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Optical detector topology for third-generation gravitational wave observatories

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Abstract

The third generation of gravitational wave observatories, with the aim of providing 100 times better sensitivity than currently operating interferometers, is expected to establish the evolving field of gravitational wave astronomy. A key element, required to achieve this ambitious sensitivity goal, is the exploration of new interferometer geometries, topologies and configurations. In this article we review the current status of the ongoing design work for third-generation gravitational wave observatories. The main focus is the evaluation of the detector geometry and detector topology. In addition we discuss some promising detector configurations and potential noise reduction schemes.

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Authors and Affiliations

  1. School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK

    Andreas Freise & Simon Chelkowski

  2. Institute for Gravitational Research, University of Glasgow, Glasgow, G12 8QQ, UK

    Stefan Hild & Ken A. Strain

  3. Theoretical Astrophysics, California Institute of Technology, Pasadena, CA, 91125, USA

    Kentaro Somiya

  4. INFN, Sezione di Firenze, Universitá degli Studi di Urbino “Carlo Bo”, Urbino, Italy

    Andrea Viceré

  5. AstroParticule et Cosmologie, CNRS UMR7164, Paris, France

    Matteo Barsuglia

Authors
  1. Andreas Freise
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  2. Stefan Hild
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  3. Kentaro Somiya
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  4. Ken A. Strain
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  5. Andrea Viceré
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  6. Matteo Barsuglia
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  7. Simon Chelkowski
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Correspondence to Andreas Freise.

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Freise, A., Hild, S., Somiya, K. et al. Optical detector topology for third-generation gravitational wave observatories. Gen Relativ Gravit 43, 537–567 (2011). https://doi.org/10.1007/s10714-010-1018-0

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