A5101227094- Particle physics theoretical and experimental studies
- High-Energy Particle Collisions Research
- Particle Detector Development and Performance
- Quantum Chromodynamics and Particle Interactions
- Dark Matter and Cosmic Phenomena
- Computational Physics and Python Applications
- CCD and CMOS Imaging Sensors
- Neutrino Physics Research
- Cosmology and Gravitation Theories
- Radiation Detection and Scintillator Technologies
- Calibration and Measurement Techniques
- Infrared Target Detection Methodologies
- Distributed and Parallel Computing Systems
- Astrophysical Phenomena and Observations
- Medical Imaging Techniques and Applications
- Atomic and Subatomic Physics Research
- Advanced Data Storage Technologies
- Advanced Optical Sensing Technologies
- Optical Systems and Laser Technology
- Advanced X-ray and CT Imaging
- Astrophysics and Cosmic Phenomena
- Advanced Measurement and Detection Methods
- Superconducting Materials and Applications
- Nuclear Physics and Applications
- Surface Roughness and Optical Measurements
University of Tsukuba
2021-2025
Istituto Nazionale di Fisica Nucleare, Sezione di Trieste
2023-2024
Istituto Nazionale di Fisica Nucleare, Gruppo Collegato di Udine
2023-2024
The Abdus Salam International Centre for Theoretical Physics (ICTP)
2023-2024
A. Alikhanyan National Laboratory
2024
Atlas Scientific (United States)
2024
University of Sussex
2023
The University of Adelaide
2023
Hamamatsu Photonics (United Kingdom)
2020
Hamamatsu Photonics (Japan)
1993-2017
Abstract The Hyper Suprime-Cam (HSC) is an 870 megapixel prime focus optical imaging camera for the 8.2 m Subaru telescope. wide-field corrector delivers sharp images of 0${^{\prime\prime}_{.}}$2 (FWHM) in HSC-i band over entire 1${^{\circ}_{.}}$5 diameter field view. collimation with respect to axis primary mirror done hexapod actuators, mechanical accuracy which a few microns. Analysis remaining wavefront error off-focus stellar reveals that components meets design specifications. While...
Hyper Suprime-Cam (HSC) is an 870 Mega pixel prime focus camera for the 8.2 m Subaru telescope. The wide field corrector delivers sharp image of 0.25 arc-sec FWHM in r-band over entire 1.5 degree (in diameter) view. collimation with respect to optical axis primary mirror realized by hexapod actuators whose mechanical accuracy few microns. As a result, we expect have seeing limited most time. Expected median 0.67 i-band. sensor p-ch fully depleted CCD 200 micron thickness (2048 x 4096 15 μm...
The x-ray properties of multinested thin-foil mirror telescopes (XRT's) on board ASCA, the Advanced Satellite for Cosmology and Astrophysics, were fully evaluated with an pencil beam.Scanning over telescope aperture 35 cm in diameter beam, we found effective area a set XRT's to be 325, 200, 113 cm(2) at energies 1.5, 4.5, 8.0 keV, respectively. We derive point-spread functions (PSF's) by measuring image profile focal plane CCD. PSF is exhibit sharp core concentrated within 30 arcsec broad...
Hyper Suprime-Cam (HSC) is a second-generation wide field imaging camera for Subaru telescope with 10 times wider of view (FOV) compared (SC) currently being used. HSC makes the survey speed considerably faster than SC, while maintaining high image quality SC. The 1.5 degrees in diameter FOV covered 116 2K × 4K fully depleted back-illuminated CCDs 15 μm pixels developed by HAMAMATSU Photonics K. and National Astronomical Observatory Japan (NAOJ). are designed to have higher quantum...
Hyper Suprime-Cam (HSC)<sup>1</sup>,<sup>2</sup> is a wide field imaging camera with the of view (FOV) 1.5 degree diameter, which to be installed at prime focus Subaru Telescope. The large FOV realized by 116 2K × 4K pixels fully depleted back-illuminated CCD (FDCCD) 15 μm pixel square. acceptance inspection CCDs started around end 2009 and finished June 2011. We measured basic characteristics such as charge transfer efficiency (CTE), dark current, readout noise, linearity number...
Abstract Uncovering neutrinoless double beta decay (0ν2β) is crucial for confirming neutrinos’ Majorana characteristics. The rate of 0νββ theoretically uncertain, influenced by nuclear matrix elements that vary across nuclides. To reduce this uncertainty, precise measurement the half-life neutrino-emitting (2ν2β) in different nuclides essential. We have launched PIKACHU (Pure Inorganic scintillator experiment KAmioka CHallenging Underground sciences) project to fabricate high-purity Ce-doped...
We have been developing fully-depleted CCDs fabricated on N-type silicon wafer in collaboration with HAMAMATSU Photonics K.K.We made several runs to optimize the basic characteristics of devices such as charge transfer efficiency (CTE), full-well capacity and amplifier gain, followed by optimization backside treatment improve quantum (QE) blue wavelengths. The process is successfully completed, Hamamatsu recently started deliver 2k × 4k (15 μm pixel) four-side buttable for acceptance...
Quantum Efficiency (QE) of CCDs decreases at λ >~ 0.7 μm since photons penetrate a depletion layer CCD. If one makes the thicker, QE will be largely improved. In collaboration with HAMAMATSU Photonics, we have been developing thicker which are implemented on high resistivity n-type silicon wafers. We made several wafer runs to optimize basic characteristics devices such as charge transfer efficiency (CTE), full-well and node sensitivities amplifiers. The results obtained so far mostly...
In order to improve the quantum efficiency (QE) at longer wavelength, we have developed fully-depleted backilluminated CCDs in collaboration with Hamamatsu Photonics K.K (HPK). Recently, HPK delivered 10 for Subaru Prime Focus Camera (Suprime-Cam). These are made on N-type, high resistivity silicon wafers. Each CCD has a 200 μm thick depletion layer. The format is four-side buttable, 2k × 4k, 15 square pixels 4 low noise output amplifiers. characteristics of been tested laboratory before...
A 30-m-long X-ray beam line has been built at the Institute of Space and Astronautical Science (ISAS) to evaluate performance optical instruments for space programs, in particular telescope onboard Astro-D (Asca) satellite. This consists an generator, a vacuum duct, measuring chambers. Strong stable pencil beams from Al, Ti, Cu, Mo W targets are available with parallelism several arcs [full width half maximum (FWHM)]. Three kinds detectors prepared: conventional gas proportional counter...
We are developing an X-ray charge-coupled device (CCD) for the next Japanese astronomical satellite mission, NeXT (New Telescope/Nonthermal energy eXploration Telescope). developed a trial product of p-channel CCD fabricated on n-type silicon wafer. It is possible to have thick depletion layer ∼300 µm with because it easy obtain high resistivity using wafer compared p-type evaluated performance CCD. The imaging area consists 512×512 pixels pixel size 24×24 2 . horizontal charge transfer...
Athermal silica-based interferometer-type planar light-wave circuits were realized by a newly developed multicore fabrication method. In this method, inductively coupled chemical-vapor deposition and polishing technologies are adopted on silica substrate with trench-type waveguide pattern prepared reactive ion etching. Two kinds of deposited core material, 10GeO2-90SiO2 (mol. %) 8GeO2-5B2O3-87SiO2 %), which show wavelength temperature dependence 9.7 8.1 pm/degree C, respectively, used to...
We report on the development of X-ray CCD for soft imager (SXI) onboard ASTRO-H. SXI CCDs are P-channel, back-illuminated type manufactured by Hamamatsu Photonics K. Experiments with prototype shows device has a depletion layer as thick 200μm, high efficiency hard X-rays. By irradiating X-rays to SXI. At same time, we found significant low energy tail in response CCD. thus made several small size chips different treatment processing surface layers. one layers show which intensity is order...
Uncovering neutrinoless double beta decay (0$\nu$2$\beta$) is crucial for confirming neutrinos' Majorana characteristics. The rate of 0$\nu\beta\beta$ theoretically uncertain, influenced by nuclear matrix elements that vary across nuclides. To reduce this uncertainty, precise measurement the half-life neutrino-emitting (2$\nu$2$\beta$) in different nuclides essential. We have launched PIKACHU (Pure Inorganic scintillator experiment KAmioka CHallenging Underground sciences) project to...
Neutrinoless double beta decay (0v2b) has been investigated as a physical process that can provide evidence for the Majorana nature of neutrinos. The theoretical predictions 0v2b rate are subject to significant uncertainty, primarily due nuclear matrix elements (NME). To reduce this experimental measurements half-lives two-neutrino (2v2b) in various nuclei essential benchmark NME calculations. PIKACHU (Pure Inorganic scintillator experiment KAmioka CHallenging Underground sciences) project...
The NeXT (New X-ray Telescope) satellite to be launched around 2010, has a large effective area in the 0.1-80 keV band with use of multilayer super mirror (HXT). As one focal plane detectors for NeXT, we have been developing Soft Imager (SXI). SXI consists charge coupled devices (CCDs). In order increase quantum efficiency (Q.E.) as high possible, i.e., detect X-rays collected by HXT many developed "fully-depleted and back-illuminated CCD" attempt improve Q.E. soft structure that hard...
The next Japanese X-ray astronomical satellite mission, <i>NeXT</i>, was proposed to ISAS/JAXA following the Astro-E2 <i>Suzaku</i> which launched in July 2005. We develop an CCD camera system, SXI (Soft Imager), for <i>NeXT</i>. Hard Telescope (HXT) onboard <i>NeXT</i> provides imaging capability up 80 keV, using multilayer-coated mirror technology, called "Supermirror", newly developed Japan. is one of focal plane detectors HXT, covers soft energy band 0.5-12 keV baseline and 0.3-25 goal....
The x-ray optical properties of X-Ray Telescopes (XRTs) on board Asca were evaluated with an pencil beam at ISAS 30 m line. total effective area four XRTs is obtained to be about 1300 cm<SUP>2</SUP>, 800 and 450 cm<SUP>2</SUP> each energy 1.5 keV, 4.5 8.0 respectively. These values are 15% less than those calculated by ray tracing method in ideal case. shadow effect closely packed foils might the main reason for degradation area. Point Spread Function XRT was also measured CCD. We have...