Site-selection criteria for the Einstein Telescope

Amann, Florian; Bonsignorio, Fabio; Bulik, T.; Bulten, H. J.; Cuccuru, Stefano; Dassargues, Alain; DeSalvo, R.; Fenyvesi, E.; Fidecaro, F.; Fiori, I.; Giunchi, C.; Grado, A.; Harms, J.; Koley, S.; Kovács, László; Losurdo, G.; Mandic, V.; Meyers, P. M.; Naticchioni, L.; Nguyen, Frédéric; Oggiano, G.; Olivieri, Marco; Paoletti, F.; Paoli, A.; Plastino, W.; Razzano, M.; Ruggi, P.; Saccorotti, Gilberto; Sintes, A. M.; Somlai, L.; Ván, P.; Vasúth, M.

doi:10.1063/5.0018414

Cited by 46 publications

(42 citation statements)

References 115 publications

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“…A deep NN correlation study has yet to be carried out. The present analysis follows the prescription in [17] where the noise projection on the whole ET sensitivity is obtained by considering the effect of NN on a single Detector, without accounting for the 60 angle, and considering the body waves polarization p = 1/3. (see the section Newtonian "Noise estimation by Seismic Noise" )…”

Section: Et Optical Layoutmentioning

confidence: 99%

“…Under this condition, the main contribution to NN is expected to come from body waves [17,20]. In the rest of the paper, we will follow this assumption: we will estimate the Newtonian noise on the detector by the seismic noise measurements at 84 m depth and project it on the ET sensitivity assuming that it is entirely composed by body waves.…”

Section: Newtonian Noise Estimation By Seismic Noisementioning

confidence: 99%

“…The Power Spectral Density (PSD) of the measured seismic noise S(ξ, ω) can be expressed as the superposition of P and S contribution by defining a mixing parameter p as the fraction of compressional contribution: S(ξ P , ω) = pS(ξ, ω) and S(ξ S , ω) = (1 − p)S(ξ, ω). Following the discussion in [17], we assume that all three body-wave polarizations carry the same average displacement power and set p = 1/3. Under these hypothesis, the amplitude spectral density (ASD) of the Newtonian noise contribution to the detector output h(t) N N is given by:…”

Section: Newtonian Noise Estimation By Seismic Noisementioning

confidence: 99%

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Seismic glitchness at Sos Enattos site: impact on intermediate black hole binaries detection efficiency

Allocca

Berbellini²,

Boschi

et al. 2021

Eur. Phys. J. Plus

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Third-generation gravitational wave observatories will extend the lower frequency limit of the observation band toward 2 Hz, where new sources of gravitational waves, in particular intermediate-mass black holes (IMBH), will be detected. In this frequency region, seismic noise will play an important role, mainly through the so-called Newtonian noise, i.e., the gravity-mediated coupling between ground motion and test mass displacements. The signal lifetime of such sources in the detector is of the order of tens of seconds. In order to determine whether a candidate site to host the Einstein Telescope observatory is particularly suitable to observe such sources, it is necessary to estimate the probability distributions that, in the characteristic time scale of the signal, the sensitivity of the detector is not perturbed by Newtonian noise. In this paper, a first analysis is presented, focused on the Sos Enattos site (Sardinia, Italy), a candidate to host the Einstein Telescope. Starting from a long data set of seismic noise, this distribution is evaluated considering both the presently designed triangular ET configuration and also the classical ”L” configuration.

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Section: Et Optical Layoutmentioning

confidence: 99%

Section: Newtonian Noise Estimation By Seismic Noisementioning

confidence: 99%

Section: Newtonian Noise Estimation By Seismic Noisementioning

confidence: 99%

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Seismic glitchness at Sos Enattos site: impact on intermediate black hole binaries detection efficiency

Allocca

Berbellini²,

Boschi

et al. 2021

Eur. Phys. J. Plus

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“…This list is not exhaustive; for example, magnetic requirements are not discussed because the coupling of local magnetic fields depends primarily on technical details of the detector's electronics, which are difficult to estimate without detailed modeling. Similar topics are being considered for the underground Einstein Telescope facility [29]. FIG.…”

Section: The Cosmic Explorer Facilitymentioning

confidence: 98%

Gravitational-wave physics with Cosmic Explorer: Limits to low-frequency sensitivity

et al. 2021

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Cosmic Explorer is a next-generation ground-based gravitational-wave observatory concept, envisioned to begin operation in the 2030s and expected to be capable of observing binary neutron star and black hole mergers back to the time of the first stars. Cosmic Explorer's sensitive band will extend below 10 Hz, where the design is predominantly limited by geophysical, thermal, and quantum noises. In this work, thermal, seismic, gravity-gradient, quantum, residual gas, scattered-light, and servo-control noises are analyzed in order to motivate facility and vacuum system design requirements, potential test mass suspensions, Newtonian noise reduction strategies, improved inertial sensors, and cryogenic control requirements. Our analysis shows that, with improved technologies, Cosmic Explorer can deliver a strain sensitivity better than 10 −23 Hz −1=2 down to 5 Hz. Our work refines and extends previous analysis of the Cosmic Explorer concept and outlines the key research areas needed to make this observatory a reality.

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“…Historically, the isolation of test masses from direct seismic shaking has been accomplished with complex isolation systems capable of reducing the coupling up to ten orders of magnitude [12,13]. Further improvements will require either an even better seismic isolation or the installation of the new detectors in suitable quieter sites, such as Sos Enattos, which is indeed a candidate site to host the ET underground detector [14,15].…”

Section: Introductionmentioning

confidence: 99%

Picoradiant tiltmeter and direct ground tilt measurements at the Sos Enattos site

et al. 2021

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We report the tilt sensitivity reached by the ARCHIMEDES tiltmeter in the 2–20 Hz frequency region, where seismic noise is expected to give an important limitation to the sensitivity in the next future Gravitational Waves detection, particularly through Newtonian noise. The tilt noise level $$\tilde{\theta }(f)$$ θ ~ ( f ) is about $$10^{-12} \mathrm{rad}/\sqrt{\mathrm{Hz}}$$ 10 - 12 rad / Hz in most of the band, reaching the minimum of $$\tilde{\theta } = 7\cdot 10^{-13} \mathrm{rad}/\sqrt{\mathrm{Hz}}$$ θ ~ = 7 · 10 - 13 rad / Hz around 9 Hz. The tiltmeter is a beam balance with a 0.5 m suspended arm and interferometric optical readout, working in closed loop. The results have been obtained by a direct measurement of the ground tilt at the Sos Enattos site (Sardinia, Italy). This sensitivity is a requirement to use the tiltmeter as part of an effective Newtonian noise reduction system for present Gravitational Waves detectors, and also confirms that Sos Enattos is among the quietest sites in the world, suitable to host the third-generation Gravitational Waves detector Einstein Telescope.

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Site-selection criteria for the Einstein Telescope

Cited by 46 publications

References 115 publications

Seismic glitchness at Sos Enattos site: impact on intermediate black hole binaries detection efficiency

Seismic glitchness at Sos Enattos site: impact on intermediate black hole binaries detection efficiency

Gravitational-wave physics with Cosmic Explorer: Limits to low-frequency sensitivity

Picoradiant tiltmeter and direct ground tilt measurements at the Sos Enattos site

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