Sensitivity Studies for Third-Generation Gravitational Wave Observatories

TL;DR

This paper develops a detailed sensitivity model for the Einstein Telescope, a third-generation gravitational wave detector, analyzing fundamental noise sources and their impact on low-frequency detection capabilities.

Contribution

It introduces the most accurate sensitivity model, ET-D, for the Einstein Telescope, incorporating key fundamental noise sources and focusing on low-frequency performance.

Findings

ET-D model provides improved sensitivity estimates.

Fundamental noise sources dominate below 10Hz.

Potential detection limits are identified for third-generation detectors.

Abstract

Advanced gravitational wave detectors, currently under construction, are expected to directly observe gravitational wave signals of astrophysical origin. The Einstein Telescope, a third-generation gravitational wave detector, has been proposed in order to fully open up the emerging field of gravitational wave astronomy. In this article we describe sensitivity models for the Einstein Telescope and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10Hz where a complex mixture of seismic, gravity gradient, suspension thermal and radiation pressure noise dominates. We develop the most accurate sensitivity model, referred to as ET-D, for a third-generation detector so far, including the most relevant fundamental noise contributions.