Abstract
This chapter is meant to introduce the reader to the forthcoming network of second-generation interferometric detectors of gravitational waves, at a time when their construction is close to completion and there is the ambition to detect gravitational waves for the first time in the next few years and open the way to gravitational wave astronomy. The legacy of first-generation detectors is discussed before giving an overview of the technology challenges that have been faced to make advanced detectors possible. The various aspects outlined here are then discussed in more detail in the subsequent chapters of the book.
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Notes
- 1.
This is expected in Advanced Virgo, which is designed with so-called marginally stable recycling cavities. With such a design the detector is more sensitive to aberrations induced by thermal effects and optical defects. For instance, an inhomogeneous pattern of the refraction index of the mirrors, which can be non-axisymmetric, can cause important aberrations and must be compensated for.
- 2.
Vibration isolators act as very steep low-pass filters. Therefore, the residual seismic noise transmitted to the mirrors has a spectrum that behaves as \(\sim \) \(1/f^N\) with \(N\gg 1\), looking like a “wall” limiting the sensitivity at very low frequencies.
- 3.
GW analog of the standard candles.
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Losurdo, G. (2014). Towards Gravitational Wave Astronomy. 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_1
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