A5039405577- Pulsars and Gravitational Waves Research
- Geophysics and Sensor Technology
- Geophysics and Gravity Measurements
- Radio Astronomy Observations and Technology
- Atomic and Subatomic Physics Research
- Superconducting Materials and Applications
- Advanced Frequency and Time Standards
- Adaptive optics and wavefront sensing
- Astrophysical Phenomena and Observations
- Astronomical Observations and Instrumentation
- Advanced Fiber Laser Technologies
- Cold Atom Physics and Bose-Einstein Condensates
- Advanced X-ray Imaging Techniques
- Mechanical and Optical Resonators
- Crystallography and Radiation Phenomena
- Particle Accelerators and Free-Electron Lasers
- Seismic Waves and Analysis
- Gamma-ray bursts and supernovae
- Hydraulic and Pneumatic Systems
- Advanced Electrical Measurement Techniques
- Numerical methods for differential equations
- GNSS positioning and interference
- Photonic and Optical Devices
- Model Reduction and Neural Networks
- Advanced Semiconductor Detectors and Materials
Japan Aerospace Exploration Agency
2020-2024
Institute of Space and Astronautical Science
2019-2024
The University of Tokyo
1992-1997
NEC (Japan)
1997
Abstract The Deci-hertz Interferometer Gravitational Wave Observatory (DECIGO) is a future Japanese space mission with frequency band of 0.1 Hz to 10 Hz. DECIGO aims at the detection primordial gravitational waves, which could have been produced during inflationary period right after birth Universe. There are many other scientific objectives DECIGO, including direct measurement acceleration expansion Universe, and reliable accurate predictions timing locations neutron star/black hole binary...
Calibration of the Advanced LIGO detectors is quantification detectors' response to gravitational waves. Gravitational waves incident on cause phase shifts in interferometer laser light which are read out as intensity fluctuations at detector output. Understanding this crucial producing accurate and precise wave strain data. Estimates binary black hole neutron star parameters tests general relativity require well-calibrated data, miscalibrations will lead biased results. We describe method...
KAGRA is a newly built gravitational wave observatory, laser interferometer with 3 km arm length, located in Kamioka, Gifu, Japan. In this series of articles, we present an overview the baseline KAGRA, for which finished installing designed configuration 2019. This article describes method calibration (CAL) used reconstructing signals from detector outputs, as well characterization (DET). We also review physical environmental monitors (PEM) system and geophysics (GIF). Both are...
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...
The two interferometers of the Laser Interferometry Gravitational-wave Observatory (LIGO) recently detected gravitational waves from mergers binary black hole systems. Accurate calibration output these detectors was crucial for observation events and extraction parameters sources. principal tools used to calibrate responses second-generation (Advanced) LIGO are systems based on radiation pressure referred as photon calibrators. These systems, which were completely redesigned Advanced LIGO,...
Advanced LIGO's raw detector output needs to be calibrated compute dimensionless strain h(t). Calibrated data is produced in the time domain using both a low-latency, online procedure and high-latency, offline procedure. The low-latency h(t) stream two stages, first of which performed on same computers that operate detector's feedback control system. This stage, referred as front-end calibration, uses infinite impulse response (IIR) filtering performs all operations at 16384 Hz digital...
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 detection primordial gravitational waves, which could be produced during inflationary period right after birth universe. There are many other scientific objectives DECIGO, including direct measurement acceleration expansion universe, and reliable accurate predictions timing locations neutron star/black hole binary coalescences....
Calibration of the second-generation LIGO interferometric gravitational-wave detectors employs a method that uses injected periodic modulations to track and compensate for slow temporal variations in differential length response instruments. These utilize feedback control loops maintain resonance conditions by suppressing arm variations. We describe how sensing actuation functions these servo are parameterized parameters quantified using modulations. report results applying this show it...
Abstract Future gravitational wave observation in space will demand improvement the sensitivity of local sensor for drag-free control. This paper presents proposal, design, and demonstration a new laser interferometric named Quadrature Interferometric Metrology Translation Tilt (QUIMETT) sensor. QUIMETT enables simultaneous measurements both translational displacement tilts reflective object with single interferometer package. offers characteristic feature where to tilt is independent...
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,...
Gravitational-wave (GW) laser interferometers such as Advanced LIGO (The Scientific Collaboration 2015 Class. Quantum Grav. 32 074001) transduce spacetime strain into optical power fluctuation. Converting this fluctuation back an estimated requires a calibration process that accounts for both the interferometer's optomechanical response and feedback control loop used to interferometer test masses. Systematic errors in parameters lead systematic GW estimate, hence astrophysical parameter...
This study investigates the effects of space environmental radiation on performance In <sub xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">0.53</sub> Ga xmlns:xlink="http://www.w3.org/1999/xlink">0.47</sub> As Quadrant Photodiodes (QPDs) and assesses their suitability for Laser Interferometer Space Antenna (LISA) mission. QPDs 1.0 mm, 1.5 2.0 mm diameter were irradiated with 20 60 MeV protons, 0.5 1 electrons, Co...
We propose and demonstrate a method to, in principle, completely remove shot noise of optical beat-note detection using squeezed light. This leads to improving the sensitivity various spatial/temporal measurements.
Interference between x-ray beams scattered from a nuclear resonance in stainless-steel foils of different thicknesses has been observed. In-phase and out-of-phase oscillations have measured for yields with three time windows, which exist because sign change the amplitude describing evolution nuclear-resonant forward scattering. This confirms modulation subsequent decays brought about by dispersion addition to increase decay rate.
Abstract Direct observations of gravitational waves at frequencies below 10 Hz will play a crucial role in fully exploiting the potential wave astronomy. One approach to pursue this direction is utilization laser interferometers equipped with Fabry–Pérot optical cavities space. However, there are number practical challenges following path. In particular, implementation precision control for cavity lengths and suppression phase noises may prevent detector design. To circumvent such...
Detuning the signal-recycling cavity length from a resonance significantly improves quantum noise beyond standard limit, while there is no km-scale gravitational-wave detector successfully implemented technique. The detuning technique known to introduce great excess noise, and such can be reduced by laser modulation system with two Mach-Zehnder interferometers in series. This system, termed Modulator (MZM), also makes control of more robust introducing third field which non-resonant any part...
The torsion pendulum is a prevailing instrument for measuring small forces acting on solid body or those between bodies. While it offers powerful advantages, the measurement precision suffers from thermal noises of suspending wires giving rise to stochastic torque noises. This letter proposes new scheme reduce effect such noise by employing double and cross-correlation technique based theoretical analysis that appears at each end wire differentially. Cross-correlating two synthesized data...
Optical phase-insensitive heterodyne (beat-note) detection, which measures the relative phase of two beams at different frequencies through their interference, is a key sensing technology for various spatial/temporal measurements, such as frequency measurements in optical combs. However, its sensitivity limited not only by shot noise from signal band but also extra an image band, known 3-dB penalty. Here, we propose method to remove all these bands using squeezed light. We demonstrate...
The Kamioka Gravitational wave detector (KAGRA) cryogenic gravitational-wave observatory has commenced joint observations with the worldwide gravitational network. Precise calibration of response is essential for accurately estimating parameters sources. A photon calibrator a crucial tool used in laser interferometer observatory, Virgo, and KAGRA, it was utilized observation 3 GEO600 Germany April 2020. In this paper, KAGRA implemented three key enhancements: high-power laser, power...
The back-linked Fabry-Perot interferometer (BLFPI) is an topology proposed for space gravitational wave antennas with the use of inter-satellite interferometers. BLFPI offers simultaneous and independent control over all length degrees freedom by controlling laser frequencies. Therefore, does not require active system physical lengths To achieve a high sensitivity, implementation must rely on offline signal process subtracting frequency noises. However, subtraction has been experimentally...
Optical phase-insensitive heterodyne (beat-note) detection, which measures the relative phase of two beams at different frequencies through their interference, is a key sensing technology for various spatial/temporal measurements, such as frequency measurements in optical combs. However, its sensitivity limited not only by shot noise from signal band but also extra an image band, known 3-dB penalty. Here, we propose method to remove all these bands using squeezed light. We demonstrate...