Michèle Heurs
Abstract
Since the first direct detection of gravitational waves in 2015, we have gained an entirely new observation window to the universe – now, we not only have electromagnetic telescopes and neutrino detectors to view astrophysical events, but we can also listen to the cosmos using interferometric gravitational wave detectors (GWDs). The sensitivity of these laser interferometers is so incredible that the quantum effects of the employed light have already become limiting. Ultra-precisely stabilised lasers do not suffice; non-classical light is already routinely employed in the current (second) generation GWDs (such as Advanced LIGO and Advanced Virgo). Other noise sources, such as seismic and thermal noise, pose further challenges for next-generation detectors.
To achieve ever-higher detection rates for meaningful gravitational wave astronomy, ever-greater detection sensitivity is required. In this talk, I will introduce the principle of interferometric gravitational wave detection, briefly describe the current status of the field, and highlight some of the advanced technologies employed in current GWDs. I will end with an outlook on the next (third) generation of GWDs, such as the planned European gravitational wave observatory, the Einstein Telescope.
Presentation
