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Journal Article

Linear projection of technical noise for interferometric gravitational-wave detectors

MPS-Authors

Smith,  J. R.
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;
AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

Ajith,  J. R.
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;
AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Grote,  Hartmut
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Hewitson,  Martin
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Hild,  Stefan
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Lück,  Harald
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Willke,  Benno
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Danzmann,  Karsten
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

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Fulltext (public)

cqg6_2_016.pdf
(Publisher version), 180KB

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Citation

Smith, J. R., Ajith, J. R., Grote, H., Hewitson, M., Hild, S., Lück, H., et al. (2006). Linear projection of technical noise for interferometric gravitational-wave detectors. Classical and Quantum Gravity, 23(2), 527-537. doi:10.1088/0264-9381/23/2/016.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0013-4AB3-7
Abstract
An international network of interferometric gravitational-wave detectors is now in operation, and has entered a period of intense commissioning focused on bringing the instruments to their theoretical sensitivity limits. To expedite this process, noise analysis techniques have been developed by the groups associated with each instrument. We present methods of noise analysis that were developed and utilized for the commissioning of the GEO 600 detector. The focal point of this paper is a technique called noise projection that is used to determine the levels of contribution of various noise sources to the detector output. Example applications of this method to control loops typical of those employed in an interferometric GW detector are presented. Possible extensions of noise projections, including technical noise subtraction and gravitational-wave vetoes are also discussed.