Benefits of artificially generated gravity gradients for interferometric gravitational-wave detectors

Creators: Matone, L.; Raffai, P.; Márka, S.; Grossman, R.; Kalmus, P.; Márka, Z.; Rollins, J.; Sannibale, V.

Abstract

We present an approach to experimentally evaluate gravity gradient noise, a potentially limiting noise source in advanced interferometric gravitational-wave detectors. In addition, the method can be used to provide sub-percent calibration in phase and amplitude. Knowledge of calibration to such certainties shall enhance the scientific output of the instruments in the case of an eventual detection of gravitational waves. The method relies on a rotating symmetrical two-body mass, a dynamic gravity field generator (DFG). The placement of the DFG in the proximity of one of the interferometer's suspended test masses generates a change in the local gravitational field detectable with current interferometric gravitational-wave detectors.

Additional Information

Copyright © Institute of Physics and IOP Publishing Limited 2007. Received 2 February 2007, in final form 14 March 2007. Published 11 April 2007. Print publication: Issue 9 (7 May 2007) The authors are grateful for the support of the United States National Science Foundation under cooperative agreement PHY-04-57528 and Columbia University in the City of New York. We greatly appreciate the support of LIGO Collaboration. We are indebted to many of our colleagues for frequent and fruitful discussion and for the LIGO Scientific Collaboration Review. In particular we would like to thank G Giordano, R Adhikari, V Sandberg, M Landry, P Sutton, P Shawhan, D Sigg, R DeSalvo, H Yamamoto, Y Aso and C Matone for their valuable comments on the manuscript. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Particle Physics and Astronomy Research Council of the United Kingdom, the Max-Planck-Society and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Natural Sciences and Engineering Research Council of Canada, the Council of Scientific and Industrial Research of India, the Department of Science and Technology of India, the Spanish Ministerio de Educacion y Ciencia, The National Aeronautics and Space Administration, the John Simon Guggenheim Foundation, the Alexander von Humboldt Foundation, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation and the Alfred P Sloan Foundation. The LIGO Observatories were constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation under cooperative agreementPHY-9210038. The LIGO Laboratory operates under cooperative agreement PHY-0107417. This paper has been assigned LIGO Document Number LIGOP060056-00-Z.

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