A5086005157- Pulsars and Gravitational Waves Research
- Geophysics and Sensor Technology
- Gamma-ray bursts and supernovae
- Geophysics and Gravity Measurements
- Advanced Frequency and Time Standards
- High-pressure geophysics and materials
- Cosmology and Gravitation Theories
- Seismic Waves and Analysis
- Astronomical Observations and Instrumentation
- Adaptive optics and wavefront sensing
- Astrophysical Phenomena and Observations
- Radio Astronomy Observations and Technology
- Advanced Measurement and Metrology Techniques
- Superconducting Materials and Applications
- Cold Atom Physics and Bose-Einstein Condensates
- Atomic and Subatomic Physics Research
- Calibration and Measurement Techniques
- Astrophysics and Cosmic Phenomena
- Quantum, superfluid, helium dynamics
- Advanced Thermodynamic Systems and Engines
- Magnetic confinement fusion research
- Advanced MEMS and NEMS Technologies
- Spacecraft and Cryogenic Technologies
- Superconducting and THz Device Technology
- Mechanical and Optical Resonators
The University of Tokyo
2012-2024
National Astronomical Observatory of Japan
1998-2023
Kavli Institute for the Physics and Mathematics of the Universe
2022
Institute for Cosmic Ray Research
1999-2018
University of Electro-Communications
2011
High Energy Accelerator Research Organization
2002-2011
California Institute of Technology
2002-2006
Sumitomo Heavy Industries (Japan)
2005
Japan Aviation Electronics Industry (Japan)
2002
Hofstra University
2002
The objectives of the DECi-hertz Interferometer Gravitational Wave Observatory (DECIGO) are to open a new window observation for gravitational wave astronomy and obtain insight into significant areas science, such as verifying characterizing inflation, determining thermal history universe, dark energy, describing formation mechanism supermassive black holes in center galaxies, testing alternative theories gravity, seeking hole matter, understanding physics neutron stars searching planets...
DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) is the future Japanese space gravitational antenna. It aims at detecting various kinds of waves between 1 mHz and 100 Hz frequently enough to open a new window observation for astronomy. The pre-conceptual design DECIGO consists three drag-free satellites, 1000 km apart from each other, whose relative displacements are measured by Fabry–Perot Michelson interferometer. We plan launch in 2024 after long intense development...
DECIGO (DECi-hertz Interferometer Gravitational wave Observatory) is the planned Japanese space gravitational antenna, aiming to detect waves from astrophysically and cosmologically significant sources mainly between 0.1 Hz 10 thus open a new window for astronomy universe. will consists of three drag-free spacecraft arranged in an equilateral triangle with 1000 km arm lengths whose relative displacements are measured by differential Fabry-Perot interferometer, four units triangular...
TAMA300, an interferometric gravitational-wave detector with 300-m baseline length, has been developed and operated sufficient sensitivity to detect events within our galaxy stability for observations; the interferometer was over 10 hours stably continuously. With a strain-equivalent noise level of $h\ensuremath{\sim}5\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}21}/\sqrt{\mathrm{Hz}}$, signal-to-noise ratio 30 is expected gravitational waves generated by coalescence...
DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) is the future Japanese space gravitational antenna. DECIGO expected to open a new window of observation for astronomy especially between 0.1 Hz and 10 Hz, revealing various mysteries universe such as dark energy, formation mechanism supermassive black holes, inflation universe. The pre-conceptual design consists three drag-free spacecraft, whose relative displacements are measured by differential Fabry-Perot Michelson...
DECi-hertz Interferometer Gravitational-wave Observatory (DECIGO) is a future Japanese space gravitational-wave antenna. The most important objective of DECIGO, among various sciences to be aimed at, detect gravitational waves coming from the inflation universe. DECIGO consists four clusters spacecraft, and each cluster three spacecraft with Fabry–Perot Michelson interferometers. As pathfinder mission B-DECIGO will launched, hopefully in 2020s, demonstrate technologies necessary for as well...
Major construction and initial-phase operation of a second-generation gravitational-wave detector KAGRA has been completed. The entire 3-km is installed underground in mine order to be isolated from background seismic vibrations on the surface. This allows us achieve good sensitivity at low frequencies high stability detector. Bare-bones equipment for interferometer first test run was accomplished March April 2016 with rather simple configuration. initial configuration named {\it iKAGRA}. In...
KAGRA is a gravitational-wave (GW) detector constructed in Japan with two unique key features: It was underground, and the test-mass mirrors are cooled to cryogenic temperatures. These features not included other kilometer-scale detectors but will be adopted future such as Einstein Telescope. performed its first joint observation run GEO600 2020. In this observation, sensitivity of GWs inferior that LIGO Virgo. However, further upgrades ongoing reach for detecting next run, which scheduled...
We present here the Large-scale Cryogenic Gravitational wave Telescope (LCGT) project which is aimed to improve sensitivity of existing gravitational projects by ten times. LCGT constructing km-scale detector in Japan succeeding TAMA project, adopts cryogenic mirrors with a higher power laser. are planing build it an underground site Kamioka mine. If its target attained, we will be able catch few events per month.
DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) is the future Japanese space gravitational antenna. The goal of DECIGO to detect waves from various kinds sources mainly between 0.1 Hz and 10 thus open a new window observation for astronomy. will consist three drag-free spacecraft, 1000 km apart each other, whose relative displacements are measured by Fabry—Perot Michelson interferometer. We plan launch pathfinder first demonstrate technologies required realize and, if...
KAGRA is a second-generation interferometric gravitational-wave detector with 3-km arms constructed at Kamioka, Gifu in Japan. It now its final installation phase, which we call bKAGRA (baseline KAGRA), scientific observations expected to begin late 2019. One of the advantages underground location least 200 m below ground surface, brings small seismic motion low frequencies and high stability detector. Another advantage that it cools down sapphire test mass mirrors cryogenic temperatures...
We analyzed 6 hours of data from the TAMA300 detector by matched filtering, searching for gravitational waves inspiraling compact binaries. incorporated a two-step hierarchical search strategy in filtering. obtained an upper limit 0.59/hour (C.L.=90%) on event rate inspirals binaries with mass between 0.3M⊙ and 10M⊙ signal-to-noise ratio greater than 7.2. The distance 1.4M⊙(0.5M⊙) which produce 7.2 was estimated to be 6.2 kpc (2.9 kpc) when position source sky inclination angle were...
A space gravitational-wave antenna, DECIGO (DECI-hertz interferometer Gravitational wave Observatory), will provide fruitful insights into the universe, particularly on formation mechanism of supermassive black holes, dark energy and inflation universe. In current pre-conceptual design, be comprising four units; each unit formed by three drag-free spacecraft with 1000 km separation. Since an extremely challenging mission high-precision flight long baseline, it is important to increase...
The large-scale cryogenic gravitational wave telescope (LCGT) is the future project of Japanese group. Two sets 3 km arm length laser interferometric detectors will be built in a tunnel Kamioka mine Japan. LCGT detect chirp waves from binary neutron star coalescence at 240 Mpc away with S/N 10. expected number detectable events year two or three. To achieve required sensitivity, several advanced techniques employed such as low-frequency vibration-isolation system, suspension point...
DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) is the planned Japanese space gravitational antenna, aiming to detect waves from astrophysically and cosmologically significant sources mainly between 0.1 Hz 10 thus open a new window for astronomy universe. DECIGO will consist of three drag-free spacecraft, 1000 km apart each other, whose relative displacements are measured by differential Fabry-Perot interferometer. We plan launch in middle 2020s, after sequence two...
The thermal fluctuation of mirror surfaces is the fundamental limitation for interferometric gravitational wave (GW) detectors. Here, we experimentally demonstrate first time a reduction in mirror's GW detector with sapphire mirrors from Cryogenic Laser Interferometer Observatory at 17 and 18 K. sensitivity, which was limited by room temperature, improved frequency range 90 to 240 Hz cooling mirrors. sensitivity reached maximum 2.2×10(-19) m/√Hz 165 Hz.
A laser strainmeter with a 1500-m baseline was constructed at an underground site in Kamioka, Gifu Prefecture, Japan, and has been operating since August 2016. The interferometer measures the change distance between two retroreflectors housed vacuum chambers separation of 1500 m. are fixed to ground tunnel KAGRA gravitational wave telescope. high-frequency-stabilized is used as light source; it achieves Allan variance 3 × 10−13. Since operations began, motions large amplitude timescale...
Abstract We report the mirror suspension design for large-scale cryogenic gravitational wave telescope, KAGRA, during bKAGRA phase 1. Mirror thermal noise is one of fundamental noises room-temperature gravitational-wave detectors such as Advanced LIGO and Virgo. Thus, reduction required further improvement their sensitivity. One effective approach reducing to cool mirrors. There are many technical challenges that must be overcome mirrors, cryocooler induced vibrations, drift in suspensions,...
The Large-scale Cryogenic Gravitational wave Telescope (LCGT) is planned as a future Japanese project for gravitational detection. A 3 km interferometer will be built in an underground mine at Kamioka. sapphire mirrors are going to employed the test masses. For demonstration of LCGT technologies, two prototype interferometers, TAMA300 and CLIO, being developed. This paper describes current status interferometers.
CLIO (Cryogenic Laser Interferometer Observatory) is a Japanese gravitational wave detector project. One of the main purposes to demonstrate thermal-noise suppression by cooling mirrors for future project, LCGT (Large-scale Cryogenic Gravitational Telescope). The site in Kamioka mine, as LCGT. progress between 2005 and 2007 (room- cryogenic-temperature experiments) introduced this article. In room-temperature experiment, we made efforts improve sensitivity. current best sensitivity at 300 K...
The CLIO project involves the Cryogenic Laser Interferometer Observatory (CLIO) detector complex for gravitational wave detection and Kamioka Interferometric Strainmeter acquisition of geophysical data. has been constructed to demonstrate feasibility a future project, Large-scale Gravitational Telescope (LCGT). It will utilize low seismic stable environment mine as well sapphire mirrors suspension fibres at temperature reduce thermal noise. We designed have noise level limited by fibres,...