JPS Conference Proceedings of VHEPA2014


The 7th International Workshop on Very High Energy Particle Astronomy (VHEPA2014) with the subtitle of ”Next Generation Explorers for Cosmic Ray Origins” was held on the date of March 19- 20, 2014 at the location of Media Hall, Kashiwa Library, The University of Tokyo. VHEPA is a series of workshops aiming for comprehensive study with multi-particle observations toward Very High Energy Particle Astronomy.

The purpose of the VHEPA2014 Workshop is to discuss Next Generation Explorer(s) for Cosmic Ray Origins as subtitled, and to share a common interest in the field with scientists from different countries. We expect front-line invited speakers from around the world to present aspects of forefront research achievements at this Workshop, in accordance with its purpose. Contributions to the Workshop, we believe, will be of great value to all participants.

The International Advisory Committee (IAC) includes F. Halzen (Wisconsin-Madison), T. Kifune (Tokyo), A. Watson (Leeds). The Local Organizing Committee (LOC) includes G. W.-S. Hou (Taiwan), S. Ogawa (Toho) (Chair), M. Sasaki (Tokyo). N. Sugiyama (Nagoya).

Editorial Commitee February 23, 2015.




Ashra Neutrino Telescope Array (NTA): Combined Imaging Observation of Astroparticles — For Clear Identification of Cosmic Accelerators and Fundamental Physics Using Cosmic Beams —

Makoto Sasaki, and Tadashi Kifune for the NTA Collaboration

011013, 10.7566/JPSCP.15.011013


ニュートリノ&ガンマ線水チェレンコフ検出器 LENA — 素粒子的宇宙像研究会 1988

Proposal for a Large Area Water Cerenkov Detector
Dedicated to Neutrino and Gamma-ray Astrophysics
M.Sasaki, et al.,
The 2nd Workshop on Elementary-Particle Picture of the Universe
KEK, February 4-6, 1988

We propose a large area (=10^4 m^2) water Cerenkov observatory for high energy neutrino and gamma-ray with good angular resolution about l degree. This detector is 100 m radius and 30 m high, and is located in a lake. It contains two optically isolated layers: an outer layer with 10 m thick and inner layer with 20m thick. The cross section of this detector is shown in Fig l. The inner layer is surrounded by inward-facing 20 inch-photomultipliers (PMTs) and outward-facing 20 inch-PMTs on a 5 m-grid. Each layer is covered with a blackplastic to be isolated optically. The direction or interaction point of charged particle is decided with the 2-dimensional pattern of TDC and ADC data from PMTs in each layer. In this report,we confirm that it is possible to

  1. establish gamma-ray astronomy and search for unknown gamma-ray stars without the time variable in formation,
  2. open a new window of neutrino astronomy if the present theoretical model of binary stars is true,
  3. investigate neutrino oscillation to the limit of dm^2 = 10^-4 and sin^2 2θ~0.06, and
  4. search for high energy (>1GeV) neutrinos from the Sun induced by a dark matter candidate, for example, photino on the basis of the detector performance studied by Monte Carlo (MC) method.