Abstract
At the commencement of a new era in astrophysics, with added information from direct detections of gravitational-wave (GW) signals, this paper is a testament to the quasi-monolithic suspensions of the test masses of the GW detectors that have enabled the opening of a new window on the universe. The quasi-monolithic suspensions are the final stages in the seismic isolation of the test masses in GW detectors, and are specifically designed to introduce as little thermal noise as possible. The history of the development of the fused-silica quasi-monolithic suspensions, which have been so essential for the first detections of GWs, is outlined and a glimpse into the status of research towards quasi-monolithic suspensions made of sapphire and silicon is given.This article is part of a discussion meeting issue ‘The promises of gravitational-wave astronomy’.
Highlights
The first detection of a gravitational-wave (GW) signal by the Advanced LIGO GW detectors in September 2015 [1] was a huge milestone for the field of physics
Thermal noise is another important noise source in GW detectors between 10 and 100 Hz, which is the reason pendulum suspensions are chosen for the final stage
Following a delay in installing monolithic suspensions in the advanced configuration of the Virgo detector due to vacuum cleanliness issues [57], Virgo is currently installing its monolithic suspensions in time for the start of the observation run in late 2018 [58,59]
Summary
The first detection of a gravitational-wave (GW) signal by the Advanced LIGO (aLIGO) GW detectors in September 2015 [1] was a huge milestone for the field of physics. This paper is aimed to be, as well as a glimpse to the future, a testament to the many years of research and development of a vital part of the ground-based interferometric GW detectors that are observing GW signals: the quasi-monolithic fused-silica pendulum suspensions of the test masses. GW (such as a binary black hole merger 1 billion light years away) can be detected Thermal noise is another important noise source in GW detectors between 10 and 100 Hz, which is the reason pendulum suspensions are chosen for the final stage. The dominant sources of thermal noise are Brownian noise and thermo-elastic noise arising from the different parts of the final stage of the suspension and test mass [13]. We will review the status of research for upgrades to the current detectors as well as future generations of detectors
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