Littérature scientifique sur le sujet « Interferometry »

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Articles de revues sur le sujet "Interferometry":

1

Chesneau, O., K. Rousselet-Perraut et F. Vakili. « Interferometry and Stellar Magnetism ». International Astronomical Union Colloquium 175 (2000) : 174–77. http://dx.doi.org/10.1017/s0252921100055792.

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AbstractThe classical detection of magnetic fields in Be stars remains a challenge due to the sensitivity threshold and geometrical cancelation of the field effects. We propose to study the Zeeman effect using Spectro-Polarimetric INterferometry (SPIN) which consists of the simultaneous use of polarimetry and very high angular resolution provided by long baseline interferometers. As monitoring of the instrumental polarisation is mandatory in order to calibrate interferometric observations in any case, the polarised signal is a natural by-product of interferometers. This method will be tested on the GI2T interferometer thanks to its high spectral resolution and its polarimetric capabilities.
2

McAlister, Harold A. « Overview of Multiple–Aperture Interferometry Binary Star Results from the Northern Hemisphere ». Proceedings of the International Astronomical Union 2, S240 (août 2006) : 35–44. http://dx.doi.org/10.1017/s1743921307003778.

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AbstractLong-baseline optical interferometry (LBI) can nearly close the gap in selection space between astrometric and spectroscopic detection of binary star systems, bringing the complementary powers of astrometry and spectroscopy to bear on a complete dynamical understanding of such systems, particularly including the determination of the masses of the individual stellar components. In the case of double-lined spectroscopic systems, their resolution by long-baseline interferometry also yields the orbital parallax and hence the luminosities of the individual stars. In some of these cases, the angular diameters of one or more components are accessible, and so a complete specification of a star in terms of its mass, radius and luminosity is made.The northern hemisphere is now equipped with several interferometers of unprecedented capability in terms of their baseline sizes, numbers of telescopes and telescope apertures. These instruments, most notably the Palomar Testbed Interferometer at Mt. Palomar Observatory, have produced very significant results of a number of interesting systems fulfilling interferometry's promise to produce fundamental astrophysical data at levels of accuracy that challenge or confirm astrophysical theory.This paper presents basic principles of long-baseline interferometric study of binary stars and summarizes results from northern interferometers with specific examples of their broad impact on binary star astronomy.
3

Jankov, S. « Astronomical optical interferometry, I : Methods and instrumentation ». Serbian Astronomical Journal, no 181 (2010) : 1–17. http://dx.doi.org/10.2298/saj1081001j.

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Previous decade has seen an achievement of large interferometric projects including 8-10m telescopes and 100m class baselines. Modern computer and control technology has enabled the interferometric combination of light from separate telescopes also in the visible and infrared regimes. Imaging with milli-arcsecond (mas) resolution and astrometry with micro-arcsecond (?as) precision have thus become reality. Here, I review the methods and instrumentation corresponding to the current state in the field of astronomical optical interferometry. First, this review summarizes the development from the pioneering works of Fizeau and Michelson. Next, the fundamental observables are described, followed by the discussion of the basic design principles of modern interferometers. The basic interferometric techniques such as speckle and aperture masking interferometry, aperture synthesis and nulling interferometry are discussed as well. Using the experience of past and existing facilities to illustrate important points, I consider particularly the new generation of large interferometers that has been recently commissioned (most notably, the CHARA, Keck, VLT and LBT Interferometers). Finally, I discuss the longer-term future of optical interferometry, including the possibilities of new large-scale ground-based projects and prospects for space interferometry.
4

Trolinger, James D., Amit Lal, Joshua Jo et Stephen Kupiec. « Programmable Holographic Optical Elements as Adaptive Optics in Optical Diagnostics Devices ». Key Engineering Materials 437 (mai 2010) : 108–12. http://dx.doi.org/10.4028/www.scientific.net/kem.437.108.

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This paper reports a combined, Hartmann/Digital Holographic interferometry inspection system for inspecting optical components that do not easily lend themselves to conventional interferometric or Hartmann inspection. A programmable holographic optical element (HOE) preconditions wavefronts to extend the dynamic range of interferometry measurements and also transforms the same system into a scanning Hartmann operation, which has lower resolution but higher dynamic range. Inspecting aspherical surfaces with existing interferometers requires special, computer generated holographic optical elements to transform the wavefront to within the dynamic range of the interferometer. The Hartmann measurement provides the information required to precondition a reference wave that avails the measurement process to the more precise phase shifting interferometry. The SLM offers yet other benefits including a method for minimizing the effects of speckle on the measurement. The paper provides example measurements, discusses the limitations, and suggests other potential applications.
5

Cavedo, Federico, Parisa Esmaili, Alessandro Pesatori et Michele Norgia. « Self-mixing Interferometer : Frequency Modulation Noise Dependence on Laser Source ». Journal of Physics : Conference Series 2698, no 1 (1 février 2024) : 012019. http://dx.doi.org/10.1088/1742-6596/2698/1/012019.

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Abstract The acquisition of frequency modulation in self-mixing interferometry opens the way to a new generation of instruments, with significantly superior performance compared to traditional self-mixing interferometers. In this work, we experimentally confirm the noise limit dependence of this kind of interferometer on the laser source linewidth. The obtained results confirm the theoretical prediction, opening the way for a deeper improvement in sensitivity, by employing narrow-line lasers in this interferometric configuration.
6

Yankelev, Dimitry, Chen Avinadav, Nir Davidson et Ofer Firstenberg. « Atom interferometry with thousand-fold increase in dynamic range ». Science Advances 6, no 45 (novembre 2020) : eabd0650. http://dx.doi.org/10.1126/sciadv.abd0650.

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The periodicity inherent to any interferometric signal entails a fundamental trade-off between sensitivity and dynamic range of interferometry-based sensors. Here, we develop a methodology for substantially extending the dynamic range of such sensors without compromising their sensitivity, stability, and bandwidth. The scheme is based on simultaneous operation of two nearly identical interferometers, providing a moiré-like period much larger than 2π and benefiting from close-to-maximal sensitivity and from suppression of common-mode noise. The methodology is highly suited to atom interferometers, which offer record sensitivities in measuring gravito-inertial forces but suffer from limited dynamic range. We experimentally demonstrate an atom interferometer with a dynamic-range enhancement of more than an order of magnitude in a single shot and more than three orders of magnitude within a few shots for both static and dynamic signals. This approach can considerably improve the operation of interferometric sensors in challenging, uncertain, or rapidly varying conditions.
7

Stee, Ph, D. Bonneau, F. Morand, D. Mourard et F. Vakili. « Current studies and future prospects in stellar-structure imaging with the GI2T ». Symposium - International Astronomical Union 176 (1996) : 191–98. http://dx.doi.org/10.1017/s0074180900083224.

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The capability of optical long baseline interferometry for measuring the angular diameter of stars or binary separation is now well established. However, for the imaging of photospheric disk structures one needs very long baseline interferometers operated in the multi-telescope phase-closure technique. In this paper we will stress the capability of spectro-interferometric measurements to constrain the physics of hot stars. We will report our study of the interacting binary, β Lyrae, and the mass-losing Be star γ Cassiopeiae. We will look at the interpretation of both the modulus and phase data recorded by the long baseline interferometer GI2T in the southern France. The performances and limitations of spectro-interferometric techniques will also be discussed through some of the most exciting prospects within the reach of current interferometers.
8

Noordam, J. E. « European Space Interferometry ». Symposium - International Astronomical Union 166 (1995) : 345. http://dx.doi.org/10.1017/s0074180900228349.

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Optical interferometry is ensconced as an ‘area of future interest’ (a socalled Green Dream) in Horizon 2000, the long-term scientific plan of ESA. Over the years, there have been three large ESA workshops on Space interferometry, where many different concepts and designs were proposed, and several ESA committees have studied the possibilities. These committees were also involved, in an advisory role, in a modest technological research program (TRP) by ESTEC. In 1990, the Space Interferometry Study Team (SIST) recommended building an optical interferometer, consisting of 10-15 small telescopes attached to an 100m inflatable structure, as a scientifically interesting first step. The SIST even produced a workable design. It quickly became clear, however, that such an undertaking would cost much more than an ESA cornerstone mission, and was thus far too ambitious. Simultaneously, another ESA study team (LIST) came to the conclusion that the Moon, contrary to earlier beliefs, does not offer a particularly suitable environment for interferometry. At the Beaulieu workshop in 1992, it was decided to try to achieve cornerstone status for one or two smaller interferometry missions in Space: a 10m UV imaging interferometer, or an interferometric successor to the astrometry satellite Hipparchos. The latter seems to have a good chance at the moment, in the form of the GAIA proposal which has been selected for further study for the new ‘post-Horizon 2000’ program. GAIA may have some limited imaging capability, but a true imaging interferometer in Space will have to wait for a few decades yet.
9

Pushin, D. A., M. G. Huber, M. Arif, C. B. Shahi, J. Nsofini, C. J. Wood, D. Sarenac et D. G. Cory. « Neutron Interferometry at the National Institute of Standards and Technology ». Advances in High Energy Physics 2015 (2015) : 1–7. http://dx.doi.org/10.1155/2015/687480.

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Neutron interferometry has proved to be a very precise technique for measuring the quantum mechanical phase of a neutron caused by a potential energy difference between two spatially separated neutron paths inside interferometer. The path length inside the interferometer can be many centimeters (and many centimeters apart) making it very practical to study a variety of samples, fields, potentials, and other macroscopic medium and quantum effects. The precision of neutron interferometry comes at a cost; neutron interferometers are very susceptible to environmental noise that is typically mitigated with large, active isolated enclosures. With recent advances in quantum information processing especially quantum error correction (QEC) codes we were able to demonstrate a neutron interferometer that is insensitive to vibrational noise. A facility at NIST’s Center for Neutron Research (NCNR) has just been commissioned with higher neutron flux than the NCNR’s older interferometer setup. This new facility is based on QEC neutron interferometer, thus improving the accessibility of neutron interferometry to the greater scientific community and expanding its applications to quantum computing, gravity, and material research.
10

Monnier, John D. « Infrared interferometry of circumstellar envelopes ». Symposium - International Astronomical Union 191 (1999) : 321–30. http://dx.doi.org/10.1017/s0074180900203239.

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This paper will review the technical progress of interferometric infrared observing techniques from the first 2-element interferometer 25 years ago to the 3+ element arrays now coming into service. To date, only the Infrared Spatial Interferometer (ISI) has published separate-element interferometric data on circumstellar dust shells in the infrared and many of these scientific results will be discussed. Speckle interferometry has also evolved significantly over the last few decades as slit-scanning techniques over single-pixel detectors have largely been replaced by fast-readout of large format detector arrays. Important near-infrared and mid-infrared results derived from speckle data will also be reviewed.Until recently, two-dimensional information about circumstellar dust distributions has been sorely lacking, hence detections of dust shell asymmetries have been difficult and uncertain. New speckle observations using modern, 10-m class telescopes have yielded surprising results, demonstrating the importance of accurate closure phase information in interpreting interferometric data. These discoveries hopefully precursor those to be made from closure-phase imaging with the new generation of separate-element, interferometric arrays.

Thèses sur le sujet "Interferometry":

1

Ho, Lap. « High precision short-baseline pointing system using GPS interferometry ». Ohio : Ohio University, 1995. http://www.ohiolink.edu/etd/view.cgi?ohiou1179435242.

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2

Lemes, Andryos da Silva [UNESP]. « Novas configurações de interferômetros de quadratura e de técnicas de detecção de fase óptica baseadas em phase unwrapping ». Universidade Estadual Paulista (UNESP), 2014. http://hdl.handle.net/11449/111112.

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Interferômetros ópticos de saída única são muito sensíveis quando operam nas proximidades do ponto de quadratura de fase da sua curva característica de entrada e saída. Entretanto, as flutuações ambientais de baixa frequência produzem derivas aleatórias entre os caminhos ópticos do interferômetro que desviam o ponto quiescente da quadratura, levando ao fenômeno de desvanecimento de sinal. Através de processamento eletrônico de dois sinais interferométricos de saída, defasados a 90º entre si, consegue-se demodular o sinal independentemente das derivas ambientais. Esses interferômetros chamados de interferômetros de quadratura são amplamente utilizados em laboratórios de metrologia, porém, devido à grande quantidade de componentes ópticos normalmente envolvidos, são de difícil alinhamento e de elevado custo. Neste trabalho estuda-se a interferometria homódina de dois feixes em quadratura e as suas complexidades inerentes. Propõe-se uma nova arquitetura, baseada na configuração de Michelson, de alinhamento mais simples e de baixo custo. Descreve-se matematicamente o processo de obtenção dos sinais em quadratura deste arranjo. Também, se explora uma técnica capaz de obter dois sinais interferométricos em quadratura através da configuração tradicional de Michelson explorando-se a distribuição espacial do padrão de franjas. Desenvolve-se, ainda, um novo algoritmo de phase unwrapping aplicável como método de detecção de fase óptica, capaz de reconstruir a forma de onda de sinais de modulação e fornecer a diferença de fase estática entre os braços do interferômetro, quando o sinal de modulação possui valor médio nulo. Testes computacionais são realizados para corroborar na tarefa de evidenciar o potencial da técnica. Por meio do método de demodulação apresentado, em adição com o interferômetro proposto e da técnica explorada, realiza-se testes experimentais em um atuador piezoelétrico ...
Optical interferometers with single outputs are very sensitive when operating close to the phase quadrature point of their input-output characteristic curves. However, low frequency environmental fluctuations generate random drifts between the optical paths of the interferometer that deviate the quiescent point from the quadrature condition. This problem causes the phenomenon called signal fading. By electronically processing these two interferometry output signals, shifted by 90º, it is possible to demodulate the signal regardless of environmental drift. These kinds of interferometers, known as quadrature interferometers, are widely used in metrology laboratories, but, due to the large amount of optical components, they are expensive and difficult to design. In this work a low cost homodyne interferometer with two output quadrature beams based on the Michelson configuration is studied, and the procedure to achieve the quadrature signals is mathematically described. Also, a recent technique, not widely known in the literature and that is able to obtain two quadrature signals by using the standard configuration of the Michelson interferometer is explored, exploiting the spatial distribution of the fringe pattern. A new method for optical phase shift demodulation based on phase unwrapping is developed. This approach is able to recover not only the modulation signal waveform, but can also calculate the static phase shift between the interferometer arms when the modulation signal has an average value equal to zero. The method also has the ability to demodulate signals which vary arbitrarily in time. Computational test were done aiming to demonstrate the technique potential. By using this new optical phase shift demodulation method, combined with the proposed interferometer and exploiting the spatial distribution of the fringe pattern, a piezoelectric flextensional actuator is characterized. Displacement versus drive voltage and frequency ...
3

Lemes, Andryos da Silva. « Novas configurações de interferômetros de quadratura e de técnicas de detecção de fase óptica baseadas em phase unwrapping / ». Ilha Solteira, 2014. http://hdl.handle.net/11449/111112.

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Orientador: Cláudio Kitano
Banca: Ricardo Tokio Higuti
Banca: Ronny Calixto Carbonari
Resumo: Interferômetros ópticos de saída única são muito sensíveis quando operam nas proximidades do ponto de quadratura de fase da sua curva característica de entrada e saída. Entretanto, as flutuações ambientais de baixa frequência produzem derivas aleatórias entre os caminhos ópticos do interferômetro que desviam o ponto quiescente da quadratura, levando ao fenômeno de desvanecimento de sinal. Através de processamento eletrônico de dois sinais interferométricos de saída, defasados a 90º entre si, consegue-se demodular o sinal independentemente das derivas ambientais. Esses interferômetros chamados de interferômetros de quadratura são amplamente utilizados em laboratórios de metrologia, porém, devido à grande quantidade de componentes ópticos normalmente envolvidos, são de difícil alinhamento e de elevado custo. Neste trabalho estuda-se a interferometria homódina de dois feixes em quadratura e as suas complexidades inerentes. Propõe-se uma nova arquitetura, baseada na configuração de Michelson, de alinhamento mais simples e de baixo custo. Descreve-se matematicamente o processo de obtenção dos sinais em quadratura deste arranjo. Também, se explora uma técnica capaz de obter dois sinais interferométricos em quadratura através da configuração tradicional de Michelson explorando-se a distribuição espacial do padrão de franjas. Desenvolve-se, ainda, um novo algoritmo de phase unwrapping aplicável como método de detecção de fase óptica, capaz de reconstruir a forma de onda de sinais de modulação e fornecer a diferença de fase estática entre os braços do interferômetro, quando o sinal de modulação possui valor médio nulo. Testes computacionais são realizados para corroborar na tarefa de evidenciar o potencial da técnica. Por meio do método de demodulação apresentado, em adição com o interferômetro proposto e da técnica explorada, realiza-se testes experimentais em um atuador piezoelétrico...
Abstract: Optical interferometers with single outputs are very sensitive when operating close to the phase quadrature point of their input-output characteristic curves. However, low frequency environmental fluctuations generate random drifts between the optical paths of the interferometer that deviate the quiescent point from the quadrature condition. This problem causes the phenomenon called signal fading. By electronically processing these two interferometry output signals, shifted by 90º, it is possible to demodulate the signal regardless of environmental drift. These kinds of interferometers, known as quadrature interferometers, are widely used in metrology laboratories, but, due to the large amount of optical components, they are expensive and difficult to design. In this work a low cost homodyne interferometer with two output quadrature beams based on the Michelson configuration is studied, and the procedure to achieve the quadrature signals is mathematically described. Also, a recent technique, not widely known in the literature and that is able to obtain two quadrature signals by using the standard configuration of the Michelson interferometer is explored, exploiting the spatial distribution of the fringe pattern. A new method for optical phase shift demodulation based on phase unwrapping is developed. This approach is able to recover not only the modulation signal waveform, but can also calculate the static phase shift between the interferometer arms when the modulation signal has an average value equal to zero. The method also has the ability to demodulate signals which vary arbitrarily in time. Computational test were done aiming to demonstrate the technique potential. By using this new optical phase shift demodulation method, combined with the proposed interferometer and exploiting the spatial distribution of the fringe pattern, a piezoelectric flextensional actuator is characterized. Displacement versus drive voltage and frequency ...
Mestre
4

Nečesal, Daniel. « Fázové zobrazování pod difrakčním limitem ». Master's thesis, Vysoké učení technické v Brně. Fakulta strojního inženýrství, 2020. http://www.nusl.cz/ntk/nusl-417067.

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Tato diplomová práce se zabývá konstrukcí interferenčních zařízení pro výzkum měření fáze světla na mikro-strukturách a fáze plazmonů na nano-strukturách. V první kapitole je vybudován teoretický základ pro optiku a nano-fotoniku používané v budoucích kapitolách. Následně je popsána interference vln a jejich praktické použití pro prolomení difrakčního limitu pomocí holografie plazmonů. Prvním experimentální sestavou je Machův-Zehnderův holografický mikroskop. Je popsán způsob, jak ho sestavit z běžně dostupných součástek a jak je navržen ovládací software k jeho používání. Následně jsou popsány výsledky naměřené pomocí tohoto zařízení. V poslední kapitole se zaměříme na sestavení holografického SNOM přístroje pro studování plazmonů a jejich interference. Nejdříve popíšeme základní princip a navržení softwaru pro automatizaci měření, pro zrychlení vědeckých postupů. Nakonec předložíme výsledky měření mikroskopu.
5

Guo, Yifan. « Developments in moire interferometry : carrier pattern technique and vibration insensitive interferometers ». Diss., Virginia Polytechnic Institute and State University, 1989. http://hdl.handle.net/10919/54181.

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Due to the rapid expansion of applications of composite materials, investigations of their properties have greatly increased. Since theoretical and numerical methods have many limitations for anisotropic materials, experimental methods are sometimes the only way to answer the questions. It has been proved that moire interferometry is a powerful technique in the study of composite materials. The high sensitivity and resolution of a measurement technique is the key to determining the properties of a material which has a fine and complicated structure such as fiber reinforced composite laminates. In this paper, a carrier fringe method is introduced to increase the resolution of the fringe gradient in the moire technique. The ability of measurement is extended to the micromechanics region. High strain concentrations and the dramatic displacement variations can be determined by measuring the slopes of carrier fringes. Strain distributions across the plies (with the thickness of 125 μm) in graphite/epoxy composites and strain concentrations in the resin-rich zones (with the thickness of 10 μm) between neighboring plies are revealed by the carrier fringe technique. Three experiments are presented to show the effectiveness of the application of carrier fringes to resolve fringe gradients and obtain strains. The current moire technique is limited to the optical laboratory because it is extremely sensitive to the disturbance of the environment. A vibration with magnitude of 0.2 μm can completely wash out the contrast of a moire fringe pattern. The study has been done in moving moire interferometry off the optical table. Vibration insensitive moire systems are investigated to extend the moire technique to the tests of large structures and using testing machines for loading. Vibration problems are discussed and the new ideas for eliminating vibration effects are presented. Six representative schemes are analyzed and three of these systems are built to perform experiments in rough environments such as on a hydraulic testing machine. The results show the great success of these new systems.
Ph. D.
6

Iacchetta, Alexander S. « Spatio-Spectral Interferometric Imaging and the Wide-Field Imaging Interferometry Testbed ». Thesis, University of Rochester, 2018. http://pqdtopen.proquest.com/#viewpdf?dispub=10936092.

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The light collecting apertures of space telescopes are currently limited in part by the size and weight restrictions of launch vehicles, ultimately limiting the spatial resolution that can be achieved by the observatory. A technique that can overcome these limitations and provide superior spatial resolution is interferometric imaging, whereby multiple small telescopes can be combined to produce a spatial resolution comparable to a much larger monolithic telescope. In astronomy, the spectrum of the sources in the scene are crucial to understanding the material composition of the sources. So, the ultimate goal is to have high-spatial-resolution imagery and obtain sufficient spectral resolution for all points in the scene. This goal can be accomplished through spatio-spectral interferometric imaging, which combines the aperture synthesis aspects of a Michelson stellar interferometer with the spectral capabilities of Fourier transform spectroscopy.

Spatio-spectral interferometric imaging can be extended to a wide-field imaging modality, which increases the collecting efficiency of the technique. This is the basis for NASA’s Wide-field Imaging Interferometry Testbed (WIIT). For such an interferometer, there are two light collecting apertures separated by a variable distance known as the baseline length. The optical path in one of the arms of the interferometer is variable, while the other path delay is fixed. The beams from both apertures are subsequently combined and imaged onto a detector. For a fixed baseline length, the result is many low-spatial-resolution images at a slew of optical path differences, and the process is repeated for many different baseline lengths and orientations. Image processing and synthesis techniques are required to reduce the large dataset into a single high-spatial-resolution hyperspectral image.

Our contributions to spatio-spectral interferometry include various aspects of theory, simulation, image synthesis, and processing of experimental data, with the end goal of better understanding the nature of the technique. We present the theory behind the measurement model for spatio-spectral interferometry, as well as the direct approach to image synthesis. We have developed a pipeline to preprocess experimental data to remove unwanted signatures in the data and register all image measurements to a single orientation, which leverages information about the optical system’s point spread function. In an experimental setup, such as WIIT, the reference frame for the path difference measured for each baseline is unknown and must be accounted for. To overcome this obstacle, we created a phase referencing technique that leverages point sources within the scene of known separation in order to recover unknown information regarding the measurements in a laboratory setting. We also provide a method that allows for the measurement of spatially and spectrally complicated scenes with WIIT by decomposing them prior to scene projection.

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Vieira, Marcio Alexandre Pinto. « Analise vibracional de viga engastada utilizando a tecnica de moire : um estudo de caso ». [s.n.], 2005. http://repositorio.unicamp.br/jspui/handle/REPOSIP/257093.

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Orientador: Inacio Maria Dal Fabbro
Dissertação (mestrado) - Universidade Estadual de Campinas, Faculdade de Engenharia Agricola
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Resumo: O fenômeno de vibração é de ocorrência comum na mecânica, geralmente associado à membros estruturais assim como elementos de maquinas. Particularmente, no campo da engenharia agrícola, vibração vem associada à ferimentos em vegetais nas operações de campo, que claramente inclui colheita, transporte e processamento. A escolha de membros estruturais simples, como as viga engastada, para validar o método, quando uma estrutura mais complexa for ser considerada. O nome moiré tem sua origem na língua francesa, referindo-se ao padrão de onda formado. O fenômeno é gerado quando telas são sobrepostas, produzindo padrões de ondas ou franjas, que se movem quando suas posições relativas são alteradas. O método selecionado é chamado método geométrico de moiré, que consiste em projetar uma grade sobre a superfície do objeto em estudo e superpor a foto original e a grade deformada. Software's especificos são empregados na análise de imagens. O objetivo do presente trabalho é determinar o deslocamento transversal da linha elástica na Teoria da viga engastada de Euler-Bernoulli, excitada por um excitador eletromagnético, utilizado em analise modal, utilizando a técnica de moiré descrita acima
Abstract: Vibration phenomena are of common occurrence in mechanics, generally associated to structural members as well as to machine elements. Particularly, in the field of agricultural engineering, vibration comes also associated to vegetable bruising during field operations, which clearly includes harvesting, transportation and processing. The selection of a simple structural member as a cantilever beam to support the utility of a moiré technique in studying vibration analysis is to validate the method when more complex structures are being considered. Vibration modes of a cantilever beam are easily determined by analytical methods. The name moiré has its origin in the French language, referring to wave like pattern. The phenomenon is generated when screens superposed, producing wave like patterns or fringes, which move when its relative positions are displaced. The selected method is named geometric moiré, which consists in projecting a grid onto the object in study and superposing both, the original and the deformed grid. Specific software's were employed in the image analysis. The objective of the present work is to determine the transversal displacement of the elastic line of Euler-Bernoulli cantilever beam being excited by an electromagnetic varying field using the moiré technique described above. Keywords: vibration, geometric moiré
Mestrado
Projetos, Desenvolvimento e Otimização de Maquinas Agricolas
Mestre em Engenharia Agrícola
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Bins, Leonardo Sant'Anna 1961. « Estimação de fase absoluta e de linha de base em radar interferométrico de abertura sintética com múltiplas antenas ». [s.n.], 2014. http://repositorio.unicamp.br/jspui/handle/REPOSIP/261023.

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Orientador: Max Henrique Machado Costa
Tese (doutorado) - Universidade Estadual de Campinas, Faculdade de Engenharia Elétrica e de Computação
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Resumo: Dois problemas importantes na interferometria SAR (Synthetic Aperture Radar) são a estimação da fase absoluta e das linhas de base. O conhecimento preciso da fase absoluta e das linhas de base são fundamentais para a geração de modelos digitais de superfície ou terreno com alta precisão planimétrica e altimétrica. A estimação de fase absoluta consiste de duas etapas. A primeira etapa efetua o desdobramento da fase, o qual recupera a fase absoluta com os correspondentes múltiplos de 2?. A segunda etapa consiste na estimação do deslocamento de fase, causada pela combinação de erros de sincronização no sistema de aquisição de dados com erros de processamento da Interferometria SAR (InSAR). A estimação de linha de base consiste na determinação da posição da antena escrava relativa à posição da antena mestre (ou antena de referência). As contribuições desta tese consistem na concepção e na implementação de três métodos que se valem de múltiplas antenas (múltiplos interferogramas) para resolver esses dois problemas, como se segue. O primeiro método efetua o método de desdobramento de fase pontual, através do desdobramento de fase iterativo dos interferogramas, seguido da fusão dos mesmos, usando máxima verossimilhança. O segundo método refina a estimação de fase absoluta através da estimação do deslocamento de fase usando múltiplas antenas não colineares. O método se baseia na minimização da distorção geométrica (ou erro relativo) induzida pelo processamento com a presença de deslocamentos de fase com valores diferentes do verdadeiro. Uma das vantagens do método é que ele dispensa a instalação de refletores de canto na região imageada. Por último, um algoritmo do tipo Monte Carlo foi desenvolvido para a determinação das posições relativas das antenas escravas em relação à antena mestre. O método utiliza refletores de canto, cujas posições em campo são conhecidas, para reduzir o erro quadrático médio
Abstract: Two important issues in SAR interferometry (InSAR) are absolute phase and baseline estimation. The precise knowledge of these parameters is essential for the production of digital elevation models with high accuracy. The absolute phase estimation can be done in two steps. The first step performs the unwrapping of the phase, which retrieves the 2? multiples of the phase. The second step estimates the phase offset caused by a combination of errors in the acquisition system and in SAR interferometry (InSAR) processing. The baseline estimation determines the relative position of the slave antenna with respect to the master antenna (reference antenna). The contributions of this thesis consist in the design and implementation of three methods that use multiple antennas to address the above issues. The first method performs the unwrapping of the phase in a pixel based fashion, by iteratively unfolding the phase corresponding to each interferograma, followed by maximum likelihood fusion of the unwrapped phases. The second method refines the absolute phase estimation of the first step by incorporating a phase offset estimation based on multiple, noncollinear, antennas. This is achieved by minimizing the geometrical distortion (relative error) in the reconstructed digital elevation model induced by erroneous phase offsets in the interferograms. One advantage of this method is that it does not require the deployment of corner reflector in the area to be imaged. Lastly, the third method deals with baselines estimation. A baseline is determined by the relative positions of the slave and master antennas. The estimation is performed with a greedy stochastic algorithm of Monte Carlo type which uses corner reflectors with precisely known positions. A new position for the slave antenna is accepted when the mean square error of the corner reflector positions is reduced
Doutorado
Telecomunicações e Telemática
Doutor em Engenharia Elétrica
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Ramasubramanian, Srikanth. « Design and development of a portable Moiré interferometer ». Morgantown, W. Va. : [West Virginia University Libraries], 2004. https://etd.wvu.edu/etd/controller.jsp?moduleName=documentdata&jsp%5FetdId=3460.

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Thesis (M.S.)--West Virginia University, 2004.
Title from document title page. Document formatted into pages; contains x, 132 p. : ill. (some col.). Vita. Includes abstract. Includes bibliographical references (p. 131).
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Featonby, Paul. « Atom interferometry ». Thesis, University of Oxford, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.390459.

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Livres sur le sujet "Interferometry":

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Steel, W. H. Interferometry. 2e éd. Cambridge [Cambridgeshire] : Cambridge University Press, 1986.

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Schuster, Gerard Thomas. Seismic interferometry. Cambridge : Cambridge University Press, 2009.

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R, Thompson A. Interferometry and synthesis in radio astronomy. 2e éd. New York : Wiley, 2001.

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R, Thompson A. Interferometry and synthesis in radio astronomy. New York : Wiley, 1986.

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R, Thompson A. Interferometry and synthesis in radio astronomy. Malabar, Fla : Krieger Pub., 1991.

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P, Hariharan, et Malacara Daniel 1937-, dir. Selected papers on interference, interferometry, and interferometric metrology. Bellingham, Wash : SPIE Optical Engineering Press, 1995.

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Małgorzata, Kujawińska, Pryputniewicz Ryszard J, Takeda Mitsuo 1946-, Society of Photo-optical Instrumentation Engineers. et Society for Experimental Stress Analysis (U.S.), dir. Laser interferometry VIII--techniques and analysis : 6-7 August, 1996, Denver Colorado. Bellingham, Wash : SPIE--the International Society for Optical Engineering, 1996.

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Interferometry '89 (1989 Warsaw, Poland). Interferometry '89 : 100 years after Michelson--state of the art and applications : proceedings : 8-12 May 1989, Warsaw, Poland. Sous la direction de Jaroszewicz Zbigniew, Pluta Maksymilian, Stowarzyszenie Inżynierów i Teckników Mechaników Polskich. Optics Section. et Stowarzyszenie Inżynierów i Techników Mechaników Polskich. Education Centre. Bellingham, Wash., USA : SPIE--the International Society for Optical Engeering, 1990.

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Hanssen, Ramon F. Radar Interferometry. Dordrecht : Springer Netherlands, 2001. http://dx.doi.org/10.1007/0-306-47633-9.

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Rastogi, Pramod K., dir. Holographic Interferometry. Berlin, Heidelberg : Springer Berlin Heidelberg, 1994. http://dx.doi.org/10.1007/978-3-540-48078-5.

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Chapitres de livres sur le sujet "Interferometry":

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Evans, Christopher J. « Interferometry ». Dans CIRP Encyclopedia of Production Engineering, 1–8. Berlin, Heidelberg : Springer Berlin Heidelberg, 2016. http://dx.doi.org/10.1007/978-3-642-35950-7_16700-3.

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Nolte, David D. « Interferometry ». Dans Optical Interferometry for Biology and Medicine, 3–48. New York, NY : Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4614-0890-1_1.

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Kervella, Pierre. « Interferometry ». Dans Encyclopedia of Astrobiology, 1–6. Berlin, Heidelberg : Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-27833-4_792-5.

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Iizuka, Keigo. « Interferometry ». Dans Engineering Optics, 651–82. Cham : Springer International Publishing, 2019. http://dx.doi.org/10.1007/978-3-319-69251-7_21.

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Evans, Christopher J. « Interferometry ». Dans CIRP Encyclopedia of Production Engineering, 710–17. Berlin, Heidelberg : Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-20617-7_16700.

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Kervella, Pierre. « Interferometry ». Dans Encyclopedia of Astrobiology, 1212–17. Berlin, Heidelberg : Springer Berlin Heidelberg, 2015. http://dx.doi.org/10.1007/978-3-662-44185-5_792.

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Gross, Herbert, Bernd Dörband et Henriette Müller. « Interferometry ». Dans Handbook of Optical Systems, 1–180. Weinheim, Germany : Wiley-VCH Verlag GmbH & Co. KGaA, 2015. http://dx.doi.org/10.1002/9783527699230.ch1.

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Totzeck, Michael. « Interferometry ». Dans Springer Handbook of Lasers and Optics, 1255–83. Berlin, Heidelberg : Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-19409-2_16.

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Mertz, Lawrence. « Interferometry ». Dans Excursions in Astronomical Optics, 47–77. New York, NY : Springer New York, 1996. http://dx.doi.org/10.1007/978-1-4612-2386-3_3.

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Evans, Christopher J. « Interferometry ». Dans CIRP Encyclopedia of Production Engineering, 966–73. Berlin, Heidelberg : Springer Berlin Heidelberg, 2019. http://dx.doi.org/10.1007/978-3-662-53120-4_16700.

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Actes de conférences sur le sujet "Interferometry":

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Dowling, Jonathan P., et Marian O. Scully. « Quantum-noise limits to matter-wave interferometry ». Dans OSA Annual Meeting. Washington, D.C. : Optica Publishing Group, 1993. http://dx.doi.org/10.1364/oam.1993.thoo.4.

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The field of atom interferometry1 is interesting since the potential sensitivity of matter-wave interferometers far exceeds that of their light-wave antecedents.2 As was emphasized at the recent Solvay conference on quantum optics, there is at present no paradigm available for calculating the quantum noise limits to matter-wave interferometers.3 We show that the phase uncertainty is inversely proportional to the square root of the total number, rather than the mean number, of atoms in the interferometert.4 We find that a matter-wave interferometer used as a gyroscope can be expected to be more sensitive to rotation by some four orders of magnitude than present laser gyro devices.
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Campbell, Gene, Gary E. Sommargren et Bruce E. Truax. « Image Acquisition for High Accuracy Interferometry ». Dans Optical Fabrication and Testing. Washington, D.C. : Optica Publishing Group, 1998. http://dx.doi.org/10.1364/oft.1998.owc.2.

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In phase shifting interferometry, the image acquisition electronics have largely been ignored, because the overall measurement accuracy has generally been limited by the quality of the reference wave. A recently developed interferometer, the phase shifting diffraction interferometer,[1] provides a high quality reference wave, which has been measured to be better than λ/8000 rms. With such a reference wave, the interferometer accuracy then becomes limited by systematic errors in the image acquisition electronics. This paper presents a variety of issues that arise when using image acquisition electronics of the sort commonly used in commercial interferometers. A basic fiber interferometer that isolates electronics issues is described, as are simple solutions to some of the errors.
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Reasenberg, Robert D. « POINTS Optics : Challenges and Options ». Dans Space Optics for Astrophysics and Earth and Planetary Remote Sensing. Washington, D.C. : Optica Publishing Group, 1991. http://dx.doi.org/10.1364/soa.1991.tuc2.

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It has been widely recognized for several years that interferometric instruments will play a major role in many aspects of space-based optical astronomy. More recently, optical interferometry received very favorable treatment in the AASC (Bahcall Committee) report and the POINTS mission is a close match to the Astrometric Interferometry Mission that the report lists as a moderate space-based program. In the next century, milliarcsecond-and submilliarcsecond-resolution images will likely be obtained from interferometric instruments deployed in space. An important precursor to such imaging instruments is a small astrometric optical interferometer. (Recommendations of the Interferometry Panel of the AASC.)
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Riza, Nabeel A. « In-Line Acousto-Optic Architectures for Holographic Interferometry and Sensing ». Dans Holography. Washington, D.C. : Optica Publishing Group, 1996. http://dx.doi.org/10.1364/holography.1996.hma.4.

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Novel two Bragg cell and one Bragg cell acousto-optic (AO) interferometers are introduced in this paper. These interferometers can be used as a variety of optical instruments such as holographic interferometers, interferometric sensors, material characterization tools, and diagnostic measurement systems such as turbulence and flow/temperature assessment. To this date, to the best of the author’s knowledge, no such optical systems have been proposed for interferometric sensing and measurement tools that offer high optical power (e.g., 1 W CW), high speed scanning (e.g., < 50 μs per scan spot) interferometer systems with both heterodyning and almost baseband options for accurate diagnostic measurements. The bulk optics nature of our optical system design allows for high optical power interferometric applications.
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Devoe, R. G., C. Fabre, K. Jungmann, J. Hoffnagle et R. G. Brewer. « Precision interferometry with stabilized lasers ». Dans OSA Annual Meeting. Washington, D.C. : Optica Publishing Group, 1987. http://dx.doi.org/10.1364/oam.1987.wm3.

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Interferometers are essential tools for measuring optical wavelengths and frequencies. We demonstrate a new form of interferometry that is both simpler and more precise than conventional methods. Stable laser and electrooptic FM sideband techniques make a direct electronic measurement of the mode spacing of an ultrahigh finesse cavity with subhertz precision (0.4-Hz rms) over a 50-THz region. A new interferometer equation is derived in which all variables can be measured directly in situ. Experiments indicate errors below 10−10 over a 50-THz bandwidth and that the technique can be improved to the 10−12 level or beyond. No drift due to mirror aging has been observed over 420 days for a rate of <2 × 10−12/day. Our results indicate that low-loss multilayer dielectric mirrors are far more suitable for precision interferometry than previously thought, and we show how wavelength comparisons for 10−9 accuracy can be made with simple and inexpensive apparatus.
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Stahl, H. Phil. « Performance of an Infrared Phase-Shifting Interferometric System ». Dans Optical Fabrication and Testing. Washington, D.C. : Optica Publishing Group, 1985. http://dx.doi.org/10.1364/oft.1985.thcc1.

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An infrared phase-shifting interferometric system has been developed at the University of Arizona Optical Sciences Center. It is a compact, self-contained, easy to align and operate, next generation optical shop instrument. The principle applications for an infrared interferometer are: 1) inspection of infrared materials in transmission for index homogeneity and internal defects, 2) interferometry of surfaces, such as an asphere, whose slopes are too steep for the fringes to be resolved by a visible interferometer, and 3) interferometry of surfaces that are too rough to be tested at visible wavelengths. The advantages of operating an infrared interferometer in the phase-shifting mode are: 1) improved wavefront phase measurement accuracy and resolution 2) the measurement is independent of the beam irradiance distribution and the interferogram fringe contrast, and 3) the wavefront can be sampled and analyzed rapidly over a large two dimensional area.
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Devoe, R. G., C. Fabre, K. Jungmann, J. Hoffnagle et R. G. Brewer. « Optical heterodyne interferometry ». Dans OSA Annual Meeting. Washington, D.C. : Optica Publishing Group, 1986. http://dx.doi.org/10.1364/oam.1986.mw1.

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We describe a new approach to precision interferometry that is in principle different from previous techniques in that it is free from the systematic errors usually associated with interferometry. Optical heterodyne techniques are used to directly measure the empirical mode spacing of an interferometer over a broad (10%) frequency range. The frequency difference between any two modes can then be computed by summing the spacing of the modes that lie between them, in this way optical frequency differences of up to 50 THz can be measured without the usual corrections for mirror phase shift or diffraction. The heterodyne principle is realized by a dual frequency modulation technique which resonates 4-GHz sidebands of a stabilized dye laser with adjacent interferometer modes. The interferometer has a finesse of 20,000 and a linewidth of only 10 kHz, and measurements show that its mode spacing varies quadratically around its center frequency with a maximum deviation of a few parts in 10−8.
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Ben-Chorin, Moshe, Silvia Chuartzman et Yehiam Prior. « Absolute distance measurements using a noisy interferometer ». Dans The European Conference on Lasers and Electro-Optics. Washington, D.C. : Optica Publishing Group, 1998. http://dx.doi.org/10.1364/cleo_europe.1998.cfd4.

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The spectrum of white light passing through a Michelson interferometer develops a sinusoidal modulation, the frequency of which is determined by the path difference between the interferometer arms. Dispersive white light interferometry is capable of measuring relatively large distances (hundreds of µm) with high precision, and without moving parts. However, as with all interferometric methods, it is very sensitive to phase noise arising from such factors as vibrations or air turbulence. The random phase jumps reduce the visibility of the white light fringes. This limitation imposes stringent conditions upon the stability of the interferometer, and its applicability to field measurements is thus restricted.
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Reynaud, Francois, J. J. Alleman et H. Lagorceix. « Interferometric fiber arms for stellar interferometry ». Dans Garmisch - DL tentative, sous la direction de Guy Cerutti-Maori et Philippe Roussel. SPIE, 1994. http://dx.doi.org/10.1117/12.185277.

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Williams, Rick A., et Osuk Y. Kwon. « Subaperture Interferometric Testing of Aspheric Optics ». Dans Optical Fabrication and Testing. Washington, D.C. : Optica Publishing Group, 1987. http://dx.doi.org/10.1364/oft.1987.thaa3.

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Aspheric optical surfaces fill the need to generate non-standard wavefront profiles in many modern optical systems. Interferometric tests have been developed to measure the extreme phase errors, relative to a spherical reference, which occur near the outer regions of the aperture. Several null compensation techniques have been described. For example, a null lens designed to generate an aspheric reference wavefront can be used to negate the effect of the surface figure resulting in measurement of deviations from the desired asphere. Alternatively, computer generated holograms have been used in two-beam interferometers such that the wavefront from the aspheric test surface is compared to a "perfect" wavefront generated by the hologram. A second class of techniques based on shearing interferometry have also been described. For example, a lateral shear interferometer, in which two displaced wavefronts from the same test surface are interfered, does not require compensating optics or a reference surface to measure aspheric figure errors.

Rapports d'organisations sur le sujet "Interferometry":

1

Pritchard, David E. Atom Interferometry. Fort Belvoir, VA : Defense Technical Information Center, décembre 2001. http://dx.doi.org/10.21236/ada397658.

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Eichel, P. H., D. C. Ghiglia et C. V. Jr Jakowatz. Spotlight SAR interferometry for terrain elevation mapping and interferometric change detection. Office of Scientific and Technical Information (OSTI), février 1996. http://dx.doi.org/10.2172/211364.

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Fitch, J. P. Single antenna interferometry. Office of Scientific and Technical Information (OSTI), décembre 1989. http://dx.doi.org/10.2172/7247425.

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Goldberg, Kenneth A. Extreme ultraviolet interferometry. Office of Scientific and Technical Information (OSTI), décembre 1997. http://dx.doi.org/10.2172/658173.

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Erskine, D. Techniques in Broadband Interferometry. Office of Scientific and Technical Information (OSTI), janvier 2004. http://dx.doi.org/10.2172/15009760.

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Tringe, J. W., M. C. Converse et R. J. Kane. Develop Prototype Microwave Interferometry Diagnostic. Office of Scientific and Technical Information (OSTI), novembre 2016. http://dx.doi.org/10.2172/1335776.

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Friedman. Adaptive Optics, LLLFT Interferometry, Astronomy. Fort Belvoir, VA : Defense Technical Information Center, mars 2002. http://dx.doi.org/10.21236/ada415904.

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Pritchard, David E. New Developments in Atom Interferometry. Fort Belvoir, VA : Defense Technical Information Center, juillet 1992. http://dx.doi.org/10.21236/ada254094.

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Townes, Charles H. Support of Infrared Spatial Interferometry. Fort Belvoir, VA : Defense Technical Information Center, mai 1996. http://dx.doi.org/10.21236/ada310085.

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Dainty, J. C. High Annular Resolution Stellar Interferometry. Fort Belvoir, VA : Defense Technical Information Center, juillet 1985. http://dx.doi.org/10.21236/ada168755.

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