CaltechAUTHORS
Published July 15, 2018 | Version Submitted + Published
Journal Article Open

Measurement of optical losses in a high-finesse 300 m filter cavity for broadband quantum noise reduction in gravitational-wave detectors

Creators

  • 1. ROR icon National Astronomical Observatory of Japan
  • 2. ROR icon Astroparticle and Cosmology Laboratory
  • 3. ROR icon Beijing Normal University
  • 4. ROR icon Laboratoire d'Annecy-le-Vieux de Physique des Particules
  • 5. ROR icon The Graduate University for Advanced Studies, SOKENDAI
  • 6. ROR icon University of Electro-Communications
  • 7. ROR icon Laser Interferometer Gravitational Wave Observatory
  • 8. ROR icon Claude Bernard University Lyon 1
  • 9. ROR icon Universität Hamburg
  • 10. ROR icon National Institute for Subatomic Physics

Abstract

Earth-based gravitational-wave detectors will be limited by quantum noise in a large part of their spectrum. The most promising technique to achieve a broadband reduction of such noise is the injection of a frequency-dependent squeezed vacuum state from the output port of the detector, with the squeeze angle rotated by the reflection off a Fabry-Perot filter cavity. One of the most important parameters limiting the squeezing performance is represented by the optical losses of the filter cavity. We report here the operation of a 300 m filter cavity prototype installed at the National Astronomical Observatory of Japan. The cavity is designed to obtain a rotation of the squeeze angle below 100 Hz. After achieving the resonance of the cavity with a multiwavelength technique, the round trip losses have been measured to be between 50 and 90 ppm. This result demonstrates that with realistic assumptions on the input squeeze factor and the other optical losses, a quantum noise reduction of at least 4 dB in the frequency region dominated by radiation pressure can be achieved.

Additional Information

© 2018 American Physical Society. Received 27 May 2018; published 31 July 2018. We thank Jérôme Degallaix for fruitful discussions about the loss measurement and the help with OSCAR simulations. We thank also the Advanced Technology Center of the National Astronomical Observatory of Japan for the support. This work was supported by the JSPS Grant-in-Aid for Scientific Research (Grant No. 15H02095), the JSPS Core-to-Core Program, A. Advanced Research Networks, and the European Commission under the Framework Program 7 (FP7) "People" project ELiTES (Grant Agreement No. 295153) and EU Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie Grant Agreement No. 734303. E. C. was supported by the European Gravitational Observatory, by the scholarship "For Women in Science" from the Fondation l'Oréal UNESCO, and by the scholarship "Walter Zellidja" from the Académie Française.

Attached Files

Published - PhysRevD.98.022010.pdf

Submitted - 1806.10506.pdf

Files

1806.10506.pdf

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Additional details

Identifiers

Eprint ID
88370
Resolver ID
CaltechAUTHORS:20180731-090819692

Related works

Describes
https://arxiv.org/abs/1806.10506 (URL)

Funding

Japan Society for the Promotion of Science (JSPS)
15H02095
European Research Council (ERC)
295153
Marie Curie Fellowship
734303
European Gravitational Observatory
Fondation l'Oréal UNESCO
Académie Française

Dates

Created
2018-07-31
Created from EPrint's datestamp field
Updated
2021-11-16
Created from EPrint's last_modified field

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LIGO