Speaker
Description
These lectures will explore the optical design of gravitational wave (GW) detectors, starting from fundamental interferometric principles and moving toward the specific challenges of the Einstein Telescope (ET).
We will first review the fundamental building blocks of GW detectors, incrementally discussing the Michelson interferometer, the introduction of Fabry-Perot arm cavities, and the implementation of power and signal recycling cavities. We will examine how the main noise sources, primarily quantum, thermal, and seismic noise, interact to define the characteristic shape of the detector's sensitivity curve.
The second part of the lectures will be dedicated to the optical layout of the Einstein Telescope. After a brief comparison between the Triangle and the 2L configurations, we will focus on how the principles discussed in the first part apply to the ET design. We will explore how structural and physical limitations shape the layout of such a large-scale, complex system.
