Input optics systems of the KAGRA detector during O3GK

Akutsu 1, T.; 2,; Ando1, M.; 4, 3; Arai 5, K.; Arai 5, Y.; Araki 6, S.; Araya 7, A.; Aritomi 3, N.; Asada 8, H.; Aso 9, Y.; 10,; Bae 11, S.; Bae 12, Y.; Baiotti 13, L.; Bajpai 14, R.; Barton 1, M. A.; Cannon 4, K.; Cao 15, Z.; Capocasa 1, E.; Chan16, M.; Chen 17, C.; 18,; Chen 19, K.; Chen 18, Y.; Chiang 20, C-I.; Chu19, H.; Chu20, Y-K.; Eguchi 16, S.; Enomoto 3, Y.; Flaminio 1, R.; 21,; Fujii 22, Y.; Fujikawa 23, Y.; Fukunaga5, M.; Fukushima 2, M.; Furuhata24, T.; Gao 25, D.; Ge 25, G. -G.; Ha 26, S.; Hagiwara5, A.; 27,; Haino20, S.; Han 28, W. -B.; Hasegawa 5, K.; Hattori 29, K.; Hayakawa30, H.; Hayama 16, K.; Himemoto 31, Y.; Hiranuma 32, Y.; Hirata 1, N.; Hirose 5, E.; Hong 33, Z.; Hsieh 5, B-H.; Huang 33, G-Z.; Huang 20, H-Y.; Huang 25, P.; Huang 18, Y-C.; Huang 20, Y. -J.; Hui 34, D. C. Y.; Ide 35, S.; Ikenoue 2, B.; Imam33, S.; Inayoshi 36, K.; Inoue 19, Y.; Ioka 37, K.; Ito24, K.; Itoh 38, Y.; 39,; Izumi 40, K.; Jeon41, C.; Jin 42, H. -B.; 43,; Jung 26, K.; Jung 30, P.; Kaihotsu 24, K.; Kajita 44, T.; Kakizaki 45, M.; Kamiizumi 30, M.; Kanbara 24, S.; Kanda 38, N.; 39,; Kang11, G.; Kataoka46, Y.; Kawaguchi 5, K.; Kawai 46, N.; Kawasaki 3, T.; Kim 41, C.; Kim 47, J.; Kim48, J. C.; Kim 12, W. S.; Kim 26, Y. -M.; Kimura 27, N.; Kita 3, N.; Kitazawa 24, H.; Kojima49, Y.; Kokeyama 30, K.; &#x2;, 50; Komori 3, K.; Kong 18, A. K. H.; Kotake 16, K.; Kozakai 9, C.; Kozu51, R.; Kumar52, R.; Kume 4, J.; Kuo19, C.; Kuo 33, H-S.; Kuromiya24, Y.; Kuroyanagi 53, S.; Kusayanagi 46, K.; Kwak 26, K.; Lee 54, H. K.; Lee 48, H. W.; Lee 18, R.; Leonardi 1, M.; Li 18, K. L.; Lin 26, L. C. -C.; Lin 55, C-Y.; Lin20, F-K.; Lin 33, F-L.; Lin 19, H. L.; Liu 17, G. C.; Luo 20, L. -W.; Majorana, E.; Marchio 1, M.; Michimura 3, Y.; Mio 57, N.; Miyakawa 30, O.; Miyamoto38, A.; Miyazaki 3, Y.; Miyo 30, K.; Miyoki 30, S.; Mori 24, Y.; Morisaki 5, S.; Moriwaki45, Y.; Nagano 40, K.; Nagano 58, S.; Nakamura 1, K.; Nakano 59, H.; Nakano 5, M.; 52, 29; &#x2;,; Nakashima46, R.; Nakayama 29, Y.; Narikawa 5, T.; Naticchioni 56, L.; Negishi 32, R.; Nguyen Quynh 60, L.; Ni 25, W. -T.; 61, 42; Nishizawa 4, A.; Nozaki 29, S.; Obuchi 2, Y.; Ogaki5, W.; Oh 12, J. J.; Oh 34, K.; Oh12, S. H.; Ohashi 30, M.; Ohishi 9, N.; Ohkawa 23, M.; Ohta 4, H.; Okutani 35, Y.; Okutomi 30, K.; Oohara 32, K.; Ooi 3, C.; Oshino 30, S.; Otabe 46, S.; Pan 18, K. -C.; Pang19, H.; Parisi 17, A.; Park 62, J.; Peña Arellano 30, F. E.; Pinto63, I.; Sago 64, N.; Saito2, S.; Saito30, Y.; Sakai 65, K.; Sakai32, Y.; Sakuno 16, Y.; Sato 66, S.; Sato23, T.; Sawada 38, T.; Sekiguchi 4, T.; Sekiguchi 67, Y.; Shao 36, L.; Shibagaki 16, S.; Shimizu2, R.; Shimoda 3, T.; Shimode 30, K.; Shinkai 68, H.; Shishido 10, T.; Shoda 1, A.; Somiya 46, K.; Son 12, E. J.; Sotani 69, H.; Sugimoto 24, R.; 40,; Suresh 5, J.; Suzuki 23, T.; Suzuki 5, T.; Tagoshi 5, H.; Takahashi 70, H.; Takahashi 1, R.; Takamori 7, A.; Takano3, S.; Takeda 3, H.; Takeda 38, M.; Tanaka71, H.; Tanaka38, K.; Tanaka71, K.; Tanaka 5, T.; Tanaka 72, T.; Tanioka 1, S.; 10,; Tapia San Martín1, E. N.; Telada 73, S.; Tomaru 1, T.; Tomigami 38, Y.; Tomura 30, T.; Travasso 74, F.; 75,; Trozzo 30, L.; Tsang 76, T.; Tsao33, J-S.; Tsubono3, K.; Tsuchida38, S.; Tsutsui 4, T.; Tsuzuki 2, T.; Tuyenbayev 20, D.; Uchikata 5, N.; Uchiyama 30, T.; Ueda 27, A.; Uehara 77, T.; 78,; Ueno 4, K.; Ueshima 70, G.; Uraguchi 2, F.; Ushiba 5, T.; Van Putten 79, M. H. P. M.; Vocca 75, H.; Wang, J.; Washimi 1, T.; Wu 18, C.; Wu18, H.; Wu18, S.; Xu33, W-R.; Yamada 71, T.; Yamamoto 45, K.; Yamamoto 71, K.; Yamamoto 30, T.; Yamashita 29, K.; Yamazaki35, R.; Yang 80, Y.; Yano46, K.; Yokogawa 24, K.; Yokoyama 3, J.; 4,; Yokozawa30, T.; Yoshioka 24, T.; Yuzurihara 5, H.; Zeidler 81, S.; Zhan25, M.; Zhang 33, H.; Zhao 1, Y.; Zhu 15 (The KAGRA Collaboration), Z. -H.; Goetz 78, R.; Heintze 82, M.; Liu, J.; Müller78, C.; Savage 84, R. L.; Tanner, And D. B.

doi:10.1093/ptep/ptac166

KAGRA, the underground and cryogenic gravitational-wave detector, was operated for its solo observation from February 25 to March 10, 2020, and its first joint observation with the GEO 600 detector from April 7 to April 21, 2020 (O3GK). This study presents an overview of the input optics systems of the KAGRA detector, which consist of various optical systems, such as a laser source, its intensity and frequency stabilization systems, modulators, a Faraday isolator, mode-matching telescopes, and a high-power beam dump. These optics were successfully delivered to the KAGRA interferometer and operated stably during the observations. The laser frequency noise was observed to limit the detector sensitivity above a few kilohertz, whereas the laser intensity did not significantly limit the detector sensitivity.

Input optics systems of the KAGRA detector during O3GK / Akutsu 1, T., 2, ., Ando1, M., 4, 3., Arai 5, K., Arai 5, Y., Araki 6, S., Araya 7, A., Aritomi 3, N., Asada 8, H., Aso 9, Y., 10, ., Bae 11, S., Bae 12, Y., Baiotti 13, L., Bajpai 14, R., Barton 1, M.A., Cannon 4, K., Cao 15, Z., Capocasa 1, E., et al.. - In: PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS. - ISSN 2050-3911. - (2023), pp. 1-20. [10.1093/ptep/ptac166]