Relevant bibliographies by topics / Very Large Telescope Interferometer

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers

Academic literature on the topic 'Very Large Telescope Interferometer'

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Published: 4 June 2021
Last updated: 8 February 2022

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Journal articles on the topic "Very Large Telescope Interferometer"

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Schöller, M. "The Very Large Telescope Interferometer." EAS Publications Series 28 (2008): 1–8. http://dx.doi.org/10.1051/eas:0828001.

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Lévêque, Samuel, Bertrand Koehler, and Oskar von der Lühe. "Longitudinal dispersion compensation for the Very Large Telescope Interferometer." Astrophysics and Space Science 239, no. 2 (September 1996): 305–14. http://dx.doi.org/10.1007/bf00645784.

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Schöller, Markus. "The Very Large Telescope Interferometer: Current facility and prospects." New Astronomy Reviews 51, no. 8-9 (October 2007): 628–38. http://dx.doi.org/10.1016/j.newar.2007.06.008.

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Bedding, T. R., J. M. Beckers, M. Faucherre, N. Hubin, B. Koehler, O. von der Lühe, F. Merkle, and N. Zhu. "The VLT Interferometer." Symposium - International Astronomical Union 158 (1994): 143–50. http://dx.doi.org/10.1017/s0074180900107454.

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One of the observing modes available with the ESO Very Large Telescope will be coherent combination of the light received by up to four 8 m unit telescopes and several 1.8 m 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 (u, v) coverage of the unit telescopes as well as to function as an independent interferometric array.The 8 m telescopes will be equipped with adaptive optics to correct for seeing-induced wavefront aberrations. This wavefront correction will be complete at near-infrared wavelengths, giving the interferometer very high sensitivity in this spectral regime. This paper gives a brief description of the VLT Interferometer and an update on its status.
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Woillez, J., J. A. Abad, R. Abuter, E. Aller Carpentier, J. Alonso, L. Andolfato, P. Barriga, et al. "NAOMI: the adaptive optics system of the Auxiliary Telescopes of the VLTI." Astronomy & Astrophysics 629 (September 2019): A41. http://dx.doi.org/10.1051/0004-6361/201935890.

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Context. 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. Aims. 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. Methods. We deployed a new adaptive optics module for interferometry (NAOMI) on the Auxiliary Telescopes. Results. We present its design, performance, and effect on the observations that are carried out with the interferometric instruments.
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Richichi, A. "The VLT Interferometer." Proceedings of the International Astronomical Union 3, S248 (October 2007): 44–47. http://dx.doi.org/10.1017/s1743921308018607.

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AbstractThe ESO Very Large Telescope Interferometer (VLTI) is arguably the most powerful optical interferometric facility available at present. In addition to the wide choice of baselines and the light collecting power of its 8.2 m and 1.8 m telescopes, the VLTI also offers a smooth and user-friendly operation which makes interferometry accessible to any astronomer and covers a wide range of scientific applications. Behind the routine scientific operations, however, the VLTI is in constant evolution. I will present some of the technological and instrumental improvements which are planned for the near and mid-term future, and discuss their implications for astrometry in particular. Among them, the PRIMA facility and the proposed GRAVITY instrument are designed to reach the level of 10 microarcseconds in the near-infrared.
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Abuter, R., M. Accardo, A. Amorim, N. Anugu, G. Ávila, N. Azouaoui, M. Benisty, et al. "First light for GRAVITY: Phase referencing optical interferometry for the Very Large Telescope Interferometer." Astronomy & Astrophysics 602 (June 2017): A94. http://dx.doi.org/10.1051/0004-6361/201730838.

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GRAVITY is a new instrument to coherently combine the light of the European Southern Observatory Very Large Telescope Interferometer to form a telescope with an equivalent 130 m diameter angular resolution and a collecting area of 200 m2. The instrument comprises fiber fed integrated optics beam combination, high resolution spectroscopy, built-in beam analysis and control, near-infrared wavefront sensing, phase-tracking, dual-beam operation, and laser metrology. GRAVITY opens up to optical/infrared interferometry the techniques of phase referenced imaging and narrow angle astrometry, in many aspects following the concepts of radio interferometry. This article gives an overview of GRAVITY and reports on the performance and the first astronomical observations during commissioning in 2015/16. We demonstrate phase-tracking on stars as faint as mK ≈ 10 mag, phase-referenced interferometry of objects fainter than mK ≈ 15 mag with a limiting magnitude of mK ≈ 17 mag, minute long coherent integrations, a visibility accuracy of better than 0.25%, and spectro-differential phase and closure phase accuracy better than 0.5°, corresponding to a differential astrometric precision of better than ten microarcseconds (μas). The dual-beam astrometry, measuring the phase difference of two objects with laser metrology, is still under commissioning. First observations show residuals as low as 50 μas when following objects over several months. We illustrate the instrument performance with the observations of archetypical objects for the different instrument modes. Examples include the Galactic center supermassive black hole and its fast orbiting star S2 for phase referenced dual-beam observations and infrared wavefront sensing, the high mass X-ray binary BP Cru and the active galactic nucleus of PDS 456 for a few μas spectro-differential astrometry, the T Tauri star S CrA for a spectro-differential visibility analysis, ξ Tel and 24 Cap for high accuracy visibility observations, and η Car for interferometric imaging with GRAVITY.
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Kol'tso, N. E., S. A. Grenkov, and L. V. Fedotov. "Comparison of Radio Interferometers with Analog and Digital Extraction of Recorded Signal." Journal of the Russian Universities. Radioelectronics 23, no. 2 (April 28, 2020): 6–18. http://dx.doi.org/10.32603/1993-8985-2020-23-2-6-18.

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Introduction. Radio telescopes of Very Long Baseline Interferometry (VLBI) networks usually record several signals with relatively narrow (up to 32 MHz) bands, which are extracted by means of base band converters (BBC) from an analog noise signal of an intermediate frequency (IF) with bands up to 1 GHz. When processing data, frequency band synthesis is used. At new small radio telescopes (for example, RT-13), directly wideband IF signals are digitized. An ability to connect the RT-13 radio telescope to the “Quasar” VLBI complex and to international VLBI networks provides by a digital narrow-band signal extraction module developed in 2019.Aim. Determining the measuring accuracy of an interferometric group delay of a signal by a radio interferometer with a digital narrow-band signal extraction module and comparing the sensitivity of interferometers with analog and digital signal extraction systems.Materials and methods. Sensitivity losses of interferometers with different systems for detecting recorded signals were calculated. The accuracy of a multi-channel interferometer with the synthesis of a frequency band and of an interferometer with recording of digital broadband IF signals without band synthesis was compared. The results were confirmed by VLBI observations in the observatories of the “Quasar” complex.Results. When replacing the analog system of signal extraction with digital system the sensitivity losses of the interferometer were slightly reduced. The measurement accuracy of the interferometric group delay had not changed. Accuracy increased when digitally recording broadband IF signals and when synthesizing a frequency band significantly larger than the IF bandwidth. Conditions and minimum synthesized bands were determined under which the accuracy of the interferometer with the registration of narrowband signals can be higher than the accuracy of the interferometer with the registration of wideband IF signals.Conclusion. The problem of combining RT-13 radio telescopes with VLBI networks with recording of video frequency signals was solved. The efficiency of the installation of digital signal conversion systems at radio telescopes was shown.
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Merkle, Fritz. "Interferometry with the European Very Large Telescope." Optics News 14, no. 3 (March 1, 1988): 15. http://dx.doi.org/10.1364/on.14.3.000015.

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Stee, Ph, A. Meilland, and O. L. Creevey. "Interferometry of massive stars: the next step." Proceedings of the International Astronomical Union 9, S307 (June 2014): 480–89. http://dx.doi.org/10.1017/s174392131400742x.

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AbstractWe present some new and interesting results on the complementarity between asteroseismology and interferometry, the detection of non-radial pulsations in massive stars and the possibility for evidencing differential rotation on the surface of Bn stars. We also discuss the curretn interferometric facilities, namely the Very Large Telescope Interferometer (VLTI)/AMBER, VLTI/MIDI, VLTI/PIONIER within the European Southern Observatory (ESO) context and the Center for High Angular Resolution Astronomy (CHARA) array with their current limitations. The forthcoming second-generation VLTI instruments GRAVITY and MATISSE are presented as well as the FRIEND prototype in the visible spectral domain and an update of the Navy Precision Optical Interferometer (NPOI). A conclusion is presented with a special emphasis on the foreseen difficulties for a third generation of interferometric instruments within the (budget limited) Extremely Large Telescope framework and the need for strong science cases to push a future visible beam combiner.
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Dissertations / Theses on the topic "Very Large Telescope Interferometer"

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Correia, Serge. "Haute résolution angulaire et interférométrie optique en astrophysique : applications au Large Binocular Telescope et au Very Large Telescope Interferometer." Nice, 2002. http://www.theses.fr/2002NICE5796.

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Schuhler, Nicolas Meyrueis Patrick. "Frequency-comb stabilized laser sources for absolute distance metrology at the very large telescope interferometer." Strasbourg : Université Louis Pasteur, 2007. http://eprints-scd-ulp.u-strasbg.fr:8080/684/01/Schuhler2006.pdf.

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Schuhler, Nicolas. "Frequency-comb stabilized laser sources for absolute distance metrology at the very large telescope interferometer." Université Louis Pasteur (Strasbourg) (1971-2008), 2006. https://publication-theses.unistra.fr/public/theses_doctorat/2006/SCHUHLER_Nicolas_2006.pdf.

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PRIMA, un futur instrument du VLTI, utilise un système de métrologie laser pour mesurer les variations de chemin optique internes à l’interféromètre. L’étude présentée dans ce mémoire porte sur le développement, l’intégration et le test de sources lasers stabilisées en fréquence pour ce système de métrologie. Dans une première partie, nous présentons le cahier des charges du système dans le contexte de PRIMA et du VLTI. Nous rappelons les bases de l’interférométrie laser et les problèmes qu’impose son application à PRIMA. Nous en déduisons la nécessité de stabiliser la longueur d’onde du laser sur une référence absolue et exposons l’intérêt de transformer ce système en un système de mesure de distances absolues. Dans une seconde partie, nous décrivons notre contribution à la stabilisation en fréquence d’un laser Nd:YAG sur une raie d’absorption de l’iode. Nous mesurons précisément les performances du système avec un peigne de fréquences optiques auto-référencé. Nous améliorons le système pour satisfaire aux exigences du cahier des charges. La troisième partie est consacrée à la transformation du système en un système de mesure de distances absolues par l’utilisation de l’interférométrie à deux longueurs d’onde. Nous proposons un nouveau concept de source laser qui utilise un peigne de fréquences optiques comme référence de fréquence. Cette source permet de générer un choix sans précédent de longueurs d’onde synthétiques avec une précision relative dans le vide meilleure que 10−11. Nous validons le concept sur un prototype et montrons qu’il peut être utilisé en interférométrie à deux longueurs d’onde pour résoudre une longueur d’onde optique
The forthcoming instrument of the Very Large Telescope Interferometer (VLTI), called Phase-Referenced Imaging and Micro-arcsecond Astrometry facility (PRIMA), uses a laser metrology system to monitor the variations of internal path lengths. This dissertation addresses the development, integration and test of frequency stabilized laser sources for the PRIMA Metrology system (PRIMET). In the first part, we present in the context of PRIMA and the VLTI the specifications of PRIMET. We recall the basics of single-wavelength laser interferometry and introduce the problems raised by its application to PRIMET. We present the need for the absolute frequency stabilization of PRIMET laser and the interest for an upgrade of PRIMET towards absolute distance measurements. In the second part, we present our contribution to the absolute frequency stabilization of PRIMET Nd:YAG laser on a transition of iodine. We characterize the system and measure precisely its performance with a self-referenced optical frequency comb. We improve the system to reach the specifications in terms of accuracy and stability of the locking frequency. The third part addresses the upgrade of PRIMET towards absolute distance measurements by the use of two-wavelength interferometry. We propose a new concept of two-wavelength laser source frequency stabilized on an optical frequency comb. This permits the generation of an unprecedented large choice of synthetic wavelength with a relative accuracy better than 10−11 in vacuum. We validate the concept on a prototype and shows that it can be used to resolve an optical wavelength. Finally, we propose to apply this concept to the upgrade of PRIMET
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Ferrari, Marc. "Optique active et grandes déformations élastiques : application à la réalisation d'un miroir à focale variable pour le Very Large Telescope Interferometer." Aix-Marseille 1, 1994. http://www.theses.fr/1994AIX11017.

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Une etude theorique des grandes deformations elastiques, c'est-a-dire dont l'amplitude est superieure a l'epaisseur de la piece deformee, a ete entreprise dans le cadre de l'optique active afin d'accroitre les possibilites d'utilisation de cette technique. Cette etude prend en compte les deformations de la surface mediane d'un miroir soumis a une charge ou une force centrale, ainsi que les contraintes associees. La resolution numerique des equations d'equilibre d'un tel miroir nous a notamment permis de determiner la limite de validite de la theorie des faibles deformations. Un code de calcul specifique a ete elabore afin de calculer la distribution d'epaisseur d'un miroir permettant d'engendrer une deformation particuliere. Les profils necessaires a l'obtention d'une flexion purement parabolique ont ainsi ete determines dans deux cas de charges exterieures. De tels miroirs a courbure fortement variable, pouvant passer de la forme plane a des rapports d'ouverture de l'ordre de f/2, sont le seul moyen pratique de compenser le champ des futurs interferometres geants tels que le very large telescope interferometer. Ils constituent le cur meme des lignes a retard a il de chat, leur rayon de courbure variant continument pendant le deplacement du systeme. Du fait de la grande flexibilite demandee, les alliages metalliques a la fois tres lineaires et de haute limite elastique sont les seuls materiaux utilisables. La realisation de ces miroirs a courbure variable en acier inoxydable est abordee en detail, ainsi que les resultats des premiers tests de qualification d'un prototype. La comparaison entre la phase experimentale et les predictions theoriques nous permet ainsi de valider le modele numerique utilise
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Muthusubramanian, Balaji [Verfasser], and Lucas [Gutachter] Labadie. "Simulations of group-delay tracking strategies in the astronomical K and L bands. For improved sensitivities at the Very Large Telescope Interferometer / Balaji Muthusubramanian ; Gutachter: Lucas Labadie." Köln : Universitäts- und Stadtbibliothek Köln, 2018. http://d-nb.info/1185067140/34.

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Lange, Werner R., and Martin Ravensbergen. "TIME REFERENCE SYSTEM OF THE ESO VERY LARGE TELESCOPE." International Foundation for Telemetering, 1995. http://hdl.handle.net/10150/608540.

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International Telemetering Conference Proceedings / October 30-November 02, 1995 / Riviera Hotel, Las Vegas, Nevada
The necessity of supplying precise time information in large telemetry ground stations and astronomical observatories is very similar. Therefore the way of solving this problem as it is done in the Very Large Telescope of the European Southern Observatory can be easily adopted to telemetry stations and ranges, especially when fiber optics are used. The European Southern Observatory (ESO) is building a new observatory in Chile for the Very Large Telescope (VLT). This VLT consists of 4 telescopes, each of them has a primary mirror diameter of 8 meters. the control architecture is based on workstations and VMEbus computers. The VMEbus computers are distributed over the whole building and are using real time operating system. Since the availability of the Global Positioning System (GPS) the generation of highly accurate timing signals on remote locations without the use of expensive Cesium standards does not create problems any more. However, distribution of a timing signal to many computer with high accuracy is an issue. The accuracy of the commonly used IRIG B-code is not adequate if the requirements are in the 10 microseconds range. This paper presents the design of a timing system that is adopted to the VLT. An overview of the requirements of the Time Reference System (TRS) is given. These requirements have been defined on the basis of experiences with the timing system of the ESO NTT telescope. The hardware units are described. These are a Central Time Standard, a Time Distribution System and a VME Time Interface Module. The distribution is based on fiber optic transmission, using a simple digital modulation that outperforms the analog IRIG B modulation. The Time Interface Module in the computer does not only perform the timing signal decoding but contains also user-programmable timers that are synchronously clocked from the time source. Presently all units of the TRS have been tested and the series production of the distribution and the Time Interface Modules are in progress.
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Kervella, Pierre. "Interférométrie optique avec le Very Large Telescope - Application aux étoiles Céphéides." Phd thesis, Université Paris-Diderot - Paris VII, 2001. http://tel.archives-ouvertes.fr/tel-00258928.

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Installé au cœur de l'interféromètre du Very Large Telescope (le VLTI, situé au sommet du Mont Paranal, dans le nord du Chili), l'instrument VINCI permet de recombiner la lumière infrarouge de deux télescopes séparés de manière cohérente. Il ouvre ainsi un accès vers la très haute résolution angulaire (quelques millisecondes d'angle), et des programmes de recherche novateurs dans des domaines aussi divers que la physique stellaire, les disques protoplanétaires ou bien encore l'étude des exoplanètes. Mon travail de thèse sur l'instrument VINCI a porté sur sa conception, en particulier la définition fonctionnelle de son logiciel d'exploitation, son installation au sommet du Mont Paranal et ses premières observations scientifiques. Le principe de fonctionnement et les performances de cet instrument sont décrits dans la première partie de ce document.
Dans une seconde partie, j'aborde l'étude des étoiles variables Céphéides par interférométrie. Ces étoiles pulsantes jouent un rôle primordial dans l'estimation des distances astronomiques depuis qu'il a été établi que leur période de variation était liée à leur luminosité intrinsèque par la célèbre relation période-luminosité. Leur observation photométrique permet donc de calculer directement leur distance. Toutefois, notre connaissance du point zéro de cette relation est encore imparfaite, car elle repose sur la mesure des distances aux Céphéides galactiques les plus proches, encore mal connues. La très haute résolution angulaire apportée par l'instrument VINCI et le VLTI permettra bientôt l'étude fine de la pulsation de ces étoiles. Par la mesure simultanée de la vitesse radiale de pulsation et de la variation du diamètre angulaire de l'étoile, il sera possible de calculer directement la distance aux Céphéides les plus proches, et donc d'étalonner la relation période-luminosité. L'enjeu de ce programme : la calibration de cette relation avec une précision de 0,01 magnitude, soit un gain d'un facteur dix par rapport à notre connaissance actuelle.
Au-delà de ce programme fondamental, je décris également les possibilités offertes par VINCI dans le domaine de l'étude des étoiles naines de la séquence principale, notamment de type solaire (avec application au couple d'étoiles Alpha Centauri A et B), et j'aborde brièvement l'étude des exoplanètes.
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Rabien, Sebastian. "Wirtsgalaxien von Quasaren und der Laserleitstern für das Very Large Telescope." Diss., lmu, 2005. http://nbn-resolving.de/urn:nbn:de:bvb:19-46209.

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Defrère, D., P. M. Hinz, B. Mennesson, W. F. Hoffmann, R. Millan-Gabet, A. J. Skemer, V. Bailey, et al. "NULLING DATA REDUCTION AND ON-SKY PERFORMANCE OF THE LARGE BINOCULAR TELESCOPE INTERFEROMETER." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621383.

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The Large Binocular Telescope Interferometer (LBTI) is a versatile instrument designed for high angular resolution and high-contrast infrared imaging (1.5-13 mu m). In this paper, we focus on the mid-infrared (8-13 mu m) nulling mode and present its theory of operation, data reduction, and on-sky performance as of the end of the commissioning phase in 2015 March. With an interferometric baseline of 14.4 m, the LBTI nuller is specifically tuned to resolve the habitable zone of nearby main-sequence stars, where warm exozodiacal dust emission peaks. Measuring the exozodi luminosity function of nearby main-sequence stars is a key milestone to prepare for future exo-Earth direct imaging instruments. Thanks to recent progress in wavefront control and phase stabilization, as well as in data reduction techniques, the LBTI demonstrated in 2015 February a calibrated null accuracy of 0.05% over a 3 hr long observing sequence on the bright nearby A3V star beta Leo. This is equivalent to an exozodiacal disk density of 15-30. zodi for a Sun-like star located at 10 pc, depending on the adopted disk model. This result sets a new record for high-contrast mid-infrared interferometric imaging and opens a new window on the study of planetary systems.
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Kim, Jihun. "Assembly of a large common mount astronomical interferometer." Thesis, The University of Arizona, 2013. http://pqdtopen.proquest.com/#viewpdf?dispub=3559991.

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A large multi-aperture telescope has the potential to reach the diffraction limit corresponding to its baseline. To do so, Adaptive Optics (AO) and beam combination are critical to good performance. Operation as an interferometer is a complicated mode for the telescope. The system now has much tighter tolerances and is difficult to align. The alignment process needs to be planned in multiple steps, and tolerance and sensitivity analysis needs to be performed for each step. Alignment tools can be prepared based on the resolution found in the sensitivity analysis in each step.

Random fluctuation is another critical factor that reduces system performance. If noise sources near the telescope are characterized and identified, image quality can be improved by post-image processing.

Measuring the outer scale of atmosphere is also helpful for understanding the system performance. The fringe tracking method in the Large Binocular Telescope Interferometer (LBTI) system provides optical path difference (OPD) variation, and the power spectral density of the OPD variation is used to estimate the size of the outer scale. However, this method is limited by the baseline of the LBTI by 5[special characters omitted] B, where B is the baseline, and by this equation the outer scale size which is able to be estimated should be more than 125 m.

AO simulation can provide an understanding of new AO system concepts and parameter variations before they are applied to the real system. In this dissertation study, we simulated an LBTI system with structural vibration of 10 Hz and 20 Hz and with various amplitudes. From the simulation, we learned that the slower bandwidth of piston-correcting systems allows stars as faint as ~13the magnitude to be observed. If there is significant vibration on the structure, the increased bandwidth will limit the phasing stars to 10~11th magnitudes. This demonstrates the limits of the LBTI system regarding structural vibration.

An alternative phasing sensor for the LBTI system, the pseudo phasing sensor, can be used for more than 1000 m of outer scale of atmosphere. If the direct phasing sensor embedded in the LBTI system cannot be used for a very faint star, the pseudo phasing sensor, which approximately estimates the phase difference by AO wavefront sensor, can be useful for atmospheric conditions with estimated outer scale of about 1000 m.

The analyses in this dissertation provide a partial guide for developing large-scale telescopes and astronomical instruments.

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Books on the topic "Very Large Telescope Interferometer"

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Garcia, Paulo J. V., Andreas Glindemann, Thomas Henning, and Fabien Malbet, eds. The Very Large Telescope Interferometer Challenges for the Future. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0.

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Joint European and National Astronomical Meeting (2002 Porto, Portugal). The very large telescope interferometer-challenges for the future: A JENAM 2002 Workshop, Porto, Portugal 3-5 September, 2002. Dordrecht: Kluwer Academic Publishers, 2003.

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ESO, Workshop (2005 Garching Germany). The power of optical/IR interferometry: Recent scientfic results and 2nd generation instrumentation : proceedings of the ESO Workshop held in Garching, Germany, 4-8 April 2005. Berlin: Springer, 2007.

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Andrea, Richichi, and European Southern Observatory, eds. The power of optical/IR interferometry: Recent scientfic results and 2nd generation instrumentation : proceedings of the ESO Workshop held in Garching, Germany, 4-8 April 2005. Berlin: Springer, 2007.

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S, D'Odorico, Swings J. -P, and European Southern Observatory, eds. Second Workshop on ESO's Very Large Telescope, Venice, 29 September-2 October 1986: Proceedings. Garching bei München, Federal Republic of Germany: European Southern Observatory, 1986.

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ESO Workshop (1994 Garching bei München, Germany). Science with the VLT: Poster paper supplement : an ESO workshop held 28 June - 1 July 1994, Garching bei München, Germany. [Garching bei Munchen, Germany: European Southern Observatory], 1995.

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Workshop on ESO's Very Large Telescope (2nd 1986 Venice, Italy). ESO's Very Large Telescope: Proceedings of the Workshop on ESO's Very Large Telescope held Sept. 29-Oct. 2, 1986 in Venice. Garching-bei-Munchen, Germany: European Southern Observatory, 1986.

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ESO, Workshop on High Resolution Spectroscopy with the VLT (1992 Garching bei München Germany). ESO Workshop on High Resolution Spectroscopy with the VLT: Garching, 11-13 February 1992 : proceedings. Garching bei München: European Southern Observatory, 1992.

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ESO/ST-ECF Workshop on Calibrating and Understanding HST and ESO Instruments (1995 Garching bei München, Germany). ESO/ST-ECF Workshop on Calibrating and Understanding HST and ESO Instruments: Garching, Germany, 25-28 April, 1995 : proceedings. Garching bei München, Germany: European Southern Observatory, 1995.

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Death stars, weird galaxies, and a quasar-spangled universe: The discoveries of the Very Large Array telescope. Albuquerque: University of New Mexico Press, 2006.

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Book chapters on the topic "Very Large Telescope Interferometer"

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Herbst, Tom. "Interferometry with the Large Binocular Telescope." In The Very Large Telescope Interferometer Challenges for the Future, 45–53. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_4.

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von der Lühe, Oskar. "An Introduction to Interferometry with the ESO Very Large Telescope." In Science with the VLT Interferometer, 13–34. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-540-69398-7_2.

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Quirrenbach, A. "Next Generation Instrumentation for the Very Large Telescope Interferometer." In The Very Large Telescope Interferometer Challenges for the Future, 277–89. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_32.

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Mouillet, David. "Interferometry Theory Primer." In The Very Large Telescope Interferometer Challenges for the Future, 3–15. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_1.

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Wilkin, F. P., and R. L. Akeson. "Palomar Testbed Interferometer Observations of Young Stellar Objects." In The Very Large Telescope Interferometer Challenges for the Future, 145–50. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_15.

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Schöller, Markus. "Optical Interferometry — A Practice Primer." In The Very Large Telescope Interferometer Challenges for the Future, 17–31. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_2.

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Delplancke, F., F. Derie, F. Paresce, A. Glindemann, F. Lévy, S. Lévêque, and S. Ménardi. "PRIMA for the VLTI — Science." In The Very Large Telescope Interferometer Challenges for the Future, 99–104. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_10.

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Percheron, Isabelle, Andrea Richichi, and Markus Wittkowski. "The VLTI Calibrators Program: Getting Ready for High Accuracy Measurements." In The Very Large Telescope Interferometer Challenges for the Future, 105–12. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_11.

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Pascucci, Ilaria, Thomas Henning, Jürgen Steinacker, and Sebastian Wolf. "2D/3D Dust Continuum Radiative Transfer Codes to Analyze and Predict VLTI Observations." In The Very Large Telescope Interferometer Challenges for the Future, 113–18. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_12.

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Meisner, J. A. "Scientific and Technical Results from VINCI Using Coherent Estimation of Fringe Visibility." In The Very Large Telescope Interferometer Challenges for the Future, 119–27. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_13.

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Conference papers on the topic "Very Large Telescope Interferometer"

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Haguenauer, Pierre, Roberto Abuter, Luigi Andolfato, Jaime Alonso, Guillaume Blanchard, Jean-Philippe Berger, Pierre Bourget, et al. "The Very Large Telescope Interferometer v2012+." In SPIE Astronomical Telescopes + Instrumentation, edited by Françoise Delplancke, Jayadev K. Rajagopal, and Fabien Malbet. SPIE, 2012. http://dx.doi.org/10.1117/12.925323.

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Haguenauer, Pierre, Jaime Alonso, Pierre Bourget, Stephane Brillant, Philippe Gitton, Stephane Guisard, Sébastien Poupar, et al. "The very large telescope Interferometer: 2010 edition." In SPIE Astronomical Telescopes + Instrumentation. SPIE, 2010. http://dx.doi.org/10.1117/12.857070.

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Haguenauer, Pierre, Roberto Abuter, Jaime Alonso, Javier Argomedo, Bertrand Bauvir, Guillaume Blanchard, Henri Bonnet, et al. "The Very Large Telescope Interferometer: an update." In SPIE Astronomical Telescopes + Instrumentation. SPIE, 2008. http://dx.doi.org/10.1117/12.788209.

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Schöller, Markus, Javier Argomedo, Bertrand Bauvir, Leonardo Blanco-Lopez, Henri Bonnet, Stephane Brillant, Michael Cantzler, et al. "Recent progress at the Very Large Telescope Interferometer." In SPIE Astronomical Telescopes + Instrumentation, edited by John D. Monnier, Markus Schöller, and William C. Danchi. SPIE, 2006. http://dx.doi.org/10.1117/12.672231.

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Ballester, Pascal, Alberto M. Chavan, Bill Cotton, Vincent Coude du Foresto, Andreas Glindemann, Carlos Guirao, Walter Jaffe, et al. "Data flow system for the very large telescope interferometer." In International Symposium on Optical Science and Technology, edited by Jean-Luc Starck and Fionn D. Murtagh. SPIE, 2001. http://dx.doi.org/10.1117/12.447178.

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Salvade, Yves, Alain Courteville, and Rene Daendliker. "Absolute metrology for the Very Large Telescope Interferometer (VLTI)." In Astronomical Telescopes and Instrumentation, edited by Pierre J. Lena and Andreas Quirrenbach. SPIE, 2000. http://dx.doi.org/10.1117/12.390235.

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Ferrari, Marc, Gerard R. Lemaitre, Silvio P. Mazzanti, Oskar von der Luehe, Bernard di Biagio, Pierre Montiel, Daniel Revest, Patrice Joulie, and Jean-Francois Carre. "Highly variable curvature mirrors for the Very Large Telescope Interferometer." In 1994 Symposium on Astronomical Telescopes & Instrumentation for the 21st Century, edited by Mark A. Ealey and Fritz Merkle. SPIE, 1994. http://dx.doi.org/10.1117/12.176116.

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Leveque, Samuel A., Bertrand Koehler, and Oskar von der Luehe. "Optical path difference model for the Very Large Telescope Interferometer." In Optical Telescopes of Today and Tomorrow, edited by Arne L. Ardeberg. SPIE, 1997. http://dx.doi.org/10.1117/12.269082.

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Beckers, Jacques M. "Interferometry with ESO's Very Large Telescope." In 15th Int'l Optics in Complex Sys. Garmisch, FRG, edited by F. Lanzl, H. J. Preuss, and G. Weigelt. SPIE, 1990. http://dx.doi.org/10.1117/12.34794.

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von der Luehe, Oskar, Frederic Derie, Didier Ferrand, Bertrand Koehler, Samuel A. Leveque, Francesco Paresce, and Luigi D'Arcio. "Interferometry with the ESO Very Large Telescope." In SPIE's 1995 International Symposium on Optical Science, Engineering, and Instrumentation, edited by Natalie Clark and John D. Gonglewski. SPIE, 1995. http://dx.doi.org/10.1117/12.217366.

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