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A Third Generation Gravitational Wave Observatory: The Einstein Telescope

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Advanced Interferometers and the Search for Gravitational Waves

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 404))

Abstract

The first decade of the second millenium has seen the realization and the operation of the initial generation of large interferometric gravitational wave detectors, like Virgo and LIGO; these detectors demonstrated the capability of reaching their design sensitivity, which due to the novelty of their design was quite a challenging task. Achieving the target of the detection of gravitational waves still requires a large improvement in sensitivity. This is promised by the operation of the advanced detectors that are dominating the gravitational wave scene in the second decade of this century. But, in order to open the era of routine gravitational wave astronomy a new (third) generation of gravitational wave observation instruments will be needed. Will the third generation (3G) of gravitational wave observatories be the core of the gravitational astronomy in the third decade of this century? An overview of the technological progress needed to realize a 3G observatory, like the Einstein Telescope (ET), and a possible evolution scenario are discussed in this chapter.

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Notes

  1. 1.

    Indicating with displacement noises the pile-up of all the noise sources that are causing an effective movement of the test masses, like seismic noise, thermal noise, ...

  2. 2.

    The higher the Young’s modulus of a body, the less deformation is generated by the same thermal energy, thus less thermal noise.

  3. 3.

    Useful to realize high dilution factor suspensions.

  4. 4.

    Currently used coatings are based on alternate layers of dielectric materials (see Chap. 8 for a detailed description); the high refraction index material \(\mathrm{Ta_2O_5}\) is dissipative and generates the largest fraction of the thermal noise. Grating reflectors are based on resonant waveguide grating nanostructures, grown on the surfaces of the mirror substrates. With this design it is possible to obtain high reflectivity with a single layer of high refraction index material or even without the deposition of \(\mathrm{Ta_2O_5}\) on a Silicon test mass. See [69] for an introduction.

  5. 5.

    Optical losses due, roughly, to the finite size of the mirrors with respect to the nominally infinite radial extension of a Gaussian beam.

  6. 6.

    The optical power deposited by the ligh impinging on the mirror surfaces, is extracted through the suspension fibers; the amount of heat to be extracted constrains the minimal diameter of the suspension fibers to a value that conflicts with the requirement to have very thin suspension fibers imposed by the request to have a high dilution factor in order to minimize the thermal noise.

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Acknowledgments

This work has been performed with the support of the European Commission under the Framework Programme 7 (FP7), project ELiTES (Grant Agreement 295153), http://www.et--gw.eu/descriptionelites.

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Authors and Affiliations

  1. Istituto Nazionale di Fisica Nucleare—Sezione di Perugia, Via Pascoli 06123,   Perugia, Italy

    Michele Punturo

  2. Institut für Gravitationsphysik, Leibniz Universität Hannover, Callinstr. 38, 30167,   Hannover, Germany

    Harald Lück

  3. Nikhef—National Institute for Subatomic Physics, Sciencepark 105, 1098 XG,  Amsterdam, The Netherlands

    Mark Beker

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    Massimo Bassan

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Punturo, M., Lück, H., Beker, M. (2014). A Third Generation Gravitational Wave Observatory: The Einstein Telescope. In: Bassan, M. (eds) Advanced Interferometers and the Search for Gravitational Waves. Astrophysics and Space Science Library, vol 404. Springer, Cham. https://doi.org/10.1007/978-3-319-03792-9_13

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