CaltechAUTHORS
Published October 2023 | Version Published
Journal Article Open

Performance of the KAGRA detector during the first joint observation with GEO 600 (O3GK)

Creators

  • 1. ROR icon Tokyo Institute of Technology
  • 2. ROR icon California Institute of Technology
  • 3. ROR icon National Astronomical Observatory of Japan
  • 4. ROR icon University of Tokyo
  • 5. ROR icon Hirosaki University
  • 6. ROR icon The Graduate University for Advanced Studies, SOKENDAI
  • 7. ROR icon Korea Institute of Science & Technology Information
  • 8. ROR icon National Institute for Mathematical Sciences
  • 9. ROR icon Syracuse University
  • 10. ROR icon Beijing Normal University
  • 11. ROR icon University of Paris
  • 12. ROR icon Fukuoka University
  • 13. ROR icon Tamkang University
  • 14. ROR icon National Tsing Hua University
  • 15. ROR icon National Central University
  • 16. ROR icon Academia Sinica
  • 17. ROR icon Laser Interferometer Gravitational Wave Observatory
  • 18. ROR icon Université Savoie Mont Blanc
  • 19. ROR icon Niigata University
  • 20. Department of Physics, Graduate School of Science, Osaka City University, 3-3-138 Sugimoto-cho, Sumiyoshi-ku, Osaka City, Osaka 558-8585, Japan
  • 21. ROR icon Chinese Academy of Sciences
  • 22. ROR icon Ulsan National Institute of Science and Technology
  • 23. ROR icon Shanghai Astronomical Observatory
  • 24. ROR icon University of Toyama
  • 25. ROR icon Nihon University
  • 26. ROR icon Chungnam National University
  • 27. ROR icon Aoyama Gakuin University
  • 28. ROR icon Peking University
  • 29. ROR icon Osaka City University
  • 30. ROR icon Institute of Space and Astronautical Science
  • 31. ROR icon Ewha Womans University
  • 32. ROR icon National Astronomical Observatories
  • 33. ROR icon University of Chinese Academy of Sciences
  • 34. ROR icon Myongji University
  • 35. ROR icon Inje University
  • 36. ROR icon High Energy Accelerator Research Organization
  • 37. ROR icon Cardiff University
  • 38. ROR icon Institute for Theoretical Physics
  • 39. ROR icon Nagoya University
  • 40. ROR icon National Cheng Kung University
  • 41. ROR icon Wuhan University
  • 42. ROR icon National Center for High-Performance Computing
  • 43. ROR icon National Taiwan Normal University
  • 44. ROR icon Sapienza University of Rome
  • 45. ROR icon University of Wisconsin–Milwaukee
  • 46. ROR icon Ryukoku University
  • 47. ROR icon University of Notre Dame
  • 48. ROR icon Scuola Normale Superiore di Pisa
  • 49. ROR icon INFN Sezione di Pisa
  • 50. ROR icon Korea Astronomy and Space Science Institute
  • 51. ROR icon National Institute of Technology
  • 52. ROR icon Toho University
  • 53. ROR icon Gunma University
  • 54. ROR icon Chapman University
  • 55. ROR icon Osaka Institute of Technology
  • 56. ROR icon Université Catholique de Louvain
  • 57. ROR icon Tokyo City University
  • 58. ROR icon Kyoto University
  • 59. ROR icon INFN Sezione di Napoli
  • 60. ROR icon Chinese University of Hong Kong
  • 61. ROR icon National Defense Academy of Japan
  • 62. ROR icon University of Florida
  • 63. ROR icon Nagaoka University of Technology
  • 64. ROR icon Sejong University
  • 65. ROR icon National Chiao Tung University
  • 66. ROR icon Rikkyo University

Abstract

KAGRA, the kilometer-scale underground gravitational-wave detector, is located at Kamioka, Japan. In April 2020, an astrophysics observation was performed at the KAGRA detector in combination with the GEO 600 detector; this observation operation is called O3GK. The optical configuration in O3GK is based on a power-recycled Fabry–Pérot–Michelson interferometer; all the mirrors were set at room temperature. The duty factor of the operation was approximately 53%, and the displacement sensitivity was approximately 1 × 10⁻¹⁸ m/√Hz at 250 Hz. The binary-neutron-star (BNS) inspiral range was about 0.6 Mpc. The contributions of various noise sources to the sensitivity of O3GK were investigated to understand how the observation range could be improved; this study is called a "noise budget". According to our noise budget, the measured sensitivity could be approximated by adding up the effect of each noise. The sensitivity was dominated by noise from the sensors used for local controls of the vibration isolation systems, acoustic noise, shot noise, and laser frequency noise. Further, other noise sources that did not limit the sensitivity were investigated. This paper provides a detailed account of the KAGRA detector in O3GK, including interferometer configuration, status, and noise budget. In addition, strategies for future sensitivity improvements, such as hardware upgrades, are discussed.

Copyright and License

© The Author(s) 2022. Published by Oxford University Press on behalf of the Physical Society of Japan.
This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.

Acknowledgement

This work was supported by MEXT, the JSPS Leading-edge Research Infrastructure Program, a JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grants-in-Aid for Scientific Research on Innovative Areas 2905: JP17H06358, JP17H06361, and JP17H06364, the JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grants-in-Aid for Scientific Research (S) 17H06133 and 20H05639, JSPS Grants-in-Aid for Transformative Research Areas (A) 20A203: JP20H05854, the joint research program of the Institute for Cosmic Ray Research, the University of Tokyo, the National Research Foundation (NRF), the Mitsubishi Foundation, the Computing Infrastructure Project of KISTI-GSDC in Korea, Academia Sinica (AS), the AS Grid Center (ASGC) and the Ministry of Science and Technology (MoST) in Taiwan under grants including AS-CDA-105-M06, the Advanced Technology Center (ATC) of NAOJ, the Mechanical Engineering Center of KEK, the LIGO project, the Virgo project, and Terri Pearce. Finally, we would like to thank all of the essential workers in the KAGRA observatory; we would not have been able to complete this work without them.

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Additional details

Related works

Is new version of
Discussion Paper: arXiv:2203.07011 (arXiv)

Funding

Ministry of Education, Culture, Sports, Science and Technology
26000005
Japan Society for the Promotion of Science
JP17H06358
Japan Society for the Promotion of Science
JP17H06361
Japan Society for the Promotion of Science
JP17H06364
Japan Society for the Promotion of Science
17H06133
Japan Society for the Promotion of Science
20H05639
Japan Society for the Promotion of Science
JP20H05854
Institute for Cosmic Ray Research
National Research Foundation
Mitsubishi Foundation
Academia Sinica
Ministry of Science and Technology
AS-CDA-105-M06
Advanced Technology Center
National Astronomical Observatory of Japan
High Energy Accelerator Research Organization

Dates

Accepted
2022-06-24
Available
2022-06-28
Published
Available
2022-10-06
Corrected and typeset

Caltech Custom Metadata

Caltech groups
LIGO, Division of Physics, Mathematics and Astronomy (PMA)
Publication Status
Published