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Artículos de revistas sobre el tema "Interferometry"

Autor: Grafiati

Publicado: 4 de junio de 2021

Última modificación: 25 de julio de 2025

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1

Chesneau, O., K. Rousselet-Perraut, and 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 o

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2

McAlister, Harold A. "Overview of Multiple–Aperture Interferometry Binary Star Results from the Northern Hemisphere." Proceedings of the International Astronomical Union 2, S240 (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

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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

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4

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 elemen

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5

Cavedo, Federico, Parisa Esmaili, Alessandro Pesatori, and Michele Norgia. "Self-mixing Interferometer: Frequency Modulation Noise Dependence on Laser Source." Journal of Physics: Conference Series 2698, no. 1 (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.

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6

Yankelev, Dimitry, Chen Avinadav, Nir Davidson, and Ofer Firstenberg. "Atom interferometry with thousand-fold increase in dynamic range." Science Advances 6, no. 45 (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 interferomete

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7

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

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8

Pushin, D. A., M. G. Huber, M. Arif, et al. "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 mitiga

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9

Naeem, Muddasir, and Tayyab Imran. "ZEMAX Simulations and Experimental Validation of Laser Interferometers." Photonics 12, no. 3 (2025): 206. https://doi.org/10.3390/photonics12030206.

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This study presents the design, simulation, and experimental validation of six fundamental laser interferometer types: Sagnac, Mach–Zehnder, Michelson, Twyman–Green, Fizeau, and Fabry–Pérot. Using ZEMAX OpticStudio in non-sequential mode with the physical optics propagation (POP) algorithm, the simulations provide detailed insights into the optical performance of these interferometers. A direct comparison is made between the simulated and experimental fringe patterns, coherent irradiance distributions, and phase plots, demonstrating strong agreement and validating the accuracy of computational

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10

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

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11

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 forma

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12

Müller, André F., Claas Falldorf, Gerd Ehret, and Ralf B. Bergmann. "Messen von asphärischen Linsenformen mittels räumlicher Kohärenz." tm - Technisches Messen 86, no. 6 (2019): 325–34. http://dx.doi.org/10.1515/teme-2019-0025.

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ZusammenfassungWir zeigen den Vergleich zweier interferometrischer Verfahren zur Formprüfung anhand einer Messung an einer Zylinderlinse. Das erste Verfahren, die Multiple Aperture Shear Interferometry (MArS), basiert auf der Messung der Kohärenzfunktion mittels eines Scher-Interferometers. Es erlaubt interferometrische Messungen unter gleichzeitiger Verwendung mehrerer unabhängiger und teilkohärenter Lichtquellen, und ermöglicht so eine flexible, an den Prüfling anpassbare Ausleuchtung. Als Vergleichsverfahren kommt die Computational Shear Interferometry (CoSI) zur Messung von Wellenfronten z

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13

Petrov, R. G., S. Lagarde, and M. N'GUYEN Van KY. "Differential interferometry imaging." Symposium - International Astronomical Union 176 (1996): 181–90. http://dx.doi.org/10.1017/s0074180900083212.

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Differential Interferometry (DI) combines high spectral and high spatial resolution. On non resolved objects, it yields the angular variation of the source photocenter as a function of wavelength which has been shown theoretically and experimentally to complement very usefully both interferometric and spectroscopic data in a large number of astrophysical problems. This paper presents the general characteristics of DI which are likely to allow improvements of the Doppler images of stellar surface structures as soon as interferometers with large apertures and baselines approaching 100 m are avai

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14

TEN BRUMMELAAR, T., P. TUTHILL, and G. VAN BELLE. "INTRODUCTION." Journal of Astronomical Instrumentation 02, no. 02 (2013): 1303001. http://dx.doi.org/10.1142/s2251171713030013.

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After nearly one and a half centuries of effort, one of the most pernicious problems in observational astronomy — obtaining resolved images of the stars — is finally yielding to advances in modern instrumentation. The exquisite precision delivered by today's interferometric observatories is rapidly being applied to more and more branches of optical astronomy. The most capable interferometers in the Northern Hemisphere, both located in the United States are the Navy Precision Optical Interferometer (NPOI) in Arizona and the Center for High Angular Resolution Astronomy Array (CHARA) run by Georg

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15

Samoylenko, O., O. Adamenko, and V. Kalynichenko. "The Method and the Results of the Direct Comparison of the Laser Interferometers Renishaw Xl-80." Metrology and instruments, no. 4 (August 30, 2018): 15–21. http://dx.doi.org/10.33955/2307-2180(4)2018.15-21.

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The method of the direct comparison of the laser interferometers and method processing of the interferometry measurement results by the least square method (LSM) is present. The additive part of the measurement error for each pair of the interferometers is evaluated and the multiplicative part of the measurement error for each interferometer is evaluated too by LSM. Uncertainty by A tape by LSM is evaluated for all parameters. Results of the comparison of the three interferometers are presented.

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16

ten Brummelaar, Theo A. "Reducing Binary Star Data from Long-Baseline Interferometers." Proceedings of the International Astronomical Union 2, S240 (2006): 178–87. http://dx.doi.org/10.1017/s1743921307003997.

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AbstractProcessing long-baseline interferometry data presents a unique set of complications: How does one derive relative astrometry from interferometric data? How can 1-D interferometric results be used to solve a 2-D orbit? How can baseline-only solutions be combined with historical data and how should interferometric data be published so that they can be combined with archived data? What new techniques for interferometers are coming on line? This paper contains a brief review of interferometric data analysis in the context of binary star astrometry.

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17

Rodríguez, Luis F. "SpS1-Instrumentation for sub-millimeter spectroscopy." Proceedings of the International Astronomical Union 5, H15 (2009): 527–28. http://dx.doi.org/10.1017/s1743921310010525.

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The fields of millimeter and sub-millimeter interferometry have been developing for more than 30 years. At millimeter wavelengths the most important interferometers are the Combined Array for Research in Millimeter-Wave Astronomy (CARMA), the Plateau de Bure Interferometer (PdBI), and the Nobeyama Millimeter Array (NMA). At sub-millimeter wavelenghts, the most powerful interferometer is the SubMillimeter Array (SMA, for a detailed description, see Ho et al. 2004).

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18

Jalil, Muhammad Arif Bin. "An Overview on Several Types of the Optical Interferometers." International Journal for Research in Applied Science and Engineering Technology 12, no. 6 (2024): 454–58. http://dx.doi.org/10.22214/ijraset.2024.63070.

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Abstract: A common research instrument in many branches of science and engineering is the interferometer. Because they can identify and analyse interference patterns caused by the combination of light sources, these mid- to late-19th-century technologies are known as interferometers. The tool used for this process is called a "interferometer" or "interfere-meter." Interferometers are remarkably versatile devices that enable the development of highly accurate optical sensors for a wide range of applications. This article discussed the principles of interferometry as well as three different inte

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19

Yang, Yichao, Kohei Yamamoto, Miguel Dovale Álvarez, et al. "On-Axis Optical Bench for Laser Ranging Instruments in Future Gravity Missions." Sensors 22, no. 5 (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,

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20

Pérez-Callejo, G., V. Bouffetier, L. Ceurvorst, et al. "TIA: A forward model and analyzer for Talbot interferometry experiments of dense plasmas." Physics of Plasmas 29, no. 4 (2022): 043901. http://dx.doi.org/10.1063/5.0085822.

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Interferometry is one of the most sensitive and successful diagnostic methods for plasmas. However, owing to the design of most common interferometric systems, the wavelengths of operation and, therefore, the range of densities and temperatures that can be probed are severely limited. Talbot–Lau interferometry offers the possibility of extending interferometry measurements to x-ray wavelengths by means of the Talbot effect. While there have been several proof-of-concept experiments showing the efficacy of this method, it is only recently that experiments to probe High Energy Density (HED) plas

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21

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

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AbstractWe present some new and interesting results on the complementarity between asteroseismology and interferometry, the detection of non-radial pulsations in massive stars and the possibility for evidencing differential rotation on the surface of Bn stars. We also discuss the curretn interferometric facilities, namely the Very Large Telescope Interferometer (VLTI)/AMBER, VLTI/MIDI, VLTI/PIONIER within the European Southern Observatory (ESO) context and the Center for High Angular Resolution Astronomy (CHARA) array with their current limitations. The forthcoming second-generation VLTI instr

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22

Volkov, Petr, Andrey Lukyanov, Alexander Goryunov, Daniil Semikov, and Oleg Vyazankin. "Low-Coherence Homodyne Interferometer for Sub-Megahertz Fiber Optic Sensor Readout." Sensors 24, no. 2 (2024): 552. http://dx.doi.org/10.3390/s24020552.

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This study proposes a method for interferometric fiber optic sensor readouts. The method utilizes the advantages of the active homodyne demodulation technique and low-coherence interferometry. The usage of the tandem low-coherence interferometer enables modulating the reference interferometer without any changes to the sensor. This achieves high sensitivity, high stability, and a wide frequency band. A sensitivity of up to 0.1 nm (RMS) in the frequency range of 5 kHz is demonstrated by detecting acoustic signals with a fiber Michelson interferometer as a sensor.

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23

Scholz, Gregor, Ling Yang, Markus Schake, and Ines Fortmeier. "Concept for improving the form measurement results of aspheres and freeform surfaces in a tilted-wave interferometer." Journal of Sensors and Sensor Systems 13, no. 1 (2024): 89–97. http://dx.doi.org/10.5194/jsss-13-89-2024.

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Abstract. Accurate and flexible form measurements for aspherical and freeform surfaces are in high demand, and non-null-test interferometric methods such as tilted-wave interferometry have gained attention as a promising response to this need. Interferometric methods, however, display ambiguities between the measurement of certain form errors and the misalignment of the measured specimen. Therefore, improved knowledge of the absolute measurement position of the specimen in relation to the interferometer setup may improve the form measurement result. In this work, we propose a concept that uses

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24

Aydin, Deniz, Jack A. Barnes, and Hans-Peter Loock. "In-fiber interferometry sensors for refractive index." Applied Physics Reviews 10, no. 1 (2023): 011307. http://dx.doi.org/10.1063/5.0105147.

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Compact interferometers based on waveguiding structures have found countless applications in refractive index measurements, chemical sensing, as well as temperature and pressure measurements. The most common fiber devices are based on Mach–Zehnder interferometry and Michelson interferometry—two design concepts that can readily be implemented using simple fiber optic components, such as mode splitters and combiners, fiber optic gratings, and fiber tapers, among others. Fiber interferometry can also be conducted based on the Sagnac effect and the Young (double-slit) interferometer. In this revie

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25

Roh, Kyungmin, Youngmin Lee, Hyunil Benjamin Kim, Seongjin Jeon, Hyojeong Lee, and Hyyong Suk. "Highly sensitive double-grating interferometer for direct measurement of a neutral helium gas density in a capillary cell." Optics Express 33, no. 8 (2025): 18591. https://doi.org/10.1364/oe.562060.

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We developed a highly sensitive double-grating interferometer using four probe beams, which can measure one order of magnitude smaller phase shifts compared with other conventional interferometers. To achieve the unprecedented sensitivity, a highly dynamic 16-bit CCD camera was used and the balanced detection technique with four probe beams was employed in the 2-dimensional (2-D) interferometry for the first time. By using this interferometer, we could directly measure a low helium (He) gas density of n ≃ 1 × 1017 cm−3 in a capillary gas cell for the laser-plasma acceleration research, which i

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26

Thuering, T., and M. Stampanoni. "Performance and optimization of X-ray grating interferometry." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 372, no. 2010 (2014): 20130027. http://dx.doi.org/10.1098/rsta.2013.0027.

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The monochromatic and polychromatic performance of a grating interferometer is theoretically analysed. The smallest detectable refraction angle is used as a metric for the efficiency in acquiring a differential phase-contrast image. Analytical formulae for the visibility and the smallest detectable refraction angle are derived for Talbot-type and Talbot–Lau-type interferometers, respectively, providing a framework for the optimization of the geometry. The polychromatic performance of a grating interferometer is investigated analytically by calculating the energy-dependent interference fringe v

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27

Davis, John. "Stellar angular diameter measurements by interferometry." Symposium - International Astronomical Union 189 (1997): 31–38. http://dx.doi.org/10.1017/s0074180900116468.

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Stellar angular diameter measurements have been made with a range of interferometric techniques including speckle, aperture masking and long baseline optical/infrared interferometry. The current status of these measurements are summarised in terms of the range of spectral types and luminosity classes measured, the accuracies achieved, the wavelengths used for observations, and the reliability of the results. A number of major long-baseline interferometers are coming on-line, or are under development, and their potential is assessed in terms of wavelength cover, accuracy, angular resolution, an

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28

Kol'tso, N. E., S. A. Grenkov, and L. V. Fedotov. "Comparison of Radio Interferometers with Analog and Digital Extraction of Recorded Signal." Journal of the Russian Universities. Radioelectronics 23, no. 2 (2020): 6–18. http://dx.doi.org/10.32603/1993-8985-2020-23-2-6-18.

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Introduction. Radio telescopes of Very Long Baseline Interferometry (VLBI) networks usually record several signals with relatively narrow (up to 32 MHz) bands, which are extracted by means of base band converters (BBC) from an analog noise signal of an intermediate frequency (IF) with bands up to 1 GHz. When processing data, frequency band synthesis is used. At new small radio telescopes (for example, RT-13), directly wideband IF signals are digitized. An ability to connect the RT-13 radio telescope to the “Quasar” VLBI complex and to international VLBI networks provides by a digital narrow-ba

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29

Zou, Yi-Quan, Ling-Na Wu, Qi Liu, et al. "Beating the classical precision limit with spin-1 Dicke states of more than 10,000 atoms." Proceedings of the National Academy of Sciences 115, no. 25 (2018): 6381–85. http://dx.doi.org/10.1073/pnas.1715105115.

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Interferometry is a paradigm for most precision measurements. Using N uncorrelated particles, the achievable precision for a two-mode (two-path) interferometer is bounded by the standard quantum limit (SQL), 1/N, due to the discrete (quanta) nature of individual measurements. Despite being a challenging benchmark, the two-mode SQL has been approached in a number of systems, including the Laser Interferometer Gravitational-Wave Observatory and today’s best atomic clocks. For multimode interferometry, the SQL becomes 1/[(M−1)N] using M modes. Higher precision can also be achieved using entangled

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30

VETRANO, FLAVIO, GIANLUCA M. GUIDI, ANDREA VICERÉ, et al. "PRINCIPLES OF GRAVITATIONAL WAVES DETECTION THROUGH ATOM INTERFEROMETRY." International Journal of Modern Physics: Conference Series 23 (January 2013): 135–43. http://dx.doi.org/10.1142/s2010194513011185.

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The output of a simple Mach-Zehnder atom interferometer (with light field beam splitters) is studied in order to obtain sensitivity curves for GW signals in the paraxial approximation by using the ABCD matrices techniques and first order perturbation theory for mirroratom interaction; order of magnitude of relevant physical parameters for a realistic GW detector through atom interferometry is deduced, both for single- and coupled-interferometers configurations. Finally a synthetic overview of ongoing activities of the Florence-Urbino group in this field is presented.

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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 sensitivit

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32

Haniff, Chris A. "High Angular Resolution Studies of Stellar Atmospheres." Symposium - International Astronomical Union 205 (2001): 288–95. http://dx.doi.org/10.1017/s0074180900221256.

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The advent of long-baseline optical and infrared interferometers has meant that spatially resolved studies of stellar atmospheres have now become routinely possible. While prototype arrays, which have typically operated with short baselines and limited sensitivity, have produced exciting preliminary results, it is the development of larger dedicated facility arrays, such as the CHARA, Keck, and VLT interferometers, that offer the best prospects for advancing astrophysics. In this paper I review the possibilities and limitations of interferometric studies of stellar atmospheres, and highlight s

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33

Hartkopf, William I. "Twenty Years of Speckle Interferometry." International Astronomical Union Colloquium 135 (1992): 459–68. http://dx.doi.org/10.1017/s0252921100006977.

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The purpose of my talk is to briefly review the results of two decades of astrometric research using the technique of speckle interferometry. Although speckle, invented by Labeyrie in 1970 (Gezari et al. 1972), is the most well–known and widely–used interferometric technique in the visible and near infra-red, it neither the only technique in use, nor was it the first. Karl Schwarzschild made the first interferometric measurements of binary stars in 1895, using the then–new technique of Michelson interferometry and following a suggestion by Michelson himself that his technique was amenable to b

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34

Hou, X. X., G. M. Huang, and Z. Zhao. "Extracting DEM from airborne X-band data based on PolInSAR." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XL-7/W4 (June 26, 2015): 35–39. http://dx.doi.org/10.5194/isprsarchives-xl-7-w4-35-2015.

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Polarimetric Interferometric Synthetic Aperture Radar (PolInSAR) is a new trend of SAR remote sensing technology which combined polarized multichannel information and Interferometric information. It is of great significance for extracting DEM in some regions with low precision of DEM such as vegetation coverage area and building concentrated area. In this paper we describe our experiments with high-resolution X-band full Polarimetric SAR data acquired by a dual-baseline interferometric airborne SAR system over an area of Danling in southern China. Pauli algorithm is used to generate the double

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35

Chen, Zhenkai, Wenjing Zhou, Yingjie Yu, Vivi Tornari, and Gilberto Artioli. "Defect Isolation from Whole to Local Field Separation in Complex Interferometry Fringe Patterns through Development of Weighted Least-Squares Algorithm." Digital 4, no. 1 (2023): 104–13. http://dx.doi.org/10.3390/digital4010004.

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In this paper, based on Gaussian 1σ-criterion and histogram segmentation, a weighted least-squares algorithm is applied and validated on digital holographic speckle pattern interferometric data to perform phase separation on the complex interference fields. The direct structural diagnosis tool is used to investigate defects and their impact on a complex antique wall painting of Giotto. The interferometry data is acquired with a portable off-axis interferometer set-up with a phase-shifted reference beam coupled with the object beam in front of the digital photosensitive medium. A digital hologr

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36

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 astro

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37

Marklund, O., and L. Gustafsson. "Interferometry-based measurements of oil-film thickness." Proceedings of the Institution of Mechanical Engineers, Part J: Journal of Engineering Tribology 215, no. 3 (2001): 243–59. http://dx.doi.org/10.1243/1350650011543510.

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Measurement of the thickness of thin lubricant films separating rotating surfaces in elastohydrodynamic experiments presents some challenging problems. The nature of the experimental apparatus inhibits the use of most commonly applied interferometric phase measurement methods. Also the absolute thickness of the separating film must be determined, as opposed to relative distances that would be sufficient in most other measurement scenarios where interferometry methods are used. In this paper, computer-based analysis of interferograms recorded using an elastohydrodynamic lubrication Fitzeu inter

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38

Sweedler, Jonathan V., Rafi D. Jalkian, Gary R. Sims, and M. Bonner Denton. "Crossed Interferometric Dispersive Spectroscopy." Applied Spectroscopy 44, no. 1 (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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39

Simon, R. S., K. J. Johnston, D. Mozurkewich, et al. "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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40

Yang, Yichao, Kohei Yamamoto, Victor Huarcaya, et al. "Single-Element Dual-Interferometer for Precision Inertial Sensing." Sensors 20, no. 17 (2020): 4986. http://dx.doi.org/10.3390/s20174986.

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Tracking moving masses in several degrees of freedom with high precision and large dynamic range is a central aspect in many current and future gravitational physics experiments. Laser interferometers have been established as one of the tools of choice for such measurement schemes. Using sinusoidal phase modulation homodyne interferometry allows a drastic reduction of the complexity of the optical setup, a key limitation of multi-channel interferometry. By shifting the complexity of the setup to the signal processing stage, these methods enable devices with a size and weight not feasible using

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41

Fiorucci, D., A. Fassina, and M. La Matina. "Feasibility study of an enhanced heterodyne dispersion interferometer." Journal of Instrumentation 18, no. 02 (2023): C02057. http://dx.doi.org/10.1088/1748-0221/18/02/c02057.

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Abstract Interferometry is the commonly exploited technique for electron density measurements in magnetically confined fusion plasma experiments. Reliable electron density measurements are fundamental both for machine protection and for plasma physics understanding. In the last years, attention was drawn on the dispersion interferometer concept, because of its robustness and simplicity. Nevertheless, the heterodyne version of this configuration, which has several advantages over the homodyne scheme, loses one of the main benefits of the dispersion interferometer technique, that is its inherent

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42

Crosetto, M., O. Monserrat, N. Devanthéry, M. Cuevas-González, A. Barra, and B. Crippa. "PERSISTENT SCATTERER INTERFEROMETRY USING SENTINEL-1 DATA." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLI-B7 (June 22, 2016): 835–39. http://dx.doi.org/10.5194/isprs-archives-xli-b7-835-2016.

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This paper is focused on deformation monitoring using a Persistent Scatterer Interferometry technique and the interferometric SAR data acquired by the Sentinel-1 satellite of the European Space Agency. The first part of the paper describes the procedure used to process and analyze Sentinel-1 interferometric SAR data. Two main approaches are described. The first one is a simplified Persistent Scatterer Interferometry approach that exploits two key properties of the Sentinel-1 data: the high coherence of the 12-day interferograms and the reduced orbital tube. The second approach is a full Persis

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43

Crosetto, M., O. Monserrat, N. Devanthéry, M. Cuevas-González, A. Barra, and B. Crippa. "PERSISTENT SCATTERER INTERFEROMETRY USING SENTINEL-1 DATA." ISPRS - International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XLI-B7 (June 22, 2016): 835–39. http://dx.doi.org/10.5194/isprsarchives-xli-b7-835-2016.

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This paper is focused on deformation monitoring using a Persistent Scatterer Interferometry technique and the interferometric SAR data acquired by the Sentinel-1 satellite of the European Space Agency. The first part of the paper describes the procedure used to process and analyze Sentinel-1 interferometric SAR data. Two main approaches are described. The first one is a simplified Persistent Scatterer Interferometry approach that exploits two key properties of the Sentinel-1 data: the high coherence of the 12-day interferograms and the reduced orbital tube. The second approach is a full Persis

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44

Armstrong, J. T. "Sub-Milliarcsecond Optical Astrometry and Binary Stars." Symposium - International Astronomical Union 166 (1995): 193–202. http://dx.doi.org/10.1017/s0074180900228064.

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Long-baseline optical interferometry has made it possible to measure the visual orbits of binary stars with major axes as small as 5 mas and errors of ≲ 100 μas. Interferometers now nearing completion will extend these values to ≳ 500 μas and σa ∼ 10 μas. Observations of double-lined spectroscopic binaries with current interferometers have already yielded some mass estimates with precisions rivaling those from fitting the light curves of eclipsing double-lined systems. Luminosity estimates based on combined visual interferometric observations and velocity curves are often more precise than tho

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45

Hoque, Nabil Md Rakinul, and Lingze Duan. "Impact of Soil-Based Insulation on Ultrahigh-Resolution Fiber-Optic Interferometry." Sensors 23, no. 1 (2022): 259. http://dx.doi.org/10.3390/s23010259.

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High resolution optical interferometry often requires thermal and acoustic insultation to reduce and remove environment-induced fluctuations. Broader applications of interferometric optical sensors in the future call for low-cost materials with both low thermal diffusivity and good soundproofing capability. In this paper, we explore the feasibility and effectiveness of natural soil as an insulation material for ultrahigh-resolution fiber-optic interferometry. An insulation chamber surrounded by soil is constructed, and its impact on the noise reduction of a Mach-Zehnder Fabry-Perot hybrid fibe

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46

Kovačević, Andjelka B., Yu-Yang Songsheng, Jian-Min Wang, and Luka Č. Popović. "Probing the elliptical orbital configuration of the close binary of supermassive black holes with differential interferometry." Astronomy & Astrophysics 644 (December 2020): A88. http://dx.doi.org/10.1051/0004-6361/202038733.

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Context. Obtaining detections of electromagnetic signatures from the close binaries of supermassive black holes (CB-SMBH) is still a great observational challenge. The Very Large Telescope Interferometer (VLTI) and the Extremely Large Telescope (ELT) will serve as a robust astrophysics suite offering the opportunity to probe the structure and dynamics of CB-SMBH at a high spectral and angular resolution. Aims. Here, we explore and illustrate the application of differential interferometry on unresolved CB-SMBH systems in elliptical orbital configurations. We also investigate certain peculiariti

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47

Kolkiran, Aziz. "High-NOON States with High Flux of Photons Using Coherent Beam Stimulated Noncollinear Parametric Down Conversion." International Journal of Optics 2019 (December 30, 2019): 1–7. http://dx.doi.org/10.1155/2019/6871979.

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We show how to reach high fidelity NOON states with a high count rate inside optical interferometers. Previously, it has been shown that by mixing squeezed and coherent light at a beam splitter, it is possible to generate NOON states of arbitrary N with a fidelity as high as 94%. The scheme is based on higher-order interference between “quantum” down-converted light and “classical” coherent light. However, this requires optimizing the amplitude ratio of classical to quantum light, thereby limiting the overall count rate for the interferometric super-resolution signal. We propose using coherent

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48

Vasconcelos, Ivan, Roel Snieder, and Brian Hornby. "Imaging internal multiples from subsalt VSP data — Examples of target-oriented interferometry." GEOPHYSICS 73, no. 4 (2008): S157—S168. http://dx.doi.org/10.1190/1.2944168.

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Seismic interferometry has become a technology of growing interest for imaging borehole seismic data. We demonstrate that interferometry of internal multiples can be used to image targets above a borehole receiver array. By internal multiples, we refer to all types of waves that scatter multiple times inside the model. These include, for instance, interbed, intrasalt, and water-bottom multiples as well as conversions among them. We use an interferometry technique that is based on representation theorems for perturbed media and targets the reconstruction of specific primary reflections from mul

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49

Pringkasemchai, A., J. Wongsaroj, and K. Mongkolsuttirat. "Determination of phase change correction on gauge block measurement in two different interferometric measurement systems." Journal of Physics: Conference Series 2431, no. 1 (2023): 012012. http://dx.doi.org/10.1088/1742-6596/2431/1/012012.

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Abstract Phase change correction (PCC) is an important correction value of the end effect in an optical interferometry system. Normally, this value is used to compensate for gauge block measurement by an optical interferometry system based on ISO 3650:1998. Two different interferometric measurement systems in terms of fringe fraction measurement were performed to determine the phase change correction by a five-stacking method. These results are used to determine the length measurement of gauge blocks in an optical interferometer technique and consequently, to evaluate the uncertainty of gauge

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50

McAlister, H. A. "The Potential of Long–Baseline Optical Interferometry of Binary Stars." International Astronomical Union Colloquium 135 (1992): 527–35. http://dx.doi.org/10.1017/s0252921100007053.

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AbstractInterferometric arrays possessing sub-milliarcsecond resolution are either about to be fully scientifically productive, as in the case of the Sydney University Stellar Interferometer, or are under various stages of planning and development. The 1990’s will thus witness a hundred–fold gain in resolution over speckle interferometry at the largest telescopes and 5,000 times the resolution of classical direct imaging. Where speckle interferometry can now resolve binary stars with periods of 1 to 2 years, interferometric arrays with baselines of hundreds of meters will resolve binaries with

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