Deci-hertz Interferometer Gravitational Wave Observatory (DECIGO) is the future Japanese space mission with a frequency band of 0.1 Hz to 10 Hz. DECIGO aims at the detection of primordial gravitational waves, which could be produced during the inflationary period right after the birth of the universe. There are many other scientific objectives of DECIGO, including the direct measurement of the acceleration of the expansion of the universe, and reliable and accurate predictions of the timing and locations of neutron star/black hole binary coalescences. DECIGO consists of four clusters of observatories placed in the heliocentric orbit. Each cluster consists of three spacecraft, which form three Fabry-Perot Michelson interferometers with an arm length of 1,000 km. Three clusters of DECIGO will be placed far from each other, and the fourth cluster will be placed in the same position as one of the three clusters to obtain the correlation signals for the detection of the primordial gravitational waves. We plan to launch B-DECIGO, which is a scientific pathfinder of DECIGO, before DECIGO in the 2030s to demonstrate the technologies required for DECIGO, as well as to obtain fruitful scientific results to further expand the multi-messenger astronomy.
Initial acquisition requirements for optical cavities in the space gravitational wave antennae DECIGO and B-DECIGO
University of Tokyo（东京大学）；Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU)（宇宙物理数学 Kavli 研究所）；Yokohama National University（横滨国立大学）；LQUOM, Inc.（LQUOM 公司）；Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency（日本宇宙航空研究开发机构宇宙科学研究所）；National Astronomical Observatory of Japan（日本国立天文台）；University of Electro-Communications（电气通信大学）；Hosei University（法政大学）
Optimization of quantum noise in space gravitational-wave antenna DECIGO with optical-spring quantum locking considering mixture of vacuum fluctuations in homodyne detection
Quantum Noise Reduction in the Space-based Gravitational Wave Antenna DECIGO Using Optical Springs and Homodyne Detection scheme
Nagoya University（名古屋大学）；University of Tokyo（东京大学）；Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency（日本宇宙航空研究开发机构宇宙科学研究所）；LIGO Laboratory, California Institute of Technology（加州理工学院LIGO实验室）；Cardiff University（卡迪夫大学）
Detectability of Gravitational Waves from Extreme-Mass-Ratio Inspirals on Periodic Orbits around Bardeen Black Holes
School of Physics and Electronic Information, Yunnan Normal University（云南师范大学物理与电子信息学院）；School of Mathematics and Physics, Shangrao Normal University（上饶师范学院数学与物理学院）
Deci hertz Laser Interferometer can determine the position of the Coalescing Binary Neutron Stars within an arc minute a week before the final merging event to Black Hole
MIGA: Combining laser and matter wave interferometry for mass distribution monitoring and advanced geodesy
物质波激光干涉仪引力天线（MIGA）将是一种混合仪器，由水平排列的原子干涉仪网络组成，并由光学腔的谐振场进行询问。该探测器将提供引力应变张量的亚赫兹变化的测量。MIGA将为地球物理学带来新的方法，用于描述当地重力场的空间和时间变化，也将是未来低频引力波探测的示范。MIGA将能够更好地理解这些不同信号之间的低频耦合。该探测器将安装在Rustrel（FR）的地下“Souterrain Bas Bruit”（LSBB），这是一个环境噪音极低的设施，远离主要的人为干扰源。我们在本文中给出的操作模式和仪器的状态的概述之前，详细模拟的重力背景噪声在多边投资担保机构的安装地点。
