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CAOL . International Conference on Advanced Optoelectronics and Lasers

Optical quantuma non-demolition meter for gravitational wave detection

S. L. Danilishin, Farid Ya Khalili

Published Jan 5, 2006• 0 citations
Publisher

Abstract

We propose new gravitational wave detector design and new method of measurement that is based on principle of quantum non-demolition (QND) measurement. New design implies the so called "intracavity" measurement of the optical field parameters inside the cavity of interferometer without disturbing light quantum state. It is shown that using a technique called discrete sampling variation measurement (DSVM) in a local meter it is possible to overcome the standard quantum limit by an arbitrary amount limited only by the amount of optical energy circulating in the cavity of local meter and optical losses in the local meter mirrors. This technique being implemented will also be a demonstration of QND measurement and therefore can be used to demonstrate the detector moveable mirrors quantum behaviour.

DOI
10.1109/caol.2005.1553962

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•Jan 1, 2016•0 citations
We propose new gravitational wave detector design and new method of measurement that is based on principle of quantum non-demolition (QND) measurement. New design implies the so called "intracavity" measurement of the optical field parameters inside the cavity of interferometer without disturbing light quantum state. It is shown that using a technique called discrete sampling variation measurement (DSVM) in a local meter it is possible to overcome the standard quantum limit by an arbitrary amount limited only by the amount of optical energy circulating in the cavity of local meter and optical losses in the local meter mirrors. This technique being implemented will also be a demonstration of QND measurement and therefore can be used to demonstrate the detector moveable mirrors quantum behaviour.
ru Abstract - Wepropose newgravitational wavedetector design andnewmethod ofmeasurement that isbased on principle ofQuantum Non-Demolition (QND) measurement. Newdesign implies thesocalled intracavity measurement oftheoptical field parameters inside thecavity ofinterferometer without disturbing light quantum state. Itisshown that using atechnique called discrete sampling variation measurement (DSVM) inalocal meter itispossible toovercometheStandard Quantum Limit byanarbitrary amountlimited only bytheamount of optical energy circulating inthecavity oflocal meterandoptical losses inthelocal metermirrors. This technique being implemented will also beademonstration ofQNDmeasurement andtherefore canbeused todemonstrate thedetector moveable mirrors quantum behaviour.
The quantum nondemolition (QND) intracavity topologies of gravitational-wave detectors proposed several years ago allow us, in principle, to obtain sensitivity significantly better than the standard quantum limit using relatively small amount of optical pumping power. In this article we consider an improved more practical version of the optical lever intracavity scheme. It differs from the original version by the symmetry which allows to suppress influence of the input light amplitude fluctuation. In addition, it provides the means to inject optical pumping inside the scheme without increase of optical losses. We consider also sensitivity limitations imposed by the local meter which is the key element of the intracavity topologies. Two variants of the local meter are analyzed, which are based on the spectral variation measurement and on the discrete sampling variation measurement, correspondingly. The former one, while can not be considered as a candidate for a practical implementation, allows, in principle, to obtain the best sensitivity and thus can be considered as an ideal ``asymptotic case'' for all other schemes. The DSVM-based local meter can be considered as a realistic scheme but its sensitivity, unfortunately, is by far not so good just due to a couple of peculiar numeric factors specific for this scheme. From our point of view search of new methods of mechanical QND measurements probably based on improved DSVM scheme or which combine the local meter with the pondermotive squeezing technique, is necessary.
We propose new measurement concept that can be implemented in the third generation of gravitational-wave (GW) detectors: the discrete sampling variation measurement (DSVM). We demonstrate that this method allows to overcome the standard quantum limit (SQL) for free body and improve the sensitivity of interferometric gravitational wave detectors in wide frequency band. DSVM technique is based on well known method of quantum variation measurement that suggests to modulate in the optimal way the local oscillator phase in homodyne readout scheme of interferometric detector in order to measure such quadrature of the output light wave that has minimal uncertainty at the moment and therefore can be measured with precision, higher than SQL. The main disadvantage of variation measurement is the necessity to know a priori the form of detected signal in order to choose optimally the modulation function. It can be overcome if one modulates the local oscillator phase periodically with period less than sampling period required by Nyquist-Kotel'nikov-Shannon sampling theorem, and then fllters the output data using optimally chosen fllter functions.
The intracavity topologies of laser gravitational-wave detectors proposed several years ago are the promising way to obtain sensitivity of these devices significantly better than the Standard Quantum Limit (SQL). In essence, the intracavity detector is a two-stage device where the end mirrors displacement created by the gravitational wave is transferred to the displacement of an additional local mirror by means of the optical rigidity. The local mirror positions have to be monitored by an additional local meter. It is evident that the local meter precision defines the sensitivity of the detector. To overcome the SQL, the quantum variational measurement can be used in the local meter. In this method a frequency-dependent correlation between the meter backaction noise and measurement noise is introduced, which allows us to eliminate the backaction noise component from the meter output signal. This correlation is created by means of an additional filter cavity. In this article the sensitivity limitations of this scheme imposed by the optical losses both in the local meter itself and in the filter cavity are estimated. It is shown that the main sensitivity limitation stems from the filter cavity losses. In order to overcome it, it is necessary to increase the filter cavity length. In a preliminary prototype experiment, an approximate 10 m long filter cavity can be used to obtain sensitivity approximately 2--3 times better than the SQL. For future Quantum Non-Demolition (QND) gravitational-wave detectors with sensitivity about 10 times better than the SQL, the filter cavity length should be within kilometer range.
Abstract The recent discovery of gravitational waves (GW) by Advanced LIGO (Laser Interferometric Gravitational-wave Observatory) has impressively launched the novel field of gravitational astronomy and allowed us to glimpse exciting objects about which we could previously only speculate. Further sensitivity improvements at the low-frequency end of the detection band of future GW observatories must rely on quantum non-demolition (QND) methods to suppress fundamental quantum fluctuations of the light fields used to readout the GW signal. Here we present a novel concept of how to turn a conventional Michelson interferometer into a QND speed-meter interferometer with coherently suppressed quantum back-action noise. We use two orthogonal polarizations of light and an optical circulator to couple them. We carry out a detailed analysis of how imperfections and optical loss influence the achievable sensitivity. We find that the proposed configuration significantly enhances the low-frequency sensitivity and increases the observable event rate of binary black-hole coalescences in the range of 102−103 M⊙10^2 - 10^3\,M_ \odot102−103M⊙​ 1 0 2 - 1 0 3 M ⊙ by a factor of up to ~300.
Gravitational waves manifest as a time varying straining of space: they arise from the accelerating motions of large bodies of mass and propagate across the universe at the speed of light as ripples in the fabric of space-time, a fleetingly weak effect so far eluding direct detection. The detection of gravitation waves is expected to yield a rich vein to observational astronomy, complementing existing electromagnetic surveys and revealing a hitherto unexplored range of phenomena. First generation interferometric gravitational wave detectors, notably Enhanced LIGO, achieved strain sensitivities of one part in ten to power twenty-one per square-root-Hertz at 100 Hz with an expected detection rate of 2-3 events per year. Commissioning of a new generation of Advanced LIGO interferometric detectors has concluded recently with a resultant ten-fold sensitivity improvement. Overall their potential event detection space has increased by a factor of 1000. The quantum nature of light within these detectors now limits their sensitivity over most of their frequency range. This quantum noise limit is driven by the vacuum quadrature fluctuations propagated through their open detection ports and represents a fundamental noise floor to their strain sensitivity. This thesis addresses two distinct approaches to quantum noise improvement for future upgrades to advanced detectors. The first addresses the issue of quantum noise by adopting a quantum non-demolition approach to detector readout variables, the so-called `speed-meter’ design. Such a modified instrument samples test mass momentum, a quantity for which time separated measurements commute and are therefore not bound by Heisenberg-like limits. A novel polarisation-folded sloshing cavity type speed-meter is proposed where readout fields are stored and delayed in the orthogonal polarisation of the interferometer’s arms cavities. Here frequency dependence is selected to cancel position like measurements so that only test mass momentum information remains. A quantum noise propagation model is developed and a sensitivity performance is demonstrated that beats the standard quantum limit below 100 Hz over a broad range of frequencies. A second approach to achieve quantum noise enhancement in advanced detectors involves injection of quadrature-squeezed states in the place of vacuum. This dissertation details the development of a prototype squeezed vacuum source suitable to the demanding enhancement requirements for an Advanced LIGO squeezing installation. The construction of a doubly resonant, bow-tie cavity source is presented. This employs a novel monolithic all-glass cavity construction and is vacuum compatible. This design demonstrates the viability of building a cavity using optical contacting as a construction technique for attaching mounting prisms to highly polished fused-silica breadboards. Such a design can be expected to have excellent length noise stability, provide low intrinsic phase noise and would be suitable to mount on seismic isolation stages within the LIGO vacuum envelope. Further, the travelling wave cavity design should provide excellent 50 dB intrinsic backscatter isolation. We demonstrate the first operation of such a complex non-linear device under vacuum, producing 8.6 dB of measured vacuum squeezing down to 10 Hz across the advanced LIGO ‘audio-band’ detection range.