Towards a first design of a Newtonian-noise cancellation system for Advanced LIGO

M. Coughlin, N. Mukund, J. Harms, J. Driggers, R. Adhikari, S. Mitra

Research output: Contribution to journalArticlepeer-review

20 Scopus citations

Abstract

Newtonian gravitational noise from seismic fields is predicted to be a limiting noise source at low frequency for second generation gravitational-wave detectors. Mitigation of this noise will be achieved by Wiener filtering using arrays of seismometers deployed in the vicinity of all test masses. In this work, we present optimized configurations of seismometer arrays using a variety of simplified models of the seismic field based on seismic observations at LIGO Hanford. The model that best fits the seismic measurements leads to noise reduction limited predominantly by seismometer self-noise. A first simplified design of seismic arrays for Newtonian-noise cancellation at the LIGO sites is presented, which suggests that it will be sufficient to monitor surface displacement inside the buildings.

Original languageEnglish (US)
Article number244001
JournalClassical and Quantum Gravity
Volume33
Issue number24
DOIs
StatePublished - Nov 14 2016
Externally publishedYes

Bibliographical note

Funding Information:
MC was supported by the National Science Foundation Graduate Research Fellowship Program, under NSF grant number DGE 1144152. NM acknowledges Council of Scientific and Industrial Research (CSIR), India for providing financial support as Senior Research Fellow. SM acknowledges the support of the Science and Engineering Research Board (SERB), India through the fast track grant SR/FTP/PS-030/2012. 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 PHY-0757058. This paper has been assigned LIGO document number LIGO-P1600146.

Publisher Copyright:
© 2016 IOP Publishing Ltd.

Keywords

  • Newtonian noise
  • Wiener filter
  • seismometers

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