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Improving the stability of frequency-dependent squeezing with bichromatic control of filter cavity length, alignment, and incident beam pointing

Zhao, Yuhang and Capocasa, Eleonora and Eisenmann, Marc and Aritomi, Naoki and Page, Michael and Guo, Yuefan and Polini, Eleonora and Arai, Koji and Aso, Yoichi and van Beuzekom, Martin and Huang, Yao-Chin and Lee, Ray-Kuang and Lück, Harald and Miyakawa, Osamu and Prat, Pierre and Shoda, Ayaka and Tacca, Matteo and Takahashi, Ryutaro and Vahlbruch, Henning and Vardaro, Marco and Wu, Chien-Ming and Leonardi, Matteo and Barsuglia, Matteo and Flaminio, Raffaele (2022) Improving the stability of frequency-dependent squeezing with bichromatic control of filter cavity length, alignment, and incident beam pointing. Physical Review D, 105 (8). Art. No. 082003. ISSN 2470-0010. doi:10.1103/physrevd.105.082003.

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Frequency-dependent squeezing is the main upgrade for achieving broadband quantum noise reduction in upcoming observation runs of gravitational wave detectors. The proper frequency dependence of the squeezed quadrature is obtained by reflecting squeezed vacuum from a Fabry-Perot filter cavity detuned by half of its line width. However, since the squeezed vacuum contains no classical amplitude, copropagating auxiliary control beams are required to achieve the filter cavity’s length, alignment, and incident beam pointing stability. In our frequency-dependent squeezing experiment at the National Astronomical Observatory of Japan, we used a control beam at a harmonic of squeezed vacuum wavelength and found visible detuning variation related to the suspended mirrors angular drift. These variations can degrade interferometer quantum noise reduction. We investigated various mechanisms that can cause the filter cavity detuning variation. The detuning drift is found to be mitigated sufficiently by fixing the incident beam pointing and applying filter cavity automatic alignment. It was also found that there is an optimal position of the beam on the filter cavity mirror that helps to reduce the detuning fluctuations. Here, we report a stabilized filter cavity detuning variation of less than 10 Hz compared to the 113 Hz cavity line width. Compared to previously published results [Phys. Rev. Lett. 124, 171101 (2020), such detuning stability would be sufficient to make filter cavity detuning drift induced gravitational wave detector detection range fluctuation reduce from 11% to within 2%.

Item Type:Article
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URLURL TypeDescription Paper Information
Zhao, Yuhang0000-0003-2542-4734
Capocasa, Eleonora0000-0003-3762-6958
Aritomi, Naoki0000-0003-4424-7657
Page, Michael0000-0002-5298-7914
Guo, Yuefan0000-0002-6959-9870
Polini, Eleonora0000-0003-4059-0765
Arai, Koji0000-0001-8916-8915
Aso, Yoichi0000-0002-1902-6695
van Beuzekom, Martin0000-0002-0500-1286
Huang, Yao-Chin0000-0001-8786-7026
Lee, Ray-Kuang0000-0002-7171-7274
Lück, Harald0000-0001-9350-4846
Miyakawa, Osamu0000-0002-9085-7600
Shoda, Ayaka0000-0002-0236-4735
Tacca, Matteo0000-0003-1353-0441
Takahashi, Ryutaro0000-0003-1367-5149
Vahlbruch, Henning0000-0003-2357-2338
Vardaro, Marco0000-0001-8604-3797
Wu, Chien-Ming0000-0003-3191-8845
Leonardi, Matteo0000-0002-7641-0060
Barsuglia, Matteo0000-0002-1180-4050
Flaminio, Raffaele0000-0003-4462-6737
Additional Information:© 2022 The Author(s). Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. (Received 6 December 2021; accepted 1 March 2022; published 26 April 2022) We thank J. Degallaix, X. Ding, and T. Liu for their contributions and discussions. We thank G. Hartmut and A. Jones for their comments on this work. We thank also Advanced Technology Center of National Astronomical Observatory of Japan for the support. We acknowledge the help from members of KAGRA Collaboration, Virgo Collaboration, and LIGO Collaboration. This work was supported by the JSPS Grant-in-Aid for Scientific Research (Grants No. 15H02095, No. 18H01235, and No. 21H04476), the JSPS Core-to-Core Program, and the EU Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie Grant Agreement No. 734303. Y. Z. was supported by the Graduate University for Advanced Studies, SOKENDAI, by the Japanese government Ministry of Education, Culture, Sports, Science and Technology scholarship, and by the Institute for Cosmic Ray Research Young Researcher’s Fund. M. E. was supported by the JSPS Standard Postdoctoral Fellowship (Grant No. 20F20803). M. P. was supported by the JSPS Standard Postdoctoral Fellowship (Grant No. 20F20713). H. L. and H. V. were supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy—EXC 2123 QuantumFrontiers—390837967. N. A. was supported by JSPS Grant-in-Aid for Scientific Research (Grant No. 18H01224), JSPS Grant-in-Aid for Challenging Research (Exploratory) (Grant No. 18K18763), and Japan Science and Technology Agency, Core Research for Evolutional Science and Technology (Grant No. JPMJCR1873).
Funding AgencyGrant Number
National Astronomical Observatory of JapanUNSPECIFIED
Japan Society for the Promotion of Science15H02095
Japan Society for the Promotion of Science18H01235
Japan Society for the Promotion of Science21H04476
Marie Curie Fellowship734303
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
Institute for Cosmic Ray ResearchUNSPECIFIED
Japan Society for the Promotion of Science20F20803
Japan Society for the Promotion of Science20F20713
Deutsche Forschungsgemeinschaft (DFG)EXC 2123 - 390837967
Japan Society for the Promotion of Science18H01224
Japan Society for the Promotion of Science18K18763
Japan Science and Technology AgencyJPMJCR1873
Issue or Number:8
Record Number:CaltechAUTHORS:20220601-257672000
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:114985
Deposited By: George Porter
Deposited On:02 Jun 2022 14:47
Last Modified:02 Jun 2022 14:47

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