论文标题
在与GEO 600(O3GK)的第一个联合观察期间,Kagra检测器的性能
Performance of the KAGRA detector during the first joint observation with GEO 600 (O3GK)
论文作者
论文摘要
Kagra是公里尺度的地下引力波检测器,位于日本的Kamioka。 2020年4月,在Kagra检测器中进行了天体物理学观察,并结合了GEO 600检测器。这种观察操作称为O3GK。 O3GK中的光学配置基于功率回收的Fabry-PérotMichelson干涉仪;所有镜子均设置在室温下。操作的占空比约为53%,应变灵敏度为$ 3 \ times10^{ - 22}〜/\ sqrt {\ rm {hz}} $在250 Hz处。此外,二进制内部星(BNS)灵感范围约为0.6 MPC。研究了各种噪声源对O3GK敏感性的贡献,以了解如何改善观察范围;这项研究称为“噪声预算”。根据我们的噪声预算,可以通过添加每个噪声的效果来近似测得的灵敏度。灵敏度由用于振动隔离系统的局部控制,声音噪声,射击噪声和激光频率噪声的传感器中的噪声主导。此外,研究了其他未限制灵敏度的噪声源。本文提供了O3GK中Kagra检测器的详细说明,包括干涉仪配置,状态和噪声预算。此外,讨论了未来灵敏度改进(例如硬件升级)的策略。
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 strain sensitivity was $3\times10^{-22}~/\sqrt{\rm{Hz}}$ at 250 Hz. In addition, the binary-neutron-star (BNS) inspiral range was approximately 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.