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41 results on '"GRAVITATIONAL-WAVE DETECTION"'

1. Robust attitude coordinated control for gravitational-wave detection spacecraft formation with large-scale communication delays.

Author: Song, Yinsheng, Chen, Xiaofang, Yin, Zeyang, Liao, Yuxin, and Wei, Caisheng
Subjects: *ARTIFICIAL satellite attitude control systems, *SPACE vehicles, *GRAVITATIONAL waves, *ROBUST control, *CLOSED loop systems, *SLIDING mode control
Abstract: This paper concentrates on robust attitude control issues for spacecraft formation in gravitational-wave detection missions. Notably, with the large-scale communication delays brought by the million kilometers-scale inter-satellite distance, the exponential convergence of the closed-loop delayed system is firstly achieved via a new delay-dependent nominal attitude coordinated control scheme. Then, a finite-time disturbance observer is deployed to reconstruct the unknown lumped disturbance from internal uncertainties and the external environment. Meanwhile, an integral sliding manifold is embedded in the delay-dependent attitude controller for superior systems' robustness. Finally, two simulation examples illustrate the feasibility and effectiveness of the proposed attitude control strategy for in-orbit gravitational-wave detection spacecraft systems. • Spacecraft formation attitude control in gravitational-wave detection is studied. • Large-scale communication delays (LCD) among formation members are firstly modeled. • An attitude coordinated controller is put forward to handle the LCD. • An integral sliding manifold with disturbance observer is embedded for superior robustness. [ABSTRACT FROM AUTHOR]
Published: 2024
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2. Opportunities and limits of lunar gravitational-wave detection.

Author: Cozzumbo, Andrea, Mestichelli, Benedetta, Mirabile, Marco, Paiella, Lavinia, Tissino, Jacopo, and Harms, Jan
Subjects: *LUNAR exploration, *COMPLEXITY (Philosophy), *TECHNOLOGICAL complexity, *SCIENTIFIC experimentation, *OBSERVATORIES, *GRAVITATIONAL waves, *LUNAR craters
Abstract: A new era of lunar exploration has begun with participation of all major space agencies. This activity brings opportunities for revolutionary science experiments and observatories on the Moon. The idea of a lunar gravitational-wave detector was already proposed during the Apollo programme. The key characteristic of the Moon is that it is seismically extremely quiet. It was also pointed out that the permanently shadowed regions at the lunar poles provide ideal conditions for gravitational-wave detection. In recent years, three different detector concepts were proposed with varying levels of technological complexity and science potential. In this paper, we confront the three concepts in terms of their observational capabilities based on a first more detailed modelling of instrumental noise. We identify important technological challenges and potential show-stoppers. This article is part of a discussion meeting issue 'Astronomy from the Moon: the next decades (part 2)'. [ABSTRACT FROM AUTHOR]
Published: 2024
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3. Development of Amorphous-silicon-based Optical Coatings for Gravitational-wave Detectors

Author: Zhou, Ruinan
Subjects: Materials Science, Physics, Engineering, amorphous materials, gravitational-wave detection, materials characterization, physical vapor deposition, semiconductor materials
Abstract: The search for new coating materials, particularly high-refractive-index layers, is crucial in the field of interferometric gravitational-wave (GW) detectors. These detectors require coatings with low mechanical loss to minimize thermal noise and low optical absorption to maintain measurement stability and precision. The development of novel high-index coating materials with improved mechanical and optical properties has the potential to advance GW detection and enable more precise measurements of astrophysical phenomena.This study investigated the structural and mechanical properties of amorphous silicon (a-Si), hydrogenated amorphous silicon (a-Si:H), and amorphous silicon carbide (a-SiC) films deposited using magnetron sputtering (MS). The effects of deposition parameters, such as working gas, gas pressure, substrate temperature, and post-growth treatments including vacuum annealing and post-hydrogenation, were explored. The choice of working gas and its pressure, which influences the kinetic energy of the sputtered atoms upon arrival at the substrate, was found to significantly affect the properties of the deposited films. The impact of energetic incoming atoms is reflected in compressive film stress and film densification, a phenomenon known as the atomic peening effect. Additionally, a transition in dominant defects from nanovoids in e-beam a-Si to divacancies and self-interstitials in MS a-Si was observed, which can be attributed to the higher kinetic energy of incident atoms. By selecting appropriate working gas and deposition conditions, such as low gas pressure and high growth temperature, the structural order was improved, as indicated by lower bond angle deviation, and the mechanical loss of MS a-Si was reduced at both low temperatures and room temperature.Introduction of hydrogen to a-Si had a significant impact on its optical absorption at infrared wavelengths and the room-temperature mechanical loss. We propose that hydrogen plays a dual role in a-Si:H, acting as a passivating agent for dangling bonds, particularly at high temperatures, and facilitating structural relaxation, and the latter is responsible for the observed changes in the physical properties of a-Si:H. The incorporation of carbon in a-SiC films resulted in higher mechanical loss and optical absorption compared to pure a-Si films. These findings provide insights into the underlying mechanisms and offer potential solutions for optimizing the performance of a-Si-based coatings for GW detector mirrors.
Published: 2023

4. "Quantum Weirdness" in Exploitation by the International Gravitational‐Wave Observatory Network.

Author: Schnabel, Roman
Subjects: *SQUEEZED light, *QUANTUM theory, *QUANTUM correlations, *PHOTON counting, *OBSERVATORIES, *QUANTUM wells
Abstract: The detectors of the international gravitational‐wave (GW) observatory network are currently taking data with sensitivities improved via squeezing the photon counting noise of the laser light used. Several GW candidate events, such as black‐hole mergers, are already in the pipeline to be analyzed in detail. While the brand‐new field of GW astronomy relies on squeezed light for reaching higher sensitivities, the physical understanding of such light, although being well described by quantum theory, is still under discussion. Herein, a physical description of why squeezed light, as now being exploited by GW observatories, constitutes rather remarkable physics is presented. Consideration of the Fourier transform seems to provide an argument why the measurement of squeezed photon statistics from quasi‐monochromatic light is "weird." It is further argued that the measurement of squeezed photon statistics is related to the famous gedanken experiment formulated by Einstein, Podolsky, and Rosen in 1935. This work illuminates "quantum weirdness" in a clear way and might be the starting point for finding the physics of quantum correlations in general, which scientists have been seeking for decades. [ABSTRACT FROM AUTHOR]
Published: 2020
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5. Anderson Photon-Phonon Colocalization in Certain Random Superlattices

Subjects: Gravitational-wave detection, Localization phenomena, Longitudinal acoustic waves, Anderson localization, Nanomechanical oscillators, Cavity optomechanics, Light-matter interactions, Quantum ground state
Published: 2021

6. Astrodynamical Space Test of Relativity using Optical Devices I (ASTROD I)-a class-M fundamental physics mission proposal for cosmic vision 2015-2025: 2010 Update.

Author: Braxmaier, Claus, Dittus, Hansjörg, Foulon, Bernard, Göklü, Ertan, Grimani, Catia, Guo, Jian, Herrmann, Sven, Lämmerzahl, Claus, Ni, Wei-Tou, Peters, Achim, Rievers, Benny, Samain, Étienne, Selig, Hanns, Shaul, Diana, Svehla, Drazen, Touboul, Pierre, Wang, Gang, Wu, An-Ming, and Zakharov, Alexander
Subjects: *GRAVITATIONAL waves, *RELATIVITY (Physics), *GRAVITY, *GRAVITATIONAL constant, *SPACE vehicles, *SOLAR system
Abstract: ASTROD I is a planned interplanetary space mission with multiple goals. The primary aims are: to test General Relativity with an improvement in sensitivity of over 3 orders of magnitude, improving our understanding of gravity and aiding the development of a new quantum gravity theory; to measure key solar system parameters with increased accuracy, advancing solar physics and our knowledge of the solar system; and to measure the time rate of change of the gravitational constant with an order of magnitude improvement and the anomalous Pioneer acceleration, thereby probing dark matter and dark energy gravitationally. It is envisaged as the first in a series of ASTROD missions. ASTROD I will consist of one spacecraft carrying a telescope, four lasers, two event timers and a clock. Two-way, two-wavelength laser pulse ranging will be used between the spacecraft in a solar orbit and deep space laser stations on Earth, to achieve the ASTROD I goals.For this mission, accurate pulse timing with an ultra-stable clock, and a drag-free spacecraft with reliable inertial sensor are required. T2L2 has demonstrated the required accurate pulse timing; rubidium clock on board Galileo has mostly demonstrated the required clock stability; the accelerometer on board GOCE has paved the way for achieving the reliable inertial sensor; the demonstration of LISA Pathfinder will provide an excellent platform for the implementation of the ASTROD I drag-free spacecraft. These European activities comprise the pillars for building up the mission and make the technologies needed ready. A second mission, ASTROD or ASTROD-GW (depending on the results of ASTROD I), is envisaged as a three-spacecraft mission which, in the case of ASTROD, would test General Relativity to one part per billion, enable detection of solar g-modes, measure the solar Lense-Thirring effect to 10 parts per million, and probe gravitational waves at frequencies below the LISA bandwidth, or in the case of ASTROD-GW, would be dedicated to probe gravitational waves at frequencies below the LISA bandwidth to 100 nHz and to detect solar g-mode oscillations. In the third phase (Super-ASTROD), larger orbits could be implemented to map the outer solar system and to probe primordial gravitational-waves at frequencies below the ASTROD bandwidth. This paper on ASTROD I is based on our 2010 proposal submitted for the ESA call for class-M mission proposals, and is a sequel and an update to our previous paper (Appouchaux et al., Exp Astron 23:491-527, ; designated as Paper I) which was based on our last proposal submitted for the 2007 ESA call. In this paper, we present our orbit selection with one Venus swing-by together with orbit simulation. In Paper I, our orbit choice is with two Venus swing-bys. The present choice takes shorter time (about 250 days) to reach the opposite side of the Sun. We also present a preliminary design of the optical bench, and elaborate on the solar physics goals with the radiation monitor payload. We discuss telescope size, trade-offs of drag-free sensitivities, thermal issues and present an outlook. [ABSTRACT FROM AUTHOR]
Published: 2012
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7. Gravitational-wave detection with matter-wave interferometers based on standing light waves.

Author: Dongfeng Gao, Peng Ju, Baocheng Zhang, and Mingsheng Zhan
Subjects: *GRAVITY, *ATOMS, *INTERFEROMETERS, *DETECTORS, *SCATTERING (Physics)
Abstract: We study the possibility of detecting gravitational-waves with matter-wave interferometers, where atom beams are split, deflected and recombined totally by standing light waves. Our calculation shows that the phase shift is dominated by terms proportional to the time derivative of the gravitational wave amplitude. Taking into account future improvements on current technologies, it is promising to build a matter-wave interferometer detector with desired sensitivity. [ABSTRACT FROM AUTHOR]
Published: 2011
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8. Astrodynamical Space Test of Relativity Using Optical Devices I (ASTROD I)—A class-M fundamental physics mission proposal for Cosmic Vision 2015–2025.

Author: Appourchaux, Thierry, Burston, Raymond, Chen, Yanbei, Cruise, Michael, Dittus, Hansjörg, Foulon, Bernard, Gill, Patrick, Gizon, Laurent, Klein, Hugh, Klioner, Sergei, Kopeikin, Sergei, Krüger, Hans, Lämmerzahl, Claus, Lobo, Alberto, Luo, Xinlian, Margolis, Helen, Ni, Wei-Tou, Patón, Antonio, Peng, Qiuhe, and Peters, Achim
Subjects: *SPACE vehicles, *INTERPLANETARY voyage research, *ASTRODYNAMICS, *GENERAL relativity (Physics), *QUANTUM gravity, *ULTRASHORT laser pulses, *SOLAR system
Abstract: ASTROD I is a planned interplanetary space mission with multiple goals. The primary aims are: to test general relativity with an improvement in sensitivity of over three orders of magnitude, improving our understanding of gravity and aiding the development of a new quantum gravity theory; to measure key solar system parameters with increased accuracy, advancing solar physics and our knowledge of the solar system; and to measure the time rate of change of the gravitational constant with an order of magnitude improvement and the anomalous Pioneer acceleration, thereby probing dark matter and dark energy gravitationally. It is an international project, with major contributions from Europe and China and is envisaged as the first in a series of ASTROD missions. ASTROD I will consist of one spacecraft carrying a telescope, four lasers, two event timers and a clock. Two-way, two-wavelength laser pulse ranging will be used between the spacecraft in a solar orbit and deep space laser stations on Earth, to achieve the ASTROD I goals. A second mission, ASTROD (ASTROD II) is envisaged as a three-spacecraft mission which would test General Relativity to 1 ppb, enable detection of solar g-modes, measure the solar Lense–Thirring effect to 10 ppm, and probe gravitational waves at frequencies below the LISA bandwidth. In the third phase (ASTROD III or Super-ASTROD), larger orbits could be implemented to map the outer solar system and to probe primordial gravitational-waves at frequencies below the ASTROD II bandwidth. [ABSTRACT FROM AUTHOR]
Published: 2009
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9. GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

Author: Abbott, B.P., Abbott, R., Abbott, T.D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R.X., Adya, V.B., LIGO Scientific Collaboration and Virgo Collaboration, Affeldt, Christoph, Aufmuth, Peter, Bergmann, G., Bisht, Aparna, Bode, N., Booker, Phillip, Brinkmann, M., Cabero, M., Danilishin, Stefan L., Danzmann, Karsten, Dent, Thomas, de Varona, Omar, Doravari, S., Hanke, Manuela Melanie, Hennig, J., Heurs, M., Hochheim, Sven, Junker, J., Karvinen, K.S., Khan, S., Kaufer, S., Kirchhoff, R., Koch, P., Koehlenbeck, S.M., Koper, N., Kringel, V., Kuehn, G., Leavey, S., Lehmann, J., Lück, Harald, Mehmet, M., Mukherjee, Arunava, Nery, M., Ohme, F., Oppermann, P., Papa, M.A., Phelps, M., Puncken, O., Rüdiger, A., Schreiber, E., Schulte, B.W., Setyawati, Y., Standke, M., Steinke, M., Steinmeyer, D., Wei, L.-W., Weinert, M., Wellmann, F., Weßels, P., Wilken, D.M., Willke, B., Wimmer, M.H., Winkler, W., Wittel, H., Woehler, J., Wu, D.S., Abbott, B.P., Abbott, R., Abbott, T.D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R.X., Adya, V.B., LIGO Scientific Collaboration and Virgo Collaboration, Affeldt, Christoph, Aufmuth, Peter, Bergmann, G., Bisht, Aparna, Bode, N., Booker, Phillip, Brinkmann, M., Cabero, M., Danilishin, Stefan L., Danzmann, Karsten, Dent, Thomas, de Varona, Omar, Doravari, S., Hanke, Manuela Melanie, Hennig, J., Heurs, M., Hochheim, Sven, Junker, J., Karvinen, K.S., Khan, S., Kaufer, S., Kirchhoff, R., Koch, P., Koehlenbeck, S.M., Koper, N., Kringel, V., Kuehn, G., Leavey, S., Lehmann, J., Lück, Harald, Mehmet, M., Mukherjee, Arunava, Nery, M., Ohme, F., Oppermann, P., Papa, M.A., Phelps, M., Puncken, O., Rüdiger, A., Schreiber, E., Schulte, B.W., Setyawati, Y., Standke, M., Steinke, M., Steinmeyer, D., Wei, L.-W., Weinert, M., Wellmann, F., Weßels, P., Wilken, D.M., Willke, B., Wimmer, M.H., Winkler, W., Wittel, H., Woehler, J., and Wu, D.S.
Abstract: We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1 Ma™ during the first and second observing runs of the advanced gravitational-wave detector network. During the first observing run (O1), from September 12, 2015 to January 19, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November 30, 2016 to August 25, 2017, saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to the observation of gravitational waves from a total of seven binary black hole mergers, four of which we report here for the first time: GW170729, GW170809, GW170818, and GW170823. For all significant gravitational-wave events, we provide estimates of the source properties. The detected binary black holes have total masses between 18.6-0.7+3.2 Mâ™ and 84.4-11.1+15.8 Mâ™ and range in distance between 320-110+120 and 2840-1360+1400 Mpc. No neutron star-black hole mergers were detected. In addition to highly significant gravitational-wave events, we also provide a list of marginal event candidates with an estimated false-alarm rate less than 1 per 30 days. From these results over the first two observing runs, which include approximately one gravitational-wave detection per 15 days of data searched, we infer merger rates at the 90% confidence intervals of 110-3840 Gpc-3 y-1 for binary neutron stars and 9.7-101 Gpc-3 y-1 for binary black holes assuming fixed population distributions and determine a neutron star-black hole merger rate 90% upper limit of 610 Gpc-3 y-1. © 2019 authors. Published by the American Physical Society.
Published: 2019

10. Advanced techniques for squeezed-light-enhanced gravitational-wave detection

Author: Gniesmer, Jan and Gniesmer, Jan
Abstract: Quantum noise is one of the limiting factors in laser-interferometric gravitational-wave (GW) detectors. The application of squeezed states in these interferometers allows the reduction of quantum noise in one quadrature. Due to opto-mechanical coupling in a GW detector the squeezed quadrature needs to be rotated within the spectrum to achieve a broadband noise reduction. So far, the implementation of additional filter cavities is considered that allow for the optimal, frequency-dependent rotation of the squeezed quadrature. However, these cavities need to have low loss, a length in the order of \unit[100]{m} and must be situated in the vacuum system, making them cost-intensive. In 2017, Ma and coworkers proposed a scheme for the broadband quantum-noise reduction without the need of additional filter cavities. It was shown by Brown et al. that a similar scheme can be used to broadband-enhance interferometers with a detuned signal-recycling cavity. Here, we performed a proof-of-principle experiment of the proposal on a table-top-scale. Squeezed states were produced detuned to the carrier field of a \unit[2.5]{m}-linear cavity and read out in a bichromatic homodyne detection. The frequencies of the lower and upper local oscillator were at entangled sidebands of the squeezed field. Depending on the relations between the involved frequencies, we can address both variants of the proposal. We show, that the frequency-dependences of the resulting noise spectra fit to a theoretical model we derived from the theory used by Ma et al. With this work we set the path towards an implementation of these schemes in a GW-detector prototype, where the compatibility of the approach with a low-frequency suspended interferometer can be tested. Moreover, we used the same setup to show nonclassical interferometer enhancement at low frequencies by high-frequency squeezed states. Here, a heterodyne readout scheme was implemented to avoid limiting noises at low frequencies. The application o
Published: 2019

11. Anderson photon-phonon colocalization in certain random superlattices

Author: Pedro García, Clivia M. Sotomayor-Torres, Guillermo Arregui, Norberto D. Lanzillotti-Kimura, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, European Research Council, Catalan Institute of Nanoscience and Nanotechnology (ICN2), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Barcelona Institute of Science and Technology (BIST), Centre de Nanosciences et Nanotechnologies (C2N (UMR_9001)), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), and Institució Catalana de Recerca i Estudis Avançats (ICREA)
Subjects: Anderson localization, Localization phenomena, Photon, Phonon, FOS: Physical sciences, General Physics and Astronomy, Physics::Optics, Nanomechanical oscillators, Cavity optomechanics, 01 natural sciences, Gravitational-wave detection, Quantum mechanics, Mesoscale and Nanoscale Physics (cond-mat.mes-hall), 0103 physical sciences, [PHYS.COND]Physics [physics]/Condensed Matter [cond-mat], 010306 general physics, Quantum, Physics, Condensed Matter - Mesoscale and Nanoscale Physics, Degree (graph theory), Acoustic wave, Coupling (probability), Light-matter interactions, Quantum ground state, Wavelength, Longitudinal acoustic waves, Physics - Optics, Optics (physics.optics)
Abstract: Fundamental observations in physics ranging from gravitational wave detection to laser cooling of a nanomechanical oscillator into its quantum ground state rely on the interaction between the optical and the mechanical degrees of freedom. A key parameter to engineer this interaction is the spatial overlap between the two fields, optimized in carefully designed resonators on a case-by-case basis. Disorder is an alternative strategy to confine light and sound at the nanoscale. However, it lacks an a priori mechanism guaranteeing a high degree of colocalization due to the inherently complex nature of the underlying interference processes. Here, we propose a way to address this challenge by using GaAs/AlAs vertical distributed Bragg reflectors with embedded geometrical disorder. Because of a remarkable coincidence in the physical parameters governing light and motion propagation in these two materials, the equations for both longitudinal acoustic waves and normal-incidence light become practically equivalent for excitations of the same wavelength. This guarantees spatial overlap between the electromagnetic and displacement fields of specific photon-phonon pairs, leading to strong light-matter interaction. In particular, a statistical enhancement in the vacuum optomechanical coupling rate, go, is found, making this system a promising candidate to explore Anderson localization of high frequency (∼20 GHz) phonons enabled by cavity optomechanics. The colocalization effect shown here unlocks the access to unexplored localization phenomena and the engineering of light-matter interactions mediated by Anderson-localized states., This work was supported by the Spanish Ministerio de Ciencia, Innovacion y Universidades (MICINN) via the Severo Ochoa Program (Grant No. SEV-2017-0706) and the project PHENTOM (Grant No. Fis 2015-70862-P) as well as by the Centres de Recerca de Catalunya (CERCA), and by the European Commission in the form of the H2020 FET open project PHENOMEN (Grant No. 713450). G. A. is supported by a Barcelona Institute of Science and Technology PhD fellowship, N. D. L. K. by the ERC Starting Grant Nanophennec (Grant No. 715939) and P. D. G. by a Ramon y Cajal fellowship (Grant No. RyC-2015-18124).
Published: 2019
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12. Bayesian Inference Analysis of Unmodelled Gravitational-Wave Transients

Author: Francesco Pannarale, Patrick J. Sutton, and R. Macas
Subjects: Physics, Physics and Astronomy (miscellaneous), Data analysis, gravitational waves, gravitational-wave detection, Estimation theory, Noise (signal processing), Signal reconstruction, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Bayesian inference, 01 natural sciences, Signal, General Relativity and Quantum Cosmology, Constant false alarm rate, Binary black hole, 0103 physical sciences, Waveform, 010306 general physics, 010303 astronomy & astrophysics, Algorithm
Abstract: We report the results of an in-depth analysis of the parameter estimation capabilities of BayesWave, an algorithm for the reconstruction of gravitational-wave signals without reference to a specific signal model. Using binary black hole signals, we compare BayesWave's performance to the theoretical best achievable performance in three key areas: sky localisation accuracy, signal/noise discrimination, and waveform reconstruction accuracy. BayesWave is most effective for signals that have very compact time-frequency representations. For binaries, where the signal time-frequency volume decreases with mass, we find that BayesWave's performance reaches or approaches theoretical optimal limits for system masses above approximately 50 M_sun. For such systems BayesWave is able to localise the source on the sky as well as templated Bayesian analyses that rely on a precise signal model, and it is better than timing-only triangulation in all cases. We also show that the discrimination of signals against glitches and noise closely follow analytical predictions, and that only a small fraction of signals are discarded as glitches at a false alarm rate of 1/100 y. Finally, the match between BayesWave- reconstructed signals and injected signals is broadly consistent with first-principles estimates of the maximum possible accuracy, peaking at about 0.95 for high mass systems and decreasing for lower-mass systems. These results demonstrate the potential of unmodelled signal reconstruction techniques for gravitational-wave astronomy., 10 pages, 7 figures
Published: 2018

13. Limits on Stellar-Mass Compact Objects as Dark Matter from Gravitational Lensing of Type Ia Supernovae

Author: Zumalacarregui, Miguel, Seljak, U., Zumalacarregui, Miguel, and Seljak, U.
Abstract: The nature of dark matter (DM) remains unknown despite very precise knowledge of its abundance in the Universe. An alternative to new elementary particles postulates DM as made of macroscopic compact halo objects (MACHO) such as black holes formed in the very early Universe. Stellar-mass primordial black holes (PBHs) are subject to less robust constraints than other mass ranges and might be connected to gravitational-wave signals detected by the Laser Interferometer Gravitational-Wave Observatory (LIGO). New methods are therefore necessary to constrain the viability of compact objects as a DM candidate. Here we report bounds on the abundance of compact objects from gravitational lensing of type Ia supernovae (SNe). Current SNe data sets constrain compact objects to represent less than 35.2% (Joint Lightcurve Analysis) and 37.2% (Union 2.1) of the total matter content in the Universe, at 95% confidence level. The results are valid for masses larger than ∼0.01 M (solar masses), limited by the size SNe relative to the lens Einstein radius. We demonstrate the mass range of the constraints by computing magnification probabilities for realistic SNe sizes and different values of the PBH mass. Our bounds are sensitive to the total abundance of compact objects with M0.01 M and complementary to other observational tests. These results are robust against cosmological parameters, outlier rejection, correlated noise, and selection bias. PBHs and other MACHOs are therefore ruled out as the dominant form of DM for objects associated to LIGO gravitational wave detections. These bounds constrain early-Universe models that predict stellar-mass PBH production and strengthen the case for lighter forms of DM, including new elementary particles., QC 20190507
Published: 2018
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14. Gravitational-wave detection beyond the quantum shot-noise limit : the integration of squeezed light in GEO 600

Author: Schreiber, Emil and Schreiber, Emil
Abstract: The first detections of gravitational waves have opened an exciting new field of astronomy. One of the most fundamental limitations for the sensitivity of current and future interferometric gravitational-wave detectors is imposed by the quantum nature of light: Quantum vacuum fluctuations entering the interferometer through the readout port will contribute to the detection noise, at high frequencies in the form of shot noise and at low frequencies by radiation pressure noise. A promising way to reduce this quantum noise is the injection of squeezed states of light that have a lower uncertainty in one quadrature than the vacuum state. The GEO 600 gravitational-wave detector demonstrated the use of squeezed light in 2010 and it is now the first detector to routinely apply squeezing to improve its sensitivity beyond the limits set by classical quantum shot noise. This thesis details the practical aspects of long-term stable and efficient squeezed-light integration in a large-scale gravitational-wave detector. Imperfections that can limit the amount of observable non-classical noise improvement, such as optical losses and phase fluctuations, were studied in detail and methods for their mitigation were developed. Novel control schemes for the active stabilisation of the squeezed light field's phase and alignment were one main focus of the investigations. At the same time, important experience was gathered in the operation of the squeezed light source over long timescales. Over the course of the thesis work, improvements were implemented that significantly increased the performance of the squeezed-light application. Squeezing was injected with an overall duty cycle of 88%, reaching a noise reduction of up to 4.4 dB, corresponding to a 40% lowered shot-noise level. This work has firmly established the practical application of squeezing as a mature technology. The gained knowledge will directly inform the implementation of squeezed light for all future gravitational-wave de
Published: 2018

15. Measurement uncertainty in pulsar timing array experiments

Author: W Verbiest, J, Shaifullah, G, Joris P W Verbiest, Golam Shaifullah, W Verbiest, J, Shaifullah, G, Joris P W Verbiest, and Golam Shaifullah
Abstract: Highly precise monitoring of arrival times of pulses from pulsars will allow for gravitational-wave detection in the nano-Hertz regime in the near future. Due to the complex nature of such pulsar-timing experiments and to the large number of effects that can affect these data (starting with magnetospheric effects at the pulsars themselves but extending across the entire signal path down to the final gravitational-wave detection algorithm), any treatment of the measurement uncertainties relevant to such a gravitational-wave detection has been lacking and incomplete so far. In this review, we provide an exhaustive description of the currently known influences on measurement precision in pulsar-timing experiments in general and in gravitational-wave detection through pulsar-timing specifically. While some of these effects remain poorly understood and largely unquantified at present, we discuss both analytic and observational quantifications where available.
Published: 2018

16. Measurement uncertainty in pulsar timing array experiments

Author: G. Shaifullah, Joris P. W. Verbiest, W Verbiest, J, and Shaifullah, G
Subjects: Physics, Physics and Astronomy (miscellaneous), Astrophysics::High Energy Astrophysical Phenomena, pulsar timing, Astronomy, technique, 01 natural sciences, gravitational-wave detection, Pulsar timing array, 0103 physical sciences, Measurement uncertainty, 010306 general physics, techniques, 010303 astronomy & astrophysics
Abstract: Highly precise monitoring of arrival times of pulses from pulsars will allow for gravitational-wave detection in the nano-Hertz regime in the near future. Due to the complex nature of such pulsar-timing experiments and to the large number of effects that can affect these data (starting with magnetospheric effects at the pulsars themselves but extending across the entire signal path down to the final gravitational-wave detection algorithm), any treatment of the measurement uncertainties relevant to such a gravitational-wave detection has been lacking and incomplete so far. In this review, we provide an exhaustive description of the currently known influences on measurement precision in pulsar-timing experiments in general and in gravitational-wave detection through pulsar-timing specifically. While some of these effects remain poorly understood and largely unquantified at present, we discuss both analytic and observational quantifications where available.
Published: 2018
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17. Quantum-dense metrology for substraction of back-scatter disturbances in gravitational-wave detection

Author: Ast, Melanie, Schnabel, Roman, and Danzmann, Karsten
Subjects: Gravitationswellen-Detektion, Gravitational-wave detection, zwei-Moden-gequetschtes Licht, gequetschtes Licht, scattered light, ddc:530, Streulicht, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, quantendichte Messung, squeezed light, quantum-dense metrology, two-mode-squeezing
Abstract: [no abstract]
Published: 2017

18. Upper Limits On The Rates Of Binary Neutron Star And Neutron Star-Black Hole Mergers From Advanced Ligo's First Observing Run

Author: Ligo, The Scientific Collaboration, the Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Bejger, M., Bell, A. S., Berger, B. K., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Calder On Bustillo, J., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Casanueva Diaz, J., Casentini, C., Caudill, S., Cavagli A, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerboni Baiardi, L., Cerretani, G., Cesarini, E., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Cheeseboro, B. D., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F, Colla, A., Collette, C. G., Cominsky, L., Constancio, M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P, Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Danilishin, S. L., D Antonio, S., Danzmann, K., Darman, N. S., Dasgupta, A., Da Silva Costa, C. F., Dattilo, V., Dave, I., Davier, M., Davies, G. S., Daw, E. J., Day, R., De, S., Debra, D., Debreczeni, G., Degallaix, J., Laurentis, M., Del Eglise, S., Del Pozzo, W., Denker, T., Dent, T., Dergachev, V., Rosa, R., Derosa, R. T., Desalvo, R., Devine, R. C., Dhurandhar, S., D Iaz, M. C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B, Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Fenyvesi, E., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. -D, Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, F., Gaur, G., Gehrels, N., Gemme, G., Geng, P., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., Gonz Alez, G., Gonzalez Castro, J. M., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Paul Groot, Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J, Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Henry, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M, Isi, M., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jian, L., Jim Enez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., K, Haris, Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., K Ef Elian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chi-Woong, Kim, Chunglee, Kim, J., Kim, K., Kim, N., Kim, W., Kim, Y. -M, Kimbrell, S. J., King, E. J., King, P. J., Kissel, J. S., Klein, B., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnan, B., Kr Olak, A., Krueger, C., Kuehn, G., Kumar, P., Kumar, R., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Lewis, J. B., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Lombardi, A. L., London, L. T., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Quot, L., Uck, H., Lundgren, A. P., Lynch, R., Ma, Y., Machenschalk, B., Macinnis, M., Macleod, D. M., Magana-Sandoval, F., Magana Zertuche, L., Magee, R. M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., M Arka, S., M Arka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcguire, S. C., Mcintyre, G., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mercer, R. A., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Miller, B. B., Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Nedkova, K., Nelemans, G., Nelson, T. J. N., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, Richard J., O Reilly, B., O Shaughnessy, R., Ottaway, D. J., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Perri, L. M., Phelps, M., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poe, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Pratt, J., Predoi, V., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quot, P., Urrer, M., Qi, H., Qin, J., Qiu, S., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rajan, C., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosi Nska, D., Rowan, S., Quot, R., Udiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O. E. S., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Sch&quot, Onbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Setyawati, Y., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Shaltev, M., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A. D., Singer, A., Singer, L. P., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sunil, S., Sutton, P. J., Swinkels, B. L., Szczepa Nczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., T Apai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Toland, K., Tomlinson, C., Tonelli, M., Tornasi, Z., Torres, C. V., Torrie, C. I., Quot, T., oyr&quot, A, D., Travasso, F., Traylor, G., Trifir O, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Bakel, N., Beuzekom, M., Den Brand, J. F. J., Den Broeck, C., Vander-Hyde, D. C., Schaaf, L., Heijningen, J. V., Veggel, A. A., Vardaro, M., Vass, S., Vas Uth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Vicer E, A., Vinciguerra, S., Vine, D. J., Vinet, J. -Y, Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D. V., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. -W, Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wessels, P., Westphal, T., Wette, K., Whelan, J. T., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Worden, J., Wright, J. L., Wu, D. S., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yu, H., Yvert, M., Zadro Zny, A., Zangrando, L., Zanolin, M., Zendri, J. -P, Zevin, M., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, VIRGO, Ligo, Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Bejger, M., Bell, A. S., Berger, B. K., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callister, T., Calloni, Enrico, Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. Cerboni, Cerretani, G., Cesarini, E., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande Mottin, E., Cheeseboro, B. D., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. F., Colla, A., Collette, C. G., Cominsky, L., M., C. o. n. s. t. a. n. c. i. o. J. r., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D’Antonio, S., Danzmann, K., Darman, N. S., Dasgupta, A., Costa, C. F. Da Silva, Dattilo, V., Dave, I., Davier, M., Davies, G. S., Daw, E. J., Day, R., De, S., Debra, D., Debreczeni, G., Degallaix, J., DE LAURENTIS, Martina, Deléglise, S., Pozzo, W. Del, Denker, T., Dent, T., Dergachev, V., Rosa, R. De, DE ROSA, Rosario, Desalvo, R., Devine, R. C., Dhurandhar, S., Díaz, M. C., Fiore, L. Di, Giovanni, M., DI GIROLAMO, Tristano, Lieto, A. Di, Pace, S. Di, Palma, I. Di, Virgilio, A. Di, Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Fenyvesi, E., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, Fabio, Gaur, G., Gehrels, N., Gemme, G., Geng, P., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Henry, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh Dinh, T., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. M., Isi, M., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jian, L., Jiménez Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., K, Hari, Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chi Woong, Kim, Chunglee, Kim, J., Kim, K., Kim, N., Kim, W., Kim, Y. M., Kimbrell, S. J., King, E. J., King, P. J., Kissel, J. S., Klein, B., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnan, B., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kumar, R., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Lewis, J. B., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Lombardi, A. L., London, L. T., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Lynch, R., Ma, Y., Machenschalk, B., Macinnis, M., Macleod, D. M., Magaña Sandoval, F., Magaña Zertuche, L., Magee, R. M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso Reid, M., Mastrogiovanni, S., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcguire, S. C., Mcintyre, G., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mercer, R. A., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, Leopoldo, Miller, A. L., Miller, A., Miller, B. B., Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow Lowry, C. M., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Nedkova, K., Nelemans, G., Nelson, T. J. N., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O’Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, Richard J., O’Reilly, B., O’Shaughnessy, R., Ottaway, D. J., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Perri, L. M., Phelps, M., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poe, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Predoi, V., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Qin, J., Qiu, S., Quetschke, V., Quintero, E. A., Quitzow James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rajan, C., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O. E. S., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Setyawati, Y., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Shaltev, M., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A. D., Singer, A., Singer, L. P., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sunil, S., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Toland, K., Tomlinson, C., Tonelli, M., Tornasi, Z., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Bakel, N. van, Beuzekom, M. van, van den Brand, J. F. J., Broeck, C. Van Den, Vander Hyde, D. C., Schaaf, L. van der, Heijningen, J. V. van, Veggel, A. A. van, Vardaro, M., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D. V., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. W., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. T., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Worden, J., Wright, J. L., Wu, D. S., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. P., Zevin, M., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), (Astro)-Particles Physics, LIGO, Louisiana State Univ, Amer Univ, Univ Salerno, Complesso Univ Monte S Angelo, Univ Florida, LIGO Livingston Observ, Lab Annecy Le Vieux Phys Particules, Univ Sannio Benevento, INFN, Max Planck Inst Gravitat Phys, Nikhef, MIT, Inst Nacl Pesquisas Espaciais, Inter Univ Ctr Astron & Astrophys, Int Ctr Theoret Sci, Univ Wisconsin Milwaukee, Leibniz Univ Hannover, Univ Pisa, Australian Natl Univ, Univ Mississippi, Calif State Univ Fullerton, Univ Paris 11, Chennai Math Inst, Univ Roma Tor Vergata, Univ Southampton, Univ Hamburg, Universidade de São Paulo (USP), Montana State Univ, Univ Perugia, EGO, Syracuse Univ, Univ Glasgow, LIGO Hanford Observ, Wigner RCP, Columbia Univ, Stanford Univ, Univ Padua, CAMK PAN, Univ Birmingham, Univ Genoa, RRCAT, Lomonosov Moscow State Univ, Univ West Scotland, Univ Western Australia, Radboud Univ Nijmegen, Univ Cote Azur, Univ Rennes 1, Washington State Univ, Univ Urbino Carlo Bo, Ist Nazl Fis Nucl, Univ Oregon, ENS PSL Res Univ, Carleton Coll, Astron Observ Warsaw Univ, Vrije Univ Amsterdam, Univ Maryland, Georgia Inst Technol, CNRS, Univ Claude Bernard Lyon 1, NASA, Univ Tokyo, Tsinghua Univ, Texas Tech Univ, Penn State Univ, Natl Tsing Hua Univ, Charles Sturt Univ, West Virginia Univ, Univ Chicago, Caltech CaRT, Korea Inst Sci & Technol Informat, Univ Roma La Sapienza, Univ Brussels, Sonoma State Univ, NW Univ, Univ Minnesota, Univ Melbourne, Inst Plasma Res, Univ Sheffield, Univ Texas Rio Grande Valley, Univ Trent, Cardiff Univ, Montclair State Univ, MTA Eotvos Univ, Natl Astron Observ Japan, Univ Edinburgh, Indian Inst Technol, Univ Szeged, Embry Riddle Aeronaut Univ, Tata Inst Fundamental Res, INAF, Univ Michigan, Rochester Inst Technol, Univ Illinois, Univ Illes Balears, Univ Bialystok, Univ Strathclyde, IISER TVM, Univ Toronto, Inst Appl Phys, Pusan Natl Univ, Hanyang Univ, Univ Adelaide, NCBJ, IM PAN, Monash Univ, Seoul Natl Univ, Chinese Univ Hong Kong, Univ Alabama Huntsville, Univ Massachusetts Amherst, Univ Camerino, A&M Coll, Southern Univ, Coll William & Mary, Universidade Estadual Paulista (Unesp), Univ Cambridge, IISER Kolkata, HSIC, Whitman Coll, Natl Inst Math Sci, Univ Lyon, Hobart & William Smith Colleges, Univ Zielona Gora, Univ London, Andrews Univ, Univ Siena, Tnnity Univ, Univ Washington, Kenyon Coll, Abilene Christian Univ, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - 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Paris 7 (UPD7), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Astronomy, gamma-ray burst: general, Astrophysics, general [gamma-ray burst], 01 natural sciences, General Relativity and Quantum Cosmology, general [binaries], Astrophysics::Solar and Stellar Astrophysics, binaries: general, gravitational waves, stars: black holes, stars: neutron, astro-ph.HE, astro-ph.CO, Astronomy and Astrophysics, Space and Planetary Science, LIGO, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), QC, POPULATION, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), GAMMA-RAY BURSTS, Settore FIS/01 - Fisica Sperimentale, SPIN, ACCRETION DISK, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics::Earth and Planetary Astrophysics, Binary Neutron Star, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Star (game theory), gr-qc, Astrophysics::High Energy Astrophysical Phenomena, Neutron Star and Black Hole, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, GRAVITATIONAL-WAVE DETECTION, [ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], O1, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], MAXIMUM MASS, neutron [stars], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, black holes [stars], Sensitivity (control systems), LIGO, O1, Binary Neutron Star, Neutron Star and Black Hole, STFC, Astrophysics::Galaxy Astrophysics, MASS-DISTRIBUTION, RADIO, EXPLOSION, 010308 nuclear & particles physics, Gravitational wave, RCUK, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Black hole, Neutron star, Physics and Astronomy, HOST GALAXY, Binaries: general, Gamma-ray burst, Dimensionless quantity
Abstract: © 2016 The American Astronomical Society. This is the publisher Version of Record Manuscript. Please refer to any applicable publisher terms of use., We report here the non-detection of gravitational waves from the merger of binary–neutron star systems and neutron star–black hole systems during the first observing run of the Advanced Laser Interferometer Gravitationalwave Observatory (LIGO). In particular, we searched for gravitational-wave signals from binary–neutron star systems with component masses Î[ ] 1, 3 M and component dimensionless spins
Published: 2016
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19. Quantum-dense metrology for substraction of back-scatter disturbances in gravitational-wave detection

Author: Schnabel, Roman, Danzmann, Karsten, Ast, Melanie, Schnabel, Roman, Danzmann, Karsten, and Ast, Melanie
Abstract: [no abstract]
Published: 2017

20. Automatic Alignment for the first science run of the Virgo interferometer

Subjects: Gravitational wave detectors, Control systems, Interferometry, Angular, GRAVITATIONAL-WAVE DETECTION, SYSTEM
Abstract: During the past few years a network of large-scale laser interferometers, including the Virgo detector, has been developed with the aim of detecting gravitational waves To properly operate the detectors, the longitudinal and angular positions of the suspended detector test masses, the interferometer mirrors, must be kept within a small range from the operating point.The design of the Virgo angular control system, called Automatic Alignment is based on a modified version of the Anderson-Giordano technique, a wave-front sensing scheme which uses the modulation-demodulation technique.This paper will present the theoretical background of the Virgo Automatic Alignment system, the implementation issues and the performances observed during the first Virgo science run (VSR1) A total RMS of 4 x 10(-2) to 3 x 10(-3) mu rad for all angular degrees of freedom has been achieved. (C) 2010 Elsevier B.V. All rights reserved.
Published: 2010

21. Building blocks for future detectors: Silicon test masses and 1550 nm laser light

Author: H. Lück, Michael Britzger, Ronny Nawrodt, Moritz Mehmet, Roman Schnabel, Frank Brückner, Sebastian Steinlechner, Daniel Friedrich, T. Eberle, Jessica Dück, Benno Willke, Karsten Danzmann, and Oliver Burmeister
Subjects: History, Physics - Instrumentation and Detectors, Testing, 02 engineering and technology, 01 natural sciences, General Relativity and Quantum Cosmology, law.invention, Gravitational wave detectors, law, Sensitivity increase, ABSORPTION, Crystalline silicon, COATINGS, Quantum Physics, Quantum noise, Gravitational effects, Silica, Instrumentation and Detectors (physics.ins-det), Laser radiation, 021001 nanoscience & nanotechnology, Computer Science Applications, Radiation detectors, Optoelectronics, 0210 nano-technology, Laser lights, Third generation, ANTENNAE, Materials science, 1550 nm, Quasi-monochromatic, Silicon, chemistry.chemical_element, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Radiation, Gravity waves, Noise (electronics), Electromagnetic radiation, LOW-TEMPERATURES, Particle detector, Crystalline silicons, Education, Gravitational-wave detection, GRAVITATIONAL-WAVE DETECTORS, 0103 physical sciences, Low temperatures, ddc:530, 010306 general physics, Konferenzschrift, Room temperature, Gravitationswelle, business.industry, 1064 nm, Building blockes, Fused silica, Laser, VITREOUS SILICA, THERMAL NOISE, chemistry, Silicon detectors, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, business, Quantum Physics (quant-ph)
Abstract: Current interferometric gravitational wave detectors use the combination of quasi-monochromatic, continuous-wave laser light at 1064 nm and fused silica test masses at room temperature. Detectors of the third generation, such as the Einstein-Telescope, will involve a considerable sensitivity increase. The combination of 1550 nm laser radiation and crystalline silicon test masses at low temperatures might be important ingredients in order to achieve the sensitivity goal. Here we compare some properties of the fused silica and silicon test mass materials relevant for decreasing the thermal noise in future detectors as well as the recent technology achievements in the preparation of laser radiation at 1064 nm and 1550 nm relevant for decreasing the quantum noise. We conclude that silicon test masses and 1550 nm laser light have the potential to form the future building blocks of gravitational wave detection. DFG/EXC/QUEST DFG/SFB/TR7 EC/FP7/2007-2013
Published: 2010
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22. Automatic Alignment for the first science run of the Virgo interferometer

Author: M. Laval, G. Ballardin, M. A. Bizouard, F. Frasconi, L. Pinard, F. Vetrano, R. Flaminio, Luca Gammaitoni, Shourov Chatterji, E. Campagna, R. Terenzi, H. J. Bulten, A. Brillet, M. Del Prete, S. Frasca, N. Letendre, M. Yvert, L. Rolland, Fabrizio Barone, M. Mohan, Silvio Pardi, V. Brisson, S. Braccini, Benjamin Canuel, P. Puppo, G. Losurdo, C. Palomba, Gianluca Persichetti, F. Travasso, R. Cavalieri, E. Coccia, G. Cagnoli, F. Ricci, K.G. Arun, F. Carbognani, A. Viceré, A. Rocchi, A. Pasqualetti, F. Paoletti, P. Ruggi, J. Trummer, M. Di Paolo Emilio, L. Di Fiore, B. Mours, R. Passaquieti, S. Birindelli, M. Barsuglia, P. Rapagnani, F. Piergiovanni, M. Davier, J.-P. Coulon, A. Di Virgilio, F. Garufi, Fabio Marchesoni, J.-D. Fournier, M. Lorenzini, P. La Penna, A. Giazotto, I. Ferrante, Simona Mosca, Y. Minenkov, Leopoldo Milano, Th. S. Bauer, N. Leroy, B. L. Swinkels, M. Granata, Alessandra Toncelli, V. Loriette, D. Huet, I. Fiori, Rosa Poggiani, Igor Neri, François Bondu, S. D'Antonio, E. Genin, M. Alshourbagy, V. Dattilo, V. Fafone, Rocco Romano, F. Antonucci, F. Fidecaro, G. M. Guidi, Fausto Acernese, V. Granata, Stefan Hild, L. Bonelli, C. Michel, M. Mantovani, E. Chassande-Mottin, D. Buskulic, R. De Rosa, S. Van Der Putten, C. Bradaschia, Claude Boccara, F. Menzinger, A. Masserot, A. Gennai, F. Cleva, C. N. Man, J.-M. Mackowski, Tania Regimbau, E. Cuoco, F. Martelli, Julien Moreau, L. Bosi, A. Di Lieto, G. Pagliaroli, Sofiane Aoudia, Patrice Hello, Stefano Bigotta, F. Cavalier, N. Morgado, E. Tournefier, C. Greverie, Alessandra Corsi, Enrico Calloni, Christian Corda, D. Passuello, J. F. J. van den Brand, Elena Cesarini, M. Punturo, J-Y. Vinet, D. Verkindt, P. Astone, J. Marque, F. Nocera, Ettore Majorana, Ludovico Carbone, F. Marion, M. Tonelli, M. Colombini, G. Vajente, B. Sassolas, H. Heitmann, Anna Dari, D. Sentenac, G. Cella, J. Colas, O. Rabaste, M. Was, H. Vocca, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Virgo, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), VIRGO, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Ecole Supérieure de Physique et de Chimie Industrielles (ESPCI), Mairie de Paris, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), F., Acernese, F., Barone, Calloni, Enrico, DE ROSA, Rosario, L., Di Fiore, Garufi, Fabio, Milano, Leopoldo, S., Mosca, M., Parisi, G., Persichetti, R., Romano, (Astro)-Particles Physics, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Angular, Virgo interferometer, onde gravitazionali, GRAVITATIONAL-WAVE DETECTION, 01 natural sciences, law.invention, allineamento, Gravitational wave detectors, Optics, Settore FIS/05 - Astronomia e Astrofisica, law, 0103 physical sciences, Astronomical interferometer, SDG 7 - Affordable and Clean Energy, 010303 astronomy & astrophysics, Physics, Operating point, Control systems, 010308 nuclear & particles physics, Gravitational wave, business.industry, Detector, Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Laser, control systems, interferometri, gravitational wave detectors, angular, interferometry, Interferometry, Control system, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], business, SYSTEM
Abstract: During the past few years a network of large-scale laser interferometers, including the Virgo detector, has been developed with the aim of detecting gravitational waves To properly operate the detectors, the longitudinal and angular positions of the suspended detector test masses, the interferometer mirrors, must be kept within a small range from the operating point.The design of the Virgo angular control system, called Automatic Alignment is based on a modified version of the Anderson-Giordano technique, a wave-front sensing scheme which uses the modulation-demodulation technique.This paper will present the theoretical background of the Virgo Automatic Alignment system, the implementation issues and the performances observed during the first Virgo science run (VSR1) A total RMS of 4 x 10(-2) to 3 x 10(-3) mu rad for all angular degrees of freedom has been achieved. (C) 2010 Elsevier B.V. All rights reserved.
Published: 2010
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23. Comparing interferometry techniques for multi-degree of freedom test mass readout

Author: Gerhard Heinzel, Karsten Danzmann, K. Isleif, Oliver Gerberding, Thomas S. Schwarze, and Moritz Mehmet
Subjects: History, Interferometry technique, Physics::Instrumentation and Detectors, Phase (waves), 02 engineering and technology, Gravity waves, 01 natural sciences, Displacement (vector), Degrees of freedom (mechanics), Education, law.invention, 010309 optics, Gravitational-wave detection, Optics, law, 0103 physical sciences, ddc:530, Gravitational physics, Dewey Decimal Classification::500 | Naturwissenschaften, Konferenzschrift, Physics, Gravitationswelle, Ultrasonic devices, Gravitational wave, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Gravitational effects, 021001 nanoscience & nanotechnology, Laser, Computer Science Applications, Interferometry, Pathfinder, Tilt (optics), Phase modulation, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, ddc:500, Laser interferometry, 0210 nano-technology, business, Space probes
Abstract: Laser interferometric readout systems with 1pm √Hz precision over long time scales have successfully been developed for LISA and LISA Pathfinder. Future gravitational physics experiments, for example in the fields of gravitational wave detection and geodesy, will potentially require similar levels of displacement and tilt readouts of multiple test masses in multiple degrees of freedom. In this article we compare currently available classic interferometry schemes with new techniques using phase modulations and complex readout algorithms. Based on a simple example we show that the new techniques have great potential to simplify interferometric readouts. DFG/SFB/1128 International Max-Planck Research School (IMPRS)
Published: 2016

24. The first observation of gravitational-waves

Author: Moutounet Cartan, Pierre and Moutounet-Cartan, Pierre G. B.
Subjects: Gravitational-wave detection, Ondes gravitationnelles, Trou noir, [PHYS.GRQC] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Black hole, LIGO, LIGO-Virgo, [PHYS.ASTR.HE] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.PHYS.PHYS-POP-PH] Physics [physics]/Physics [physics]/Popular Physics [physics.pop-ph]
Abstract: Popular science article about the first direct observation of the merger of two black holes and the gravitational-waves that this merger generated., Article de vulgarisation portant sur la première observation directe de la fusion de deux trous noirs et des ondes gravitationnelles que cette fusion a générée.
Published: 2016

25. Overview and Status of Advanced Interferometers for Gravitational Wave Detection

Author: Hartmut Grote, Fornengo, Nicolao, Regis, Marco, and Zechlin, Hannes-S.
Subjects: Status updates, History, Gravitational-wave observatory, Gravity waves, 01 natural sciences, Education, Advanced detector, Laser interferometry, Gravitational-wave detection, Optics, 0103 physical sciences, Astronomical interferometer, ddc:530, Aerospace engineering, 010306 general physics, Laser interferometer, Konferenzschrift, Dewey Decimal Classification::500 | Naturwissenschaften, Physics, Gravitationswelle, 010308 nuclear & particles physics, business.industry, Gravitational wave, Interferometers, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Gravitational effects, Second generation, LIGO, Computer Science Applications, ddc:500, World-wide networks, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, business
Abstract: The world-wide network of km-scale laser interferometers is aiming at the detection of gravitational waves of astrophysical origin. The second generation of these instruments, called advanced detectors has been, or is in the process of being completed, and a first observational run with the Advanced LIGO interferometers has been performed late in 2015. The basic functionality of advanced detectors is discussed, along with specific features and status updates of the individual projects.
Published: 2016
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26. Gravitational-wave detection with matter-wave interferometers based on standing light waves

Author: Gao, Dongfeng, Ju, Peng, Zhang, Baocheng, and Zhan, Mingsheng
Published: 2011
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27. Overview and Status of Advanced Interferometers for Gravitational Wave Detection

Author: Grote, Hartmut and Grote, Hartmut
Abstract: The world-wide network of km-scale laser interferometers is aiming at the detection of gravitational waves of astrophysical origin. The second generation of these instruments, called advanced detectors has been, or is in the process of being completed, and a first observational run with the Advanced LIGO interferometers has been performed late in 2015. The basic functionality of advanced detectors is discussed, along with specific features and status updates of the individual projects.
Published: 2016

28. Comparing interferometry techniques for multi-degree of freedom test mass readout

Author: Isleif, Katharina-Sophie, Gerberding, Oliver, Mehmet, Moritz, Schwarze, Thomas S., Heinzel, Gerhard, Danzmann, Karsten, Isleif, Katharina-Sophie, Gerberding, Oliver, Mehmet, Moritz, Schwarze, Thomas S., Heinzel, Gerhard, and Danzmann, Karsten
Abstract: Laser interferometric readout systems with 1pm √Hz precision over long time scales have successfully been developed for LISA and LISA Pathfinder. Future gravitational physics experiments, for example in the fields of gravitational wave detection and geodesy, will potentially require similar levels of displacement and tilt readouts of multiple test masses in multiple degrees of freedom. In this article we compare currently available classic interferometry schemes with new techniques using phase modulations and complex readout algorithms. Based on a simple example we show that the new techniques have great potential to simplify interferometric readouts.
Published: 2016

29. The LISA Pathfinder Mission

Author: Armano, M, Audley, H, Auger, G, Baird, J, Binetruy, P, Born, M, Bortoluzzi, D, Brandt, N, Bursi, A, Caleno, M, Cavalleri, A, Cesarini, A, Cruise, M, Danzmann, K, Diepholz, I, Dolesi, R, Dunbar, N, Ferraioli, L, Ferroni, V, Fitzsimons, E, Freschi, M, Gallegos, J, Marirrodriga, C García, Gerndt, R, Gesa, L I, Gibert, F, Giardini, D, Giusteri, R, Grimani, C, Harrison, I, Heinzel, G, Hewitson, M, Hollington, D, Hueller, M, Huesler, J, Inchauspé, H, Jennrich, O, Jetzer, P, Johlander, B, Karnesis, N, Kaune, B, Korsakova, N, Killow, C., Lloro, I, Maarschalkerweerd, R, Madden, S, Mance, D, Martín, V, Martin-Porqueras, F, Mateos, I, McNamara, P, Mendes, J, Mendes, L, Moroni, A, Nofrarias, M, Paczkowski, S, Perreur-Lloyd, M., Petiteau, A, Pivato, P, Plagnol, E, Prat, P, Ragnit, U, Ramos-Castro, J, Reiche, J, Perez, J A Romera, Robertson, D., Rozemeijer, H, Russano, G, Sarra, P, Schleicher, A, Slutsky, J, Sopuerta, C F, Sumner, T, Texier, D, Thorpe, J, Trenkel, C, Tu, H B, Vetrugno, D, Vitale, S, Wanner, G, Ward, H., Waschke, S, Wass, P, Wealthy, D, Wen, S, Weber, W, Wittchen, A, Zanoni, C, Ziegler, T, and Zweifel, P
Subjects: History, Critical technologies, Lisa technology packages, Gravity waves, Propulsion, 01 natural sciences, 7. Clean energy, Education, Gravitational wave detectors, Gravitational-wave detection, 0103 physical sciences, ddc:530, Free flight, 010303 astronomy & astrophysics, Konferenzschrift, Physical principles, 010308 nuclear & particles physics, Gravitational effects, Measurement concepts, Technology validations, Computer Science Applications, Low pass filters, Inertial navigation systems, European Space Agency, Space probes, Gravitation
Abstract: ISA Pathfinder (LPF), the second of the European Space Agency's Small Missions for Advanced Research in Technology (SMART), is a dedicated technology validation mission for future spaceborne gravitational wave detectors, such as the proposed eLISA mission. LISA Pathfinder, and its scientific payload - the LISA Technology Package - will test, in flight, the critical technologies required for low frequency gravitational wave detection: it will put two test masses in a near-perfect gravitational free-fall and control and measure their motion with unprecedented accuracy. This is achieved through technology comprising inertial sensors, high precision laser metrology, drag-free control and an ultra-precise micro-Newton propulsion system. LISA Pathfinder is due to be launched in mid-2015, with first results on the performance of the system being available 6 months thereafter.\ud \ud The paper introduces the LISA Pathfinder mission, followed by an explanation of the physical principles of measurement concept and associated hardware. We then provide a detailed discussion of the LISA Technology Package, including both the inertial sensor and interferometric readout. As we approach the launch of the LISA Pathfinder, the focus of the development is shifting towards the science operations and data analysis - this is described in the final section of the paper.
Published: 2015

30. The LISA Pathfinder Mission

Author: Armano, M., Audley, H., Auger, G., Baird, J., Binetruy, P., Born, M., Bortoluzzi, D., Brandt, N., Bursi, A., Caleno, M., Cavalleri, A., Cesarini, A., Cruise, M., Danzmann, K., Diepholz, I., Dolesi, R., Dunbar, N., Ferraioli, L., Ferroni, V., Fitzsimons, E., Freschi, M., Gallegos, J., Marirrodriga, C.G., Gerndt, R., Gesa, L.I., Gibert, F., Giardini, D., Giusteri, R., Grimani, C., Harrison, I., Heinzel, G., Hewitson, M., Hollington, D., Hueller, M., Huesler, J., Inchauspé, H., Jennrich, O., Jetzer, P., Johlander, B., Karnesis, N., Kaune, B., Korsakova, N., Killow, C., Lloro, I., Maarschalkerweerd, R., Madden, S., Mance, D., Martín, V., Martin-Porqueras, F., Mateos, I., McNamara, P., Mendes, J., Mendes, L., Moroni, A., Nofrarias, M., Paczkowski, S., Perreur-Lloyd, M., Petiteau, A., Pivato, P., Plagnol, E., Prat, P., Ragnit, U., Ramos-Castro, J., Reiche, J., Perez, J.A.R., Robertson, D., Rozemeijer, H., Russano, G., Sarra, P., Schleicher, A., Slutsky, J., Sopuerta, C.F., Sumner, T., Texier, D., Thorpe, J., Trenkel, C., Tu, H.B., Vetrugno, D., Vitale, S., Wanner, G., Ward, H., Waschke, S., Wass, P., Wealthy, D., Wen, S., Weber, W., Wittchen, A., Zanoni, C., Ziegler, T., Zweifel, P., Armano, M., Audley, H., Auger, G., Baird, J., Binetruy, P., Born, M., Bortoluzzi, D., Brandt, N., Bursi, A., Caleno, M., Cavalleri, A., Cesarini, A., Cruise, M., Danzmann, K., Diepholz, I., Dolesi, R., Dunbar, N., Ferraioli, L., Ferroni, V., Fitzsimons, E., Freschi, M., Gallegos, J., Marirrodriga, C.G., Gerndt, R., Gesa, L.I., Gibert, F., Giardini, D., Giusteri, R., Grimani, C., Harrison, I., Heinzel, G., Hewitson, M., Hollington, D., Hueller, M., Huesler, J., Inchauspé, H., Jennrich, O., Jetzer, P., Johlander, B., Karnesis, N., Kaune, B., Korsakova, N., Killow, C., Lloro, I., Maarschalkerweerd, R., Madden, S., Mance, D., Martín, V., Martin-Porqueras, F., Mateos, I., McNamara, P., Mendes, J., Mendes, L., Moroni, A., Nofrarias, M., Paczkowski, S., Perreur-Lloyd, M., Petiteau, A., Pivato, P., Plagnol, E., Prat, P., Ragnit, U., Ramos-Castro, J., Reiche, J., Perez, J.A.R., Robertson, D., Rozemeijer, H., Russano, G., Sarra, P., Schleicher, A., Slutsky, J., Sopuerta, C.F., Sumner, T., Texier, D., Thorpe, J., Trenkel, C., Tu, H.B., Vetrugno, D., Vitale, S., Wanner, G., Ward, H., Waschke, S., Wass, P., Wealthy, D., Wen, S., Weber, W., Wittchen, A., Zanoni, C., Ziegler, T., and Zweifel, P.
Abstract: LISA Pathfinder (LPF), the second of the European Space Agency's Small Missions for Advanced Research in Technology (SMART), is a dedicated technology validation mission for future spaceborne gravitational wave detectors, such as the proposed eLISA mission. LISA Pathfinder, and its scientific payload - the LISA Technology Package - will test, in flight, the critical technologies required for low frequency gravitational wave detection: it will put two test masses in a near-perfect gravitational free-fall and control and measure their motion with unprecedented accuracy. This is achieved through technology comprising inertial sensors, high precision laser metrology, drag-free control and an ultra-precise micro-Newton propulsion system. LISA Pathfinder is due to be launched in mid-2015, with first results on the performance of the system being available 6 months thereafter. The paper introduces the LISA Pathfinder mission, followed by an explanation of the physical principles of measurement concept and associated hardware. We then provide a detailed discussion of the LISA Technology Package, including both the inertial sensor and interferometric readout. As we approach the launch of the LISA Pathfinder, the focus of the development is shifting towards the science operations and data analysis - this is described in the final section of the paper.
Published: 2015

31. Design of a speed meter interferometer proof-of-principle experiment

Author: Gräf, C, Barr, B W, Bell, A S, Campbell, F, Cumming, A V, Danilishin, S L, Gordon, N A, Hammond, G D, Hennig, J, Houston, E A, Huttner, S H, Jones, R A, Leavey, S.S., Lück, H, Macarthur, J, Marwick, M, Rigby, S, Schilling, R, Sorazu, B, Spencer, A, Steinlechner, S, Strain, K A, and Hild, S
Subjects: noise, quantum non-demolition, SAGNAC INTERFEROMETER, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), coatings, General Relativity and Quantum Cosmology, NOISE, gravitational-wave detection, conceptual design, ddc:530, detectors, Gravitationswelle, gravitational wave detector, Quantum Physics, laser interferometer, Sagnac speed meter, quantum noise, Astrophysics::Instrumentation and Methods for Astrophysics, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, sagnac interferometer, optical cavities, QND, Quantum Physics (quant-ph), Optics (physics.optics), Physics - Optics
Abstract: The second generation of large scale interferometric gravitational wave detectors will be limited by quantum noise over a wide frequency range in their detection band. Further sensitivity improvements for future upgrades or new detectors beyond the second generation motivate the development of measurement schemes to mitigate the impact of quantum noise in these instruments. Two strands of development are being pursued to reach this goal, focusing both on modifications of the well-established Michelson detector configuration and development of different detector topologies. In this paper, we present the design of the world's first Sagnac speed meter interferometer which is currently being constructed at the University of Glasgow. With this proof-of-principle experiment we aim to demonstrate the theoretically predicted lower quantum noise in a Sagnac interferometer compared to an equivalent Michelson interferometer, to qualify Sagnac speed meters for further research towards an implementation in a future generation large scale gravitational wave detector, such as the planned Einstein Telescope observatory., Revised version: 16 pages, 6 figures
Published: 2014

32. Design of a speed meter interferometer proof-of-principle experiment

Author: Gräf, Christian, Barr, B.W., Bell, A.S., Campbell, F., Cumming, A.V., Danilishin, S.L., Gordon, N.A., Hammond, G.D., Hennig, J., Houston, E.A., Huttner, S.H., Jones, R.A., Leavey, Sean S., Lück, Harald, Macarthur, J., Marwick, M., Rigby, S., Schilling, R., Sorazu, B., Spencer, A., Steinlechner, S., Strain, Kenneth A., Hild, Stefan, Gräf, Christian, Barr, B.W., Bell, A.S., Campbell, F., Cumming, A.V., Danilishin, S.L., Gordon, N.A., Hammond, G.D., Hennig, J., Houston, E.A., Huttner, S.H., Jones, R.A., Leavey, Sean S., Lück, Harald, Macarthur, J., Marwick, M., Rigby, S., Schilling, R., Sorazu, B., Spencer, A., Steinlechner, S., Strain, Kenneth A., and Hild, Stefan
Abstract: The second generation of large scale interferometric gravitational wave (GW) detectors will be limited by quantum noise over a wide frequency range in their detection band. Further sensitivity improvements for future upgrades or new detectors beyond the second generation motivate the development of measurement schemes to mitigate the impact of quantum noise in these instruments. Two strands of development are being pursued to reach this goal, focusing both on modifications of the well-established Michelson detector configuration and development of different detector topologies. In this paper, we present the design of the world's first Sagnac speed meter (SSM) interferometer, which is currently being constructed at the University of Glasgow. With this proof-of-principle experiment we aim to demonstrate the theoretically predicted lower quantum noise in a Sagnac interferometer compared to an equivalent Michelson interferometer, to qualify SSM for further research towards an implementation in a future generation large scale GW detector, such as the planned Einstein telescope observatory.
Published: 2014

33. Measurements of Superattenuator seismic isolation by Virgo interferometer

Author: N. Letendre, M. A. Bizouard, F. Marion, R. Passaquieti, G. Vedovato, L. Bonelli, G. A. Prodi, F. Antonucci, F. Frasconi, F. Travasso, A. Viceré, G. Gemme, M. Drago, P. La Penna, A. Colla, R. Flaminio, M. Yvert, M. Davier, Luca Gammaitoni, G. Cella, Christine Michel, C. Palomba, N. Morgado, Igor Neri, Riccardo Sturani, Silvio Pardi, C. N. Colacino, A. Pasqualetti, M. Tonelli, E. Tournefier, A. Brillet, M. Del Prete, A. Królak, Julien Moreau, D. Rosi ska, F. Piergiovanni, K. G. Arun, S. Frasca, J. Colas, Gianluca Persichetti, M. Blom, J.-M. Mackowski, L. Rolland, Fabrizio Barone, L. Pinard, A. Di Virgilio, M. Mohan, B. L. Swinkels, Gianpietro Cagnoli, F. Cleva, N. Man, O. Rabaste, Elena Cesarini, F. Ricci, A. Morgia, V. Fafone, G. Losurdo, M. Was, R. De Rosa, M. Colombini, Alessandra Toncelli, E. Genin, V. Moscatelli, F. Paoletti, H. Vocca, D. Verkindt, P. Ruggi, L. Bosi, F. Garufi, E. Chassande-Mottin, F. Vetrano, Benoit Sassolas, M. Lorenzini, Alessandra Corsi, V. Brisson, A. Dietz, Rosa Poggiani, M. Punturo, E. Campagna, N. Leroy, M. Pichot, S. Birindelli, Enrico Calloni, J. F. J. van den Brand, G. Vajente, Fabio Marchesoni, J. Marque, Patrice Hello, J. Franc, Piotr Jaranowski, Florent Robinet, Tania Regimbau, D. Sentenac, Tomasz Bulik, P. Astone, F. Fidecaro, G. M. Guidi, Leopoldo Milano, François Bondu, S. Van Der Putten, Stefano Bigotta, V. Dattilo, H. Heitmann, Stefan Hild, A. Giazotto, A. Gennai, I. Ferrante, Y. Minenkov, Fausto Acernese, R. Day, V. Loriette, H. J. Bulten, J-Y. Vinet, M. Mantovani, L. Di Fiore, B. Mours, C. Bradaschia, S. D'Antonio, Mirko Prato, M. Barsuglia, Andrea Chincarini, E. Cuoco, Anna Dari, P. Puppo, Ettore Majorana, F. Nocera, F. Cavalier, A. Rocchi, G. Ballardin, Sofiane Aoudia, C. Greverie, M. Pietka, M. Bitossi, Tenglin Li, I. Kowalska, Christian Corda, Th. S. Bauer, R. Budzy ski, D. Passuello, Simona Mosca, S. Braccini, M. Vavoulidis, E. Coccia, A. Di Lieto, G. Pagliaroli, F. Carbognani, M. Di Paolo Emilio, D. Huet, Andreas Freise, V. Re, M. Granata, F. Martelli, Claude Boccara, M. Parisi, M. G. Beker, F. Salemi, D. S. Rabeling, Rocco Romano, Benjamin Canuel, D. Buskulic, R. Cavalieri, F. Menzinger, J.-P. Coulon, J.-D. Fournier, I. Fiori, P. Rapagnani, A. Masserot, J. Trummer, Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Gravitation ( APC-Gravitation ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Istituto Nazionale di Fisica Nucleare [Milano] ( INFN ), Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), ESPCI ParisTech, Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), (Astro)-Particles Physics, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Istituto Nazionale di Fisica Nucleare [Milano] (INFN), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), F., Acernese, F., Antonucci, S., Aoudia, K. G., Arun, P., Astone, G., Ballardin, F., Barone, M., Barsuglia, Bauer, T. h. S., M. G., Beker, S., Bigotta, S., Birindelli, M., Bitossi, M. A., Bizouard, M., Blom, C., Boccara, F., Bondu, L., Bonelli, L., Bosi, S., Braccini, C., Bradaschia, A., Brillet, V., Brisson, R., Budzynski, T., Bulik, H. J., Bulten, D., Buskulic, G., Cagnoli, Calloni, Enrico, E., Campagna, B., Canuel, F., Carbognani, F., Cavalier, R., Cavalieri, G., Cella, E., Cesarini, E., Chassande Mottin, A., Chincarini, F., Cleva, E., Coccia, C. N., Colacino, J., Cola, A., Colla, M., Colombini, C., Corda, A., Corsi, J. P., Coulon, E., Cuoco, S., D’Antonio, A., Dari, V., Dattilo, M., Davier, R., Day, DE ROSA, Rosario, M., Del Prete, L., Di Fiore, A., Di Lieto, M., Di Paolo Emilio, A., Di Virgilio, A., Dietz, M., Drago, V., Fafone, I., Ferrante, F., Fidecaro, I., Fiori, R., Flaminio, J. D., Fournier, J., Franc, S., Frasca, F., Frasconi, A., Freise, L., Gammaitoni, Garufi, Fabio, G., Gemme, E., Genin, A., Gennai, A., Giazotto, M., Granata, C., Greverie, G., Guidi, H., Heitmann, P., Hello, S., Hild, D., Huet, P., Jaranowski, I., Kowalska, A., Królak, P., La Penna, N., Leroy, N., Letendre, T. G. F., Li, M., Lorenzini, V., Loriette, G., Losurdo, J. M., Mackowski, E., Majorana, N., Man, M., Mantovani, F., Marchesoni, F., Marion, J., Marque, F., Martelli, A., Masserot, F., Menzinger, C., Michel, Milano, Leopoldo, Y., Minenkov, M., Mohan, J., Moreau, N., Morgado, A., Morgia, Mosca, Simona, V., Moscatelli, B., Mour, I., Neri, F., Nocera, G., Pagliaroli, C., Palomba, F., Paoletti, Pardi, Silvio, Parisi, Maria, A., Pasqualetti, R., Passaquieti, D., Passuello, G., Persichetti, M., Pichot, F., Piergiovanni, M., Pietka, L., Pinard, R., Poggiani, M., Prato, G. A., Prodi, M., Punturo, P., Puppo, O., Rabaste, D. S., Rabeling, P., Rapagnani, V., Re, T., Regimbau, F., Ricci, F., Robinet, A., Rocchi, L., Rolland, R., Romano, D., Rosinska, P., Ruggi, F., Salemi, B., Sassola, D., Sentenac, R., Sturani, B., Swinkel, A., Toncelli, M., Tonelli, E., Tournefier, F., Travasso, J., Trummer, G., Vajente, J. F. J., van den Brand, S., van der Putten, M., Vavoulidi, G., Vedovato, D., Verkindt, F., Vetrano, A., Viceré, J. Y., Vinet, H., Vocca, M., Wa, and M., Yvert
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Virgo interferometer, ADVANCED LIGO, GRAVITATIONAL-WAVE DETECTION, 01 natural sciences, BAND, NOISE, Gravitational wave detectors, Optics, Settore FIS/05 - Astronomia e Astrofisica, Suspensions, 0103 physical sciences, 010306 general physics, DETECTOR, seismic isolation, suspensions, gravitational wave detectors, Physics, Einstein Telescope, 010308 nuclear & particles physics, business.industry, Gravitational wave, Attenuation, Settore FIS/01 - Fisica Sperimentale, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astronomy and Astrophysics, Seismic isolation, PERFORMANCE, GEO, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Vibration, Interferometry, SUSPENSION SYSTEM, Antenna (radio), [ PHYS.ASTR.IM ] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], business
Abstract: Each mirror of the interferometric gravitational wave antenna Virgo is attached to a Superattenuator, a chain of mechanical filters designed to suppress seismic vibrations, starting from a few Hz. The filter chain attenuation has been measured by exciting its suspension point with sinuisodal forces and using the interferometer as sensor. The attenuation, measured at different frequencies, is compliant with the requirements of the next generation antenna Advanced Virgo. In the third generation detector Einstein Telescope, the attenuation is sufficient above 3 Hz, independently of the underground site choice. © 2010 Elsevier B.V. All rights reserved.
Published: 2010
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34. Astrodynamical Space Test of Relativity Using Optical Devices I (ASTROD I)-A class-M fundamental physics mission proposal for Cosmic Vision 2015-2025

Author: Sergei A. Klioner, Li Wang, Thierry Appourchaux, Qiuhe Peng, Etienne Samain, Bernard Foulon, Andreas Wicht, H. A. Klein, Sergei M. Kopeikin, Hansjoerg Dittus, R. Burston, Xiaomin Zhang, Helen S. Margolis, Ernst M. Rasel, Yanbei Chen, Xinlian Luo, Albrecht Rüdiger, A. Lobo, Laurent Gizon, Hans Krüger, Stephan Theil, Haitao Wang, Hanns Selig, Claus Lämmerzahl, Michael Cruise, Ji Wu, Antonio Pulido Paton, Slava G. Turyshev, D. Shaul, T. J. Sumner, Linqing Wen, Achim Peters, Wei-Tou Ni, Cheng Zhao, Patrick Gill, Pierre Touboul, and Science and Technology Facilities Council (STFC)
Subjects: Cosmic Vision, General relativity, ASTROD-I, FOS: Physical sciences, Exploring the microscopic origin of gravity, NASA Deep Space Network, General Relativity and Quantum Cosmology (gr-qc), Astronomy & Astrophysics, ACCELERATION, Astrophysics, General Relativity and Quantum Cosmology, Gravitational-wave detection, High Energy Physics - Phenomenology (hep-ph), GRAVITY, LASER LINK, Solar g-mode detection, GENERAL-RELATIVITY, SOLAR, Physics, LISA, Science & Technology, Spacecraft, business.industry, Gravitational wave, Astrophysics (astro-ph), Probing the fundamental laws of spacetime, Astronomy, Astronomy and Astrophysics, Solar physics, Probing the fundamental laws mof spacetime, Gravitational constant, High Energy Physics - Phenomenology, 0201 Astronomical And Space Sciences, Mapping solar-system gravity, Space and Planetary Science, ASTROD, ASTROD I, Physical Sciences, DISTURBANCES, Physics::Space Physics, Gravitational wave detection, Testing relativistic gravity, Astrophysics::Earth and Planetary Astrophysics, business, Heliocentric orbit
Abstract: ASTROD I is a planned interplanetary space mission with multiple goals. The primary aims are: to test General Relativity with an improvement in sensitivity of over 3 orders of magnitude, improving our understanding of gravity and aiding the development of a new quantum gravity theory; to measure key solar system parameters with increased accuracy, advancing solar physics and our knowledge of the solar system and to measure the time rate of change of the gravitational constant with an order of magnitude improvement and the anomalous Pioneer acceleration, thereby probing dark matter and dark energy gravitationally. It is an international project, with major contributions from Europe and China and is envisaged as the first in a series of ASTROD missions. ASTROD I will consist of one spacecraft carrying a telescope, four lasers, two event timers and a clock. Two-way, two-wavelength laser pulse ranging will be used between the spacecraft in a solar orbit and deep space laser stations on Earth, to achieve the ASTROD I goals. A second mission, ASTROD II is envisaged as a three-spacecraft mission which would test General Relativity to one part per billion, enable detection of solar g-modes, measure the solar Lense-Thirring effect to 10 parts per million, and probe gravitational waves at frequencies below the LISA bandwidth. In the third phase (ASTROD III or Super-ASTROD), larger orbits could be implemented to map the outer solar system and to probe primordial gravitational-waves at frequencies below the ASTROD II bandwidth., Comment: 26 pages, 11 figures, shortened from the original cosmic vision proposal, submitted to Experimental Astronomy; this version, shortened to 25 pages, re-organized and added references, is accepted for publication in Experimental Astronomy
Published: 2009

35. Laser with an in-loop relative frequency stability of 1.0x10(-21) on a 100-ms time scale for gravitational-wave detection

Author: Acernese, F., Alshourbagy, M., Antonucci, F., Aoudia, S., Arun, K. G., Astone, P., Ballardin, G., Barone, F., Barsotti, L., Barsuglia, M., Bauer, T. S., Bigotta, S., Birindelli, S., Bizouard, M. A., Boccara, C., Bondu, F., Bonelli, L., Bosi, L., Braccini, S., Bradaschia, C., Brillet, A., Brisson, V., Bulten, H. J., Buskulic, D., Cagnoli, G., Calloni, E., Campagna, E., Canuel, B., Carbognani, F., Carbone, L., Cavalier, F., Cavalieri, R., Cella, G., Cesarini, E., Chassande Mottin, E., Chatterji, S., Cleva, F., Coccia, E., Colas, J., Colombini, M., Corda, C., Corsi, A., Cottone, F., Coulon, J. P., Cuoco, E., D'Antonio, S., Dari, A., Dattilo, V., Davier, M., Rosa, R. D., Prete, M. D., Fiore, L. D., Lieto, A. D., Paolo, M. D., Virgilio, A. D., Fafone, V., Ferrante, I., Fidecaro, F., Fiori, I., Flaminio, R., Fournier, J. D., Frasca, S., Frasconi, F., Gammaitoni, L., Garufi, F., Gemme, G., Genin, E., Gennai, A., Giazotto, A., Granata, M., Granata, V., Greverie, C., Guidi, G., Heitmann, H., Hello, P., Hild, S., Huet, D., Penna, P. L., Laval, M., Leroy, N., Letendre, N., Lorenzini, M., Loriette, V., Losurdo, G., Mackowski, J. M., Majorana, E., Man, N., Mantovani, M., Marchesoni, Fabio, Marion, F., Marque, J., Martelli, F., Masserot, A., Menzinger, F., Michel, C., Milano, L., Minenkov, Y., Mitra, S., Mohan, M., Moreau, J., Morgado, N., Morgia, A., Mosca, S., Mours, B., Neri, I., Nocera, F., Pagliaroli, G., Palomba, C., Paoletti, F., Pardi, S., Pasqualetti, A., Passaquieti, R., Passuello, D., Persichetti, G., Piergiovanni, F., Pinard, L., Poggiani, R., Punturo, M., Puppo, P., Rabaste, O., Rapagnani, P., Regimbau, T., Ricci, F., Rocchi, A., Rolland, L., Romano, R., Ruggi, P., Sassolas, B., Sentenac, D., Swinkels, B. L., Terenzi, R., Toncelli, A., Tonelli, M., Tournefier, E., Travasso, F., Trummer, J., Vajente, G., J. F. J., Der, S. v., Verkindt, D., Vetrano, F., Vicere, A., Vinet, J. Y., Vocca, H., Was, M., and Yvert, M.
Subjects: 1064 nm lasers, Allan standard deviation, Frequency noise, Gravitational wave detectors, Gravitational waves, Gravitational-wave detection, Laser frequency, Relative frequencies, Time-scale, Detectors, Gravitation, Gravity waves, Lasers, Settore FIS/01 - Fisica Sperimentale
Published: 2009

36. Lock acquisition of the Virgo gravitational wave detector

Author: G. Losurdo, G. Cagnoli, D. Passuello, M. A. Bizouard, M. Alshourbagy, F. Antonucci, Fabio Marchesoni, F. Paoletti, P. Ruggi, F. Frasconi, R. Flaminio, Tania Regimbau, J. F. J. van den Brand, L. Baggio, R. De Rosa, Frédérique Marion, V. Fafone, F. Travasso, M. Laval, C. Palomba, A. Rocchi, S. Kreckelbergh, P. Rapagnani, D. Grosjean, G. Ballardin, V. Brisson, Luca Gammaitoni, P. Puppo, F. Cavalier, L. Bosi, N. Letendre, L. Rolland, P. Amico, Fabrizio Barone, M. Mohan, A. Gennai, A. Di Virgilio, P. La Penna, M. Del Prete, S. Frasca, Anna Dari, Stefano Bigotta, S. Hamdani, Salvatore Solimeno, K.G. Arun, A. Di Lieto, F. Garufi, S. Hebri, A. Viceré, G. Cella, F. Vetrano, S. Birindelli, A. Giazotto, I. Ferrante, J.-Y. Vinet, Rosa Poggiani, Shourov Chatterji, D. Sentenac, Igor Neri, E. Tournefier, M. Punturo, O. Rabaste, V. Loriette, S. Van Der Putten, M. Tonelli, Elena Cesarini, F. Ricci, Iolanda Ricciardi, B. Mours, S. D'Antonio, Lisa Barsotti, C. N. Man, Alessandra Toncelli, V. Granata, F. Carbognani, H. Vocca, Francesco Cottone, L. Pinard, E. Coccia, F. Fidecaro, G. M. Guidi, N. Leroy, Simona Mosca, J.-M. Mackowski, A. Masserot, M. Di Paolo Emilio, Alessandra Corsi, G. Vajente, N. Morgado, François Bondu, L. Di Fiore, A. Pasqualetti, M. Barsuglia, Saverio Avino, Fausto Acernese, R. Passaquieti, Silvio Pardi, D. Huet, Th. S. Bauer, E. Cuoco, B. Lopez, M. Mantovani, B. L. Swinkels, Rocco Romano, M. Lorenzini, E. Genin, L. Milano, H. Heitmann, M. Yvert, D. Buskulic, M. Davier, F. Menzinger, E. Chassande-Mottin, Julien Moreau, F. Piergiovanni, E. Campagna, Matthew Evans, Claude Boccara, Ettore Majorana, R. Cavalieri, J.-P. Coulon, J.-D. Fournier, I. Fiori, Y. Minenkov, Sofiane Aoudia, F. Cleva, Patrice Hello, G. Pagliaroli, C. Greverie, Christian Corda, R. Terenzi, C. Bradaschia, S. Mitra, D. Verkindt, Enrico Calloni, P. Astone, J. Marque, F. Nocera, S. Braccini, V. Dattilo, C. Michel, A. Brillet, Ecole Supérieure de Physique et de Chimie Industrielles ( ESPCI ), Mairie de Paris, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), APC - Gravitation ( APC-Gravitation ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Virgo, Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), VIRGO, Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire des matériaux avancés (LMA), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), F., Acernese, M., Alshourbagy, P., Amico, F., Antonucci, S., Aoudia, K. G., Arun, P., Astone, Avino, Saverio, L., Baggio, G., Ballardin, F., Barone, L., Barsotti, M., Barsuglia, Bauer, T. h. S., S., Bigotta, S., Birindelli, M. A., Bizouard, C., Boccara, F., Bondu, L., Bosim, S., Braccini, C., Bradaschia, A., Brillet, V., Brisson, D., Buskulic, G., Cagnoli, Calloni, Enrico, E., Campagna, F., Carbognani, F., Cavalier, R., Cavalieri, G., Cella, E., Cesarini, E., Chassande Mottin, S., Chatterji, F., Cleva, E., Coccia, C., Corda, A., Corsi, F., Cottone, J. P., Coulon, E., Cuoco, S., D’Antonio, A., Dari, V., Dattilo, M., Davier, DE ROSA, Rosario, M., Del Prete, L., Di Fiore, A., Di Lieto, M., Di Paolo Emilio, A., Di Virgilio, M., Evan, V., Fafone, I., Ferrante, F., Fidecaro, I., Fiori, R., Flaminio, J. D., Fournier, S., Frasca, F., Frasconi, L., Gammaitoni, Garufi, Fabio, E., Genin, A., Gennai, A., Giazotto, V., Granata, C., Greverie, D., Grosjean, G., Guidi, S., Hamdani, S., Hebri, H., Heitmann, P., Hello, D., Huet, S., Kreckelbergh, P., La Penna, M., Laval, N., Leroy, N., Letendre, B., Lopez, M., Lorenzini, V., Loriette, G., Losurdo, J. M., Mackowski, E., Majorana, C. N., Man, M., Mantovani, F., Marchesoni, F., Marion, J., Marque, A., Masserot, F., Menzinger, C., Michel, Milano, Leopoldo, Y., Minenkov, S., Mitra, M., Mohan, J., Moreau, N., Morgado, Mosca, Simona, B., Mour, I., Neri, F., Nocera, G., Pagliaroli, C., Palomba, F., Paoletti, Pardi, Silvio, A., Pasqualetti, R., Passaquieti, D., Passuello, F., Piergiovanni, L., Pinard, R., Poggiani, M., Punturo, P., Puppo, O., Rabaste, P., Rapagnani, T., Regimbau, F., Ricci, I., Ricciardi, A., Rocchi, L., Rolland, R., Romano, P., Ruggi, D., Sentenac, Solimeno, Salvatore, B. L., Swinkel, R., Terenzi, A., Toncelli, M., Tonelli, E., Tournefier, F., Travasso, G., Vajente, J. F. J., van den Brand, S., van der Putten, D., Verkindt, F., Vetrano, A., Viceré, J. Y., Vinet, H., Vocca, M., Yvert, Ecole Supérieure de Physique et de Chimie Industrielles (ESPCI), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), and (Astro)-Particles Physics
Subjects: Gravitational-wave observatory, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics::Instrumentation and Detectors, Physics::Optics, Optical instruments, 01 natural sciences, VIRGO detector, Gravitational wave detectors, Finesse, Data acquisition, Gravitational-wave detector, Lock acquisition, Working point, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Physics, Fabry-Perot interferometers, Gravitational effects, Gravity waves, Interferometers, Interferometry, Mergers and acquisitions, Control systems, Fabry-Perot cavities, Gravitational-wave detection, Optical configurations, Scientific data, Virgo interferometer, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Detector, Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, [ SDU.ASTR.CO ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Record locking, [ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010309 optics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optics, control systems, gravitational wave detectors, interferometry, lock acquisition, 0103 physical sciences, SDG 7 - Affordable and Clean Energy, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [ SDU.ASTR ] Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, business.industry, Gravitational wave, Astronomy and Astrophysics, business, INTERFEROMETER
Abstract: The Virgo interferometer for gravitational wave detection has concluded four months of scientific data acquisition in its final optical configuration (a power-recycled interferometer with Fabry-Perot cavities in the arms). The lock acquisition technique developed to bring and keep the Virgo detector on its working point largely proved to be very efficient and robust. In this paper we describe the variable finesse lock acquisition technique and we discuss the performance of the whole locking system. (C) 2008 Elsevier B.V. All rights reserved.
Published: 2008
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37. Optomechanical coupling, back-action and quantum limits in ultrasensitive optical measurements

Author: Caniard, Thomas, Laboratoire Kastler Brossel (LKB (Jussieu)), Université Pierre et Marie Curie - Paris 6 (UPMC)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris VI, Antoine Heidmann(heidmann@spectro.jussieu.fr), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), and Caniard, Thomas
Subjects: Couplage optomécanique, Limite Quantique Standard, Détection des ondes gravitationnelles, [PHYS.PHYS.PHYS-ATOM-PH]Physics [physics]/Physics [physics]/Atomic Physics [physics.atom-ph], Gravitational-wave detection, Cavité de grande finesse, Standard Quantum Limit, Small displacement measurement, Back-action noise in a measurement, Thermal noise of a mirror, Optomechanical coupling, [PHYS.PHYS.PHYS-ATOM-PH] Physics [physics]/Physics [physics]/Atomic Physics [physics.atom-ph], Bruit thermique d'un miroir, High-finesse cavity, Mesure de petits déplacements, Action en retour de la mesure
Abstract: We present a very sensitive optical measurement of small displacements of a mirror. Thanks to the use of a very high-finesse cavity, we have reached a sensitivity of 10-20 m.Hz-1/2 over a wide frequency band (severalhundreds of kilohertz).Our setup allows us to study accurately the noise sources in an optical measurement and the resulting limits. We are particularly interested in the optomechanical coupling induced by the radiation pressure exerted by light on a movable mirror. The mirror can move in response to the quantum fluctuations of radiation pressure, leading to an additional position noise. This back-action of the measurement on the system is responsible for quantum limits in the measurement.Among the improvements made on the experimental setup, we have injected two laser beams into the cavity in order to study the quantum effects of optomechanical coupling. We have demonstrated a cancellation of back-action noise in the measurement resulting from a destructive interference between the displacements of both mirrors of the cavity. We present the potential applications of this effect for the improvement of the sensitivity in optical measurements, especially in gravitational-wave detectors based on dual resonators., Nous présentons une expérience de mesure optique ultrasensible de petits déplacements d'un miroir. Grâce à l'utilisation d'une cavité Fabry-Perot de très grande finesse, nous avons atteint une sensibilité de 10-20 m.Hz-1/2 sur une plage de plusieurs centaines de kilohertz.Notre montage permet de mener une étude approfondie des sources de bruit dans une mesure optique et des limites de sensibilité associées. Nous nous intéressons en particulier au couplage optomécanique résultant de l'action réciproque entre la lumière et un miroir mobile. Par l'intermédiaire de la force de pression de radiation, les fluctuations quantiques d'intensité du faisceau génèrent un bruit de position supplémentaire du miroir. Ce bruit constitue l'action en retour de la mesure de position et entraîne l'existence de limites quantiques de sensibilité.Parmi les améliorations réalisées sur le montage, nous avons mis en place un système de double injection de faisceaux laser dans la cavité afin d'étudier les effets quantiques du couplage optomécanique. Nous avons mis en évidence une suppression de l'action en retour de la mesure par interférence destructive entre les réponses des deux miroirs formant la cavité. Nous discutons des applications potentielles de cet effet afin d'améliorer la sensibilité des mesures optiques, notamment pour les détecteurs doublement résonnants d'ondes gravitationnelles.
Published: 2007

38. Building blocks for future detectors: Silicon test masses and 1550 nm laser light

Author: Schnabel, Roman, Britzger, M., Brückner, F., Burmeister, O., Danzmann, Karsten, Dück, J., Eberle, Tobias, Friedrich, Daniel, Lück, Harald, Mehmet, Moritz, Nawrodt, Ronny, Steinlechner, S., Willke, Benno, Schnabel, Roman, Britzger, M., Brückner, F., Burmeister, O., Danzmann, Karsten, Dück, J., Eberle, Tobias, Friedrich, Daniel, Lück, Harald, Mehmet, Moritz, Nawrodt, Ronny, Steinlechner, S., and Willke, Benno
Abstract: Current interferometric gravitational wave detectors use the combination of quasi-monochromatic, continuous-wave laser light at 1064 nm and fused silica test masses at room temperature. Detectors of the third generation, such as the Einstein-Telescope, will involve a considerable sensitivity increase. The combination of 1550 nm laser radiation and crystalline silicon test masses at low temperatures might be important ingredients in order to achieve the sensitivity goal. Here we compare some properties of the fused silica and silicon test mass materials relevant for decreasing the thermal noise in future detectors as well as the recent technology achievements in the preparation of laser radiation at 1064 nm and 1550 nm relevant for decreasing the quantum noise. We conclude that silicon test masses and 1550 nm laser light have the potential to form the future building blocks of gravitational wave detection.
Published: 2010

39. Formulation of instrument noise analysis techniques and their use in the commissioning of the gravitational wave observatory, GEO 600

Author: Smith, Joshua Ryan
Subjects: Gravitational-wave detection, noise analysis, ddc:530, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, control systems
Abstract: [no abstract]
Published: 2006

40. The LISA Pathfinder Mission

Author: Armano, M., Audley, H., Auger, G., Baird, J., Binetruy, P., Born, M., Bortoluzzi, D., Brandt, N., Bursi, A., Caleno, M., Cavalleri, A., Cesarini, A., Cruise, M., Danzmann, K., Diepholz, I., Dolesi, R., Dunbar, N., Ferraioli, L., Ferroni, V., Fitzsimons, E., Freschi, M., Gallegos, J., Marirrodriga, C.G., Gerndt, R., Gesa, L.I., Gibert, F., Giardini, D., Giusteri, R., Grimani, C., Harrison, I., Heinzel, G., Hewitson, M., Hollington, D., Hueller, M., Huesler, J., Inchauspé, H., Jennrich, O., Jetzer, P., Johlander, B., Karnesis, N., Kaune, B., Korsakova, N., Killow, C., Lloro, I., Maarschalkerweerd, R., Madden, S., Mance, D., Martín, V., Martin-Porqueras, F., Mateos, I., McNamara, P., Mendes, J., Mendes, L., Moroni, A., Nofrarias, M., Paczkowski, S., Perreur-Lloyd, M., Petiteau, A., Pivato, P., Plagnol, E., Prat, P., Ragnit, U., Ramos-Castro, J., Reiche, J., Perez, J.A.R., Robertson, D., Rozemeijer, H., Russano, G., Sarra, P., Schleicher, A., Slutsky, J., Sopuerta, C.F., Sumner, T., Texier, D., Thorpe, J., Trenkel, C., Tu, H.B., Vetrugno, D., Vitale, S., Wanner, G., Ward, H., Waschke, S., Wass, P., Wealthy, D., Wen, S., Weber, W., Wittchen, A., Zanoni, C., Ziegler, T., and Zweifel, P.
Subjects: Critical technologies, Physical principles, Lisa technology packages, Gravitational effects, Measurement concepts, Gravity waves, Propulsion, 7. Clean energy, Technology validations, Gravitational wave detectors, Gravitational-wave detection, Low pass filters, Free flight, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, Inertial navigation systems, European Space Agency, Space probes, Konferenzschrift, Gravitation
Abstract: LISA Pathfinder (LPF), the second of the European Space Agency's Small Missions for Advanced Research in Technology (SMART), is a dedicated technology validation mission for future spaceborne gravitational wave detectors, such as the proposed eLISA mission. LISA Pathfinder, and its scientific payload - the LISA Technology Package - will test, in flight, the critical technologies required for low frequency gravitational wave detection: it will put two test masses in a near-perfect gravitational free-fall and control and measure their motion with unprecedented accuracy. This is achieved through technology comprising inertial sensors, high precision laser metrology, drag-free control and an ultra-precise micro-Newton propulsion system. LISA Pathfinder is due to be launched in mid-2015, with first results on the performance of the system being available 6 months thereafter. The paper introduces the LISA Pathfinder mission, followed by an explanation of the physical principles of measurement concept and associated hardware. We then provide a detailed discussion of the LISA Technology Package, including both the inertial sensor and interferometric readout. As we approach the launch of the LISA Pathfinder, the focus of the development is shifting towards the science operations and data analysis - this is described in the final section of the paper.

41. GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

Author: Abbott, B.P., Abbott, R., Abbott, T.D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R.X., Adya, V.B., LIGO Scientific Collaboration And Virgo Collaboration, Affeldt, Christoph, Aufmuth, Peter, Bergmann, G., Bisht, Aparna, Bode, N., Booker, Phillip, Brinkmann, M., Cabero, M., Danilishin, Stefan L., Danzmann, Karsten, Dent, Thomas, De Varona, Omar, Doravari, S., Hanke, Manuela Melanie, Hennig, J., Heurs, M., Hochheim, Sven, Junker, J., Karvinen, K.S., Khan, S., Kaufer, S., Kirchhoff, R., Koch, P., Koehlenbeck, S.M., Koper, N., Kringel, V., Kuehn, G., Leavey, S., Lehmann, J., Lück, Harald, Mehmet, M., Mukherjee, Arunava, Nery, M., Ohme, F., Oppermann, P., Papa, M.A., Phelps, M., Puncken, O., Rüdiger, A., Schreiber, E., Schulte, B.W., Setyawati, Y., Standke, M., Steinke, M., Steinmeyer, D., Wei, L.-W., Weinert, M., Wellmann, F., Weßels, P., Wilken, D.M., Willke, B., Wimmer, M.H., Winkler, W., Wittel, H., Woehler, J., and Wu, D.S.
Subjects: Neutrons, Binary neutron stars, Astrophysics::High Energy Astrophysical Phenomena, Confidence interval, Gravitational effects, Flocculation, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravity waves, False alarm rate, Population statistics, Stars, Merging, Upper limits, Neutron stars, Gravitational wave detectors, General Relativity and Quantum Cosmology, Gravitational-wave detection, 13. Climate action, Wave transients, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, Signal detection
Abstract: We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1 Ma™ during the first and second observing runs of the advanced gravitational-wave detector network. During the first observing run (O1), from September 12, 2015 to January 19, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November 30, 2016 to August 25, 2017, saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to the observation of gravitational waves from a total of seven binary black hole mergers, four of which we report here for the first time: GW170729, GW170809, GW170818, and GW170823. For all significant gravitational-wave events, we provide estimates of the source properties. The detected binary black holes have total masses between 18.6-0.7+3.2 Mâ™ and 84.4-11.1+15.8 Mâ™ and range in distance between 320-110+120 and 2840-1360+1400 Mpc. No neutron star-black hole mergers were detected. In addition to highly significant gravitational-wave events, we also provide a list of marginal event candidates with an estimated false-alarm rate less than 1 per 30 days. From these results over the first two observing runs, which include approximately one gravitational-wave detection per 15 days of data searched, we infer merger rates at the 90% confidence intervals of 110-3840 Gpc-3 y-1 for binary neutron stars and 9.7-101 Gpc-3 y-1 for binary black holes assuming fixed population distributions and determine a neutron star-black hole merger rate 90% upper limit of 610 Gpc-3 y-1. © 2019 authors. Published by the American Physical Society.

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