Author
Tatsuya Sawano
Other affiliations: Kyoto University
Bio: Tatsuya Sawano is an academic researcher from Kanazawa University. The author has contributed to research in topics: Gamma ray & Compton scattering. The author has an hindex of 15, co-authored 59 publications receiving 921 citations. Previous affiliations of Tatsuya Sawano include Kyoto University.
Papers
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Boston University1, Perimeter Institute for Theoretical Physics2, University of Waterloo3, Massachusetts Institute of Technology4, Joseph Fourier University5, University of California, Los Angeles6, Occidental College7, University of Pennsylvania8, University of Zaragoza9, University of Sheffield10, Brandeis University11, Harvard University12, Nagasaki Institute of Applied Science13, University of Edinburgh14, University of New Mexico15, University of Huelva16, University of Utah17, University of Nottingham18, Kyoto University19, Lawrence Berkeley National Laboratory20, Temple University21, University of Warwick22, New York University23, Nagoya University24, University of Tokyo25, Saga University26, University of Ioannina27
TL;DR: The case for a dark matter detector with directional sensitivity was presented at the 2009 CYGNUS workshop on directional dark matter detection, and contributions from theorists and experimental groups in the field as mentioned in this paper.
Abstract: We present the case for a dark matter detector with directional sensitivity. This document was developed at the 2009 CYGNUS workshop on directional dark matter detection, and contains contributions from theorists and experimental groups in the field. We describe the need for a dark matter detector with directional sensitivity; each directional dark matter experiment presents their project's status; and we close with a feasibility study for scaling up to a one ton directional detector, which would cost around $150M.
224 citations
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Wellesley College1, University of Zaragoza2, Istituto Nazionale di Fisica Nucleare3, Nagoya University4, University of Grenoble5, University of Lyon6, California Institute of Technology7, Massachusetts Institute of Technology8, Université Paris-Saclay9, University of Chicago10, Royal Holloway, University of London11, Saga University12, Lawrence Berkeley National Laboratory13, Middle East Technical University14, Colorado State University15, Kobe University16, University of Hawaii17, University of Florida18, Kyoto University19, Chiba University20, University of New Mexico21, University of Colorado Boulder22, KEK23, Paris Diderot University24, University of Tokyo25, Occidental College26, University of Sheffield27
TL;DR: In this paper, the authors review the various detector readout technologies used by directional detectors, summarize the challenges, advantages and drawbacks of each approach, and discuss future prospects for these technologies.
100 citations
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TL;DR: In this article, a direction-sensitive dark matter search experiment at Kamioka underground laboratory with the NEWAGE-0.3a detector was performed, which achieved a new record of 5400 pb for 150 GeV / c 2 WIMPs.
98 citations
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TL;DR: Nakamura et al. as discussed by the authors proposed a direction-sensitive dark matter search with gaseous tracking detector NEWAGE-0.3b, which was performed at Kyoto University.
Abstract: Direction-sensitive dark matter search with gaseous tracking detector NEWAGE-0.3b’ Kiseki Nakamura1,∗, Kentaro Miuchi2, Toru Tanimori1, Hidetoshi Kubo1, Atsushi Takada1, Joseph D. Parker1, Tetsuya Mizumoto1, Yoshitaka Mizumura1, Hironobu Nishimura1, Hiroyuki Sekiya3, Atsushi Takeda3, Tatsuya Sawano1, Yoshihiro Matsuoka1, Shotaro Komura1, Yushiro Yamaguchi2 and Takashi Hashimoto2 1Department of Physics, Kyoto University, Oiwakecho, Sakyo-ku Kyoto-shi, Kyoto, 606-8502, Japan 2Department of Physics, Kobe University, Rokodai, Nada-ku Kobe-shi, Hyogo, 657-8501, Japan 3Kamioka Observatory, ICRR, The University of Tokyo, Gifu, 506-1205 Japan ∗E-mail: nakamura@cr.scphys.kyoto-u.ac.jp
50 citations
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TL;DR: In this paper, an Electron-Tracking Compton Camera (ETCC) was used to measure 3D recoil electron tracks and recover the Scatter Plane Deviation (SPD) lost in Compton cameras.
Abstract: Photon imaging for MeV gammas has serious difficulties due to huge backgrounds and unclearness in images, which originate from incompleteness in determining the physical parameters of Compton scattering in detection, e.g., lack of the directional information of the recoil electrons. The recent major mission/instrument in the MeV band, Compton Gamma Ray Observatory/COMPTEL, which was Compton Camera (CC), detected a mere ∼30 persistent sources. It is in stark contrast with the ∼2000 sources in the GeV band. Here we report the performance of an Electron-Tracking Compton Camera (ETCC), and prove that it has a good potential to break through this stagnation in MeV gamma-ray astronomy. The ETCC provides all the parameters of Compton-scattering by measuring 3D recoil electron tracks; then the Scatter Plane Deviation (SPD) lost in CCs is recovered. The energy loss rate (dE/dx), which CCs cannot measure, is also obtained, and is found to be helpful to reduce the background under conditions similar to those in space. Accordingly, the significance in gamma detection is improved severalfold. On the other hand, SPD is essential to determine the point-spread function (PSF) quantitatively. The SPD resolution is improved close to the theoretical limit for multiple scattering of recoil electrons. With such a well-determined PSF, we demonstrate for the first time that it is possible to provide reliable sensitivity in Compton imaging without utilizing an optimization algorithm. As such, this study highlights the fundamental weak-points of CCs. In contrast we demonstrate the possibility of ETCC reaching the sensitivity below 1 × 10−12 erg cm−2 s−1 at 1 MeV.
45 citations
Cited by
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TL;DR: The first direct detection of gravitational waves and the first observation of a binary black hole merger were reported in this paper, with a false alarm rate estimated to be less than 1 event per 203,000 years, equivalent to a significance greater than 5.1σ.
Abstract: On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0×10(-21). It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203,000 years, equivalent to a significance greater than 5.1σ. The source lies at a luminosity distance of 410(-180)(+160) Mpc corresponding to a redshift z=0.09(-0.04)(+0.03). In the source frame, the initial black hole masses are 36(-4)(+5)M⊙ and 29(-4)(+4)M⊙, and the final black hole mass is 62(-4)(+4)M⊙, with 3.0(-0.5)(+0.5)M⊙c(2) radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.
4,375 citations
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01 Jan 2017
TL;DR: AGILE as discussed by the authors is an ASI space mission developed with programmatic support by INAF and INFN, which includes data gathered with the 1 meter Swope and 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile.
Abstract: This program was supported by the the Kavli Foundation, Danish National Research Foundation, the Niels Bohr International Academy, and the DARK Cosmology Centre. The UCSC group is supported in part by NSF grant AST-1518052, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, generous donations from many individuals through a UCSC Giving Day grant, and from fellowships from the Alfred P. Sloan Foundation (R.J.F.), the David and Lucile Packard Foundation (R.J.F. and E.R.) and the Niels Bohr Professorship from the DNRF (E.R.). AMB acknowledges support from a UCMEXUS-CONACYT Doctoral Fellowship. Support for this work was provided by NASA through Hubble Fellowship grants HST-HF-51348.001 (B.J.S.) and HST-HF-51373.001 (M.R.D.) awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. This paper includes data gathered with the 1 meter Swope and 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile.r (AGILE) The AGILE Team thanks the ASI management, the technical staff at the ASI Malindi ground station, the technical support team at the ASI Space Science Data Center, and the Fucino AGILE Mission Operation Center. AGILE is an ASI space mission developed with programmatic support by INAF and INFN. We acknowledge partial support through the ASI grant No. I/028/12/2. We also thank INAF, Italian Institute of Astrophysics, and ASI, Italian Space Agency.r (ANTARES) The ANTARES Collaboration acknowledges the financial support of: Centre National de la Recherche Scientifique (CNRS), Commissariat a l'energie atomique et aux energies alternatives (CEA), Commission Europeenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), IdEx program and UnivEarthS Labex program at Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02), Labex OCEVU (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02), Region Ile-de-France (DIM-ACAV), Region Alsace (contrat CPER), Region Provence-Alpes-Cite d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania;...
1,270 citations
01 Jan 1998
561 citations
01 Jan 2003
TL;DR: In this paper, the thermal and epithermal self-shielding factors in different materials (Al, Au, Cd, Co, Cu, Eu, Gd, In, Ir, Mo, Ni, Pt, Pb, Rh, Sc, Sm and Ta) and different geometries (foils, wires, spheres and) have been calculated using the MCNP code.
Abstract: The presence of a sample in the neutron field of a nuclear reactor creates a perturbation of the local neutron fluxes. In general, the interpretation of the sample activation due to thermal and epithermal neutrons requires the knowledge of two corrective parameters: the thermal neutron self-shielding factor, Gth, and the resonance neutron self-shielding factor, Gres. Thermal neutron self-shielding factors in different materials (Al, Au, Cd, Co, Cu, Eu, Gd, In, Ir, Mo, Ni, Pt, Pb, Rh, Sc, Sm and Ta) and different geometries (foils, wires, spheres and) have been calculated by using the MCNP code.
473 citations