Speaker
Description
F. Fidecaro, M. Razzano, A. Allocca, L. Bellizzi, S. Bianchi, V. Boschi, E. Calloni, M. Carpinelli, P. Chessa, D. D'Urso, R. De Rosa, L. Di Fiore, F. Fabrizi, I. Ferrante, A. Fiori, A. Gennai, A. Longo, L. Massaro, L. Papalini, M. Palaia, M. Montani, D. Rozza, P. Ruggi, L. Trozzo, M. Vacatello, A. Viceré
Third generation ground-based gravitational wave detectors will expand our view of the Universe. The Einstein Telescope will be an order of magnitude more sensitive than Advanced Virgo and LIGO and expand its frequency range down to 3 Hz. This low-frequency sensitivity will be crucial in addressing important scientific questions, including the formation and evolution of high-mass black holes and the physics of neutron stars. We present a new concept for suppressing seismic noise in the next generation of ground-based detectors. The model is based on the approach of the passive attenuation system achieved with the Virgo Superattenuator and aims at lowering the height of the ET mirror suspensions, 17-m high in the current design. Construction and operation complexity as well as civil engineering works would be significantly reduced. The concept has been developed within the project “Black Holes for ET in SArdinia” (BHETSA) gaining from the long experience gained in the design, simulation and construction of the Advanced Virgo seismic isolation system.
