KAGRA：2.5 代干涉式引力波探测器
广义相对论与量子宇宙学
2019-10-16 v1 天体物理仪器与方法
仪器与探测器
摘要
LIGO/Virgo 合作组近期报道的引力波（GWs）探测对物理学和天文学产生了重大影响。引力波探测器的全球网络将在通过与天文望远镜和探测器协同观测来揭示源未知性质方面发挥关键作用。在此我们介绍 KAGRA（原名 LCGT；大型低温引力波望远镜），这是一种新型引力波探测器，具有两条 3 公里基线臂呈“L”形布置，位于日本岐阜县神冈町池之山内。KAGRA 的设计类似于 Advanced LIGO/Virgo 等第二代探测器，但其将在低温下使用蓝宝石镜面运行。这一低温特性有利于提高约 100 Hz 附近的灵敏度，并被视为第三代引力波探测器概念（如欧洲 Einstein Telescope 或美国 Cosmic Explorer）的重要特征。因此，KAGRA 常被称为基于激光干涉的 2.5 代引力波探测器。KAGRA 的安装与调试正在进行中，其低温系统已于 2018 年 5 月成功测试。KAGRA 的首次观测运行计划于 2019 年底，旨在加入 Advanced LIGO/Virgo 网络的第三次观测运行（O3）。本文中，我们简述 KAGRA 的历史及其主要特征亮点，并讨论 O3 时代 KAGRA 引力波观测的前景。与现有引力波探测器协同运行时，KAGRA 将有助于更精确地定位引力波源，并更高精度地确定源参数，为引力波触发候选体的后续观测提供信息。
引用
@article{arxiv.1811.08079,
title = {KAGRA: 2.5 Generation Interferometric Gravitational Wave Detector},
author = {T. Akutsu and M. Ando and K. Arai and Y. Arai and S. Araki and A. Araya and N. Aritomi and H. Asada and Y. Aso and S. Atsuta and K. Awai and S. Bae and L. Baiotti and M. A. Barton and K. Cannon and E. Capocasa and C-S. Chen and T-W. Chiu and K. Cho and Y-K. Chu and K. Craig and W. Creus and K. Doi and K. Eda and Y. Enomoto and R. Flaminio and Y. Fujii and M. -K. Fujimoto and M. Fukunaga and M. Fukushima and T. Furuhata and S. Haino and K. Hasegawa and K. Hashino and K. Hayama and S. Hirobayashi and E. Hirose and B. H. Hsieh and C-Z. Huang and B. Ikenoue and Y. Inoue and K. Ioka and Y. Itoh and K. Izumi and T. Kaji and T. Kajita and M. Kakizaki and M. Kamiizumi and S. Kanbara and N. Kanda and S. Kanemura and M. Kaneyama and G. Kang and J. Kasuya and Y. Kataoka and N. Kawai and S. Kawamura and T. Kawasaki and C. Kim and J. Kim and J. C. Kim and W. S. Kim and Y. -M. Kim and N. Kimura and T. Kinugawa and S. Kirii and Y. Kitaoka and H. Kitazawa and Y. Kojima and K. Kokeyama and K. Komori and A. K. H. Kong and K. Kotake and R. Kozu and R. Kumar and H-S. Kuo and S. Kuroyanagi and H. K. Lee and H. M. Lee and H. W. Lee and M. Leonardi and C-Y. Lin and F-L. Lin and G. C. Liu and Y. Liu and E. Majorana and S. Mano and M. Marchio and T. Matsui and F. Matsushima and Y. Michimura and N. Mio and O. Miyakawa and A. Miyamoto and T. Miyamoto and K. Miyo and S. Miyoki and W. Morii and S. Morisaki and Y. Moriwaki and T. Morozumi and M. Musha and K. Nagano and S. Nagano and K. Nakamura and T. Nakamura and H. Nakano and M. Nakano and K. Nakao and T. Narikawa and L. Naticchioni and L. Nguyen Quynh and W. -T. Ni and A. Nishizawa and T. Ochi and J. J. Oh and S. H. Oh and M. Ohashi and N. Ohishi and M. Ohkawa and K. Okutomi and K. Ono and K. Oohara and C. P. Ooi and S-S. Pan and J. Park and F. E. Peña Arellano and I. Pinto and N. Sago and M. Saijo and Y. Saito and K. Sakai and Y. Sakai and Y. Sakai and M. Sasai and M. Sasaki and Y. Sasaki and S. Sato and T. Sato and Y. Sekiguchi and N. Seto and M. Shibata and T. Shimoda and H. Shinkai and T. Shishido and A. Shoda and K. Somiya and E. J. Son and A. Suemasa and T. Suzuki and T. Suzuki and H. Tagoshi and H. Tahara and H. Takahashi and R. Takahashi and A. Takamori and H. Takeda and H. Tanaka and K. Tanaka and T. Tanaka and S. Tanioka and E. N. Tapia San Martin and D. Tatsumi and T. Tomaru and T. Tomura and F. Travasso and K. Tsubono and S. Tsuchida and N. Uchikata and T. Uchiyama and T. Uehara and S. Ueki and K. Ueno and T. Ushiba and M. H. P. M. van Putten and H. Vocca and S. Wada and T. Wakamatsu and Y. Watanabe and W-R. Xu and T. Yamada and A. Yamamoto and K. Yamamoto and K. Yamamoto and S. Yamamoto and T. Yamamoto and K. Yokogawa and J. Yokoyama and T. Yokozawa and T. H. Yoon and T. Yoshioka and H. Yuzurihara and S. Zeidler and Z. -H. Zhu},
journal= {arXiv preprint arXiv:1811.08079},
year = {2019}
}
备注
6 pages, 3 figures (quality of some figures has been reduced)