Joint Optimization of seismometer arrays for the cancellation of Newtonian noise from seismic body waves in the Einstein Telescope

Abstract

Seismic Newtonian noise is predicted to limit the sensitivity of the Einstein Telescope. It can be reduced with coherent noise cancellation techniques using data from seismometers. To achieve the best results, it is important to place the seismic sensors in optimal positions. A preliminary study on this topic was conducted for the Einstein Telescope (ET): it focused on the optimization of the seismic array for the cancellation of Newtonian noise at an isolated test mass. In this paper, we expand the study to include the nested shape of ET, i.e., four test masses of the low-frequency interferometers at each vertex of the detector. Results are investigated in function of the polarization content of the seismic field composed of body waves. The study also examines how performance can be affected by displacing the sensor array from its optimal position or by operating at frequencies other than those used for optimization.

References in corpus (5)

• Site-selection criteria for the Einstein Telescope
• Machine learning for gravitational-wave detection: surrogate Wiener filtering for the prediction and optimized cancellation of Newtonian noise at Virgo
• Wiener filtering with a seismic underground array at the Sanford Underground Research Facility
• Seismic array measurements at Virgo's West End Building for the configuration of a Newtonian-noise cancellation system
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Cited by in corpus (4)

• The Science of the Einstein Telescope
• Correlated 0.01Hz-40Hz seismic and Newtonian noise and its impact on future gravitational-wave detectors
• Fighting Newtonian Noise with Gradient-Based Optimization at the Einstein Telescope
• True and apparent motion of optomechanical resonators, with applications to feedback cooling of gravitational wave detector test masses