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Journal articles on the topic 'Interferometric detector'

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Author: Grafiati

Published: 11 March 2023

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1

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, no. 2120 (April 16, 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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2

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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3

Chou, Chien, Hui-Kang Teng, Chien-Chung Tsai, and Li-Ping Yu. "Balanced detector interferometric ellipsometer." Journal of the Optical Society of America A 23, no. 11 (November 1, 2006): 2871. http://dx.doi.org/10.1364/josaa.23.002871.

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4

Rowan, Sheila. "Current and future status of gravitational wave astronomy - gravitational wave facilities." Proceedings of the International Astronomical Union 2, no. 14 (August 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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5

Trott, Cathryn M., Randall B. Wayth, Jean-Pierre R. Macquart, and Steven J. Tingay. "Source Detection with Interferometric Datasets." Proceedings of the International Astronomical Union 7, S285 (September 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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6

Mazilu, M., P. J. Phillips, and A. Miller. "Interferometric Hetero-Detector Phase Measurement." Optical and Quantum Electronics 36, no. 5 (April 2004): 431–42. http://dx.doi.org/10.1023/b:oqel.0000022997.34800.89.

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7

Prado, A. R. C., F. S. Bortoli, N. S. Magalhaes, R. N. Duarte, C. Frajuca, and R. C. Souza. "Obtaining the sensitivity of a calibrator for interferometric gravitational wave." Journal of Physics: Conference Series 2090, no. 1 (November 1, 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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8

Pai, Archana. "Gravitational Waves in an Interferometric Detector." Current Science 112, no. 07 (April 1, 2017): 1353. http://dx.doi.org/10.18520/cs/v112/i07/1353-1360.

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9

Prado, A. R. C., F. S. Bortoli, N. S. Magalhaes, R. N. Duarte, C. Frajuca, and 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, no. 1 (November 1, 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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10

Fritschel, Peter, Nergis Mavalvala, David Shoemaker, Daniel Sigg, Michael Zucker, and Gabriela González. "Alignment of an interferometric gravitational wave detector." Applied Optics 37, no. 28 (October 1, 1998): 6734. http://dx.doi.org/10.1364/ao.37.006734.

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11

Venkatesh, Suresh, David Shrekenhamer, Wangren Xu, Sameer Sonkusale, Willie Padilla, and David Schurig. "Interferometric direction finding with a metamaterial detector." Applied Physics Letters 103, no. 25 (December 16, 2013): 254103. http://dx.doi.org/10.1063/1.4851936.

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12

SINYUKOV, ALEXANDER M., APARAJITA BANDYOPADHYAY, AMARTYA SENGUPTA, ROBERT B. BARAT, DALE E. GARY, ZOI-HELENI MICHALOPOULOU, DAVID ZIMDARS, and JOHN F. FEDERICI. "TERAHERTZ INTERFEROMETRIC AND SYNTHETIC APERTURE IMAGING." International Journal of High Speed Electronics and Systems 17, no. 02 (June 2007): 431–43. http://dx.doi.org/10.1142/s0129156407004618.

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Experimental results of homodyne terahertz interferometric 1-D and 2-D imaging are presented. The reconstructed images of a point source are in a good agreement with theoretical predictions. The performance of an N element detector array is imitated by only one detector placed at N positions. Continuous waves at 0.25-0.3 THz are used to detect a metal object behind a barrier. 1-D images of a C-4 sample have been obtained at several terahertz frequencies. Focusing issues of 2-D imaging have been demonstrated. The terahertz interferometric imaging method can be used in defense and security applications to detect concealed weapons, explosives as well as chemical and biological agents.

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13

Seck, Hon Luen, Ying Zhang, and Y. C. Soh. "An Improved Active Homodyne Detector." Key Engineering Materials 381-382 (June 2008): 329–32. http://dx.doi.org/10.4028/www.scientific.net/kem.381-382.329.

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This paper proposes an improved active homodyne detection technique to compensate for the drift in homodyne measurement. The technique is implemented on a fiber based Michelson interferometer where a computer controller is designed to drive a piezoelectric cylinder attached to one arm of the interferometer. It is shown that the proposed technique can efficiently stabilize the interferometric output.

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14

UCHIYAMA, TAKASHI. "PRESENT STATUS OF CLIO IN 2004." International Journal of Modern Physics A 20, no. 29 (November 20, 2005): 7066–68. http://dx.doi.org/10.1142/s0217751x05030843.

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The CLIO project in Japan consists of two kinds of interferometric detectors in a tunnel of Kamioka mine. One is a geophysical strain meter and the other one is a gravitational wave (GW) detector. The GW detector is called Cryogenic Laser Interferometer Observatory (CLIO). The characteristics of CLIO are the use of cryogenic to reduce the thermal noises and an underground site for low seismic vibration. CLIO is under construction, and installation of the first cryogenic system was completed in the autumn of 2004.

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15

Swinney, Kelly, Jana Pennington, and Darryl J. Bornhop. "Universal detection in capillary electrophoresis with a micro-interferometric backscatter detector." Analyst 124, no. 3 (1999): 221–25. http://dx.doi.org/10.1039/a809691k.

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16

Bourquin, S., P. Seitz, and R. P. Salathé. "Two-dimensional smart detector array for interferometric applications." Electronics Letters 37, no. 15 (2001): 975. http://dx.doi.org/10.1049/el:20010669.

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17

Malhotra, Tanya, Wesley E. Farriss, Jeremy Hassett, Ayman F. Abouraddy, James R. Fienup, and A. Nick Vamivakas. "Interferometric spatial mode analyzer with a bucket detector." Optics Express 26, no. 7 (March 26, 2018): 8719. http://dx.doi.org/10.1364/oe.26.008719.

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18

Gleyzes, P., and A. C. Boccara. "Interferometric polarization picometric profile. I. Single detector approach." Journal of Optics 25, no. 5 (September 1994): 207–24. http://dx.doi.org/10.1088/0150-536x/25/5/005.

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19

Davis, Derek, and Marissa Walker. "Detector Characterization and Mitigation of Noise in Ground-Based Gravitational-Wave Interferometers." Galaxies 10, no. 1 (January 14, 2022): 12. http://dx.doi.org/10.3390/galaxies10010012.

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Since the early stages of operation of ground-based gravitational-wave interferometers, careful monitoring of these detectors has been an important component of their successful operation and observations. Characterization of gravitational-wave detectors blends computational and instrumental methods of investigating the detector performance. These efforts focus both on identifying ways to improve detector sensitivity for future observations and understand the non-idealized features in data that has already been recorded. Alongside a focus on the detectors themselves, detector characterization includes careful studies of how astrophysical analyses are affected by different data quality issues. This article presents an overview of the multifaceted aspects of the characterization of interferometric gravitational-wave detectors, including investigations of instrumental performance, characterization of interferometer data quality, and the identification and mitigation of data quality issues that impact analysis of gravitational-wave events. Looking forward, we discuss efforts to adapt current detector characterization methods to meet the changing needs of gravitational-wave astronomy.

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20

Sullivan, Andrew G., Doğa Veske, Zsuzsa Márka, Imre Bartos, and Szabolcs Márka. "Probing the dark Solar system: detecting binary asteroids with a space-based interferometric asteroid explorer." Monthly Notices of the Royal Astronomical Society 512, no. 3 (March 11, 2022): 3738–53. http://dx.doi.org/10.1093/mnras/stac669.

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ABSTRACT With the inception of gravitational wave astronomy, astrophysical studies using interferometric techniques have begun to probe previously unknown parts of the Universe. In this work, we investigate the potential of a new interferometric experiment to study a unique group of gravitationally interacting sources within our Solar system: binary asteroids. We present the first study into binary asteroid detection via gravitational signals. We identify the interferometer sensitivity necessary for detecting a population of binary asteroids in the asteroid belt. We find that the space-based gravitational wave detector LISA will have negligible ability to detect these sources as these signals will be well below the LISA noise curve. Consequently, we propose a 4.6 au and a 1 au arm-length interferometer specialized for binary asteroid detection, targeting frequencies between 10−6 and 10−4 Hz. Our results demonstrate that the detection of binary asteroids with space-based gravitational wave interferometers is possible though very difficult, requiring substantially improved interferometric technology over what is presently proposed for space-based missions. If that threshold can be met, an interferometer may be used to map the asteroid belt, allowing for new studies into the evolution of our Solar system.

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21

Tischer, Christian, Arnd Pralle, and Ernst-Ludwig Florin. "Determination and Correction of Position Detection Nonlinearity in Single Particle Tracking and Three-Dimensional Scanning Probe Microscopy." Microscopy and Microanalysis 10, no. 4 (August 2004): 425–34. http://dx.doi.org/10.1017/s1431927604040140.

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A general method is presented for determining and correcting nonlinear position detector responses in single particle tracking as used in three-dimensional scanning probe microscopy based on optical tweezers. The method uses locally calculated mean square displacements of a Brownian particle to detect spatial changes in the sensitivity of the detector. The method is applied to an optical tweezers setup, where the position fluctuations of a microsphere within the optical trap are measured by an interferometric detection scheme with nanometer precision and microsecond temporal resolution. Detector sensitivity profiles were measured at arbitrary positions in solution with a resolution of approximately 6 nm and 20 nm in the lateral and axial directions, respectively. Local detector sensitivities are used to reconstruct the real positions of the particle from the measured position signals.

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22

Biswas, Tanmoy, María García Díaz, and Andreas Winter. "Interferometric visibility and coherence." Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences 473, no. 2203 (July 2017): 20170170. http://dx.doi.org/10.1098/rspa.2017.0170.

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Recently, the basic concept of quantum coherence (or superposition) has gained a lot of renewed attention, after Baumgratz et al. ( Phys. Rev. Lett. 113 , 140401. (doi:10.1103/PhysRevLett.113.140401)), following Åberg ( http://arxiv.org/abs/quant-ph/0612146 ), have proposed a resource theoretic approach to quantify it. This has resulted in a large number of papers and preprints exploring various coherence monotones, and debating possible forms for the resource theory. Here, we take the view that the operational foundation of coherence in a state, be it quantum or otherwise wave mechanical, lies in the observation of interference effects. Our approach here is to consider an idealized multi-path interferometer, with a suitable detector, in such a way that the visibility of the interference pattern provides a quantitative expression of the amount of coherence in a given probe state. We present a general framework of deriving coherence measures from visibility, and demonstrate it by analysing several concrete visibility parameters, recovering some known coherence measures and obtaining some new ones.

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23

Crouzier, A., F. Malbet, F. Henault, A. Léger, C. Cara, J. M. LeDuigou, O. Preis, et al. "A detector interferometric calibration experiment for high precision astrometry." Astronomy & Astrophysics 595 (November 2016): A108. http://dx.doi.org/10.1051/0004-6361/201526321.

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24

Acernese, F., M. Agathos, K. Agatsuma, D. Aisa, N. Allemandou, A. Allocca, J. Amarni, et al. "Advanced Virgo: a second-generation interferometric gravitational wave detector." Classical and Quantum Gravity 32, no. 2 (December 18, 2014): 024001. http://dx.doi.org/10.1088/0264-9381/32/2/024001.

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25

Ni, Wei-Tou. "Gravitational Wave (GW) Classification, Space GW Detection Sensitivities and AMIGO (Astrodynamical Middle-frequency Interferometric GW Observatory)." EPJ Web of Conferences 168 (2018): 01004. http://dx.doi.org/10.1051/epjconf/201816801004.

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After first reviewing the gravitational wave (GW) spectral classification. we discuss the sensitivities of GW detection in space aimed at low frequency band (100 nHz–100 mHz) and middle frequency band (100 mHz–10 Hz). The science goals are to detect GWs from (i) Supermassive Black Holes; (ii) Extreme-Mass-Ratio Black Hole Inspirals; (iii) Intermediate-Mass Black Holes; (iv) Galactic Compact Binaries; (v) Stellar-Size Black Hole Binaries; and (vi) Relic GW Background. The detector proposals have arm length ranging from 100 km to 1.35×109 km (9 AU) including (a) Solar orbiting detectors and (b) Earth orbiting detectors. We discuss especially the sensitivities in the frequency band 0.1-10 μHz and the middle frequency band (0.1 Hz–10 Hz). We propose and discuss AMIGO as an Astrodynamical Middlefrequency Interferometric GW Observatory.

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26

Frajuca, Carlos, Andre R. C. Prado, Marco A. Souza, and Nadja S. Magalhaes. "The challenge of calibrating a laser‐interferometric gravitational wave detector." Astronomische Nachrichten 342, no. 1-2 (January 2021): 115–22. http://dx.doi.org/10.1002/asna.202113890.

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27

Robertson, D. I., E. Morrison, J. Hough, S. Killbourn, B. J. Meers, G. P. Newton, N. A. Robertson, K. A. Strain, and H. Ward. "The Glasgow 10 m prototype laser interferometric gravitational wave detector." Review of Scientific Instruments 66, no. 9 (September 1995): 4447–52. http://dx.doi.org/10.1063/1.1145339.

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28

Liao, Shaolin, Zi Wang, Lu Ou, and Yu Peng. "A Harmonics Interferometric Doppler Sensor With a Neon Lamp Detector." IEEE Sensors Journal 20, no. 10 (May 15, 2020): 5229–36. http://dx.doi.org/10.1109/jsen.2020.2970055.

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29

Miyoki, Shinji, Takayuki Tomaru, Hideki Ishitsuka, Masatake Ohashi, Kazuaki Kuroda, Daisuke Tatsumi, Takashi Uchiyama, et al. "Cryogenic contamination speed for cryogenic laser interferometric gravitational wave detector." Cryogenics 41, no. 5-6 (May 2001): 415–20. http://dx.doi.org/10.1016/s0011-2275(01)00084-4.

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30

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." IEEE Transactions on Nuclear Science 55, no. 1 (2008): 225–32. http://dx.doi.org/10.1109/tns.2007.913937.

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31

Tenorio, Rodrigo, David Keitel, and Alicia M. Sintes. "Search Methods for Continuous Gravitational-Wave Signals from Unknown Sources in the Advanced-Detector Era." Universe 7, no. 12 (December 4, 2021): 474. http://dx.doi.org/10.3390/universe7120474.

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Continuous gravitational waves are long-lasting forms of gravitational radiation produced by persistent quadrupolar variations of matter. Standard expected sources for ground-based interferometric detectors are neutron stars presenting non-axisymmetries such as crustal deformations, r-modes or free precession. More exotic sources could include decaying ultralight boson clouds around spinning black holes. A rich suite of data-analysis methods spanning a wide bracket of thresholds between sensitivity and computational efficiency has been developed during the last decades to search for these signals. In this work, we review the current state of searches for continuous gravitational waves using ground-based interferometer data, focusing on searches for unknown sources. These searches typically consist of a main stage followed by several post-processing steps to rule out outliers produced by detector noise. So far, no continuous gravitational wave signal has been confidently detected, although tighter upper limits are placed as detectors and search methods are further developed.

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32

Acernese, F., M. Agathos, A. Ain, S. Albanesi, A. Allocca, A. Amato, T. Andrade, et al. "The Virgo O3 run and the impact of the environment." Classical and Quantum Gravity 39, no. 23 (November 29, 2022): 235009. http://dx.doi.org/10.1088/1361-6382/ac776a.

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Abstract Sources of geophysical noise (such as wind, sea waves and earthquakes) or of anthropogenic noise impact ground-based gravitational-wave interferometric detectors, causing transient sensitivity worsening and gaps in data taking. During the one year-long third observing run (O3: from April 01, 2019 to March 27, 2020), the Virgo Collaboration collected a statistically significant dataset, used in this article to study the response of the detector to a variety of environmental conditions. We correlated environmental parameters to global detector performance, such as observation range, duty cycle and control losses. Where possible, we identified weaknesses in the detector that will be used to elaborate strategies in order to improve Virgo robustness against external disturbances for the next data taking period, O4, currently planned to start at the end of 2022. The lessons learned could also provide useful insights for the design of the next generation of ground-based interferometers.

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33

Balega, I. I., Y. Y. Balega, V. A. Vasyuk, and J. J. McManus. "Double and Multiple Star Speckle Observations at the 6-m Telescope." International Astronomical Union Colloquium 135 (1992): 469–76. http://dx.doi.org/10.1017/s0252921100006989.

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During the last 15 years more than 9,000 speckle interferometric measurements of binary stars have been collected using large optical telescopes (McAlister & Hartkopf 1988). Among them a significant contribution to the world speckle data has been made by the 6-m telscope near Zelenchuk. Up to now this instrument provides the maximal spatial resolution for single–aperture telescopes. First speckle images of the binary Capella were recorded at the telescope in 1977 (Balega & Tikhonov 1977), but we spent 5 more years to create special television techniques for photon counting and digital means for image processing before we started the regular interferometric program of binary observations in the wide range of stellar magnitudes. At first, the measurements were conducted in cooperation with French astronomers from the Centre d’Etudes et de Recherches Geodynamiques et Astronomiques using the optical camera and the television detector developed by Blazit et al. (1977). Since 1983 our equipment has been in use. The program of observations was oriented upon the traditional problems of multiple star speckle interferometry:1.Determination of stellar distances and masses for different types of binaries whose orbital elements can be derived. This includes already known fast visual and astrometric pairs with undetermined orbits, spectroscopic binaries that can be resolved directly, and newly discovered interferometric pairs which show fast orbital motion. The main attention was devoted to the late–type dwarfs in the vicinity of the Sun.2.Search for the secondary components whose existence could explain anomalies of stellar spectra or photometry (stars with composite spectra, occultation binaries, etc.)3.Study of unusual binaries (symbiotic stars, binaries with relativistic components, such as SS 433, etc.)

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34

Fabbroni, L., M. Vannucci, E. Cuoco, G. Losurdo, M. Mazzoni, and R. Stanga. "Wavelet Tests for the Detection of Transients in the VIRGO Interferometric Gravitational Wave Detector." IEEE Transactions on Instrumentation and Measurement 54, no. 1 (February 2005): 151–62. http://dx.doi.org/10.1109/tim.2004.838127.

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35

Hall , Evan D. "Cosmic Explorer: A Next-Generation Ground-Based Gravitational-Wave Observatory." Galaxies 10, no. 4 (August 18, 2022): 90. http://dx.doi.org/10.3390/galaxies10040090.

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Cosmic Explorer is a concept for a new laser interferometric observatory in the United States to extend ground-based gravitational-wave astrophysics into the coming decades. Aiming to begin operation in the 2030s, Cosmic Explorer will extend current and future detector technologies to a 40 km interferometric baseline—ten times larger than the LIGO observatories. Operating as part of a global gravitational-wave observatory network, Cosmic Explorer will have a cosmological reach, detecting black holes and neutron stars back to the times of earliest star formation. It will observe nearby binary collisions with enough precision to reveal details of the dynamics of the ultradense matter in neutron stars and to test the general-relativistic model of black holes.

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36

Yang, X., L. H. Yu, V. Smaluk, T. Shaftan, L. Doom, B. Kosciuk, W. X. Cheng, et al. "Interferometric bunch length measurements of 3 MeV picocoulomb electron beams." Journal of Applied Physics 131, no. 8 (February 28, 2022): 084901. http://dx.doi.org/10.1063/5.0076593.

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We report picosecond bunch length measurements using an interferometric method for a 3 MeV electron beam having bunch charge ranging from 1 to 14 pC. The method senses the single-cycle sub-terahertz (THz) pulse emitted by each electron bunch as coherent transition radiation which, in turn, is analyzed using a Michelson-type interferometer, forming an interferogram that is then processed to yield the nominal electron bunch length. This sub-THz coherent radiation intensity was measured using a quasi-optical detector (QOD) operated at room temperature. This experiment was quite challenging since the divergence angle of the sub-THz pulse emitted by the low-energy electron bunch exceeds ±10°, and its pulse energy at the entrance to the detector was as low as 100 pJ. When compared to a conventional helium-cooled silicon composite bolometer designed for frequencies above 0.5 THz, the QOD provided much better signal-to-noise ratio in the ∼80 GHz frequency range, which was critical for the successful measurement of the bunch length.

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37

Ye Song, 叶松, 孙永丰 Sun Yongfeng, 李志伟 Li Zhiwei, 施海亮 Shi Hailiang, 熊伟 Xiong Wei, 王新强 Wang Xinqiang, 汪杰君 Wang Jiejun, and 张文涛 Zhang Wentao. "High Order Nonlinearity Responses of Detector of Infrared Hyperspectral Interferometric Spectrometer." Acta Optica Sinica 38, no. 6 (2018): 0612007. http://dx.doi.org/10.3788/aos201838.0612007.

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38

Ando, Masaki, Keita Kawabe, and Kimio Tsubono. "Signal-separation technique for a power-recycled interferometric gravitational wave detector." Physics Letters A 237, no. 1-2 (December 1997): 13–20. http://dx.doi.org/10.1016/s0375-9601(97)00745-7.

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39

Sun, Bohua, Bo Zhang, and Mohamed Toriq Khan. "Modeling and Formulation of a Novel Microoptoelectromechanical Gyroscope." Journal of Nanomaterials 2008 (2008): 1–9. http://dx.doi.org/10.1155/2008/429168.

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This paper proposed a novel design of microgyroscope based on MEMS structures and optic interferometric microdisplacement measurement technique. The gyroscope consists of microvibrator and interferometric readout. Using Coriolis force, the vibrator transfers the system rotation into a forced vibration; the induced vibration can be sensed by the interferometric microdisplacement measurement system. The optic measurement system has two mirrors which will reflect two rays into a detector. The comprehensive studies on the formulation and analysis of the proposed gyroscope have been undertaken; two key sensor equations have been derived in the first time in the world: (1) relation between rotation and phase shift of lightΔφ=(4πl0/λ)+(8π/λ)(xmax⁡Qy/ωy)Ω(t)sin⁡(ωdt), (2) relation between rotation and interferometric intensity of lightI(t)≈(8π/λ)(xmax⁡Qy/ωy)Ω(t)sin⁡(ωdt)sin⁡(4πl0/λ). The comparison of the proposed gyroscope and well-know Sagnac formulation has been investigated; it shown that the proposed model is much better than Sagnac ones. The new model has finally get rid of needing very long fiber in the case of Sagnac gyroscope. The innovative model gives a new hope to fabricate high accurate and cheaper gyroscope. To date, the proposed gyroscope is the most accurate gyroscope.

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Stefanovic, Mihajlo, and Petar Spalevic. "The interferometric noise as a performance limiting factor of IM-DD systems." Facta universitatis - series: Electronics and Energetics 15, no. 3 (2002): 349–59. http://dx.doi.org/10.2298/fuee0203349s.

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In this paper, the signal propagation along the fiber, in either absence or presence of the cross talk interference appearing at different places along the fiber, for both dispersive regime cases, is considered. The optical signal that appears at transmitter output has the envelope in super-Gaussian form. The cross talk appears at the transmitter output or along the fiber The pulse shape at the receiver input is determined using Schrodinger equation. The noise sources are the photo detector and resistance in the receiver. The bit error probability of intensity modulation and direct detection (IM-DD) system in the presence of the cross talk, quantum and thermal noise is determined.

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TOMARU, TAKAYUKI, TOSHIKAZU SUZUKI, TOMIYOSHI HARUYAMA, TAKAKAZU SHINTOMI, NOBUAKI SATO, AKIRA YAMAMOTO, YUKI IKUSHIMA, et al. "SMALL VIBRATION CRYOCOOLER SYSTEM FOR CRYOGENIC GRAVITATIONAL WAVE INTERFEROMETER." International Journal of Modern Physics A 20, no. 29 (November 20, 2005): 7063–65. http://dx.doi.org/10.1142/s0217751x05030831.

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An ultra-small vibration cryocooler system for a cryogenic interferometric gravitational wave detector has been developed. The system consists of a pulse tube cryocooler and a vibration-reduction system. Its vibration level was about 50 nm for the vertical direction at 1 Hz, which was three orders of magnitude smaller than that of an original pulse tube cryocooler.

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Petrov, Romain G., and Stephane Lagarde. "Differential Speckle Interferometry Applied to Double Stars." International Astronomical Union Colloquium 135 (1992): 477–85. http://dx.doi.org/10.1017/s0252921100006990.

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AbstractDifferential Interferometry (DI) is the application of high angular resolution interferometric techniques to objects observed simultaneously at different wavelengths. When applied to unresolved double stars it makes it possible to measure the variation of the object photocenter with wavelength, which yields angular and spectral information well beyond the classical resolution limits. Signal–to–noise ratio analysis shows that, if DI experiments are limited by photon and speckle noise, the technique can be applied to a large number of double systems for the measurement of vectorial angular separations and of radial-velocity differences. With 4-m telescopes, there are a few tens of binary systems for which DI should permit the resolution and the measurement of the position angle of the rotation axis of at least one of the components. A preliminary experiment permitted a high SNR resolution of the double star Capella with a 1.52-m telescope and showed the current limitations of DI performances resulting from an imperfect correction of detector geometrical distortions.

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43

Barriga, P., D. G. Blair, D. Coward, J. Davidson, J.-C. Dumas, E. Howell, L. Ju, et al. "AIGO: a southern hemisphere detector for the worldwide array of ground-based interferometric gravitational wave detectors." Classical and Quantum Gravity 27, no. 8 (April 6, 2010): 084005. http://dx.doi.org/10.1088/0264-9381/27/8/084005.

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KANDA, NOBUYUKI. "TAMA STATUS REPORT." International Journal of Modern Physics D 09, no. 03 (June 2000): 233–36. http://dx.doi.org/10.1142/s0218271800000207.

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TAMA 300 m laser interferometric gravitational wave detector operated in August and September 1999. We had total four night operation with best strain sensitivity of 3×10-20. The longest continuous locking is over 7 hours. The calibration of the interferometer sensitivity was archived with 1% accuracy in Δh/h. TAMA Phase-I sensitivity is evaluated as S/N~10 for 10 kpc event.

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SATO, NOBUAKI, TOMIYOSHI HARUYAMA, TAKAKAZU SHINTOMI, TOSHIKAZU SUZUKI, TAKAYUKI TOMARU, AKIRA YAMAMOTO, KAZUAKI KURODA, et al. "MAKING A DATA ANALYSIS PROCESSOR WITH FPGA FOR GRAVITATIONAL-WAVE EVENT SEARCH." International Journal of Modern Physics A 20, no. 29 (November 20, 2005): 7057–59. http://dx.doi.org/10.1142/s0217751x05030818.

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We are trying to make a hardware logic-circuit for pipelines of fast Fourier transformation (FFT) with a field programmable gate array (FPGA) for data analyses of an interferometric gravitational-wave detector. That FFT processor is connected to a personal computer (PC) through PCI bus and will increase the calculation speed of FFT which is the most time-consuming step for typical gravitational-wave analyses.

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KASAHARA, Kunihiko, Takayuki TOMARU, Takashi UCHIYAMA, Toshikazu SUZUKI, Kazuhiro YAMAMOTO, Shinji MIYOKI, Masatake OHASHI, Kazuaki KURODA, and Takakazu SHINTOMI. "Study of Heat Links for a Cryogenic Laser Interferometric Gravitational Wave Detector." TEION KOGAKU (Journal of Cryogenics and Superconductivity Society of Japan) 39, no. 1 (2004): 25–32. http://dx.doi.org/10.2221/jcsj.39.25.

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Estevez, D., B. Lieunard, F. Marion, B. Mours, L. Rolland, and D. Verkindt. "First tests of a Newtonian calibrator on an interferometric gravitational wave detector." Classical and Quantum Gravity 35, no. 23 (November 9, 2018): 235009. http://dx.doi.org/10.1088/1361-6382/aae95f.

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Hayama, Kazuhiro, and Masa-Katsu Fujimoto. "Monitoring non-stationary burst-like signals in an interferometric gravitational wave detector." Classical and Quantum Gravity 23, no. 8 (March 22, 2006): S9—S15. http://dx.doi.org/10.1088/0264-9381/23/8/s02.

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Takahashi, R., F. Kuwahara, E. Majorana, Mark A. Barton, T. Uchiyama, K. Kuroda, A. Araya, et al. "Vacuum-compatible vibration isolation stack for an interferometric gravitational wave detector TAMA300." Review of Scientific Instruments 73, no. 6 (June 2002): 2428–33. http://dx.doi.org/10.1063/1.1473225.

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Cagnoli, G., J. Hough, D. DeBra, M. M. Fejer, E. Gustafson, S. Rowan, and V. Mitrofanov. "Damping dilution factor for a pendulum in an interferometric gravitational waves detector." Physics Letters A 272, no. 1-2 (July 2000): 39–45. http://dx.doi.org/10.1016/s0375-9601(00)00411-4.

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