Conveners
Suspensions for LF: Suspensions for LF
- Joris van Heijningen (UCLouvain)
- Lucia Trozzo (Istituto Nazionale di Fisica Nucleare)
Ground rotation sensors at low-frequency have a vital role in improving seismic isolation systems in advanced and 3G gravitational wave detectors. It was found that using seismometers as the sole source of ground motion measurement results in undistinguishable motion detection between horizontal and tilt motion, especially below 100 mHz. Therefore, pure angular motion measurement is necessary...
The relative motion of seismic platforms, via coupling to the auxiliary length controls of the suspended optics, are predicted to be the limiting noise source for future gravitational-wave detectors at frequencies below 1 Hz. By measuring, then stabilizing this relative motion, the effective control feedback to the optics will be reduced and hence the noise coupling will be less, and...
Seismic noise and local disturbances are dominant noise below 10 Hz (0.1-10 Hz).With the introduction of high performance seismic isolation systems based on mechanical pendula,the 2nd generation GW antennas have reached the scientific goal of the direct observation of GW signals thanks to the extension of the frequency band down to 10 Hz. Now,the 3rd generation instrument era is approaching...
This study presents a low frequency isolation system in the framework of E-TEST project which is a research facility for Einstein Telescope. The isolation system combines a passive inverted pendulum and an active inertial platform. The design of this isolator allows reducing the overall height of the isolation system. We address the isolation system design, its dynamics and the control...
Newtonian noise (NN) was predicted to represent the very last sensitivity wall in Earth based gravitational wave detectors already by their first pioneers. Virgo will soon implement the first NN cancellation system ever and the knowledge we acquired during its development will be an asset in evaluating what we need to reduce as much as possible the NN in the Einstein Telescope.
The problem...
Gravitational wave detectors like the Einstein Telescope (ET) will be built a few hundred meters underground to reduce both seismic and Newtonian noise. Underground facilities must be designed to take full advantage of the shielding properties of the rock mass to maximize the detector´s performance. A major issue with the ET design are the corner points, where caverns need to be excavated in...
