Quantum Limit for Laser Interferometric Gravitational-Wave Detectors from Optical Dissipation

Miao, H.; Evans, M.

doi:10.1103/physrevx.9.011053

Cited by 35 publications

(28 citation statements)

References 59 publications

(82 reference statements)

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“…The decreased SRM transmissivity required for a narrowband response creates an optical cavity where signal field crosses several optic surfaces and substrates such as the beamsplitter many more times than in the Aþ or wideband configurations. Because of its use of optical resonance, the detuned configuration can nearly saturate the sensitivity available given the loss [29], and squeezing tends to simply increase the bandwidth at peak sensitivity, as shown in the strain curve in Fig. 2.…”

Section: A Loss In the Signal Recycling Cavitymentioning

confidence: 99%

Tuning Advanced LIGO to kilohertz signals from neutron-star collisions

et al. 2021

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Gravitational waves produced at kilohertz frequencies in the aftermath of a neutron star collision can shed light on the behavior of matter at extreme temperatures and densities that are inaccessible to laboratory experiments. Gravitational-wave interferometers are limited by quantum noise at these frequencies but can be tuned via their optical configuration to maximize the probability of postmerger signal detection. We compare two such tuning strategies to turn Advanced LIGO into a postmerger-focused instrument: first, a wideband tuning that enhances the instrument's signal-to-noise ratio 40-80% broadly above 1 kHz relative to the baseline, with a modest sensitivity penalty at lower frequencies; second, a "detuned" configuration that provides even more enhancement than the wideband tuning, but over only a narrow frequency band and at the expense of substantially worse quantum noise performance elsewhere. With an optimistic accounting for instrument loss and uncertainty in postmerger parameters, the detuned instrument has a ≲40% sensitivity improvement compared to the wideband instrument.

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Section: A Loss In the Signal Recycling Cavitymentioning

confidence: 99%

Tuning Advanced LIGO to kilohertz signals from neutron-star collisions

et al. 2021

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“…The sensitivity of high-precision optical measurements is constrained by the quantum Cramer-Rao Bound (QCRB) which states that the variance of the measured signal due to noise is inversely proportional the variance σ N N of the photon number of the probe degree of freedom coupled to the signal [1][2][3][4][5][6]. This quantity is ultimately limited by the Heisenberg limit σ N N = N 2 , which states that the uncertainty scales quadratically with the number of resources available (in this case photons), although for most resonant detectors it is often constrained by the stronger shot noise limit (also called the standard quantum limit in quantum metrology): σ N N = N [7].…”

Section: Introductionmentioning

confidence: 99%

Designing optimal linear detectors -- a bottom-up approach

Bentley

Nurdin²,

Chen³

et al. 2021

Preprint

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We develop a systematic approach to realising linear detectors that saturate the Heisenberg limit. First, we consider the general constraints on the input-output transfer matrix of a linear detector. We then derive the physical realization of the most general transfer matrix using the quantum network synthesis technique, which allows for the inference of the physical setup directly from the input-output transfer matrix. By exploring the minimal realization which has the minimum number of internal modes, we show that such detectors that saturate the Heisenberg limit are internal squeezing schemes. Then, investigating the non-minimal realization, which is motivated by the parity-time symmetric systems, we arrive at the general quantum non-demolition measurement.

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“…In the minimum uncertainty state, it defines the best achievable quantum noise limited sensitivity, known as quantum Cramér-Rao bound (QCRB) [14], which also goes by as energetic or fundamental quantum limit [15,16] in the field of gravitational-wave instrument science. The power spectral density corresponding to this limit for a Fabry-Perot-Michelson interferometer reads [17,18]…”

Section: Introductionmentioning

confidence: 99%

Enhancing high frequency sensitivity of gravitational wave detectors with sloshing-Sagnac interferometer

Zhang,

Martynov,

Danilishin

et al. 2021

Preprint

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Sensitivity of gravitational-wave detectors is limited in the high-frequency band by quantum shot noise and eventually limited by the optical loss in signal recycling cavity. This limit is the main obstacle on the way to detect gravitational waves from the binary neutron star mergers in the current and the future generation detectors, as it does not depend on either the arm length, or the injected squeezing level. In this paper, we come up with the sloshing Sagnac interferometer topology, which can be obtained from the Michelson interferometer by optically connecting the end mirrors into an additional optical cavity. This transforms the interferometer into a triply-coupled cavity system capable of beating the loss-induced high-frequency limit of the signal-recycled Michelson interferometer. With advanced LIGO+ comparable parameters, a sloshing-Sagnac scheme can achieve 7 times better sensitivity at 2.5 kHz or 4 times better signal to noise ratio for a typical waveform of binary neutron post merge. Being an evolution of Michelson interferometer, the sloshing-Sagnac interferometer can possibly be used as a topology for the future generation detectors and upgrade of current detectors.

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Quantum Limit for Laser Interferometric Gravitational-Wave Detectors from Optical Dissipation

Cited by 35 publications

References 59 publications

Tuning Advanced LIGO to kilohertz signals from neutron-star collisions

Tuning Advanced LIGO to kilohertz signals from neutron-star collisions

Designing optimal linear detectors -- a bottom-up approach

Enhancing high frequency sensitivity of gravitational wave detectors with sloshing-Sagnac interferometer

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