Advanced LIGO two-stage twelve-axis vibration isolation and positioning platform. Part 1: Design and production overview

Matichard, F.; Lantz, B.; Mason, K.; Mittleman, R.; Abbott, B. P.; Abbott, S.; Allwine, Eric; Barnum, S.; Birch, J.; Biscans, S.; Clark, D.; Coyne, D. C.; DeBra, D.; DeRosa, R.; Foley, S.; Fritschel, P.; Giaime, J. A.; Gray, C.; Grabeel, Gregory; Hanson, J.; Hillard, Michael; Kissel, J. S.; Kucharczyk, C.; Roux, A. Le; Lhuillier, Vincent; MacInnis, M.; O’Reilly, B.; Ottaway, D. J.; Paris, H. R.; Puma, Michael; Radkins, H.; Ramet, C.; Robinson, Mitchell B.; Ruet, Laurent; Sareen, P.; Shoemaker, D. H.; Stein, Andy; Thomas, Jeremy; Vargas, M.; Warner, J.

doi:10.1016/j.precisioneng.2014.09.010

Cited by 89 publications

(70 citation statements)

References 33 publications

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“…The ISI [38] consists of three stages (each a stiff mechanical structure) that are suspended and sprung in sequence: stage 0 is the support structure connected to the HEPI frame; stage 1 is suspended and sprung from stage 0; stage 2 is suspended and sprung from stage 1. The elastic, structural modes of stages 1 and 2 are designed to be > 150 Hz in order to keep them high above the upper unity gain frequency (~40 Hz) of the control system.…”

Section: Design Descriptionmentioning

confidence: 99%

Advanced LIGO

Aasi¹,

Abbott²,

Abbott³

et al. 2015

Class. Quantum Grav.

2,873

2,281

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The Advanced LIGO gravitational wave detectors are second generation instruments designed and built for the two LIGO observatories in Hanford, WA and Livingston, LA. The two instruments are identical in design, and are specialized versions of a Michelson interferometer with 4 km long arms. As in initial LIGO, Fabry-Perot cavities are used in the arms to increase the interaction time with a gravitational wave, and power recycling is used to increase the effective laser power. Signal recycling has been added in Advanced LIGO to improve the frequency response. In the most sensitive frequency region around 100 Hz, the design strain sensitivity is a factor of 10 better than initial LIGO. In addition, the low frequency end of the sensitivity band is moved from 40 Hz down to 10 Hz. All interferometer components have been replaced with improved technologies to achieve this sensitivity gain. Much better seismic isolation and test mass suspensions are responsible for the gains at lower frequencies. Higher laser power, larger test masses and improved mirror coatings lead to the improved sensitivity at mid-and highfrequencies. Data collecting runs with these new instruments are planned to begin in mid-2015.

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Section: Design Descriptionmentioning

confidence: 99%

Advanced LIGO

Aasi¹,

Abbott²,

Abbott³

et al. 2015

Class. Quantum Grav.

2,873

2,281

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“…These passive filters have resonances as low as 0.4 Hz and provide isolation as 1/f 8 in the detection bandwidth. The pendulums are mounted on multistage active platforms [41,42]. These systems use very-lownoise inertial sensors to provide the required isolation in the detection band and at lower frequencies (below 10 Hz).…”

Section: A Seismic and Thermal Noisesmentioning

confidence: 99%

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

Мартынов¹,

Hall²,

Abbott³

et al. 2016

Phys. Rev. D

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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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“…These are quite good at reducing the lower frequency seismic noises. One can then place the mirror within a damped harmonic oscillator as an additional passive isolation [71,72], which provides vibration isolation above its resonant frequency. Let d and D denote the displacement of the mirror and the ground respectively, then we can lower the peak ratio for d/D by tuning the damping coefficient (the downside is that isolation at non-peak frequencies gets worse), make the d/D curve drop with a steeper inclination into higher seismic motion frequencies by making the oscillator multi-staged [73] (the price to pay is the appearance of multiple resonant peaks), and produce better isolation at higher frequencies by lowering the resonant frequency (this is more complex to realize).…”

Section: Noisesmentioning

confidence: 99%

Gravitational wave astronomy: the current status

Blair

Zhao

et al. 2015

Sci. China Phys. Mech. Astron.

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In the centenary year of Einstein's General Theory of Relativity, this paper reviews the current status of gravitational wave astronomy across a spectrum which stretches from attohertz to kilohertz frequencies. Sect. 1 of this paper reviews the historical development of gravitational wave astronomy from Einstein's first prediction to our current understanding the spectrum. It is shown that detection of signals in the audio frequency spectrum can be expected very soon, and that a north-south pair of next generation detectors would provide large scientific benefits. Sect. 2 reviews the theory of gravitational waves and the principles of detection using laser interferometry. The state of the art Advanced LIGO detectors are then described. These detectors have a high chance of detecting the first events in the near future. Sect. 3 reviews the KAGRA detector currently under development in Japan, which will be the first laser interferometer detector to use cryogenic test masses. Sect. 4 of this paper reviews gravitational wave detection in the nanohertz frequency band using the technique of pulsar timing. Sect. 5 reviews the status of gravitational wave detection in the attohertz frequency band, detectable in the polarisation of the cosmic microwave background, and discusses the prospects for detection of primordial waves from the big bang. The techniques described in sects. 1-5 have already placed significant limits on the strength of gravitational wave sources. Sects. 6 and 7 review ambitious plans for future space based gravitational wave detectors in the millihertz frequency band. Sect. 6 presents a roadmap for development of space based gravitational wave detectors by China while sect. 7 discusses a key enabling technology for space interferometry known as time delay interferometry. gravitational waves, ground based detectors, pulsar timing, spaced based detectors, CMB PACS number(s): 04.80. Nn, 07.20.Mc,

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Advanced LIGO two-stage twelve-axis vibration isolation and positioning platform. Part 1: Design and production overview

Cited by 89 publications

References 33 publications

Advanced LIGO

Advanced LIGO

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

Gravitational wave astronomy: the current status

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