Relevant bibliographies by topics / And optical interferometry

Academic literature on the topic 'And optical interferometry'

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Published: 14 March 2023

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Journal articles on the topic "And optical interferometry"

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Trolinger, James D., Amit Lal, Joshua Jo, and Stephen Kupiec. "Programmable Holographic Optical Elements as Adaptive Optics in Optical Diagnostics Devices." Key Engineering Materials 437 (May 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.
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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.
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McAlister, Harold A. "Overview of Multiple–Aperture Interferometry Binary Star Results from the Northern Hemisphere." Proceedings of the International Astronomical Union 2, S240 (August 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.
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Simon, R. S., K. J. Johnston, D. Mozurkewich, K. W. Weiler, D. J. Hutter, J. T. Armstrong, and T. S. Brackett. "Imaging Optical interferometry." International Astronomical Union Colloquium 131 (1991): 358–67. http://dx.doi.org/10.1017/s0252921100013646.

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AbstractInterferometry at optical wavelengths is very similar to radio interferometry, once the fundamental differences in detectors are accounted for. The Mount Wilson Mark III optical interferometer has been used for optical interferometry of stars and stellar systems. Success with the Mark III has lead to the current program at the Naval Research Laboratory to build the Big Optical Array (BOA), which will be an imaging interferometer. Imaging simulations show that BOA will be able to produce images of complex stellar systems, with a resolution as fine as 0.2 milliarcseconds.
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Stee, Ph, D. Bonneau, F. Morand, D. Mourard, and 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.
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Yang, Yichao, Kohei Yamamoto, Miguel Dovale Álvarez, Daikang Wei, Juan José Esteban Delgado, Vitali Müller, Jianjun Jia, and Gerhard Heinzel. "On-Axis Optical Bench for Laser Ranging Instruments in Future Gravity Missions." Sensors 22, no. 5 (March 7, 2022): 2070. http://dx.doi.org/10.3390/s22052070.

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The laser ranging interferometer onboard the Gravity Recovery and Climate Experiment Follow-On mission proved the feasibility of an interferometric sensor for inter-satellite length tracking with sub-nanometer precision, establishing an important milestone for space laser interferometry and the general expectation that future gravity missions will employ heterodyne laser interferometry for satellite-to-satellite ranging. In this paper, we present the design of an on-axis optical bench for next-generation laser ranging which enhances the received optical power and the transmit beam divergence, enabling longer interferometer arms and relaxing the optical power requirement of the laser assembly. All design functionalities and requirements are verified by means of computer simulations. A thermal analysis is carried out to investigate the robustness of the proposed optical bench to the temperature fluctuations found in orbit.
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Jankov, S. "Astronomical optical interferometry, II: Astrophysical results." Serbian Astronomical Journal, no. 183 (2011): 1–35. http://dx.doi.org/10.2298/saj1183001j.

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Optical interferometry is entering a new age with several ground- based long-baseline observatories now making observations of unprecedented spatial resolution. Based on a great leap forward in the quality and quantity of interferometric data, the astrophysical applications are not limited anymore to classical subjects, such as determination of fundamental properties of stars; namely, their effective temperatures, radii, luminosities and masses, but the present rapid development in this field allowed to move to a situation where optical interferometry is a general tool in studies of many astrophysical phenomena. Particularly, the advent of long-baseline interferometers making use of very large pupils has opened the way to faint objects science and first results on extragalactic objects have made it a reality. The first decade of XXI century is also remarkable for aperture synthesis in the visual and near-infrared wavelength regimes, which provided image reconstructions from stellar surfaces to Active Galactic Nuclei. Here I review the numerous astrophysical results obtained up to date, except for binary and multiple stars milliarcsecond astrometry, which should be a subject of an independent detailed review, taking into account its importance and expected results at microarcsecond precision level. To the results obtained with currently available interferometers, I associate the adopted instrumental settings in order to provide a guide for potential users concerning the appropriate instruments which can be used to obtain the desired astrophysical information.
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Sweedler, Jonathan V., Rafi D. Jalkian, Gary R. Sims, and M. Bonner Denton. "Crossed Interferometric Dispersive Spectroscopy." Applied Spectroscopy 44, no. 1 (January 1990): 14–20. http://dx.doi.org/10.1366/0003702904085967.

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A novel design is described which combines dispersive and interferometric spectrometric instrumentation for ultraviolet visible spectroscopy, offering significant advantages in comparison to conventional spectroscopic configurations. The optical system incorporates the triangular common-path interferometer with an additional cross-dispersive element, allowing spectra to be obtained in a format compatible with rectangular CTD array detectors. The use of a cross-dispersive optical element reduces the distributive multiplex effects of interferometry in a rugged, compact, optically simple system.
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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.
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Bedding, T. R., and J. G. Robertson. "Optical Aperture Synthesis with the Anglo-Australian Telescope." Publications of the Astronomical Society of Australia 8, no. 1 (1989): 78–80. http://dx.doi.org/10.1017/s1323358000022967.

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AbstractWe propose to construct an optical interferometer to produce high resolution images by aperture synthesis. The interferometer, known as the Masked Aperture Pupil-Plane Interference Telescope (MAPPIT), will be mounted at the coudé focus of the Anglo-Australian Telescope. It will use a non-redundant aperture mask, together with closure phase methods developed for radio VLBI, to overcome the wavefront distortions which are introduced by atmospheric turbulence. By using the techniques of pupil-plane interferometry and wavelength dispersion, it is hoped that MAPPIT will have more sensitivity than many other interferometric imaging projects.
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Dissertations / Theses on the topic "And optical interferometry"

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Arain, Muzamil Arshad. "INTERFEROMETRY-BASED FREE SPACE COMMUNICATION AND INFORMATION PROCESSING." Doctoral diss., University of Central Florida, 2005. http://digital.library.ucf.edu/cdm/ref/collection/ETD/id/3304.

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This dissertation studies, analyzes, and experimentally demonstrates the innovative use of interference phenomenon in the field of opto-electronic information processing and optical communications. A number of optical systems using interferometric techniques both in the optical and the electronic domains has been demonstrated in the filed of signal transmission and processing, optical metrology, defense, and physical sensors. Specifically it has been shown that the interference of waves in the form of holography can be exploited to realize a novel optical scanner called Code Multiplexed Optical Scanner (C-MOS). The C-MOS features large aperture, wide scan angles, 3-D beam control, no moving parts, and high beam scanning resolution. A C-MOS based free space optical transceiver for bi-directional communication has also been experimentally demonstrated. For high speed, large bandwidth, and high frequency operation, an optically implemented reconfigurable RF transversal filter design is presented that implements wide range of filtering algorithms. A number of techniques using heterodyne interferometry via acousto-optic device for optical path length measurements have been described. Finally, a whole new class of interferometric sensors for optical metrology and sensing applications is presented. A non-traditional interferometric output signal processing scheme has been developed. Applications include, for example, temperature sensors for harsh environments for a wide temperature range from room temperature to 1000 degree C.
Ph.D.
Optics and Photonics
Optics
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Neutze, Richard. "Acceleration and optical interferometry." Thesis, University of Canterbury. Physics, 1995. http://hdl.handle.net/10092/6569.

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The influence of acceleration on a number of physical systems is examined. We present a full relativistic treatment of a simple harmonic oscillator with relativistic velocities. The line element for Schwarzschild geometry is expanded in a set of Cartesian coordinates and is shown to be locally equivalent (neglecting curvature) to the line element of a linearly accelerating frame of reference. We consider the rate of a linearly accelerating quantum mechanical clock and the measurement of frequency by non-inertial observers, requiring this measurement to be of finite duration. These analyses demonstrate the standard measurement hypothesis for accelerating observers only approximates the physical behaviour of these systems. We derive the output of an optical ring interferometer in a variety of experimental contexts. A full relativistic reanalysis of the modified Laub drag experiment of Sanders and Ezekiel is performed, correcting a number of errors in their work and giving an overall discrepancy between experiment and theory of 1300 ppm. We examine the behaviour of a ring interferometer containing an accelerating glass sample. Our analysis predicts sideband structure will arise when a glass sample is oscillated along one arm of a Mach-Zehnder interferometer and the resulting output Fourier analysed. We also predict a resonant cavity containing a linearly accelerating glass sample will display optical ringing. A rigorous analysis of a ring interferometer with angular acceleration is presented. This predicts a resonant cavity with angular acceleration will also display optical ringing and demonstrates the beat frequency in a ring laser with angular acceleration is the instantaneous Sagnac beat frequency. Finally, we analyse the optical output of a rotating ring laser with one mirror oscillating, predicting sideband structure in spectra obtained from Fourier analysis of the beat between the opposite beams, and the beat between adjacent modes when the laser has multimode operation.
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Wang, Zuobin. "New approaches in optical interferometry." Thesis, University of Warwick, 1997. http://wrap.warwick.ac.uk/76188/.

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This thesis presents two new approaches in optical interferometry: phase difference determination by fringe pattern matching and a spatial phase-shifting interferometry (spatial PSI) algorithm. These two approaches are both theoretically described and experimentally illustrated in this thesis. The method of phase difference determination by fringe pattern matching is capable of detecting the phase difference between two interferograms with subpixel resolution. In this method, the phase curves are obtained from mean-square difference calculations of any two fringe patterns shifted pixel by pixel, and the phase difference between the interferograms can be achieved by linear interpolation or polynomial curve fitting from the phase curves. The signal to noise ratio is significantly improved due to the region-based matching and its effect of averaging noise. The equations derived from the statistical analysis of matching process clearly explain the reason that the larger image patches have a better accuracy in the measurement of phase difference. The three applications of fringe pattern matching, measurement of electrostatic force displacement, displacement measurement based on Youngs experiment, and phase-shifting interferometry with arbitrary phase steps, are also investigated in this thesis. Computer simulation and experimental results have proved that fringe pattern matching is a powerful technique for measuring some basic parameters in optical interferometry such as phase difference, fringe spacing and displacement. In the algorithm of spatial PSI, one fringe pattern is captured by a CCD camera, and the other two shifted fringe patterns with the phase steps of 90oC and 180oc are generated by computer, according to the features of the light intensity distributions and the method of interpolation. The phase is then calculated by a standard three-step algorithm of phase-shifting interferometry. Experimental results have shown that it is a useful approach to spatial PSI.
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Tenefrancia, Sandra L. "Optical pattern comparison by interferometry." Thesis, Virginia Polytechnic Institute and State University, 1988. http://hdl.handle.net/10919/53191.

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By placing two similar input transparencies adjacent to each other in the same plane, and illuminating them with coherent light, it is possible to create parallel fringes that will modulate the composite Fraunhofer diffraction pattern of the two input objects. The power spectrum of the combined inputs, i.e. test and reference signal Fourier transform, is analyzed for regularity of the fringe pattern. The method of interference used on input with small rotational errors and on relatively large displacements of the input does not affect the recognition capabilities of the system. This optical method is useful for making rapid pattern comparisons, where the signal to noise ratio is large.
Master of Science
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Kobayashi, Hirokazu. "Geometric phases in optical interferometry." 京都大学 (Kyoto University), 2011. http://hdl.handle.net/2433/142564.

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Wavering, Thomas A. "Optical Path Length Multiplexing of Optical Fiber Sensors." Thesis, Virginia Tech, 1998. http://hdl.handle.net/10919/36037.

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Optical fiber sensor multiplexing reduces cost per sensor by designing a system that minimizes the expensive system components (sources, spectrometers, etc.) needed for a set number of sensors. The market for multiplexed optical sensors is growing as fiberoptic sensors are finding application in automated factories, mines, offshore platforms, air, sea, land, and space vehicles, energy distribution systems, medical patient surveillance systems, etc. Optical path length multiplexing (OPLM) is a modification to traditional white-light interferometry techniques to multiplex extrinsic Fabry-Perot interferometers and optical path length two-mode sensors. Additionally, OPLM techniques can be used to design an optical fiber sensor to detect pressure/force/acceleration and temperature simultaneously at a single point. While power losses and operating range restrictions limit the broadscale applicability of OPLM, it provides a way to easily double or quadruple the number of sensors by modifying the demodulation algorithm. The exciting aspect of OPLM is that no additional hardware is needed to multiplex a few sensors. In this way OPLM works with conventional technology and algorithms to drastically increase their efficiency. [1]
Master of Science
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Frater, Eric, and Eric Frater. "Optical Alignment with CGH Phase References." Diss., The University of Arizona, 2016. http://hdl.handle.net/10150/621452.

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The growing field of high-order aspheric and freeform optical fabrication has inspired the creation of optical surfaces and systems which are difficult to align. Advances in optical alignment technology are critical to fabricating and integrating aspheric components in advanced optical systems. This dissertation explores the field of optical alignment with a computer-generated hologram (CGH) used as a reference. A CGH is a diffractive optic which may be used to create a desired phase profile across a beam of light, project irradiance patterns, or serve as a mask for an incident beam. The alignment methods presented in this dissertation are concerned with the use of a CGH to create reference phase profiles, or "wavefronts" , in a beam. In one application a set of axisymmetric CGH references are co-aligned. Each CGH has also been aligned to an aspheric mirror so the co-alignment of the CGH references is also a co-alignment of the aspheric mirrors. Another application is concerned with aligning an interferometer to test an aspheric mirror surface. The interferometer measures a "null" interference pattern when its wavefront accommodates a known surface profile. In this alignment application the CGH creates wavefronts which accommodate a known set of small spherical reference features at the test surface. An interference null from all the "phase fiducial" reference features indicates an aligned projection of the CGH. The CGH co-alignment method is implemented on a 4-mirror prime focus corrector known as the Hobby-Eberly Telescope Wide Field Corrector (HET WFC). It is shown that this method was very successful for centration alignment of some mirrors, whereas mechanical stability was the hardware limitation for other degrees of freedom. The additional alignment methods used in this project are described in detail and the expected alignment of the HET WFC is reported.The fabrication, characterization and application of spherical phase fiducials is demonstrated in a CGH-corrected Fizeau test prototype. It is shown that these reference features achieve <±1.5µm transverse alignment precision. A pair of phase fiducials is also applied to constrain the clocking and magnification of a projected wavefront. Fabrication and coordinate measurement of the features present the dominant challenges in these demonstrations.
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Ireland, Michael. "Optical interferometry and Mira variable stars /." Connect to full text, 2005. http://hdl.handle.net/2123/721.

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Ireland, Michael James. "Optical Interferometry and Mira Variable Stars." Thesis, The University of Sydney, 2005. http://hdl.handle.net/2123/721.

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This thesis describes the development of a red tip/tilt and fringe detection system at the Sydney University Stellar Interferometer (SUSI), modelling the instrumental performance and effects of seeing at SUSI, making observations of Mira variable stars and finally modelling the atmospheres of Mira variables with physically self-consistent models. The new SUSI tip/tilt system is based around a CCD detector and has been successfully used to both track the majority of tip/tilt power in median seeing at an R magnitude of 4.5, and to provide seeing measures for post processing. The new fringe-detection system rapidly scans 33 to 140 $\mu$m in delay and detects the fringes using two avalanche-photodiodes. It has been used to acquire fringe data, provide user feedback and to track the fringe group-delay position. The system visibility (fringe visibility for a point source) and throughput were found to be consistent with models of the SUSI optical beam train. Observations were made of a variety of sources, including the Mira variables R Car and RR Sco, which were observed in two orthogonal polarization states. These measurements were the first successful use of Optical Interferometric Polarimetry (OIP), and enabled scattered light to be separated from bright photospheric flux. Dust scattering was found to originate from a thin shell 2-3 continuum radii from these stars, with an optical depth of 0.1 to 0.2 at 900 nm. Physical models of Mira variables including dust formation were developed, providing consistent explanations for these results as well as many other photometric and interferometric observations.
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Ireland, Michael James. "Optical Interferometry and Mira Variable Stars." University of Sydney. Physics, 2005. http://hdl.handle.net/2123/721.

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This thesis describes the development of a red tip/tilt and fringe detection system at the Sydney University Stellar Interferometer (SUSI), modelling the instrumental performance and effects of seeing at SUSI, making observations of Mira variable stars and finally modelling the atmospheres of Mira variables with physically self-consistent models. The new SUSI tip/tilt system is based around a CCD detector and has been successfully used to both track the majority of tip/tilt power in median seeing at an R magnitude of 4.5, and to provide seeing measures for post processing. The new fringe-detection system rapidly scans 33 to 140 $\mu$m in delay and detects the fringes using two avalanche-photodiodes. It has been used to acquire fringe data, provide user feedback and to track the fringe group-delay position. The system visibility (fringe visibility for a point source) and throughput were found to be consistent with models of the SUSI optical beam train. Observations were made of a variety of sources, including the Mira variables R Car and RR Sco, which were observed in two orthogonal polarization states. These measurements were the first successful use of Optical Interferometric Polarimetry (OIP), and enabled scattered light to be separated from bright photospheric flux. Dust scattering was found to originate from a thin shell 2-3 continuum radii from these stars, with an optical depth of 0.1 to 0.2 at 900 nm. Physical models of Mira variables including dust formation were developed, providing consistent explanations for these results as well as many other photometric and interferometric observations.
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Books on the topic "And optical interferometry"

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Optical interferometry. 2nd ed. Amsterdam: Academic Press, 2003.

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Optical interferometry. Sydney: Academic Press, 1985.

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1937-, Malacara Daniel, ed. Optical shop testing. 3rd ed. Hoboken, N.J: Wiley-Interscience, 2007.

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1937-, Malacara Daniel, ed. Optical Shop Testing. New York: Wiley, 1992.

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Gezari, Daniel Y. Spatial interferometry in optical astronomy. Washington, D.C: National Aeronautics and Space Administration, Office of Management, Scientific and Technical Information Division, 1990.

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Wang, Zuobin. New approaches in optical interferometry. [s.l.]: typescript, 1997.

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Gezari, Daniel Y. Spatial interferometry in optical astronomy. Washington, D.C: NASA, Office of Management, Scientific and Technical Information Division, 1990.

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Eric, Udd, Tatam Ralph P, Society of Photo-optical Instrumentation Engineers. Poland Chapter., Politechnika Warszawska, and Foundation for Promotion and Development of Optical Techniques (Poland), eds. Interferometric fiber sensing: Interferometry '94, 16-20 May, 1994, Warsaw, Poland. Bellingham, Wash., USA: SPIE--the International Society for Optical Engineering, 1994.

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Interferometry for precision measurement. Bellingham, Washington, USA: SPIE Press, 2014.

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Nolte, David D. Optical Interferometry for Biology and Medicine. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4614-0890-1.

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Book chapters on the topic "And optical interferometry"

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Wiora, Georg, Mark Weber, and Sirichanok Chanbai. "Optical Interferometry." In Encyclopedia of Tribology, 2483–88. Boston, MA: Springer US, 2013. http://dx.doi.org/10.1007/978-0-387-92897-5_317.

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Fehle, R., J. Klas, and B. Vogel. "Holographic Interferometry." In Optical Measurements, 51–73. Berlin, Heidelberg: Springer Berlin Heidelberg, 1994. http://dx.doi.org/10.1007/978-3-662-02967-1_5.

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Memmel, R., and J. Straub. "Differential Interferometry." In Optical Measurements, 75–90. Berlin, Heidelberg: Springer Berlin Heidelberg, 1994. http://dx.doi.org/10.1007/978-3-662-02967-1_6.

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Gross, Herbert, Bernd Dörband, and Henriette Müller. "Interferometry." In 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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Nolte, David D. "Interferometry." In 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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Ridgway, Stephen T. "Solar Optical Interferometry." In Infrared Solar Physics, 567–78. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1926-9_68.

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Løkberg, Ole J. "Electronic Speckle Pattern Interferometry." In Optical Metrology, 542–72. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3609-6_36.

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Donges, Axel, and Reinhard Noll. "Laser Interferometry." In Springer Series in Optical Sciences, 145–64. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-662-43634-9_6.

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Donges, Axel, and Reinhard Noll. "Holographic Interferometry." In Springer Series in Optical Sciences, 165–94. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-662-43634-9_7.

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Mayinger, F. "Fundamentals of Holography and Interferometry." In Optical Measurements, 27–50. Berlin, Heidelberg: Springer Berlin Heidelberg, 1994. http://dx.doi.org/10.1007/978-3-662-02967-1_4.

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Conference papers on the topic "And optical interferometry"

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Campbell, Gene, Gary E. Sommargren, and Bruce E. Truax. "Image Acquisition for High Accuracy Interferometry." In 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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Riza, Nabeel A. "In-Line Acousto-Optic Architectures for Holographic Interferometry and Sensing." In 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, and R. G. Brewer. "Optical heterodyne interferometry." In 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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Stahl, H. Phil. "Performance of an Infrared Phase-Shifting Interferometric System." In 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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Williams, Rick A., and Osuk Y. Kwon. "Subaperture Interferometric Testing of Aspheric Optics." In 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.
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Greivenkamp, J. E. "Sub-Nyquist Interferometry -- Review and Status." In Optical Fabrication and Testing. Washington, D.C.: Optica Publishing Group, 1987. http://dx.doi.org/10.1364/oft.1987.thaa2.

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Sub-Nyquist interferometry (SNI) is a new method of data analysis for phase-shifting interferometry (PSI) that greatly extends the measurement range of an interferometer for a given amount of data.1 This paper reviews the concept and principles of SNI, and details the progress towards a practical implementation of the technique.
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Reasenberg, Robert D. "POINTS Optics: Challenges and Options." In 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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Vohra, S. T., and F. Bucholtz. "Applications of Fiber Optic Interferometry in Nonlinear Dynamics." In Nonlinear Dynamics in Optical Systems. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/nldos.1992.tub6.

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The ultimate performance of a fiber optic (FO) interferometer depends on its ability to resolve small differential optical phase shifts. Due to advances in FO technology it has become possible to fabricate interferometers with optical phase resolution of < 1 μrad/√Hz (f >100 Hz) [1]. Such FO interferometers have been successfully utilized in making extremely high resolution acoustic and electromagnetic field sensors [1]. Since the optical phase shift in the fiber is directly proportional to the induced strain in the material bonded to the optical fiber the FO interferometer is also well suited for studying the dynamic strain response of magnetostrictive, piezoelectric and electrostrictive materials [2].
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Li, Y., G. Eichmann, and R. R. Alfano. "Phase-conjugate optics and optical switching using a pulsed mode Sagnac interferometer." In OSA Annual Meeting. Washington, D.C.: Optica Publishing Group, 1985. http://dx.doi.org/10.1364/oam.1985.thu5.

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A Sagnac interferometer, because of its fringe stability and ease of alignment, is a promising tool for pulsed mode interferometry. Unlike a Mach-Zehnder-type of pulsed interferometer, a Sagnac interferometer does not require active fringe stabilization. In this paper, nonlinear optical pulsed mode interferometry—an interferometer where one of the arms contains a nonlinear optical material—is considered. The optical source is a mode-locked pulsed picosecond Nd3+: YAG laser. Properties of this setup are analyzed. Experimental results, based on phase-conjugate nonlinear optics, are presented. Applications to picosecond optical switching are demonstrated.
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Saxer, Christopher, and Duncan T. Moore. "Harmonic Phase Shifting Interferometry." In Optical Fabrication and Testing. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/oft.1992.wa8.

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The technique of harmonic phase shifting interferometry (PSI), originally developed by Joseph Miceli in 19821, is a quasi-heterodyne method to continuously measure the optical phase of a point in an interferogram. The optical phase of the interferometer reference arm is modulated with the sum of prescribed amplitudes of a sine wave and its second harmonic. The interference phase at the detector is directly related to the electrical phase of the detected signal's fundamental frequency component. Harmonic phase-shifting interferometry may be executed by using a piezoelectric transducer (PZT) to shift the reference surface of the interferometer and a lock-in amplifier to measure the phase of the detected signal. Phase measurements may be made with peak reference arm phase changes less than 3λ/4, where λ is the wavelength of the light source, using either polarized or unpolarized light. This technique is best suited to single point measurements and line scans of interference patterns since each detector produces a continuous signal from which the interference phase must be extracted.
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Reports on the topic "And optical interferometry"

1

Nabeel A. Riza. Ultra-High Temperature Sensors Based on Optical Property Modulation and Vibration-Tolerant Interferometry. Office of Scientific and Technical Information (OSTI), September 2006. http://dx.doi.org/10.2172/901548.

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Nabeel A. Riza. Ultra-High Temperature Sensors Based on Optical Property Modulation and Vibration-Tolerant Interferometry. Office of Scientific and Technical Information (OSTI), March 2007. http://dx.doi.org/10.2172/908233.

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Nabeel A. Riza. ULTRA-HIGH TEMPERATURE SENSORS BASED ON OPTICAL PROPERTY MODULATION AND VIBRATION-TOLERANT INTERFEROMETRY. Office of Scientific and Technical Information (OSTI), November 2004. http://dx.doi.org/10.2172/835509.

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Nabeel A. Riza. ULTRA-HIGH TEMPERATURE SENSORS BASED ON OPTICAL PROPERTY MODULATION AND VIBRATION-TOLERANT INTERFEROMETRY. Office of Scientific and Technical Information (OSTI), April 2004. http://dx.doi.org/10.2172/824009.

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Nabeel A. Riza. ULTRA-HIGH TEMPERATURE SENSORS BASED ON OPTICAL PROPERTY MODULATION AND VIBRATION-TOLERANT INTERFEROMETRY. Office of Scientific and Technical Information (OSTI), July 2005. http://dx.doi.org/10.2172/842444.

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Nabeel A. Riza. Ultra-High Temperature Sensors Based on Optical Property Modulation and Vibration-Tolerant Interferometry. Office of Scientific and Technical Information (OSTI), January 2006. http://dx.doi.org/10.2172/875888.

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7

Swimm, Randall T. Thermal Transport Studies of Optical Coatings, Interfaces and Surfaces by Thermal Diffusion-Wave Interferometry. Fort Belvoir, VA: Defense Technical Information Center, August 1990. http://dx.doi.org/10.21236/ada231607.

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Steele, Thomas R. Interferometric Optical High Pressure Sensor. Fort Belvoir, VA: Defense Technical Information Center, January 1992. http://dx.doi.org/10.21236/ada245100.

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DeWeerd, Herman. Interferometric Optical Synchro for Alignment Transfer. Fort Belvoir, VA: Defense Technical Information Center, February 1989. http://dx.doi.org/10.21236/ada205089.

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SRICO OPTICAL ENGINEERING POWELL OH. Optical Interferometers for Sensing Electromagnetic Fields. Fort Belvoir, VA: Defense Technical Information Center, March 1991. http://dx.doi.org/10.21236/ada273712.

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