Sensitivity studies for third-generation gravitational wave observatories

By S. Hild, M. Abernathy, F. Acernese, P. Amaro-Seoane, N. Andersson, K. Arun, F. Barone, B. Barr, M. Barsuglia, M. Beker and 129 more. 2010

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Advanced gravitational wave detectors, currently under construction, are expected to directly observe gravitational wave signals of astrophysical origin. The Einstein Telescope (ET), a third-generation gravitational wave detector, has been proposed in order to fully open up the emerging field of gravitational wave astronomy. In this paper we describe sensitivity models for ET and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10 Hz 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.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/156cc9fafd31d46288fca8a3b70cb7f8f1e5c539

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Citations in the corpus

Gravitational wave energy budget in strongly supercooled phase transitions (2019, methodology): “compare the produced GW signal to the sensitivities of dierent phases of LIGO [71{73], as well as the projected experiments LISA [74], MAGIS [75,76] and AION [77] 12. and the Einstein Telescope (ET) [78,79]. We also show the envisioned sensitivities of the proposed future missions DECIGO [80] and Bi”
The evolution of primordial black holes and their final observable spins (2020, neutral): “and future GW experiments like aLIGO and Einstein Telescope (ET) [65] may reach at a given redshift.”
On the maximal strength of a first-order electroweak phase transition and its gravitational wave signal (2018, background): “the current and future sensitivities (see also [88]) of the European Pulsar Timing Array (EPTA) [89] and LIGO [90{92], as well as the projected sensitivities of LISA [93], the Einstein Telescope (ET) [94,95], the Cosmic Explorer (CE) [96], and the Square Kilometre Array (SKA) [97]. Finally, we also ”
Science case for the Einstein telescope (2019, methodology): “This has lead to the ET-C sensitivity curve and, after some further refinement of some noise models, to the ET-D sensitivity curve [25], again shown in the left panel Fig.”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “For the proposed Einstein Telescope (ET) in the “D” configuration (Punturo et al. 2010; Hild et al. 2011), which we take as a representative third-generation detector, the corresponding S/Ns are ∼20 and ∼110.”
Improved reconstruction of a stochastic gravitational wave background with LISA (2020, background): “milli-Hertz regime which is not accessible with present and future ground-based detectors [2–7], and will open a new window for GW physics.”
Probing the pre-BBN universe with gravitational waves from cosmic strings (2018, background): “f the cosmos. Indeed, GWs emitted as far back as in ation could potentially be detected by LIGO/Virgo [31] or proposed future detectors such as LISA [32], BBO/DECIGO [33], the Einstein Telescope (ET) [34,35], and Cosmic Explorer (CE) [36]. A stable and predictable source of primordial GWs is needed ”
Dark, cold, and noisy: constraining secluded hidden sectors with gravitational waves (2018, methodology): “We employ the ET-D noise projections [95], assuming an observation period of 5 years and considering a stochastic background as detectable if it produces an signal-to-noise of 5 in a single ET detector [66].”