학술논문
KAGRA: 2.5 Generation Interferometric Gravitational Wave Detector
Document Type
Working Paper
Author
Akutsu, T.; Ando, M.; Arai, K.; Arai, Y.; Araki, S.; Araya, A.; Aritomi, N.; Asada, H.; Aso, Y.; Atsuta, S.; Awai, K.; Bae, S.; Baiotti, L.; Barton, M. A.; Cannon, K.; Capocasa, E.; Chen, C-S.; Chiu, T-W.; Cho, K.; Chu, Y-K.; Craig, K.; Creus, W.; Doi, K.; Eda, K.; Enomoto, Y.; Flaminio, R.; Fujii, Y.; Fujimoto, M. -K.; Fukunaga, M.; Fukushima, M.; Furuhata, T.; Haino, S.; Hasegawa, K.; Hashino, K.; Hayama, K.; Hirobayashi, S.; Hirose, E.; Hsieh, B. H.; Huang, C-Z.; Ikenoue, B.; Inoue, Y.; Ioka, K.; Itoh, Y.; Izumi, K.; Kaji, T.; Kajita, T.; Kakizaki, M.; Kamiizumi, M.; Kanbara, S.; Kanda, N.; Kanemura, S.; Kaneyama, M.; Kang, G.; Kasuya, J.; Kataoka, Y.; Kawai, N.; Kawamura, S.; Kawasaki, T.; Kim, C.; Kim, J.; Kim, J. C.; Kim, W. S.; Kim, Y. -M.; Kimura, N.; Kinugawa, T.; Kirii, S.; Kitaoka, Y.; Kitazawa, H.; Kojima, Y.; Kokeyama, K.; Komori, K.; Kong, A. K. H.; Kotake, K.; Kozu, R.; Kumar, R.; Kuo, H-S.; Kuroyanagi, S.; Lee, H. K.; Lee, H. M.; Lee, H. W.; Leonardi, M.; Lin, C-Y.; Lin, F-L.; Liu, G. C.; Liu, Y.; Majorana, E.; Mano, S.; Marchio, M.; Matsui, T.; Matsushima, F.; Michimura, Y.; Mio, N.; Miyakawa, O.; Miyamoto, A.; Miyamoto, T.; Miyo, K.; Miyoki, S.; Morii, W.; Morisaki, S.; Moriwaki, Y.; Morozumi, T.; Musha, M.; Nagano, K.; Nagano, S.; Nakamura, K.; Nakamura, T.; Nakano, H.; Nakano, M.; Nakao, K.; Narikawa, T.; Naticchioni, L.; Quynh, L. Nguyen; Ni, W. -T.; Nishizawa, A.; Ochi, T.; Oh, J. J.; Oh, S. H.; Ohashi, M.; Ohishi, N.; Ohkawa, M.; Okutomi, K.; Ono, K.; Oohara, K.; Ooi, C. P.; Pan, S-S.; Park, J.; Arellano, F. E. Peña; Pinto, I.; Sago, N.; Saijo, M.; Saito, Y.; Sakai, K.; Sakai, Y.; Sasai, M.; Sasaki, M.; Sasaki, Y.; Sato, S.; Sato, T.; Sekiguchi, Y.; Seto, N.; Shibata, M.; Shimoda, T.; Shinkai, H.; Shishido, T.; Shoda, A.; Somiya, K.; Son, E. J.; Suemasa, A.; Suzuki, T.; Tagoshi, H.; Tahara, H.; Takahashi, H.; Takahashi, R.; Takamori, A.; Takeda, H.; Tanaka, H.; Tanaka, K.; Tanaka, T.; Tanioka, S.; Martin, E. N. Tapia San; Tatsumi, D.; Tomaru, T.; Tomura, T.; Travasso, F.; Tsubono, K.; Tsuchida, S.; Uchikata, N.; Uchiyama, T.; Uehara, T.; Ueki, S.; Ueno, K.; Ushiba, T.; van Putten, M. H. P. M.; Vocca, H.; Wada, S.; Wakamatsu, T.; Watanabe, Y.; Xu, W-R.; Yamada, T.; Yamamoto, A.; Yamamoto, K.; Yamamoto, S.; Yamamoto, T.; Yokogawa, K.; Yokoyama, J.; Yokozawa, T.; Yoon, T. H.; Yoshioka, T.; Yuzurihara, H.; Zeidler, S.; Zhu, Z. -H.
Source
Nature Astronomy 3, 35 (2019)
Subject
Language
Abstract
The recent detections of gravitational waves (GWs) reported by LIGO/Virgo collaborations have made significant impact on physics and astronomy. A global network of GW detectors will play a key role to solve the unknown nature of the sources in coordinated observations with astronomical telescopes and detectors. Here we introduce KAGRA (former name LCGT; Large-scale Cryogenic Gravitational wave Telescope), a new GW detector with two 3-km baseline arms arranged in the shape of an "L", located inside the Mt. Ikenoyama, Kamioka, Gifu, Japan. KAGRA's design is similar to those of the second generations such as Advanced LIGO/Virgo, but it will be operating at the cryogenic temperature with sapphire mirrors. This low temperature feature is advantageous for improving the sensitivity around 100 Hz and is considered as an important feature for the third generation GW detector concept (e.g. Einstein Telescope of Europe or Cosmic Explorer of USA). Hence, KAGRA is often called as a 2.5 generation GW detector based on laser interferometry. The installation and commissioning of KAGRA is underway and its cryogenic systems have been successfully tested in May, 2018. KAGRA's first observation run is scheduled in late 2019, aiming to join the third observation run (O3) of the advanced LIGO/Virgo network. In this work, we describe a brief history of KAGRA and highlights of main feature. We also discuss the prospects of GW observation with KAGRA in the era of O3. When operating along with the existing GW detectors, KAGRA will be helpful to locate a GW source more accurately and to determine the source parameters with higher precision, providing information for follow-up observations of a GW trigger candidate.
Comment: 6 pages, 3 figures (quality of some figures has been reduced)
Comment: 6 pages, 3 figures (quality of some figures has been reduced)