Digital Twins. InterTwin WP7 will provide the aforementioned sets of software components, called thematic modules, for the use cases defined in WP4. The current document consists of a report on the high-level description of the physics domain use cases and of the related designed thematic modules. Additionally, this deliverable includes the set of common requirements derived from the analysis of the use cases and thematic modules that will need to be available in the DTE core modules, designed in WP6.

Published
2023
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2. Study of correlations between seismic data and Virgo's gravitational-wave detector data

Author

Przemysław Figura, Tomasz Bulik, Jan Harms, Enrico Calloni, Luciano Errico, Rosario De Rosa, Alberto Gennai, Figura, P., Bulik, T., Harms, J., Calloni, E., Errico, L., De Rosa, R., and Gennai, A.

Subjects
General Relativity and Quantum Cosmology, Physics and Astronomy (miscellaneous), Virgo, tiltmeter, gravitational waves, Newtonian noise
Abstract

It is expected that noise produced by terrestrial gravity fluctuations will start to limit the sensitivity of the ground-based, gravitational-wave detector Virgo in coming observation runs. A system is under preparation at Virgo to cancel this noise, also known as Newtonian noise. This Newtonian noise cancelation system requires the deployment of seismometer arrays inside the Virgo buildings. Crucial for the design of such a system is a detailed understanding of correlations between ground vibrations and Virgo’s gravitational waves detector data. In this article, we present first analyses of such correlations observed with a tiltmeter. We find that revealed correlations are stronger than predicted by possible pure gravitational coupling, which is pointing towards additional coupling mechanisms. These findings might impact the design of the Newtonian noise cancelation system if the additional couplings cannot be mitigated.

Published
2022

3. The VLT Interferometer

Author

Francesco Paresce, Pierre Kervella, Bertrand Koehler, Philippe B. Gitton, Samuel Lévêque, Andrea Richichi, M. Tarenghi, Frederic Derie, Than Phan Duc, Francoise Delplancke, Alain Michel, Serge Menardi, Franco Carbognani, Rainer Wilhelm, Anders Wallander, Markus Schöller, Alberto Gennai, Andreas Glindemann, and Roberto Abuter

Subjects
Physics, Very Large Telescope, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, General Physics and Astronomy, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrometry, Interferometry, Optics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, business, Astrophysics::Galaxy Astrophysics
Abstract

One of the observing modes available with the ESO Very Large Telescope will be coherent combination of the light received by up to four 8m unit telescopes and several 1.8m auxiliary telescopes. The location of the main telescopes is fixed, while auxiliary telescopes can be moved among some 30 observing stations. The locations of these stations were chosen to augment the (µ, υ) coverage of the unit telescopes as well as to function as an independent interferometric array.

Published
2001
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4. Low-loss coatings for the VIRGO large mirrors

Author

Roland Geyl, Laurent Mazuray, Jean Pierre Chatard, Claude Amra, F. Beauville, D. Buskulic, R. Flaminio, F. Marion, A. Masserot, L. Massonnet, B. Mours, F. Moreau, J. Ramonet, E. Tournefier, D. Verkindt, O. Veziant, M. Yvert, Regis Barille, Vincenzino Dattilo, Daniel Enard, Franco Frasconi, Alberto Gennai, Paolo La Penna, Magali Loupias, Federico Paoletti, L. Bracci, Giovanni Calamai, E. Campagna, G. Conforto, E. Cuoco, I. Fiori, G. Guidi, G. Losurdo, Fabrizio Martelli, Massimo Mazzoni, B. Perniola, Ruagero N. Stanga, Flavio Vetrano, A. Vicere, D. Babusci, Gianfranco Giordano, Jean Marie Mackowski, Nazario Morgado, Laurent Pinard, Alban Remillieux, Fausto Acernese, Fabrizio Barone, Luciano Di Fiore, Antonio Eleuteri, Leopoldo Milano, Ketevan Qipiani, Iolanda Ricciardi, RUSSO, GUIDO, Salvatore Solimeno, M. Varvella, Francois Bondu, Alain Brillet, Eric Chassande Mottin, Frederic Cleva, T. Cokelaer, J. P. Coulon, B. Dujardin, J. D. Fournier, H. Heitmann, Catherine N. Man, F. Mornet, J. Pacheco, A. Pai, Herve Trinquet, J. Y. Vinet, N. Arnaud, M. Barsuglia, M. A. Bizouard, V. Brisson, F. Cavalier, M. Davier, P. Hello, P. Heusse, S. Kreckelberg, A. Claude Boccara, Vincent Loriette, J. Moreau, V. Reita, P. Amico, L. Bosi, Luca Gammaitoni, M. Punturo, F. Travasso, H. Vocca, L. Barsotti, S. Braccini, C. Bradaschia, G. Cella, C. Corda, A. Di Virgilio, I. Ferrante, F. Fidecaro, Adalberto Giazotto, E. Majorana, L. Holloway, R. Passaquieti, D. Passuello, R. Poggiani, A. Toncelli, M. Tonelli, L. Brocco, S. Frasca, C. Palomba, P. Puppo, P. Rapagnani, F. Ricci, David Rimmer, Philip J. Rogers, Norbert Kaiser, Peter N. J. Dennis, Lingli Wang, H. Angus Macleod, Rolf Wartmann, CALLONI, ENRICO, DE ROSA, ROSARIO, Roland, Geyl, Laurent, Mazuray, Jean Pierre, Chatard, Claude, Amra, F., Beauville, D., Buskulic, R., Flaminio, F., Marion, A., Masserot, L., Massonnet, B., Mour, F., Moreau, J., Ramonet, E., Tournefier, D., Verkindt, O., Veziant, M., Yvert, Regis, Barille, Vincenzino, Dattilo, Daniel, Enard, Franco, Frasconi, Alberto, Gennai, Paolo La, Penna, Magali, Loupia, Federico, Paoletti, L., Bracci, Giovanni, Calamai, E., Campagna, G., Conforto, E., Cuoco, I., Fiori, G., Guidi, G., Losurdo, Fabrizio, Martelli, Massimo, Mazzoni, B., Perniola, Ruagero N., Stanga, Flavio, Vetrano, A., Vicere, D., Babusci, Gianfranco, Giordano, Jean Marie, Mackowski, Nazario, Morgado, Laurent, Pinard, Alban, Remillieux, Fausto, Acernese, Fabrizio, Barone, Calloni, Enrico, DE ROSA, Rosario, Luciano Di, Fiore, Antonio, Eleuteri, Leopoldo, Milano, Ketevan, Qipiani, Iolanda, Ricciardi, Russo, Guido, Salvatore, Solimeno, M., Varvella, Francois, Bondu, Alain, Brillet, Eric Chassande, Mottin, Frederic, Cleva, T., Cokelaer, J. P., Coulon, B., Dujardin, J. D., Fournier, H., Heitmann, Catherine N., Man, F., Mornet, J., Pacheco, A., Pai, Herve, Trinquet, J. Y., Vinet, N., Arnaud, M., Barsuglia, M. A., Bizouard, V., Brisson, F., Cavalier, M., Davier, P., Hello, P., Heusse, S., Kreckelberg, A., Claude Boccara, Vincent, Loriette, J., Moreau, V., Reita, P., Amico, L., Bosi, Luca, Gammaitoni, M., Punturo, F., Travasso, H., Vocca, L., Barsotti, S., Braccini, C., Bradaschia, G., Cella, C., Corda, A., Di Virgilio, I., Ferrante, F., Fidecaro, Adalberto, Giazotto, E., Majorana, L., Holloway, R., Passaquieti, D., Passuello, R., Poggiani, A., Toncelli, M., Tonelli, L., Brocco, S., Frasca, C., Palomba, P., Puppo, P., Rapagnani, F., Ricci, David, Rimmer, Philip J., Roger, Norbert, Kaiser, Peter N. J., Denni, Lingli, Wang, H., Angus Macleod, Rolf, Wartmann, Amra, Claude, Beauville, F., Buskulic, D., Flaminio, R., Marion, F., Masserot, A., Massonnet, L., Mours, B., Moreau, F., Ramonet, J., Tournefier, E., Verkindt, D., Veziant, O., Yvert, M., Barillé, R., Dattilo, V., Enard, D., Frasconi, F., Gennai, A., la Penna, P., Loupias, M., Paoletti, F., Bracci, L., Calamai, G., Campagna, E., Conforto, MARIA LETIZIA, Cuoco, E., Fiori, I., Guidi, G., Losurdo, G., Martelli, F., Mazzoni, M., Perniola, B., Stanga, R., Vetrano, F., Viceré, A., Babusci, D., Giordano, G., Mackowski, J. -M., Morgado, N., Pinard, L., Remillieux, A., Acernese, F., Barone, F., Calloni, E., de Rosa, R., di Fiore, L., Eleuteri, A., Milano, L., Qipiani, K., Ricciardi, I., Russo, G., Solimeno, S., Varvella, M., Bondu, F., Brillet, A., Chassande-Mottin, E., Cleva, F., Cokelaer, T., Coulon, J. -P., Dujardin, B., Fournier, J. -D., Heitmann, H., Man, C. N., Mornet, F., Pacheco, J., Pai, A., Trinquet, H., Vinet, J. -Y., Arnaud, N., Barsuglia, M., Bizouard, M. A., Brisson, V., Cavalier, F., Davier, M., Hello, P., Heusse, P., Kreckelberg, S., Boccara, C., Loriette, V., Moreau, J., Reita, V., Amico, P., Bosi, L., Gammaitoni, L., Punturo, M., Travasso, F., Vocca, H., Barsotti, L., Braccini, S., Bradaschia, C., Celia, G., Corda, C., di Virgilio, A., Ferrante, I., Fidecaro, F., Giazotto, A., Majorana, E., Holloway, L., Passaquieti, R., Passuello, D., Poggiani, R., Toncelli, A., Tonelli, M., Brocco, L., Frasca, S., Palomba, C., Puppo, P., Rapagnani, P., Ricci, F., Beauville, F, Buskulic, D, Flaminio, R, Marion, F, Masserot, A, Massonnet, L, Mours, B, Moreau, F, Ramonet, J, Tournefier, E, Verkindt, D, Veziant, O, Yvert, M, Barille, R, Dattilo, V, Enard, D, Frasconi, F, Gennai, A, La Penna, P, Loupias, M, Paoletti, F, Bracci, L, Calamai, G, Campagna, E, Conforto, G, Cuoco, E, Fiori, I, Guidi, G, Losurdo, G, Martelli, F, Mazzoni, M, Perniola, B, Stanga, R, Vetrano, F, Vicere, A, Babusci, D, Giordano, G, Mackowski, Jm, Morgado, N, Pinard, L, Remillieux, A, Acernese, F, Barone, F, Di Fiore, L, Eleuteri, A, Milano, L, Qipiani, K, Ricciardi, I, Solimeno, S, Varvella, M, Bondu, F, Brillet, A, Chassande Mottin, E, Cleva, F, Cokelaer, T, Coulon, Jp, Dujardin, B, Fournier, Jd, Heitmann, H, Man, Cn, Mornet, F, Pacheco, J, Pai, A, Trinquet, H, Vinet, Jy, Arnaud, N, Barsuglia, M, Bizouard, Ma, Brisson, V, Cavalier, F, Davier, M, Hello, P, Heusse, P, Kreckelberg, S, Boccara, C, Loriette, V, Moreau, J, Reita, V, Amico, P, Bosi, L, Gammaitoni, L, Punturo, M, Travasso, F, Vocca, H, Barsotti, L, Braccini, S, Bradaschia, C, Cella, G, Corda, C, Di Virgilio, A, Ferrante, I, Fidecaro, F, Giazotto, A, Majorana, E, Holloway, L, Passaquieti, R, Passuello, D, Poggiani, R, Toncelli, A, Tonelli, M, Brocco, L, Frasca, S, Palomba, C, Puppo, P, and Rapagnani, P

Subjects
Wavefront, Physics, Scattering, business.industry, Electronic, Optical and Magnetic Material, Virgo interferometer, Computer Science Applications1707 Computer Vision and Pattern Recognition, Condensed Matter Physic, Sputter deposition, optics, Applied Mathematic, Interferometry, Optics, Optical coating, Astronomical interferometer, Optical system design, Electrical and Electronic Engineering, business, Absorption (electromagnetic radiation)
Abstract

The goal of the VIRGO program is to build a giant Michelson type interferometer (3 kilometer long arms) to detect gravitational waves. Large optical components (350 mm in diameter), having extremely low loss at 1064 nm, are needed. Today, the Ion beam Sputtering is the only deposition technique able to produce optical components with such performances. Consequently, a large ion beam sputtering deposition system was built to coat large optics up to 700 mm in diameter. The performances of this coater are described in term of layer uniformity on large scale and optical losses (absorption and scattering characterization). The VIRGO interferometer needs six main mirrors. The first set was ready in June 2002 and its installation is in progress on the VIRGO site (Italy). The optical performances of this first set are discussed. The requirements at 1064 nm are all satisfied. Indeed, the absorption level is close to 1 ppm (part per million), the scattering is lower than 5 ppm and the R.M.S. wavefront of these optics is lower than 8 nm on 150 mm in diameter. Finally, some solutions are proposed to further improve these performances, especially the absorption level (lower than 0.1 ppm) and the mechanical quality factor Q of the mirrors (thermal noise reduction).

Published
2004

5. Growing Up - The Completion of the VLTI

Author

M. Tarenghi, Alberto Gennai, Frederic Derie, Nico Housen, Sebastien Morel, Pierre Kervella, Andrea Richichi, Anders Wallander, Andreas Glindemann, Francesco Paresce, Than Phan Duc, Francoise Delplancke, Bertrand Bauvir, Serge Menardi, Rainer Wilhelm, Bertrand Koehler, Samuel Lévêque, Serge Correia, Philippe B. Gitton, Markus Wittkowski, Markus Schöller, Alexis Huxley, Roy van Boekel, and Emmanuel di Folco

Subjects
Point spread function, Optical fiber, business.industry, Computer science, Tracking (particle physics), law.invention, Interferometry, Optics, law, Astronomical interferometer, Integrated optics, Instrumentation (computer programming), Guide star, business
Abstract

The completed VLTI with eight Delay Lines and eight ATs forms the basis for the second generation instrumentation. We describe the events up to first fringes with the test instrument VINCI using the siderostats, and the planning for the immediate future. Multi beam combination for ‘smoother images’ will be briefly discussed as well as artificial guide stars for fringe tracking. New technological developments like fiber optics amplifiers and integrated optics in combination with STJ open the door for a new type of interferometric arrays. Baselines as long as a a few kilometres come into reach. Examples of these second generation interferometers will be given.

Published
2006
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6. The VLTI — A Status Report

Author

Samuel Lévêque, Frederic Derie, Serge Menardi, Rainer Wilhelm, Pascal Ballester, Andrea Richichi, Mario Kiekebusch, Sebastien Morel, Francisco Delgado, Andreas Glindemann, Paul Giordano, Philippe Duhoux, Than Phan Duc, Emmanuel di Folco, Markus Schoeller, Alberto Gennai, Nico Housen, M. Tarenghi, Rodrigo Amestica, Francesco Paresce, Antonio Longinotti, Markus Wittkowski, Bruno Gilli, Pierre Kervella, Bertrand Koehler, Philippe B. Gitton, Stephane Guisard, Serge Correia, E. Bugueño, Alexis Huxley, Francoise Delplancke, Anders Wallander, J. Algomedo, and Bertrand Bauvir

Subjects
Physics, Very Large Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrometry, First light, Status report, Interferometry, Observatory, Astronomical interferometer, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Geology
Abstract

The Very Large Telescope (VLT) Observatory on Cerro Paranal (2635 m) in Northern Chile is approaching completion. After the four 8-m Unit Telescopes (UT) individually saw first light in the last years, two of them were combined for the first time on October 30, 2001 to form a stellar interferometer, the VLT Interferometer. The remaining two UTs will be integrated into the interferometric array later this year. In this article, we will describe the subsystems of the VLTI and the planning for the following years.

Published
2003
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7. Status of VLTI control system: how to make an optical interferometer a data producing facility

Author

Bruno Gilli, Anders Wallander, Bertrand Bauvir, Pascal Ballester, Philippe Duhoux, Antonio Longinotti, Nico Housen, Than Phan Duc, Mauro Comin, Mario Kiekebush, Javier Argomedo, Rob Donaldson, Robert Karban, Ivan M. Munoz, Alberto Gennai, and Alexis Huxley

Subjects
Physics, Operability, Real-time computing, Bandwidth (signal processing), Astrophysics::Instrumentation and Methods for Astrophysics, law.invention, Data flow diagram, Telescope, Interferometry, law, Observatory, Control system, Astronomical interferometer, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Remote sensing
Abstract

After having established routine science operations for four 8 m single dish telescopes and their first set of instruments at the Paranal Observatory, the next big engineering challenge for ESO has been the VLT Interferometer. Following an intense integration period at Paranal, first fringes were obtained in the course of last year, first with two smaller test siderostats and later with two 8 m VLT telescopes. Even though optical interferometry today may be considered more experimental than single telescope astronomy, we have aimed at developing a system with the same requirements on reliability and operability as for a single VLT telescope. The VLTI control system is responsible for controlling and co-ordinating all devices making up VLTI, where a telescope is just one out of many subsystems. Thus the pure size of the complete system increases the complexity and likelihood of failure. Secondly, some of the new subsystems introduced, in particular the delay lines and the associated fringe-tracking loop, have more demanding requirements in terms of control loop bandwidth, computing power and communication. We have developed an innovative generic multiprocessor controller within the VLT framework to address these requirements. Finally, we have decided to use the VLT science operation model, whereby the observation is driven by observation blocks with minimum human real-time interaction, which implies that VLTI is seen as one machine and not as a set of telescopes and other subsystems by the astronomical instrument. In this paper we describe the as-built architecture of the VLTI control and data flow system, emphasising how new techniques have been incorporated, while at the same time the investments in technology and know-how obtained during the VLT years have been protected. The result has been a faster development cycle, a robustness approaching that of VLT single dish telescopes and a "look and feel" identical to all other ESO observing facilities. We present operation, performance and development cost data to confirm this. Finally we discuss the plans for the coming years, when more and more subsystems will be added in order to explore the full potential of the VLTI.

Published
2002
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8. Commissioning the VLT interferometer: from first fringes toward a general user facility

Author

Sebastien Morel, Roy van Boekel, Antonio Longinotti, Emmanuel di Folco, Pascal Ballester, Serge Menardi, Arno van Kesteren, Anders Wallander, Walter Jaffe, Andrea Richichi, Philippe Duhoux, Toomas Erm, Gerhard Huedepohl, Markus Schoeller, Bertrand Bauvir, M. Tarenghi, A. Rijo, Andres Pino, Stefan Sandrock, Rainer Wilhelm, Alexis Huxley, Jason Spyromilio, S. Jackisch, Alberto Gennai, Andreas Glindemann, Samuel Lévêque, Sylvie Robbe-Dubois, Francesco Paresce, Damien Ségransan, Isabelle Percheron, Francoise Delplancke, D. Rabeling, Mario Kiekebusch, Serge Correia, Roberto Tamai, Cyrus Sabet, T. Phan Duc, Vincent Coudé du Foresto, Frederic Derie, Bertrand Koehler, Javier Argomedo, Philippe B. Gitton, Lothar Noethe, Paul Giordano, Michael Cantzler, Stephane Guisard, Nico Housen, Pablo Gutierrez, A. Ramirez, W. D. Cotton, Bruno Gilli, Pierre Kervella, Markus Wittkowski, 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), Pôle Astronomie du LESIA, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
Physics, Interferometry, Sky, Project commissioning, media_common.quotation_subject, Astronomical interferometer, User Facility, Baseline (configuration management), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], media_common, Remote sensing
Abstract

On March 17, 2001, the VLT interferometer saw for the first time interferometric fringes on sky with its two test siderostats on a 16m baseline. Seven months later, on October 29, 2001, fringes were found with two of the four 8.2m Unit Telescopes (UTs), named Antu and Melipal, spanning a baseline of 102m. First shared risk science operations with VLTI will start in October 2002. The time between these milestones is used for further integration as well as for commissioning of the interferometer with the goal to understand all its characteristics and to optimize performance and observing procedures. In this article we will describe the various commissioning tasks carried out and present some results of our work.

Published
2002

9. The VLTI and Its Subsystems

Author

Glindemann, A., Algomedo, J., Amestica, R., Ballester, P., Bauvir, B., Bugueño, E., Correia, S., Delgado, F., Delplancke, F., Derie, F., Duhoux, Ph, Di Folco, E., Alberto Gennai, Gilli, B., Giordano, P., Gitton, Ph, Guisard, S., Housen, N., Huxley, A., Kervella, P., Kiekebusch, M., Koehler, B., Lévêque, S., Longinotti, A., Ménardi, S., Morel, S., Paresce, F., Phan Duc, T., Richichi, A., Schöller, M., Tarenghi, M., Wallander, A., Wittkowski, M., Wilhelm, R., 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), Pôle Astronomie du LESIA, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

Published
2002

10. FINITO: A Fringe Sensor for VLTI in Two and Three Beam Configuration

Author

Daniele Gardiol, Giuseppe Massone, Davide Loreggia, Leonardo Corcione, Mario G. Lattanzi, Alberto Gennai, Serge Menardi, D. Bonino, and Mario Gai

Subjects
Physics, Time delay and integration, Very Large Telescope, business.industry, law.invention, Telescope, Interferometry, Optics, Observatory, law, Closure phase, Astronomical interferometer, business, Optical path length, Remote sensing
Abstract

ESO and the Astronomical Observatory of Torino (OATo) are collaborating for development of a Fringe Sensor Unit (FSU) for the Very Large Telescope Interferometer (VLTI, see [1] and references therein): FINITO (Fringe-tracking Instrument of Nice and Torino), derived from the concept demonstrated by a prototype from the Observatoire de la Cote d’Azur. It will be used for stabilisation of the Optical Path Difference (OPD) between telescope beams for the first generation scientific interferometers (AMBER, MIDI, VINCI), providing an improvement of up to five magnitudes in limiting sensitivity, thanks to the integration time increased from a few ten milliseconds up to minutes. Accordingly to current planning, FINITO is the only FSU able to support three-beam observations, allowing closure phase measurements in the near and mid IR range.

Published
2002
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11. The VLT Interferometer: a unique instrument for high-resolution astronomy

Author

Samuel Lévêque, Alain Michel, Francesco Paresce, Bertrand Koehler, Philippe B. Gitton, Roberto Abuter, Pierre Kervella, Francoise Delplancke, Frederic Derie, M. Tarenghi, Franco Carbognani, Andrea Richichi, Rainer Wilhelm, Markus Schoeller, Andreas Glindemann, Anders Wallander, Than Phan Duc, Alberto Gennai, and Serge Menardi

Subjects
Physics, Very Large Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, High resolution, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrometry, First light, Interferometry, Observatory, Astronomical interferometer, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Adaptive optics, Astrophysics::Galaxy Astrophysics
Abstract

The Very Large Telescope (VLT) Observatory on Cerro Paranal (2635 m) in Northern Chile is approaching completion in this year when the fourth of the 8-m Unit Telescopes will see first light. At the same time, the preparation for first fringes of the VLT Interferometer (VLTI) is advancing rapidly with the goal of having the first fringes with two siderostats within this year. In this article we describe the status of the VLTI and its subsystems, we discuss the planning for first fringes with the different telescopes and instruments. Eventually, we present an outlook for the future of interferometry with Very Large Telescopes.

Published
2000
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12. The VLTI and its Subsystems

Author

Markus Schöller, Bruno Gilli, Pierre Kervella, Francisco Delgado, Rainer Wilhelm, Markus Wittkowski, Paul Giordano, Bertrand Koehler, Serge Menardi, Andrea Richichi, Stephane Guisard, T. Phan Duc, Andreas Glindemann, Sebastien Morel, Serge Correia, Frederic Derie, Antonio Longinotti, Mario Kiekebusch, Nico Housen, S. Cabanero, Francoise Delplancke, Alexis Huxley, Ph. Gitton, P. Duhoux, Anders Wallander, J. Algomedo, Bertrand Bauvir, Pascal Ballester, Samuel Lévêque, Francesco Paresce, E. Di Folco, M. Tarenghi, Alberto Gennai, E. Bugueño, and Rodrigo Amestica

Subjects
Physics, Interferometry, Very Large Telescope, Space and Planetary Science, Observatory, General Engineering, Astronomy and Astrophysics, First light, Astrophysics
Abstract

The Very Large Telescope (VLT) Observatory on Cerro Paranal (2635 m) in Northern Chile is approaching completion. After the four 8-m Unit Telescopes (UT) individually saw first light in the last years, two of them were combined for the first time on October 30, 2001 to form a stellar interferometer, the VLT Interferometer. The remaining two UTs will be integrated into the interferometric array later this year, so that any two UTs can be used for interferometry. In this article, we will describe the subsystems of the VLTI and the planning for the following years.

Published
2003
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