Neutrino Water Ji Qilun Markov Calorimeter

Nowadays, neutrino physics has been one of most important frontier physical fields due to the ceaseless great developments of neutrino experiment in the last decade. Meanwhile, the long baseline neutrino experiment has unique advantages for the refined investigation of the neutrino oscillation parameters,such as the mixing parameters sin² 2θ₁₃, the CP phase, the matter effect and the sign of the dominant neutrino mass-squared difference. Inspired by the above idea, A full size water tank prototype, with a dimension of 1 × 1 × 13m³, made of PVC with reflective inner liner was built for the far detector of long baseline neutrino experiment.Firstly, we summarize the history of neutrino and some solar neutrino and atmosphere neutrino experiments, which are the.direct evidence for the neutrino oscillation. Then the physical targets of the long baseline neutrino oscillation experiments are discussed. Sec.2 presents a water tank for the Cherenkov calorimeter. Sec. 3 outlines the optical process of GEANT4 package and the Monte Carlo simulation program G4WT for a water tank. In Sec.4, we summarize the measurements of the water tank, including the effective attenuation length and the angular dependent response of the tank. In last section, we use the G4WT, GEANT3-based simulation program WCC, and neutrino generator to analysis the performance of the detector.In this paper, the effective attenuation length and the angular response of the tank was measured, and good agreement with a GEANT4 based full Monte Carlo simulation was obtained. The light yield, the total light collection efficiency, the effective attenuation length and the angular dependent response of the tank are all good enough for the long baseline neutrino oscillation experiment, and can be further improved. The performance is excellent for v_e and v_Τ appearance and v_μ disappearance from the The water Cherenkov calorimeter is a cheap and effective detector for v factories and v beams. And such a detector is also very desirable for cosmic-ray physics and astrophysics. There are no major technical difficulties although further R&D and detector optimization are needed.