Linear projection of technical noise for interferometric gravitational-wave detectors

J.R. Smith; P. Ajith; H. Grote; M. Hewitson; S. Hild; H. Luck; K.A. Strain; B. Willke; J. Hough; K. Danzmann

doi:10.1088/0264-9381/23/2/016

Linear projection of technical noise for interferometric gravitational-wave detectors

J.R. Smith^*, P. Ajith, H. Grote, M. Hewitson, S. Hild, H. Luck, K.A. Strain, B. Willke, J. Hough, K. Danzmann

^*Corresponding author for this work

Research output: Contribution to journal › Article › Academic › peer-review

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.

Original language	English
Pages (from-to)	527-537
Number of pages	11
Journal	Classical and Quantum Gravity
Volume	23
Issue number	2
DOIs	https://doi.org/10.1088/0264-9381/23/2/016
Publication status	Published - 21 Jan 2006
Externally published	Yes

Access to Document

10.1088/0264-9381/23/2/016

Cite this

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title = "Linear projection of technical noise for interferometric gravitational-wave detectors",

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.",

author = "J.R. Smith and P. Ajith and H. Grote and M. Hewitson and S. Hild and H. Luck and K.A. Strain and B. Willke and J. Hough and K. Danzmann",

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T1 - Linear projection of technical noise for interferometric gravitational-wave detectors

AU - Smith, J.R.

AU - Ajith, P.

AU - Grote, H.

AU - Hewitson, M.

AU - Hild, S.

AU - Luck, H.

AU - Strain, K.A.

AU - Willke, B.

AU - Hough, J.

AU - Danzmann, K.

PY - 2006/1/21

Y1 - 2006/1/21

N2 - 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.

AB - 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.

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DO - 10.1088/0264-9381/23/2/016

M3 - Article

SN - 0264-9381

VL - 23

SP - 527

EP - 537

JO - Classical and Quantum Gravity

JF - Classical and Quantum Gravity

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