Seismic isolation of Advanced LIGO: Review of strategy, instrumentation and performance

Matichard, F.; Lantz, B.; Mittleman, R.; Mason, K.; Kissel, J. S.; Abbott, B. P.; Biscans, S.; McIver, J.; Abbott, R.; Abbott, S.; Allwine, Eric; Barnum, S.; Birch, J.; Celerier, C.; Clark, D.; Coyne, D. C.; DeBra, D.; DeRosa, R. T.; Evans, M.; Foley, S.; Fritschel, P.; Giaime, J. A.; Gray, C.; Grabeel, Gregory; Hanson, J.; Hardham, C.; Hillard, Michael; Hua, W.; Kucharczyk, C.; Landry, M.; Roux, A. Le; Lhuillier, Vincent; Macleod, D. M.; MacInnis, M.; Mitchell, Robert W.; O’Reilly, B.; Ottaway, D. J.; Paris, H. R.; Pele, A.; Puma, Michael; Radkins, H.; Ramet, C.; Robinson, Mitchell B.; Ruet, Laurent; Sarin, P.; Shoemaker, D. H.; Stein, Andy; Thomas, Jeremy; Vargas, M.; Venkateswara, K.; Warner, J.; Wen, S.

doi:10.1088/0264-9381/32/18/185003

Cited by 171 publications

(153 citation statements)

References 43 publications

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“…The response of the Advanced LIGO interferometers is diminished at high frequencies due to common and differential coupled cavity poles (f + and f − ) according to the transfer functions Several critical improvements distinguish Advanced LIGO from the initial detectors [15]. The much improved seismic isolation system [23] reduces the impact of ground vibrations. All photodetectors, used in the observing mode, are installed in vacuum to avoid the coupling of ambient acoustic noise to the gravitational wave channel.…”

Section: Interferometer Configurationmentioning

confidence: 99%

Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

Мартынов¹,

Hall²,

Abbott³

et al. 2016

Phys. Rev. D

356

268

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The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than 10 −23 / √ Hz was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the astrophsyical strain sensitivity. The average distance at which coalescing binary black hole systems with individual masses of 30 M could be detected above a signal-to-noise ratio (SNR) of 8 was 1.3 Gpc, and the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of the Universe increased by a factor 69 and 43, respectively. These improvements helped Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914.

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Section: Interferometer Configurationmentioning

confidence: 99%

Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

Мартынов¹,

Hall²,

Abbott³

et al. 2016

Phys. Rev. D

356

268

View full text Add to dashboard Cite

show abstract

“…Each of these systems consists of four stages, suspended as cascading pendulums [8,9], which isolate the test mass from residual motion of the supporting active isolation system [10]. Each suspension system also includes an adjacent, nearlyidentical, cascaded reaction mass pendulum chain which can be used to independently generate reaction forces on each mass of the test mass pendulum chain.…”

Section: B Actuation Functionmentioning

confidence: 99%

Calibration of the Advanced LIGO detectors for the discovery of the binary black-hole merger GW150914

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. D

123

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In Advanced LIGO, detection and astrophysical source parameter estimation of the binary black hole merger GW150914 requires a calibrated estimate of the gravitational-wave strain sensed by the detectors. Producing an estimate from each detector's differential arm length control loop readout signals requires applying time domain filters, which are designed from a frequency domain model of the detector's gravitational-wave response. The gravitational-wave response model is determined by the detector's optomechanical response and the properties of its feedback control system. The measurements used to validate the model and characterize its uncertainty are derived primarily from a dedicated photon radiation pressure actuator, with cross-checks provided by optical and radio frequency references. We describe how the gravitational-wave readout signal is calibrated into equivalent gravitational-wave-induced strain and how the statistical uncertainties and systematic errors are assessed. Detector data collected over 38 calendar days, from September 12 to October 20, 2015, contain the event GW150914 and approximately 16 days of coincident data used to estimate the event false alarm probability. The calibration uncertainty is less than 10% in magnitude and 10°in phase across the relevant frequency band, 20 Hz to 1 kHz.

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“…3 To be successful, the LIGO detectors must reach an extreme displacement sensitivity in the audio frequency band. At the low frequency end of this band (10)(11)(12)(13)(14)(15)(16)(17)(18)(19)(20), the horizontal motion of the 40 kg fused silica mirrors, acting as test masses, must be only about 10 −19 m/ √ Hz. Since the detector is located on the ground, it employs complex seismic isolation systems to reduce the contamination of the sensitivity by local seismic activity.…”

Section: Introductionmentioning

confidence: 99%

“…Since the detector is located on the ground, it employs complex seismic isolation systems to reduce the contamination of the sensitivity by local seismic activity. The Advanced LIGO test mass suspension system, 5, 18 shown schematically in Fig. 1, consists of a quadruple pendulum for horizontal isolation and incorporates three stages of 50 cmlong cantilever spring pairs, made of maraging steel 10 for vertical isolation.…”

Section: Introductionmentioning

confidence: 99%

An instrument to measure mechanical up-conversion phenomena in metals in the elastic regime

Vajente

Quintero

et al. 2016

Review of Scientific Instruments

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Physical aging of plastoferrites under tensile stress and its effect on microwave properties J. Appl. Phys. 104, 064108 (2008) Crystalline materials, such as metals, are known to exhibit deviation from a simple linear relation between strain and stress when the latter exceeds the yield stress. In addition, it has been shown that metals respond to varying external stress in a discontinuous way in this regime, exhibiting discrete releases of energy. This crackling noise has been extensively studied both experimentally and theoretically when the metals are operating in the plastic regime. In our study, we focus on the behavior of metals in the elastic regime, where the stresses are well below the yield stress. We describe an instrument that aims to characterize non-linear mechanical noise in metals when stressed in the elastic regime. In macroscopic systems, this phenomenon is expected to manifest as a non-stationary noise modulated by external disturbances applied to the material, a form of mechanical up-conversion of noise. The main motivation for this work is for the case of maraging steel components (cantilevers and wires) in the suspension systems of terrestrial gravitational wave detectors. Such instruments are planned to reach very ambitious displacement sensitivities, and therefore mechanical noise in the cantilevers could prove to be a limiting factor for the detectors' final sensitivities, mainly due to non-linear up-conversion of low frequency residual seismic motion to the frequencies of interest for the gravitational wave observations. We describe here the experimental setup, with a target sensitivity of 10 −15 m/ √Hz in the frequency range of 10-1000 Hz, a simple phenomenological model of the non-linear mechanical noise, and the analysis method that is inspired by this model. Published by AIP Publishing. [http://dx

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Seismic isolation of Advanced LIGO: Review of strategy, instrumentation and performance

Cited by 171 publications

References 43 publications

Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

Calibration of the Advanced LIGO detectors for the discovery of the binary black-hole merger GW150914

An instrument to measure mechanical up-conversion phenomena in metals in the elastic regime

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