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

2022; University of Oxford; Volume: 2023; Issue: 10 Linguagem: Inglês

10.1093/ptep/ptac093

2050-3911

H. Abe, R. X. Adhikari, T. Akutsu, Masaki Ando, A. Araya, N. Aritomi, Hideki Asada, Y. Aso, S. Bae, Y Bae, R. Bajpai, S. W. Ballmer, K. C. Cannon, Z. Cao, E. Capocasa, M. Chan, Chang lin Chen, D. Chen, K. Chen, Y. Chen, C-Y. Chiang, Y-K. Chu, J. C. Driggers, S. E. Dwyer, A. Effler, S. Eguchi, M. Eisenmann, Yutaro Enomoto, R. Flaminio, H. K. Fong, V. V. Frolov, Yoshinori Fujii, Y. Fujikawa, Y. Fujimoto, Mitsuhiro Fukushima, D. Gao, G-G Ge, S. Ha, I. P. W. Hadiputrawan, S. Haino, Wen-Biao Han, K. Hasegawa, Kentaro Hattori, H. Hayakawa, K. Hayama, Y. Himemoto, N. Hirata, C. Hirose, T-C. Ho, B-H. Hsieh, H-F. Hsieh, C Hsiung, H-Y. Huang, P. Huang, Y-C. Huang, Y.-J. Huang, C. Y. Hui, Shotaro Ide, B. Ikenoue, Kohei Inayoshi, Yuki Inoue, K. Ito, Y. Itoh, K. Izumi, Chanhyung Jeon, H-B Jin, K. Jung, P. Jung, K. Kaihotsu, T. Kajita, M. Kakizaki, M Kamiizumi, Nobuyuki Kanda, T. Kato, K Kawabe, K. Kawaguchi, Chunglee Kim, J Kim, J C Kim, Y.-M. Kim, N. Kimura, Y. Kobayashi, Kazunori Kohri, K. Kokeyama, A. K. H. Kong, Naoki Koyama, C. Kozakai, J Kume, Y. Kuromiya, Sachiko Kuroyanagi, Kyujin Kwak, E. Lee, H. W. Lee, Ray‐Kuang Lee, M. Leonardi, Kwan-Lok Li, P Li, L C-C Lin, Chun-Yu Lin, E. T. Lin, F-K. Lin, Feng-Li Lin, H. Lin, G C Liu, L.-W. Luo, M Ma’arif, E. Majorana, Y Michimura, N. Mio, O. Miyakawa, K. Miyo, S Miyoki, Y. Mori, S. Morisaki, N. Morisue, Y. Moriwaki, A Mullavey, K Nagano, K. Nakamura, Hiroyuki Nakano, Masayuki Nakano, Y. Nakayama, Tatsuya Narikawa, L. Naticchioni, L. Nguyen Quynh, W-T Ni, T. Nishimoto, A Nishizawa, S. Nozaki, Y. Obayashi, Y. Obuchi, W Ogaki, J. J. Oh, Kyuseok Oh, M. Ohashi, T. Ohashi, Masashi Ohkawa, H. Ohta, Y. Okutani, K Oohara, Shoichi Oshino, S. Otabe, K. Pan, A. Parisi, J. Park, F E Peña Arellano, Surojit Saha, S. Saito, Y. Saito, K Sakai, T. Sawada, Y. Sekiguchi, Lijing Shao, Yutaka Shikano, H. Shimizu, Ryuma Shimizu, K. Shimode, H. Shinkai, T. Shishido, A. Shoda, K. Somiya, I. Song, R. Sugimoto, J. Suresh, Takamasa Suzuki, Takashi Suzuki, Takamasa Suzuki, H. Tagoshi, Hirotaka Takahashi, R. Takahashi, S. Takano, H. Takeda, M. Takeda, M. Tamaki, K. Tanaka, Takahiro Tanaka, Taiki Tanaka, S. Tanioka, Atsushi Taruya, T. Tomaru, T. Tomura, L. Trozzo, T. Tsang, J-S. Tsao, S. Tsuchida, T. Tsutsui, Toshihiro Tsuzuki, D. Tuyenbayev, Nami Uchikata, Takashi Uchiyama, A. Ueda, T. Uehara, K. Ueno, G. Ueshima, F. Uraguchi, T Ushiba, Maurice H. P. M. van Putten, J Wang, T. Washimi, Chien-Ming Wu, H. Wu, Takatoshi Yamada, K. Yamamoto, K. Yamamoto, K. Yamashita, R Yamazaki, Yi Yang, Sang‐Wook Yeh, J. Yokoyama, T. Yokozawa, T. Yoshioka, H. Yuzurihara, S. Zeidler, M. Zhan, H Zhang, Yang Zhao, Z-H Zhu,

Seismic Waves and Analysis

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 ${\rm m}/\sqrt{\rm {Hz}}$ 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.