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
(LENA)
M.Sasaki, et al.,
The 2nd Workshop on Elementary-Particle Picture of the Universe
KEK, February 4-6, 1988

1.INTRODUCTION
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 lOO m radius and 30 m high, and is located in a lake. It contains two optically isolated layers: an outer layer with lO m thick and inner layer with 20m thick. The crosssection 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.

——————————————————