A xylophone configuration for a third-generation gravitational wave detector

By S. Hild, S. Chelkowski, A. Freise, J. Franc, N. Morgado, R. Flaminio, R. DeSalvo. 2009

160 citations recorded by the source corpus.

Achieving the demanding sensitivity and bandwidth, envisaged for third-generation gravitational wave (GW) observatories, is extremely challenging with a single broadband interferometer. Very high optical powers (megawatts) are required to reduce the quantum noise contribution at high frequencies, while the interferometer mirrors have to be cooled to cryogenic temperatures in order to reduce thermal noise sources at low frequencies. To resolve this potential conflict of cryogenic test masses with high thermal load, we present a conceptual design for a 2-band xylophone configuration for a third-generation GW observatory, composed of a high-power, high-frequency interferometer and a cryogenic low-power, low-frequency instrument. Featuring inspiral ranges of 3200 Mpc and 38 000 Mpc for binary neutron stars and binary black holes coalesences, respectively, we find that the potential sensitivity of xylophone configurations can be significantly wider and better than what is possible in a single broadband interferometer.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Oceanography

View Paper: https://www.semanticscholar.org/paper/d33f256c92285d3b9f8056e0f840b76b265040a9

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Citations in the corpus

Quantum squeezed light in gravitational-wave detectors (2014, background): “Third generation GW detectors now being designed, such as the Einstein Telescope [43, 44] and third generation LIGO [45], include squeezing technology as part of their baseline operation.”
Gravitational waves and non-axisymmetric oscillation modes in mergers of compact object binaries (2011, methodology): “…12135 – Top panel: Time evolution of the GW amplitude h+. Middle panel: Total (black), pre-merger (red) and post-merger (green) scaled power spectral density, compared to the Advanced LIGO and ET unity SNR sensitivity curves (Harry & the LIGO Scientific Collaboration (2010); Hild et al. (2010)).”
A cryogenic silicon interferometer for gravitational-wave detection (2020, methodology): “To operate an interferometer at temperatures in the 10 – 20 K regime requires imposing an austere heat budget on the test mass, which in turn makes it difficult to achieve high circulating power in the arms [20, 11].”
The Einstein Telescope: a third-generation gravitational wave observatory (2010, unknown): “A possible realization of such a xylophone strategy, evaluated in [34] (‘ET-C’) for the ET design study, is plotted in figure 3 and compared with the single-interferometer implementation (‘ET-B’) of the ET observatory, described in [9].”
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae (2016, methodology): “We calculate the SNR from equation (27) for the zero-detuning high power conﬁguration of Advanced LIGO (LIGO Laboratory & Shoemaker 2010) and the B (Hild, Chelkowski & Freise 2008) and C (Hild et al. 2010) conﬁgurations for the Einstein Telescope.”