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= Einstein Telescope = | = Einstein Telescope = | ||
[[File:ETArtist.jpg|Einstein Telescope (artistic conception)|thumb]] | [[File:ETArtist.jpg|Einstein Telescope (artistic conception)|thumb]] | ||
| + | The Einstein Telescope (ET) is a proposed next-generation, gravitational-wave (GW) detector in a new underground facility. It will achieve a sensitivity to GWs vastly superior to the current GW detectors LIGO and Virgo. Key factors are the increased baseline of 10km (compared to 3km for the Virgo detector and 4km for the LIGO detectors), increased light power inside the arms, and cryogenics to cool the suspended test masses and the suspension fibers. Furthermore, ET will extend the observation band to lower frequencies, i.e., down to a few Hertz. Essential for this purpose is to construct the detector at an extremely quiet site since noise produced in ET by the environment contributes most strongly at low frequencies. In Europe, such a low-noise environment can only be guaranteed at remote underground sites. This also impacts the detector configuration. It was found that a so-called xylophone configuration of ET where two separate interferometers, one optimized for low frequencies, one for high frequencies, is the best way to realize an observation band that ranges from a few Hertz to a few thousand Hertz [https://arxiv.org/abs/1012.0908 [Hild et al; 2010<nowiki>]</nowiki>]. | ||
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| + | It is predicted that black-hole binaries It was proposed with a | ||
== Site Characterization and Evaluation == | == Site Characterization and Evaluation == | ||
Revision as of 08:52, 21 February 2020
Contents
GSSI gravity group
Members
Einstein Telescope
The Einstein Telescope (ET) is a proposed next-generation, gravitational-wave (GW) detector in a new underground facility. It will achieve a sensitivity to GWs vastly superior to the current GW detectors LIGO and Virgo. Key factors are the increased baseline of 10km (compared to 3km for the Virgo detector and 4km for the LIGO detectors), increased light power inside the arms, and cryogenics to cool the suspended test masses and the suspension fibers. Furthermore, ET will extend the observation band to lower frequencies, i.e., down to a few Hertz. Essential for this purpose is to construct the detector at an extremely quiet site since noise produced in ET by the environment contributes most strongly at low frequencies. In Europe, such a low-noise environment can only be guaranteed at remote underground sites. This also impacts the detector configuration. It was found that a so-called xylophone configuration of ET where two separate interferometers, one optimized for low frequencies, one for high frequencies, is the best way to realize an observation band that ranges from a few Hertz to a few thousand Hertz [Hild et al; 2010].
It is predicted that black-hole binaries It was proposed with a
Site Characterization and Evaluation
Site-evaluation parameters
Results from Sardinia
R&D
Newtonian Noise
Physics with Einstein Telescope
Cosmology: Probing the Early Universe
Electromagnetic counterpart of gravitational waves
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