Limiting noises in gravitational wave detectors: guidance from their statistical properties

Details Limiting noises in gravitational wave detectors: guidance from their statistical properties Limiting noises in gravitational wave detectors: guidance from their statistical properties

2003-04-29

arxiv.org/abs/gr-qc/0304108v1

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

7 Pages, Latex,figures included

Scientific paper

10.1117/12.497024

It is expected that interferometric gravitational wave detectors such as LIGO \cite{Barish99} will be eventually limited by fundamental noise sources like shot noise and Brownian motion, as well as by seismic noise. In the commissioning process, other technical noise sources (electronics noise, alignment fluctuations) limit the sensitivity and are eliminated one by one. We propose here a way to correlate the noise in the output of the gravitational wave detector with other detector and environmental signals not through their linear transfer functions (often unknown), but through their statistical properties. This could prove useful for identifying the frequency bands dominated by different noise sources in the final configuration, and also to help the commissioning process.

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