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Implications of Dedicated Seismometer Measurements on Newtonian-Noise Cancellation for Advanced LIGO

Coughlin, M. W. and Harms, J. and Driggers, J. and McManus, D. J. and Mukund, N. and Ross, M. P. and Slagmolen, B. J. J. and Venkateswara, K. (2018) Implications of Dedicated Seismometer Measurements on Newtonian-Noise Cancellation for Advanced LIGO. Physical Review Letters, 121 (22). Art. No. 221104. ISSN 0031-9007. doi:10.1103/physrevlett.121.221104.

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Newtonian gravitational noise from seismic fields will become a limiting noise source at low frequency for second-generation, gravitational-wave detectors. It is planned to use seismic sensors surrounding the detectors’ test masses to coherently subtract Newtonian noise using Wiener filters derived from the correlations between the sensors and detector data. In this Letter, we use data from a seismometer array deployed at the corner station of the Laser Interferometer Gravitational Wave Observatory (LIGO) Hanford detector combined with a tiltmeter for a detailed characterization of the seismic field and to predict achievable Newtonian-noise subtraction levels. As was shown previously, cancellation of the tiltmeter signal using seismometer data serves as the best available proxy of Newtonian-noise cancellation. According to our results, a relatively small number of seismometers is likely sufficient to perform the noise cancellation due to an almost ideal two-point spatial correlation of seismic surface displacement at the corner station, or alternatively, a tiltmeter deployed under each of the two test masses of the corner station at Hanford will be able to efficiently cancel Newtonian noise. Furthermore, we show that the ground tilt to differential arm-length coupling observed during LIGO’s second science run is consistent with gravitational coupling.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Coughlin, M. W.0000-0002-8262-2924
Harms, J.0000-0002-7332-9806
Mukund, N.0000-0002-8666-9156
Additional Information:© 2018 American Physical Society. (Received 18 July 2018; revised manuscript received 20 August 2018; published 28 November 2018) M. C. was supported by the David and Ellen Lee Postdoctoral Fellowship at the California Institute of Technology. N. M. acknowledges the Council of Scientific and Industrial Research (CSIR), India for providing financial support as Senior Research Fellow. B. S. was supported by ARC Future Fellowship FT130100329 and D. M. and B. S. are supported by the ARC Centre of Excellence for Gravitational Wave Discovery. Thanks to the Seismic Working Group of the LIGO Scientific Collaboration for the suspension model. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative Agreement No. PHY-0757058. The authors thank the LIGO Scientific Collaboration for access to the data and gratefully acknowledge the support of the U.S. National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO, as well as the Science and Technology Facilities Council (STFC) of the United Kingdom and the Max-Planck-Society (MPS) for support of the construction of Advanced LIGO. Additional support for Advanced LIGO was provided by the Australian Research Council. This Letter has been assigned LIGO document number LIGO-P1800049.
Funding AgencyGrant Number
David and Ellen Lee Postdoctoral ScholarshipUNSPECIFIED
Council of Scientific and Industrial Research (India)UNSPECIFIED
Australian Research CouncilFT130100329
Science and Technology Facilities Council (STFC)UNSPECIFIED
Max Planck SocietyUNSPECIFIED
Other Numbering System:
Other Numbering System NameOther Numbering System ID
LIGO DocumentLIGO-P1800049
Issue or Number:22
Record Number:CaltechAUTHORS:20181128-113129201
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:91286
Deposited By: George Porter
Deposited On:28 Nov 2018 21:12
Last Modified:16 Nov 2021 03:40

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