T. Tanimori
A5059330648- Particle Detector Development and Performance
- Astrophysics and Cosmic Phenomena
- Radiation Detection and Scintillator Technologies
- Dark Matter and Cosmic Phenomena
- Gamma-ray bursts and supernovae
- Nuclear Physics and Applications
- Particle physics theoretical and experimental studies
- Neutrino Physics Research
- Medical Imaging Techniques and Applications
- Atomic and Subatomic Physics Research
- CCD and CMOS Imaging Sensors
- Quantum Chromodynamics and Particle Interactions
- High-Energy Particle Collisions Research
- Radiation Therapy and Dosimetry
- Pulsars and Gravitational Waves Research
- Solar and Space Plasma Dynamics
- Astronomy and Astrophysical Research
- Astronomical Observations and Instrumentation
- Advanced X-ray and CT Imaging
- Geophysics and Gravity Measurements
- Astrophysical Phenomena and Observations
- Radio Astronomy Observations and Technology
- Particle Accelerators and Free-Electron Lasers
- Advanced Radiotherapy Techniques
- Adaptive optics and wavefront sensing
Kyoto University
2015-2024
Japan Aerospace Exploration Agency
2023
Institute of Space and Astronautical Science
2023
Smile Train
2020
The University of Tokyo
1983-2017
Kobe University
1993-2017
Laboratoire de Physique Subatomique et de Cosmologie
2016
Université Grenoble Alpes
2016
Institut National de Physique Nucléaire et de Physique des Particules
2016
Centre National de la Recherche Scientifique
2016
A neutrino burst was observed in the Kamiokande II detector on 23 February, 7:35:35 UT (\ifmmode\pm\else\textpm\fi{}1 min) during a time interval of 13 sec. The signal consisted 11 electron events energy 7.5 to 36 MeV, which first two point back Large Magellanic Cloud with angles 18\ifmmode^\circ\else\textdegree\fi{}\ifmmode\pm\else\textpm\fi{}18\ifmmode^\circ\else\textdegree\fi{} and 15\ifmmode^\circ\else\textdegree\fi{}\ifmmode\pm\else\textpm\fi{}27\ifmmode^\circ\else\textdegree\fi{}.
Results from 1036 days of solar neutrino data accumulated in the upgraded Kamiokande detector (Kamiokande III) are presented. The $^{8}\mathrm{B}$ flux observed III is ${2.82}_{\ensuremath{-}0.24}^{+0.25}$ (stat) \ifmmode\pm\else\textpm\fi{} 0.27 (syst) \ifmmode\times\else\texttimes\fi{} ${10}^{6}$ ${\mathrm{cm}}^{\ensuremath{-}2}$${\mathrm{s}}^{\ensuremath{-}1}$; combined II and (2079 total) 2.80 0.19 0.33 ${\mathrm{cm}}^{\ensuremath{-}2}$${\mathrm{s}}^{\ensuremath{-}1}$, which 49% to 64%...
Neutrinos from the decay of $^{8}\mathrm{B}$ in Sun have been observed Kamiokande-II detector. Based on 450 days data time period January 1987 through May 1988; measured flux obtained with ${E}_{e}$\ensuremath{\ge}9.3 MeV is 0.46\ifmmode\pm\else\textpm\fi{}0.13(stat)\ifmmode\pm\else\textpm\fi{}0.08(sys) value predicted by standard solar model. Within experimental errors, agreement corresponding $^{37}\mathrm{Cl}$ radiochemical detector essentially same period.
A data sample of 1040 days from the Kamiokande II detector, consisting subsamples 450 at electron-energy threshold Ee≥9.3 MeV and 590 Ee≥7.5 MeV, yields a clear directional correlation solar-neutrino-induced electron events with respect to Sun measurement differential distribution. These provide unequivocal evidence for production B8 by fusion in Sun. The measured flux solar neutrinos two relative prediction standard model is 0.46±0.05(stat)±0.06(syst). total tested short-term time...
The properties of the Kamiokande-II detector and method measurement are described in detail. data on neutrino burst from supernova SN1987A 23 February 1987 at 7:35:35 UT\ifmmode\pm\else\textpm\fi{}1 min presented, with records earlier later observation periods which other events possibly associated might have occurred. There is no evidence for any excess neutrino-induced events, either a few seconds duration or over longer time interval, relative to usual count rate, excepting only UT....
The method of $^{8}\mathrm{B}$ solar-neutrino measurement by means the reaction ${\ensuremath{\nu}}_{e}e\ensuremath{\rightarrow}{\ensuremath{\nu}}_{e}e$ in Kamiokande II detector is described detail. A data sample 1040 live days time period January 1987 through April 1990 yields a clear directional correlation solar-neutrino-induced electron events with respect to Sun and differential energy distribution. measured flux solar neutrinos from subsamples 450 at threshold...
This paper reports the first discovery of TeV gamma-ray emission from a supernova remnant made with CANGAROO 3.8 m Telescope. gamma rays were detected at sky position and extension coincident north-east (NE) rim shell-type Supernova (SNR) SN1006 (Type Ia). has been most likely candidate for an extended Gamma-ray source, since clear synchrotron X-ray rims was recently observed by ASCA (Koyama et al. 1995), which is strong evidence existence very high energy electrons up to hundreds in SNR....
We present the case for a dark matter detector with directional sensitivity. This document was developed at 2009 CYGNUS workshop on detection, and contains contributions from theorists experimental groups in field. describe need sensitivity; each experiment presents their project's status; we close feasibility study scaling up to one ton detector, which would cost around $150M.
We have detected sub-TeV gamma-ray emission from the direction of Galactic center (GC) using CANGAROO-II Imaging Atmospheric Cerenkov Telescope. a statistically significant excess at energies greater than 250 GeV. The flux was 1 order magnitude lower that Crab Nebula TeV with soft spectrum proportional to E-4.6±0.5. signal centroid is consistent GC direction, and observed profile pointlike source. Our data suggest GeV source 3EG J1746-2851 identical this source, we study combined spectra...
An analysis of the Mikheyev-Smirnov-Wolfenstein effect using 1040 days Kamiokande-II data is reported, which provides constraints on neutrino-oscillation parameters. The measured recoil-electron energy spectrum alone leads to conclusion that adiabatic region, 7.2\ifmmode\times\else\texttimes\fi{}${10}^{\mathrm{\ensuremath{-}}4}$${\mathrm{sin}}^{2}$2\ensuremath{\theta}6.3\ifmmode\times\else\texttimes\fi{}${10}^{\mathrm{\ensuremath{-}}3}$,...
The flux of upward through-going muons minimum (mean) threshold energy >1.6 (3.0) GeV is measured, based on a total 372 events observed by the Kamiokande II+III detector during 2456 live days. muon was Φobs=[1.94±0.10(stat.)−0.06+0.07sys.)]×10−13cm−2s−1sr−1, which compared to an expected value Φtheo=[2.46±0.54(theo.)]×10−13cm−2s−1sr−1. observation in agreement with prediction within errors. zenith-angle dependence supports previous indication neutrino oscillations made using sub- and...
Searches for possible day-night and semiannual variations of the $^{8}\mathrm{B}$ solar neutrino flux are reported based on 1040 days Kamiokande-II data. Within statistical error, no such short-time were observed. The limit difference sets a constraint neutrino-oscillation parameters. A region defined by ${\mathrm{sin}}^{2}$2\ensuremath{\theta}>0.02...
Abstract A new scenario is presented for the cause of magnetospheric relativistic electron decreases (REDs) and potential effects in atmosphere on climate. High‐density solar wind heliospheric plasmasheet (HPS) events impinge onto magnetosphere, compressing it along with remnant noon‐sector outer‐zone ~10‐100 keV protons. The betatron accelerated protons generate coherent electromagnetic ion cyclotron (EMIC) waves through a temperature anisotropy (T ⊥ /T || > 1) instability. turn interact...
view Abstract Citations (124) References (21) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Very High Energy Gamma Rays from PSR 1706-44 Kifune, T. ; Tanimori, Ogio, S. Tamura, Fujii, H. Fujimoto, M. Hara, Hayashida, N. Kabe, Kakimoto, F. Matsubara, Y. Mizumoto, Muraki, Suda, Teshima, Tsukagoshi, Watase, Yoshikoshi, Edwards, P. G. Patterson, J. R. Roberts, D. Rowell, Thornton, We have obtained evidence of gamma-ray emission above 1 TeV PSR1706-44, using a...
Gamma rays with energies greater than 7 TeV from the Crab pulsar/nebula have been observed at large zenith angles, using Imaging Atmospheric Technique Woomera, South Australia. CANGAROO data taken in 1992, 1993 and 1995 indicate that energy spectrum extends up to least 50 TeV, without a change of index power law spectrum. The differential is \noindent $(2.01\pm 0.36)\times 10^{-13}(E/{7 TeV})^{-2.53 \pm 0.18} TeV^{-1}cm^{-2}s^{-1}$ between TeV. There no apparent cut-off. for photon above...
Abstract MeV gamma-rays provide a unique window for the direct measurement of line emissions from radioisotopes, but observations have made little significant progress since COMPTEL on board Compton Gamma-ray Observatory (CGRO). To observe celestial objects in this band, we are developing an electron-tracking camera (ETCC) that realizes both bijective imaging spectroscopy and efficient background reduction gleaned recoil-electron track information. The energy spectrum observation target can...