scholarly journals Estimation of losses in a 300 m filter cavity and quantum noise reduction in the KAGRA gravitational-wave detector

2016 ◽  
Vol 93 (8) ◽  
Author(s):  
Eleonora Capocasa ◽  
Matteo Barsuglia ◽  
Jérôme Degallaix ◽  
Laurent Pinard ◽  
Nicolas Straniero ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Noise Reduction ◽  
Quantum Noise ◽  
Gravitational Wave Detector ◽  
Wave Detector ◽  
Quantum Noise Reduction

Gravitational wave detection using laser interferometry beyond the standard quantum limit

2018 ◽  
Vol 376 (2120) ◽  
pp. 20170289 ◽  
Author(s):  
M. Heurs
Keyword(s):  
Gravitational Wave ◽  
Quantum Noise ◽  
Detection Sensitivity ◽  
Quantum Limit ◽  
Gravitational Wave Detector ◽  
Emission Frequency ◽  
Standard Quantum ◽  
Standard Quantum Limit ◽  
Detector Noise ◽  
Wave Detector

Interferometric gravitational wave detectors (such as advanced LIGO) employ high-power solid-state lasers to maximize their detection sensitivity and hence their reach into the universe. These sophisticated light sources are ultra-stabilized with regard to output power, emission frequency and beam geometry; this is crucial to obtain low detector noise. However, even when all laser noise is reduced as far as technically possible, unavoidable quantum noise of the laser still remains. This is a consequence of the Heisenberg Uncertainty Principle, the basis of quantum mechanics: in this case, it is fundamentally impossible to simultaneously reduce both the phase noise and the amplitude noise of a laser to arbitrarily low levels. This fact manifests in the detector noise budget as two distinct noise sources—photon shot noise and quantum radiation pressure noise—which together form a lower boundary for current-day gravitational wave detector sensitivities, the standard quantum limit of interferometry. To overcome this limit, various techniques are being proposed, among them different uses of non-classical light and alternative interferometer topologies. This article explains how quantum noise enters and manifests in an interferometric gravitational wave detector, and gives an overview of some of the schemes proposed to overcome this seemingly fundamental limitation, all aimed at the goal of higher gravitational wave event detection rates. This article is part of a discussion meeting issue ‘The promises of gravitational-wave astronomy’.

scholarly journals First Demonstration of 6 dB Quantum Noise Reduction in a Kilometer Scale Gravitational Wave Observatory

2021 ◽  
Vol 126 (4) ◽  
Author(s):  
James Lough ◽  
Emil Schreiber ◽  
Fabio Bergamin ◽  
Hartmut Grote ◽  
Moritz Mehmet ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Noise Reduction ◽  
Quantum Noise ◽  
Quantum Noise Reduction

scholarly journals China’s first step towards probing the expanding universe and the nature of gravity using a space borne gravitational wave antenna

2021 ◽  
Vol 4 (1) ◽  
Author(s):  
Keyword(s):  
Gravitational Wave ◽  
Hubble Constant ◽  
Gravitational Wave Detector ◽  
Expanding Universe ◽  
Satellite Mission ◽  
Gravitational Wave Detection ◽  
Wave Detection ◽  
Wave Detector ◽  
Wave Antenna ◽  
Gravitational Wave Antenna

AbstractIn this perspective, we outline that a space borne gravitational wave detector network combining LISA and Taiji can be used to measure the Hubble constant with an uncertainty less than 0.5% in ten years, compared with the network of the ground based gravitational wave detectors which can measure the Hubble constant within a 2% uncertainty in the next five years by the standard siren method. Taiji is a Chinese space borne gravitational wave detection mission planned for launch in the early 2030 s. The pilot satellite mission Taiji-1 has been launched in August 2019 to verify the feasibility of Taiji. The results of a few technologies tested on Taiji-1 are presented in this paper.

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