13 research outputs found
The optical module of the Baikal deep underwater neutrino telescope
A deep underwater Cherenkov telescope has been operating since 1993 in stages
of growing size at 1.1 km depth in Lake Baikal. The key component of the
telescope is the Optical Module (OM) which houses the highly sensitive
phototube QUASAR-370. We describe design and parameters of the QUASAR-370, the
layout of the optical module, the front-end electronics and the calibration
procedures, and present selected results from the five-year operation
underwater. Also, future developments with respect to a telescope consisting
from several thousand OMs are discussed.Comment: 30 pages, 24 figure
Status of the Lake Baikal Experiment
We review the present status of the Baikal Underwater Neutrino Experiment and
report on neutrino events recorded with the detector stages NT-36 and NT-96.Comment: 5 pages, 4 PostScript figures, uses here.sty and mine.sty, submitted
to the Proc. of 5th Int. Workshop on Topics in Astroparticle and Underground
Physics (LNGS INFN, Assergi, September 7-11, 1997
The Baikal Deep Underwater Neutrino Experiment: Results, Status, Future
We review the present status of the Baikal Underwater Neutrino Experiment and
present results obtained with the various stages of the stepwise increasing
detector: NT-36 (1993-95), NT-72 (1995-96) and NT-96 (1996-97). Results cover
atmospheric muons, first clear neutrino events, search for neutrinos from WIMP
annihilation in the center of the Earth, search for magnetic monopoles, and --
far from astroparticle physics -- limnology.Comment: Talk given at the Int. School on Nuclear Physics, Erice, Sept.199
Search for neutrinos from the core of the earth with the Baikal Underwater Detector NT-36
The first stage of the Baikal Neutrino Telescope NT-200, the detector NT-36, was operated from 1993 to 95. The data obtained with this small array were analysed to search for vertically upward muons. Apart from neutrinos generated in the atmosphere at the opposite side of the Earth, such muons might be due to neutrinos produced in neutralino annihilations in the center of the Earth. We have selected two clear neutrino candidates. From this, an 90%CL upper limit of 1.3 x 10^-13 muons cm^(-2) sec^(-1) in a cone with 15 degree half-aperture around the opposite zenith is obtained for muons due to neutralino annihilation