Polarization Sagnac interferometer with a reflective grating beam splitter

Traeger, S.; Beyersdorf, P. T.; Goddard, L.C.; Gustafson, E. K.; Fejer, M. M.; Byer, Robert L.

doi:10.1364/ol.25.000722

Cited by 11 publications

(11 citation statements)

References 8 publications

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“…In parallel, it was realized by Chen and Khalili [47,89] that the zero area Sagnac interferometer [142,16,146] actually implements the initial double-measurement variant of the quantum speedmeter, shown in Figure 26. Further analysis with account for optical losses was performed in [55] and with detuned signal-recycling in [115].…”

Section: Quantum Speedmeter Topologiesmentioning

confidence: 99%

Quantum Measurement Theory in Gravitational-Wave Detectors

Danilishin

Khalili

2012

Living Rev. Relativ.

164

238

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The fast progress in improving the sensitivity of the gravitational-wave detectors, we all have witnessed in the recent years, has propelled the scientific community to the point at which quantum behavior of such immense measurement devices as kilometer-long interferometers starts to matter. The time when their sensitivity will be mainly limited by the quantum noise of light is around the corner, and finding ways to reduce it will become a necessity. Therefore, the primary goal we pursued in this review was to familiarize a broad spectrum of readers with the theory of quantum measurements in the very form it finds application in the area of gravitational-wave detection. We focus on how quantum noise arises in gravitational-wave interferometers and what limitations it imposes on the achievable sensitivity. We start from the very basic concepts and gradually advance to the general linear quantum measurement theory and its application to the calculation of quantum noise in the contemporary and planned interferometric detectors of gravitational radiation of the first and second generation. Special attention is paid to the concept of the Standard Quantum Limit and the methods of its surmounting.

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Section: Quantum Speedmeter Topologiesmentioning

confidence: 99%

Quantum Measurement Theory in Gravitational-Wave Detectors

Danilishin

Khalili

2012

Living Rev. Relativ.

164

238

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“…If the output port of the main interferometer is closed, then Eqs. (38,39) also hold with Ω B replaced by optical resonance frequency [42], I bar c by Ic, M C by the mass of the input mirrors and M E by the reduced mass of the end mirrors.…”

Section: Discussionmentioning

confidence: 99%

“…Later on, the idea to use the zero area Sagnac interferometer [36][37][38] as a speed meter was proposed independently by Chen and Khalili [33,34]. Further analysis with account for optical losses was performed in Ref.…”

Section: Overview Of Speed Meter Topologiesmentioning

confidence: 99%

“…Dynamics of the optical bars system with its three movable mirrors coupled to each other by means of frequency-dependent rigidity (38), is quite sophisticated. Depending on the values of mirrors masses, optical power I bar C and sloshing frequency Ω B , there could be either two resonances (mechanical and optical [42]), or one second-order resonance [46], which can be used to significantly increase the central mirror signal displacement in narrow band.…”

Section: Intracavity Measurementmentioning

confidence: 99%

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QND measurements for future gravitational-wave detectors

et al. 2010

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Second-generation interferometric gravitational-wave detectors will be operating at the Standard Quantum Limit, a sensitivity limitation set by the trade off between measurement accuracy and quantum back action, which is governed by the Heisenberg Uncertainty Principle. We review several schemes that allows the quantum noise of interferometers to surpass the Standard Quantum Limit significantly over a broad frequency band. Such schemes may be an important component of the design of third-generation detectors.

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“…It should be noted that use of Sagnac interferometers in gravitational-wave detection was suggested earlier in the works [14,15,16,17]. In [11,12] it was shown that to lower the value of circulating power one should use the squeezed vacuum input with squeezing factor of ∼ 0.1, and variational output detection [18].…”

Section: Introductionmentioning

confidence: 99%

Sensitivity limitations in optical speed meter topology of gravitational-wave antennas

Danilishin

2004

Phys. Rev. D

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The possible design of QND gravitational-wave detector based on speed meter principle is considered with respect to optical losses. The detailed analysis of speed meter interferometer is performed and the ultimate sensitivity that can be achieved is calculated. It is shown that unlike the position meter signal-recycling can hardly be implemented in speed meter topology to replace the arm cavities as it is done in signal-recycled detectors, such as GEO 600. It is also shown that speed meter can beat the Standard Quantum Limit (SQL) by the factor of ∼ 3 in relatively wide frequency band, and by the factor of ∼ 10 in narrow band. For wide band detection speed meter requires quite reasonable amount of circulating power ∼ 1 MW. The advantage of the considered scheme is that it can be implemented with minimal changes in the current optical layout of LIGO interferometer.

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Polarization Sagnac interferometer with a reflective grating beam splitter

Cited by 11 publications

References 8 publications

Quantum Measurement Theory in Gravitational-Wave Detectors

Quantum Measurement Theory in Gravitational-Wave Detectors

QND measurements for future gravitational-wave detectors

Sensitivity limitations in optical speed meter topology of gravitational-wave antennas

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