Gravitational wave detectors with broadband high frequency sensitivity
Abstract
Gravitational waves from the neutron star coalescence GW170817 were observed from the inspiral, but not the high frequency postmerger nuclear matter motion. Optomechanical white light signal recycling has been proposed for achieving broadband sensitivity in gravitational wave detectors, but has been reliant on development of suitable ultra-low loss mechanical components. Here we show demonstrated optomechanical resonators that meet loss requirements for a white light signal recycling interferometer with strain sensitivity below 10⁻²⁴ Hz^(−1/2) at a few kHz. Experimental data for two resonators are combined with analytic models of interferometers similar to LIGO to demonstrate enhancement across a broader band of frequencies versus dual-recycled Fabry-Perot Michelson detectors. Candidate resonators are a silicon nitride membrane acoustically isolated by a phononic crystal, and a single-crystal quartz acoustic cavity. Optical power requirements favour the membrane resonator, while thermal noise performance favours the quartz resonator. Both could be implemented as add-on components to existing detectors.
Additional Information
© The Author(s) 2021. This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons license, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons license and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this license, visit http://creativecommons.org/licenses/by/4.0/. Received 24 July 2020; Accepted 06 January 2021; Published 15 February 2021. This research was primarily supported by the Australian Research Council (ARC) Centre of Excellence for Gravitational Wave Discovery OzGrav CE170100004 and Discovery Project DP170104424. In addition, C.D. Blair is funded by the ARC Discovery Early Career Researcher Award DE190100437. The work of D. Mason, M. Rossi, and A. Schliesser was supported by the European Research Council project Q-CEOM (grant no. 638765) and the EU H2020 FET proactive project HOT (grant no. 732894). M. Goryachev and M.E. Tobar are supported by the ARC Centre of Excellence for Engineered Quantum Systems EQuS CE170100009. Y. Chen is supported by the US National Science Foundation Grants PHY-1708212 and PHY-1708213, and by the Simons Foundation (Award Number 568762). H. Miao is supported by UK Science and Technology Facilities Council Ernest Rutherford Fellowship (grant no. ST/M005844/11). M.A. Page would like to acknowledge the Japan Society for the Promotion of Science Postdoctoral Fellowship Program (grant no. P20713). We thank Eric C. Langman of Neils Bohr Institute and Carl Knox of ARC OzGrav at Swinburne University of Technology for their assistance in providing illustrations of phononic crystal resonators. Data availability: Datasets are used in Supplementary Figs. S1 and S2 and are available at figshare repository https://doi.org/10.6084/m9.figshare.13352669. Code availability: Calculations regarding the noise budget of WLSR interferometers as described in Methods were performed using Mathematica. Annotated code is available from the corresponding author upon request. Author Contributions: Calculations and models regarding GW detector interferometry and filter cavity optomechanics were performed by M.A. Page, and discussed and verified by H. Miao, Y. Ma, Y. Chen and C. Zhao. C.D. Blair and D.G. Blair provided discussion on the integration of WLSR in GW detectors. D. Mason, M. Rossi and A. Schliesser provided information regarding measured data of PNC resonators. M. Goryachev and M.E. Tobar provided information regarding measured data of BAW resonators. C. Zhao, L. Ju and D.G. Blair were the main supervisors of the project. The paper was drafted by M.A. Page, M. Goryachev, Y. Chen, A. Schliesser, and D.G. Blair, edited by M.A. Page and commented by all authors. The authors declare no competing interests.Attached Files
Published - s42005-021-00526-2.pdf
Submitted - 2007.08766.pdf
Supplemental Material - 42005_2021_526_MOESM1_ESM.pdf
Supplemental Material - 42005_2021_526_MOESM2_ESM.pdf
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Additional details
- Eprint ID
- 108409
- Resolver ID
- CaltechAUTHORS:20210312-072836413
- CE170100004
- Australian Research Council
- DP170104424
- Australian Research Council
- DE190100437
- Australian Research Council
- 638765
- European Research Council (ERC)
- 732894
- European Research Council (ERC)
- CE170100009
- Australian Research Council
- PHY-1708212
- NSF
- PHY-1708213
- NSF
- 568762
- Simons Foundation
- ST/M005844/11
- Science and Technology Facilities Council (STFC)
- P20713
- Japan Society for the Promotion of Science (JSPS)
- Created
-
2021-03-12Created from EPrint's datestamp field
- Updated
-
2023-06-01Created from EPrint's last_modified field
- Caltech groups
- TAPIR