Bibliographies thématiques / Interferometric detector

Littérature scientifique sur le sujet « Interferometric detector »

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Publié le 11 mars 2023

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Articles de revues sur le sujet "Interferometric detector"

Heurs, M. « Gravitational wave detection using laser interferometry beyond the standard quantum limit ». Philosophical Transactions of the Royal Society A : Mathematical, Physical and Engineering Sciences 376, n^o 2120 (16 avril 2018) : 20170289. http://dx.doi.org/10.1098/rsta.2017.0289.

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Interferometric gravitational wave detectors (such as advanced LIGO) employ high-power solid-state lasers to maximize their detection sensitivity and hence their reach into the universe. These sophisticated light sources are ultra-stabilized with regard to output power, emission frequency and beam geometry; this is crucial to obtain low detector noise. However, even when all laser noise is reduced as far as technically possible, unavoidable quantum noise of the laser still remains. This is a consequence of the Heisenberg Uncertainty Principle, the basis of quantum mechanics: in this case, it is fundamentally impossible to simultaneously reduce both the phase noise and the amplitude noise of a laser to arbitrarily low levels. This fact manifests in the detector noise budget as two distinct noise sources—photon shot noise and quantum radiation pressure noise—which together form a lower boundary for current-day gravitational wave detector sensitivities, the standard quantum limit of interferometry. To overcome this limit, various techniques are being proposed, among them different uses of non-classical light and alternative interferometer topologies. This article explains how quantum noise enters and manifests in an interferometric gravitational wave detector, and gives an overview of some of the schemes proposed to overcome this seemingly fundamental limitation, all aimed at the goal of higher gravitational wave event detection rates. This article is part of a discussion meeting issue ‘The promises of gravitational-wave astronomy’.

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

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

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Chou, Chien, Hui-Kang Teng, Chien-Chung Tsai et Li-Ping Yu. « Balanced detector interferometric ellipsometer ». Journal of the Optical Society of America A 23, n^o 11 (1 novembre 2006) : 2871. http://dx.doi.org/10.1364/josaa.23.002871.

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Rowan, Sheila. « Current and future status of gravitational wave astronomy - gravitational wave facilities ». Proceedings of the International Astronomical Union 2, n^o 14 (août 2006) : 526–27. http://dx.doi.org/10.1017/s1743921307011684.

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AbstractCurrently a network of interferometric gravitational wave detectors is in operation around the globe, in parallel with existing acoustic bar-type detectors. Searches are underway aimed at the first direct detection of gravitational radiation from astrophysical sources. This paper briefly summarizes the current status of operating gravitational wave facilities, plans for future detector upgrades, and the status of the planned space-based gravitational wave detector LISA.

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Trott, Cathryn M., Randall B. Wayth, Jean-Pierre R. Macquart et Steven J. Tingay. « Source Detection with Interferometric Datasets ». Proceedings of the International Astronomical Union 7, S285 (septembre 2011) : 414–16. http://dx.doi.org/10.1017/s1743921312001263.

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AbstractThe detection of sources in interferometric radio data typically relies on extracting information from images, formed by Fourier transform of the underlying visibility dataset, and CLEANed of contaminating sidelobes through iterative deconvolution. Variable and transient radio sources span a large range of variability timescales, and their study has the potential to enhance our knowledge of the dynamic universe. Their detection and classification involve large data rates and non-stationary PSFs, commensal observing programs and ambitious science goals, and will demand a paradigm shift in the deployment of next-generation instruments. Optimal source detection and classification in real time requires efficient and automated algorithms. On short time-scales variability can be probed with an optimal matched filter detector applied directly to the visibility dataset. This paper shows the design of such a detector, and some preliminary detection performance results.

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Mazilu, M., P. J. Phillips et A. Miller. « Interferometric Hetero-Detector Phase Measurement ». Optical and Quantum Electronics 36, n^o 5 (avril 2004) : 431–42. http://dx.doi.org/10.1023/b:oqel.0000022997.34800.89.

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Prado, A. R. C., F. S. Bortoli, N. S. Magalhaes, R. N. Duarte, C. Frajuca et R. C. Souza. « Obtaining the sensitivity of a calibrator for interferometric gravitational wave ». Journal of Physics : Conference Series 2090, n^o 1 (1 novembre 2021) : 012158. http://dx.doi.org/10.1088/1742-6596/2090/1/012158.

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Abstract Interferometric gravitational wave detectors (IGWD) are a very complex detector, the need to lock the detector in a dark fringe condition besides the vibrations that affect the mirrors, creates the necessity of using active suspension systems. These active systems make the system reach the desired sensitivity but make the calibration of such detectors much more difficult. To solve this problem a calibrator is proposed, a resonant mass gravitational wave detector could be used to detect the same signal in a narrower band and use the measured amplitude to calibrate the IGWD, as resonant mass gravitational wave detectors are easily calibrated. This work aims to obtain the expected sensitivity of such a calibrator by using lumped modelling in such mechanical detectors. The calibrator is modelled as a spring mass system and the sensitivity curve is presented calculated in by a matlab program. The curve shows that using state of art parameters for the detector the final sensitivity is close to the quantum limit and can be used to calibrate the IGWDs.

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Pai, Archana. « Gravitational Waves in an Interferometric Detector ». Current Science 112, n^o 07 (1 avril 2017) : 1353. http://dx.doi.org/10.18520/cs/v112/i07/1353-1360.

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Prado, A. R. C., F. S. Bortoli, N. S. Magalhaes, R. N. Duarte, C. Frajuca et R. C. Souza. « Modelling a mechanical antenna for a calibrator for interferometric gravitational wave detector using finite elements method ». Journal of Physics : Conference Series 2090, n^o 1 (1 novembre 2021) : 012157. http://dx.doi.org/10.1088/1742-6596/2090/1/012157.

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Abstract Interferometric gravitational wave detectors (IGWD) are a very complex detector, the need to lock the detector in a dark fringe condition besides the vibrations that affect the mirrors, creates the necessity of using active suspension systems. These active systems make the system reach the desired sensitivity but make the calibration of such detectors much more difficult. To solve this problem a calibrator is proposed, a resonant mass gravitational wave detector could be used to detect the same signal in a narrower band and use the measured amplitude to calibrate the IGWD, as resonant mass gravitational wave detectors are easily calibrated. This work aims to design the mechanical antenna of such a calibrator. The main difficulty is to design the calibrator is the frequencies required to make the detection. These massive detectors usually were made in frequencies close to 1 kHz and the frequency range to operate for better sensitivity is around 100 Hz. The antenna is modelled in finite elements method and a design of such an antenna is presented.

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Fritschel, Peter, Nergis Mavalvala, David Shoemaker, Daniel Sigg, Michael Zucker et Gabriela González. « Alignment of an interferometric gravitational wave detector ». Applied Optics 37, n^o 28 (1 octobre 1998) : 6734. http://dx.doi.org/10.1364/ao.37.006734.

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Thèses sur le sujet "Interferometric detector"

Casanueva, Diaz Julia. « Control of the gravitational wave interferometric detector Advanced Virgo ». Thesis, Université Paris-Saclay (ComUE), 2017. http://www.theses.fr/2017SACLS209/document.

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La première détection d'une Onde Gravitationnelle (OG) a été faite le 14 Septembre 2015 par la collaboration LIGO-Virgo avec les deux détecteurs de LIGO. Elle a été émise par la fusion de deux Trous Noirs, fournissant ainsi la première preuve directe de l’existence des Trous Noirs. Advanced Virgo est la version améliorée de l’interféromètre Virgo et il va rejoindre les détecteurs LIGO dans les mois qui suivent. Le passage d'une OG induit un changement différentiel de la distance entre masses-test (uniquement sensibles à la force gravitationnelle). Cette variation de distance est proportionnelle à l'amplitude de l'OG, néanmoins le déplacement le plus grand qui peut être observé depuis la Terre est de l'ordre de 10⁻¹⁹ m/sqrt(Hz) en terme de densité spectrale. C'est pour cela que l’interféromètre de Michelson est l'instrument idéal pour détecter cet effet différentiel. Les détecteurs d’OG utilisent des miroirs suspendus, qui se comportent comme masses-test. Le passage d'une OG va produire un changement dans la distance entre les miroirs qui va modifier la condition d’interférence et donc une variation de puissance lumineuse mesurée par la photodiode de détection. Cependant, un Michelson simple n'est pas assez sensible et des améliorations ont été ajoutées. La première génération de détecteurs a ajouté des cavités Fabry-Pérot dans les bras pour augmenter le chemin optique. De plus un nouveau miroir a été ajouté pour recirculer la lumière réfléchie vers le laser et augmenter la puissance effective, en créant une nouvelle cavité connue comme Power Recycling Cavity (PRC). Son effet est d’autant plus important que le Michelson est en fait optimalement réglé sur une frange noire. Tous les miroirs du détecteur ressentent le bruit sismique et les longueurs des cavités, entre autres, changent en permanence. Il est donc nécessaire de contrôler activement la position longitudinale et angulaire des cavités pour les maintenir en résonance. Pendant ma thèse j'ai étudié le contrôle de Advanced Virgo d’abord en simulation puis pendant le commissioning lui-même. D'abord j'ai simulé la stratégie de contrôle utilisée dans Virgo avec des simulations modales. L'objectif était de vérifier si la même stratégie pouvait être appliquée à Advanced Virgo ou s'il fallait l'adapter. Avec Advanced Virgo les cavités Fabry-Pérot ont une finesse plus grande ce qui entraîne de nouveaux effets dynamiques et qui demande une stratégie de contrôle spéciale, stratégie que j'ai modifiée pour l'adapter aux besoins du commissioning. Concernant la PRC, j’ai étudié l'impact de sa stabilité dans le fonctionnement de l’interféromètre. Comme elle est très proche de la région d’instabilité, l’onde lumineuse être très sensible à l'alignement et a l'adaptation du faisceau à la cavité. J’ai vérifié avec les simulations son impact sur les contrôles longitudinaux, qui peuvent devenir instables, et une solution a été validée. Ensuite j'ai utilisé cette information pour le commissioning d'Advanced Virgo. Dans cette thèse les détails du commissioning des contrôles longitudinal et angulaire de l’interféromètre sont présentés. La stabilisation en fréquence est aussi présentée, puisqu'elle joue un rôle très important dans le contrôle de l’interféromètre car étant le bruit dominant
The first detection of a Gravitational Wave (GW) was done on September 14 th of 2015 by the LIGO-Virgo collaboration with the two LIGO detectors. It was emitted by the merger of a Binary Black Hole, providing the first direct proof of the existence of Black Holes. Advanced Virgo is the upgraded version of the Virgo interferometer and it will join the LIGO detectors in the next months. The passage of a GW on Earth induces a change on the distance between test masses (experiencing only the gravitational interaction) in a differential way. This distance variation is proportional to the amplitude of the GW however the largest displacement observable on Earth will be of the order of 10⁻¹⁹ m/sqrt(Hz). Taking this in account, a Michelson interferometer is the ideal instrument to detect this differential effect. GWs detectors will use suspended mirrors to behave as test masses. The passage of a GW will cause a change on the distance between the mirrors that will spoil the interference condition, allowing some light to leak to the detection photodiode. However, a simple Michelson interferometer does not provide enough sensitivity. For this reason the first generation of detectors added Fabry-Perot cavities in the arms, in order to increase the optical path. A second change was the addition of an extra mirror in order to recycle the light that comes back towards the laser, to increase the effective power, creating a new cavity also known as Power Recycling Cavity (PRC). Its effect is more important when the Michelson is tuned in an optimal way in a dark fringe. All the mirrors of the detector are affected by the seismic noise and so their distance is continuously changing. It is necessary to control the longitudinal and angular position of the cavities in order to keep them at resonance. During my thesis I have studied the control of Advanced Virgo using simulation and during the commissioning itself. First of all I have simulated the control strategy used in Virgo using modal simulations. The aim was to check if the same strategy could be applied to Advanced Virgo or if it needs adaptation. In Advanced Virgo the Fabry-Perot cavities have a higher finesse, which arises new dynamical problems and requires a special control strategy that I have modified to match the commissioning needs. Regarding the PRC, we have studied the impact of its stability on the performance of the interferometer. As it is very close from the instability region, the electrical field inside will be very sensitive to alignment and matching of the laser beam. We have checked using simulations its impact on the longitudinal controls, which can become unstable, and a solution has been validated. Then I have used this information during the commissioning of the Advanced Virgo detector. In this thesis the details of the commissioning of the longitudinal and angular control of the interferometer will be presented. It includes the frequency stabilization, which has a key role in the control of the interferometer, since it is the dominant noise

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Nishizawa, Atsushi, Seiji Kawamura, Tomotada Akutsu, Koji Arai, Kazuhiro Yamamoto, Daisuke Tatsumi, Erina Nishida et al. « Laser-interferometric detectors for gravitational wave backgrounds at 100 MHz : Detector design and sensitivity ». American Physical Society, 2008. http://hdl.handle.net/2237/11308.

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Tripp, Everett. « Interferometric Optical Readout System for a MEMS Infrared Imaging Detector ». Digital WPI, 2012. https://digitalcommons.wpi.edu/etd-theses/222.

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MEMS technology has led to the development of new uncooled infrared imaging detectors. One type of these MEMS detectors consist of arrays of bi-metallic photomechanical pixels that tilt as a function of temperature associated with infrared radiation from the scene. The main advantage of these detectors is the optical readout system that measures the tilt of the beams based on the intensity of the reflected light. This removes the need for electronic readout at each of the sensing elements and reduces the fabrication cost and complexity of sensor design, as well as eliminates the electronic noise at the detector. The optical readout accuracy is sensitive to the uniformity of individual pixels on the array. The hypothesis of the present research is that direct measurements of the height change corresponding to tilt through holographic interferometry will reduce the need for high pixel uniformity. Measurements of displacements for a vacuum packaged detector with nominal responsivity of 2.4nm/K are made with a Linnik interferometer employing the four phase step technique. The interferometer can measure real-time, full-field height variations across the array. In double-exposure mode, the current height map is subtracted from a reference image so that the change in deflection is measured. A software algorithm locates each mirror on the array, extracts the measured deflection at the tip of a mirror, and uses that measurement to form a pixel of a thermogram in real-time. A blackbody target projector with temperature controllable to 0.001K is used to test the thermal resolution of the imaging system. The achieved minimum temperature resolution is better than 0.25K. The double exposure technique removes mirror non-uniformity as a source of noise. A lower than nominal measured responsivity of around 1.5nm/K combined with noise from the measurements made with the interferometric optical readout system limit the potential minimum temperature resolution. Improvements need to be made both in the holographic setup and in the MEMS detector to achieve the target temperature resolution of 0.10K.

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Regehr, Martin W. Drever Ronald W. P. Drever Ronald W. P. Yariv Amnon Raab Frederick J. « Signal extraction and control for an interferometric gravitational wave detector / ». Diss., Pasadena, Calif. : California Institute of Technology, 1995. http://resolver.caltech.edu/CaltechETD:etd-10192007-092215.

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Gossler, Stefan. « The suspension systems of the interferometric gravitational-wave detector GEO 600 ». [S.l. : s.n.], 2004. http://deposit.ddb.de/cgi-bin/dokserv?idn=972116710.

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Kerr, G. A. « Experimental developments towards a long-baseline laser interferometric gravitational radiation detector ». Thesis, University of Glasgow, 1986. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.378181.

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Tröbs, Michael. « Laser development and stabilization for the spaceborne interferometric gravitational wave detector LISA ». [S.l. : s.n.], 2005. http://deposit.ddb.de/cgi-bin/dokserv?idn=974983705.

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Hughes, Roy John. « The application of array detector technology to interferometric spectroscopy : design, analysis and development ». Thesis, Queensland University of Technology, 1994.

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Gras, Slawomir M. « Opto-acoustic interactions in high power interferometric gravitational wave detectors ». University of Western Australia. School of Physics, 2009. http://theses.library.uwa.edu.au/adt-WU2010.0093.

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[Truncated abstract] Advanced laser interferometer gravitational wave detectors require an extremely high optical power in order to improve the coupling between the gravitational wave signal and the optical field. This high power requirement leads to new physical phenomena arising from nonlinear interactions associated with radiation pressure. In particular, detectors with multi-kilometer-long arm cavities containing high density optical fields suffer the possibility of 3-mode opto-acoustic interactions. This involves the process where ultrasonic vibrations of the test mass cause the steady state optical modes to scatter. These 3-mode interactions induce transverse optical modes in the arm cavities, which then can provide positive feedback to the acoustic vibrations in the test masses. This may result in the exponential growth of many acoustic mode amplitudes, known as Parametric Instability (PI). This thesis describes research on 3-mode opto-acoustic interactions in advanced interferometric gravitational wave detectors through numerical investigations of these interactions for various interferometer configurations. Detailed analysis reveals the properties of opto-acoustic interactions, and their dependence on the interferometer configuration. This thesis is designed to provide a pathway towards a tool for the analysis of the parametric instabilities in the next generation interferometers. Possible techniques which could be helpful in the design of control schemes to mitigate this undesirable phenomenon are also discussed. The first predictions of parametric instability considered only single interactions involving one transverse mode and one acoustic mode in a simple optical cavity. ... In Chapter 6, I was able to make use of a new analytical model due to Strigin et al., which describes parametric instability in dual recycling interferometers. To make the solution tractable, it was necessary to consider two extreme cases. In the worst case, recycling cavities are assumed to be resonant for all transverse modes, whereas in the best cases, both recycling cavities are anti-resonant for the transverse modes. Results show that, for the worst case, parametric gain values as high as ~1000 can be expected, while in the best case the gain can be as low as ~ 3. The gain is shown to be very sensitive to the precise conditions of the interferometer, emphasising the importance of understanding the behaviour of the detectors when the cavity locking deviates from ideal conditions. Chapter 7 of this thesis contains work on the observation of 3-mode interactions in an optical cavity at Gingin, which confirms the analysis presented here, and also a paper which shows how the problem of 3-mode interactions can be harnessed to create new devices called opto-acoustic parametric amplifiers. In the conclusions in Chapter 8, I discuss the next important steps in understanding parametric interactions in real interferometers including the need for more automated codes relevant to the design requirements for recycling cavities. In particular, it is pointed out how the modal structure of power and signal recycling cavities must be understood in detail, including the Gouy phase for each transverse mode, to be able to obtain precise predictions of parametric gain. This thesis is organised as a series of papers which are published or have been submitted for publication. Such writing style fills the condition for Ph.D. thesis at the University of Western Australia.

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BADARACCO, FRANCESCA. « Newtonian Noise studies in 2nd and 3rd generation gravitational-wave interferometric detectors ». Doctoral thesis, Gran Sasso Science Institute, 2021. http://hdl.handle.net/20.500.12571/16065.

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This thesis work fits in the Newtonian noise (NN) cancellation framework for gravitational-wave (GW) detectors of 2nd and 3rd generation. At frequencies below 20 Hz the NN affects GW detectors by generating gravity gradients that mask the GW signals that we want to measure. My work can be divided in three main tasks: the optimization of a seismic array for the NN cancellation in underground detectors, the optimization of a seismic array for Advanced Virgo + (which, respect to the former one, relied on seismic measurements and not on a seismic model) and the evaluation of the NN and the seismic field at the KAGRA site. I will briefly summarize in the following the main results of these three works. In the first work I performed a global optimization for finding the optimal locations of an array of sensors for the NN cancellation for underground detectors. Since we need to search for the optimal positions of N sensors in a 3D space, the computational efforts required are very demanding. At the present time, seismic correlations in the relevant frequency band for ET from 3Hz to 20Hz are not available. So we modelled the seismic field as isotropic and homogeneous. With this work I was able to assess the feasibility of applying active NN reduction in underground detectors and reaching a factor 10 of noise reduction with 15 sensors at 10 Hz. In 2019 this work was published. The second work I made during my PhD was conceptually similar to the previous one but very different in the approach used to solve it. Exploiting a theoretical model in Virgo was not an option given its complicated structure. I then used Virgo's seismic data to run the optimization of sensor locations. The main challenge here was that I had to perform a gaussian process regression over a 4D space, and not enough data were available for this purpose. I found a way to bypass the regression over the 4D space by exploiting the convolution theorem. This allowed me to perform the regression over a space with reduced dimension, i.e., in 2D. The global optimization algorithm was then run hundreds of times in order to statistically prove the global minimum, exactly as done in the work for the underground optimization. The results proved that with 15 seismometers we can reach a noise reduction factor of 3-7, which is enough for the aimed sensitivity of the next observing runs. The results of this work were then used to set the array that will be used to cancel the NN in Advanced Virgo +. This work has been published in 2020. This approach could also be useful in future, where it will be needed to optimize underground seismic arrays with real seismic data. Finally, in the third work I used seismic data collected in the Kamioka mine (where the gravitational-wave detector KAGRA is hosted) to investigate the seismic noise caused by the infrastructure and to calculate a NN budget. These are important aspects that need to be investigated in view of the 3rd generation GW detector Einstein Telescope. The data indicated that the infrastructure noise starts to be important well above 10 Hz, where the NN loses its impact on the detector and where the seismic isolation system is capable of killing the noise. Moreover, I used the data from three seismometers to perform a beamforming analysis and find the seismic velocities and the seismic wave main directions. The extracted values were then used as a reference for the estimation of the NN budget. For completeness, I also estimated the NN budget coming from surface Rayleigh waves. This was made by exploiting the data of the F-net network, in Japan. I then showed that the NN from surface and body waves can be neglected for KAGRA.

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Livres sur le sujet "Interferometric detector"

Casanueva Diaz, Julia. Control of the Gravitational Wave Interferometric Detector Advanced Virgo. Cham : Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96014-2.

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Eric, Udd, Tatam Ralph P, Society of Photo-optical Instrumentation Engineers. Poland Chapter., Politechnika Warszawska et Foundation for Promotion and Development of Optical Techniques (Poland), dir. 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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Fundamentals of interferometric gravitational wave detectors. Singapore : World Scientific, 1994.

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Nguyen, Cam. Theory, analysis and design of RF interferometric sensors. New York : Springer, 2012.

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Center, NASA Glenn Research, dir. Damage detection using holography and interferometry. Cleveland, Ohio : National Aeronautics and Space Administration, Glenn Research Center, 2003.

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Decker, Arthur J. Damage detection using holography and interferometry. Cleveland, Ohio : National Aeronautics and Space Administration, Glenn Research Center, 2003.

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Gilbreath, G. Charmaine, et Chadwick T. Hawley. Active and passive signatures : 8-9 April 2010, Orlando, Florida, United States. Bellingham, Wash : SPIE, 2010.

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Gilbreath, G. Charmaine, et Chadwick T. Hawley. Active and passive signatures III : 25-26 April 2012, Baltimore, Maryland, United States. Bellingham, Washington : SPIE, 2012.

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Gilbreath, G. Charmaine, et Chadwick T. Hawley. Active and passive signatures II : 27-28 April 2011, Orlando, Florida, United States. Sous la direction de SPIE (Society). Bellingham, Wash : SPIE, 2011.

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Cho, Y. C. Fiber-optic interferometric sensors for measurements of pressure fluctuations : Experimental evaluation. Moffett Field, Calif : National Aeronautics and Space Administration, Ames Research Center, 1993.

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Chapitres de livres sur le sujet "Interferometric detector"

Giazotto, A., et S. Braccini. « VIRGO : An Interferometric Detector of Gravitational Waves ». Dans Recent Developments in General Relativity, Genoa 2000, 111–19. Milano : Springer Milan, 2002. http://dx.doi.org/10.1007/978-88-470-2101-3_8.

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Andersen, Michael I., et Anton Norup Sørensen. « An Interferometric Method for Measurement of the Detector MTF ». Dans Optical Detectors for Astronomy, 187–90. Dordrecht : Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-5262-4_28.

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Casanueva Diaz, Julia. « Introduction ». Dans Control of the Gravitational Wave Interferometric Detector Advanced Virgo, 1–5. Cham : Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96014-2_1.

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Casanueva Diaz, Julia. « Gravitational Waves ». Dans Control of the Gravitational Wave Interferometric Detector Advanced Virgo, 7–14. Cham : Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96014-2_2.

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Casanueva Diaz, Julia. « Ground Based Gravitational Wave Detectors ». Dans Control of the Gravitational Wave Interferometric Detector Advanced Virgo, 15–26. Cham : Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96014-2_3.

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Casanueva Diaz, Julia. « Advanced Virgo ». Dans Control of the Gravitational Wave Interferometric Detector Advanced Virgo, 27–35. Cham : Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96014-2_4.

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Casanueva Diaz, Julia. « Fabry-Perot Cavities in Advanced Virgo ». Dans Control of the Gravitational Wave Interferometric Detector Advanced Virgo, 37–83. Cham : Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96014-2_5.

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Casanueva Diaz, Julia. « Power Recycled Interferometer ». Dans Control of the Gravitational Wave Interferometric Detector Advanced Virgo, 85–134. Cham : Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96014-2_6.

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Casanueva Diaz, Julia. « Advanced Virgo Commissioning ». Dans Control of the Gravitational Wave Interferometric Detector Advanced Virgo, 135–98. Cham : Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96014-2_7.

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Casanueva Diaz, Julia. « Conclusion ». Dans Control of the Gravitational Wave Interferometric Detector Advanced Virgo, 199–202. Cham : Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-96014-2_8.

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Actes de conférences sur le sujet "Interferometric detector"

Hodges, Steven E., Mark T. Kern et Kwangjai Park. « An Interferometric Thermal Detector ». Dans SPIE 1989 Technical Symposium on Aerospace Sensing, sous la direction de Eustace L. Dereniak et Robert E. Sampson. SPIE, 1989. http://dx.doi.org/10.1117/12.960661.

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MIO, NOIKATSU. « INTERFEROMETRIC GRAVITATIONAL WAVE DETECTOR IN JAPAN ». Dans Proceedings of the 7th International Symposium. WORLD SCIENTIFIC, 2002. http://dx.doi.org/10.1142/9789812776716_0053.

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Robertson, N. A. « GEO 600 - A Laser Interferometric Gravitational Wave Detector ». Dans The European Conference on Lasers and Electro-Optics. Washington, D.C. : Optica Publishing Group, 1998. http://dx.doi.org/10.1364/cleo_europe.1998.cfd3.

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To search for gravitational waves from astrophysical sources, GEO 600 will use laser interferometry over a physical arm length of 600 m. The detector is currently being constructed in the North of Germany, near Hannover, by research groups from Hannover, Garching and Glasgow, with theoretical input from Cardiff and Potsdam. It will utilise a four pass delay line Michelson interferometer with power and signal recycling implemented to reduce the limitation to sensitivity set by photo-electron shot noise in the detector output. Illumination will be by single frequency Nd: YAG laser light at a level of 10 W, from a diode pumped slave laser, injection locked by a small monolithic diode pumped ring laser.

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Dykaar, Doug R. « Generation of Pulsed High Power Far Infrared Radiation ». Dans International Conference on Ultrafast Phenomena. Washington, D.C. : Optica Publishing Group, 1992. http://dx.doi.org/10.1364/up.1992.mc15.

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Using large aperture photoconductive switches(1) and interferometric detection(2), we have measured pulses of far infrared radiation (FIR) in excess of 100 nJ per pulse with pulse widths of 600 fs (FWHM). This is the most sub-picosecond FIR generated to date. Detection was accomplished using a pyroelectric detector(2).

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Crouzier, A., F. Malbet, F. Hénault, A. Léger, C. Cara, J. M. Le Duigou, O. Preis et al. « The latest results from DICE (Detector Interferometric Calibration Experiment) ». Dans SPIE Astronomical Telescopes + Instrumentation, sous la direction de Howard A. MacEwen, Giovanni G. Fazio, Makenzie Lystrup, Natalie Batalha, Nicholas Siegler et Edward C. Tong. SPIE, 2016. http://dx.doi.org/10.1117/12.2234304.

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Barone, Fabrizio, Umberto Bernini, M. Conti, Luciano DiFiore, Leopoldo Milano, G. Russo, Paolo Russo, Alberto Del Guerra et Mauro Gambaccini. « Test of a fiber optic interferometric x-ray detector ». Dans Fibers '92, sous la direction de Eric Udd et Ramon P. DePaula. SPIE, 1993. http://dx.doi.org/10.1117/12.141274.

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Larrategui, Martin Tangari, Jonathan D. Ellis et Thomas G. Brown. « Non-null interferometric surface figure testing beyond the detector pixel MTF cutoff spatial frequency limit ». Dans Frontiers in Optics. Washington, D.C. : Optica Publishing Group, 2022. http://dx.doi.org/10.1364/fio.2022.jw5a.90.

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We report a non-null interferometric surface figure measurement of a spherical mirror with slope departure angles mapping to interferogram spatial frequencies larger than the cutoff spatial frequency limit of a full-fill detector with 4.6 µm-pixels.

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RÜDIGER, ALBRECHT. « GEO 600 – A SHORT-ARM LASER-INTERFEROMETRIC GRAVITATIONAL-WAVE DETECTOR ». Dans Proceedings of the International Conference. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702999_0046.

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Acernese, F., P. Amico, M. Alshourbagy, F. Antonucci, S. Aoudia, P. Astone, S. Avino et al. « Data Acquisition System of the Virgo Gravitational Waves Interferometric Detector ». Dans 2007 15th IEEE-NPSS Real-Time Conference. IEEE, 2007. http://dx.doi.org/10.1109/rtc.2007.4382842.

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Stephenson, Gary V., et Glen A. Robertson. « Lessons for Energy Resonance HFGW Detector Designs from Mass Resonance and Interferometric LFGW Detectors ». Dans SPACE, PROPULSION & ENERGY SCIENCES INTERNATIONAL FORUM : SPESIF-2009. AIP, 2009. http://dx.doi.org/10.1063/1.3115562.

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Rapports d'organisations sur le sujet "Interferometric detector"

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

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Dudley, J. P., et S. V. Samsonov. SAR interferometry with the RADARSAT Constellation Mission. Natural Resources Canada/CMSS/Information Management, 2022. http://dx.doi.org/10.4095/329396.

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The RADARSAT Constellation Mission (RCM) is Canada's latest system of C-band Synthetic Aperture Radar (SAR) Earth observation satellites. The system of three satellites, spaced equally in a common orbit, allows for a rapid four-day repeat interval. The RCM has been designed with a selection of stripmap, spotlight, and ScanSAR beam modes which offer varied combinations of spatial resolution and coverage. Using Differential Interferometric Synthetic Aperture Radar (DInSAR) techniques, the growing archive of SAR data gathered by RCM can be used for change detection and ground deformation monitoring for diverse applications in Canada and around the world. In partnership with the Canadian Space Agency (CSA), the Canada Centre for Mapping and Earth Observation (CCMEO) has developed an automated system for generating standard and advanced deformation products and change detection from SAR data acquired by RCM and RADARSAT-2 satellites using DInSAR processing methodology. Using this system, this paper investigates four key interferometric properties of the RCM system which were not available on the RADARSAT-1 or RADARSAT-2 missions: The impact of the high temporal resolution of the four-day repeat cycle of the RCM on temporal decorrelation trends is tested and fitted against simple temporal decay models. The effect of the normalization and the precision of the radiometric calibration on interferometric spatial coherence is investigated. The performance of the RCM ScanSAR mode for wide area interferometric analysis is tested. The performance of the novel RCM Compact-polarization (CP) mode for interferometric analysis is also investigated.

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Dimopoulos, Savas, Peter W. Graham, Jason M. Hogan, Mark A. Kasevich et Surjeet Rajendran. Gravitational Wave Detection with Atom Interferometry. Office of Scientific and Technical Information (OSTI), janvier 2008. http://dx.doi.org/10.2172/922600.

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Fiedler, Curtis J. The Interferometric Detection of Ultrafast Pulses of Laser Generated Ultrasound. Fort Belvoir, VA : Defense Technical Information Center, avril 1996. http://dx.doi.org/10.21236/ada312079.

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Sorensen, K. W. Coherent change detection and interferometric ISAR measurements in the folded compact range. Office of Scientific and Technical Information (OSTI), août 1996. http://dx.doi.org/10.2172/400087.

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Yocky, David. Source Physics Experiment : Rock Valley Interferometric Synthetic Aperture RADAR Earthquake Detection Study. Office of Scientific and Technical Information (OSTI), septembre 2021. http://dx.doi.org/10.2172/1821315.

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Dudley, J. P., et S. V. Samsonov. Système de traitement automatisé du gouvernement canadien pour la détection des variations et l'analyse des déformations du sol à partir des données de radar à synthèse d'ouverture de RADARSAT-2 et de la mission de la Constellation RADARSAT : description et guide de l'utilisateur. Natural Resources Canada/CMSS/Information Management, 2021. http://dx.doi.org/10.4095/329134.

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Remote sensing using Synthetic Aperture Radar (SAR) offers powerful methods for monitoring ground deformation from both natural and anthropogenic sources. Advanced analysis techniques such as Differential Interferometric Synthetic Aperture Radar (DInSAR), change detection, and Speckle Offset Tracking (SPO) provide sensitive measures of ground movement. With both the RADARSAT-2 and RADARSAT Constellation Mission (RCM) SAR satellites, Canada has access to a significant catalogue of SAR data. To make use of this data, the Canada Centre for Mapping and Earth Observation (CCMEO) has developed an automated system for generating standard and advanced deformation products from SAR data using both DInSAR and SPO methods. This document provides a user guide for this automated processing system.

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Lukowski, T. I., et F. Charbonneau. Synthetic Aperture Radar and Search and Rescue : detection of crashed aircraft using imagery and interferometric methods. Natural Resources Canada/ESS/Scientific and Technical Publishing Services, 2002. http://dx.doi.org/10.4095/219846.

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Libby, S., V. Sonnad, S. Kreek, K. Brady, M. Matthews, B. Dubetsky, A. Vitouchkine et B. Young. Feasibility Study of a Passive, Standoff Detector of High Density Masses with a Gravity Gradiometer Based on Atom Interferometry. Office of Scientific and Technical Information (OSTI), janvier 2011. http://dx.doi.org/10.2172/1068278.

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Vogel, Sven, et Erik Watkins. Neutron Imaging Using Grating Interferometry : Exploiting phase contrast and dark-field imaging for <1μm feature detection in bulk materials. Office of Scientific and Technical Information (OSTI), septembre 2020. http://dx.doi.org/10.2172/1669072.

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