32,195 research outputs found
The Lake Baikal neutrino experiment: selected results
We review the present status of the lake Baikal Neutrino Experiment and
present selected physical results gained with the consequetive stages of the
stepwise increasing detector: from NT-36 to NT-96. Results cover atmospheric
muons, neutrino events, very high energy neutrinos, search for neutrino events
from WIMP annihilation, search for magnetic monopoles and environmental
studies. We also describe an air Cherenkov array developed for the study of
angular resolution of NT-200.Comment: 25 pages, 12 figures. To appear in the Procrrdings of International
Conference on Non-Accelerator New Physics, June 28 - July 3, 1999, Dubna,
Russi
The AMANDA Neutrino Telescope
With an effective telescope area of order m for TeV neutrinos, a
threshold near 50 GeV and a pointing accuracy of 2.5 degrees per muon
track, the AMANDA detector represents the first of a new generation of high
energy neutrino telescopes, reaching a scale envisaged over 25 years ago. We
describe early results on the calibration of natural deep ice as a particle
detector as well as on AMANDA's performance as a neutrino telescope.Comment: 12 pages, Latex2.09, uses espcrc2.sty and epsf.sty, 13 postscript
files included. Talk presented at the 18th International Conference on
Neutrino Physics and Astrophysics (Neutrino 98), Takayama, Japan, June 199
Baikal-GVD: status and prospects
Baikal-GVD is a next generation, kilometer-scale neutrino telescope under
construction in Lake Baikal. It is designed to detect astrophysical neutrino
fluxes at energies from a few TeV up to 100 PeV. GVD is formed by multi-megaton
subarrays (clusters). The array construction started in 2015 by deployment of a
reduced-size demonstration cluster named "Dubna". The first cluster in its
baseline configuration was deployed in 2016, the second in 2017 and the third
in 2018. The full scale GVD will be an array of ~10000 light sensors with an
instrumented volume of about 2 cubic km. The first phase (GVD-1) is planned to
be completed by 2020-2021. It will comprise 8 clusters with 2304 light sensors
in total. We describe the design of Baikal-GVD and present selected results
obtained in 2015-2017.Comment: 9 pages, 8 figures. Conference proceedings for QUARKS201
High Energy Cosmic Neutrinos
While the general principles of high-energy neutrino detection have been
understood for many years, the deep, remote geographical locations of suitable
detector sites have challenged the ingenuity of experimentalists, who have
confronted unusual deployment, calibration, and robustness issues. Two high
energy neutrino programs are now operating (Baikal and AMANDA), with the
expectation of ushering in an era of multi-messenger astronomy, and two
Mediterranean programs have made impressive progress. The detectors are
optimized to detect neutrinos with energies of the order of 1-10 TeV, although
they are capable of detecting neutrinos with energies of tens of MeV to greater
than PeV. This paper outlines the interdisciplinary scientific agenda, which
span the fields of astronomy, particle physics, and cosmic ray physics, and
describes ongoing worldwide experimental programs to realize these goals.Comment: 15 pages, 9 figures, talk presented at the Nobel Symposium on
Particle Physics and the Universe, Sweden, August 199
Performance of two Askaryan Radio Array stations and first results in the search for ultra-high energy neutrinos
Ultra-high energy neutrinos are interesting messenger particles since, if
detected, they can transmit exclusive information about ultra-high energy
processes in the Universe. These particles, with energies above
, interact very rarely. Therefore, detectors that
instrument several gigatons of matter are needed to discover them. The ARA
detector is currently being constructed at South Pole. It is designed to use
the Askaryan effect, the emission of radio waves from neutrino-induced cascades
in the South Pole ice, to detect neutrino interactions at very high energies.
With antennas distributed among 37 widely-separated stations in the ice, such
interactions can be observed in a volume of several hundred cubic kilometers.
Currently 3 deep ARA stations are deployed in the ice of which two have been
taking data since the beginning of the year 2013. In this publication, the ARA
detector "as-built" and calibrations are described. Furthermore, the data
reduction methods used to distinguish the rare radio signals from overwhelming
backgrounds of thermal and anthropogenic origin are presented. Using data from
only two stations over a short exposure time of 10 months, a neutrino flux
limit of is
calculated for a particle energy of 10^{18}eV, which offers promise for the
full ARA detector.Comment: 21 pages, 34 figures, 1 table, includes supplementary materia
The IceCube Neutrino Observatory Part VI: Ice Properties, Reconstruction and Future Developments
Papers on ice properties, reconstruction and future developments submitted to
the 33nd International Cosmic Ray Conference (Rio de Janeiro 2013) by the
IceCube Collaboration.Comment: 28 pages, 38 figures; Papers submitted to the 33nd International
Cosmic Ray Conference, Rio de Janeiro 2013; version 2 corrects errors in the
author lis
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