scholarly journals Hybrid detection of high-energy cosmic neutrinos with the next generation neutrino detectors at the South Pole

2019 ◽  
Author(s):  
Simona Toscano ◽  
Paul Coppin ◽  
Krijn de Vries ◽  
Nick van Eijndhoven ◽  
Juan Antonio Aguilar
Keyword(s):  
High Energy ◽  
South Pole ◽  
Next Generation ◽  
The South ◽  
Neutrino Detectors ◽  
Hybrid Detection

scholarly journals Next generation neutrino detectors at the South Pole

2019 ◽  
Vol 207 ◽  
pp. 01005
Author(s):  
Marek Kowalski
Keyword(s):  
Neutrino Physics ◽  
South Pole ◽  
Energy Window ◽  
Next Generation ◽  
The South ◽  
Neutrino Detectors ◽  
Scientific Questions

Since the construction of IceCube was completed in 2010/11, the observatory has delivered several outstanding measurements in neutrino physics and multimessenger astronomy. Additionally, a series of new scientific questions and opportunities appeared. To address these, plans have been developed to expand on the IceCube concept, targeting both lower and higher energies, as well as the central PeV-energy window at significantly improved sensitivity. In this contribution I will outline these plans.

scholarly journals On the age vs depth and optical clarity of deep ice at the South Pole

1995 ◽  
Vol 41 (139) ◽  
pp. 445-454
Author(s):  
Keyword(s):  
Visible Light ◽  
High Energy ◽  
Dust Concentration ◽  
Cherenkov Light ◽  
South Pole ◽  
The South ◽  
High Energy Neutrino ◽  
Arrival Times ◽  
Energy Neutrino ◽  
Crystal Boundaries

AbstractThe first four strings of phototubes for the AMANDA high-energy neutrino observatory are now frozen in place at a depth of 800-1000 m in ice at the South Pole, During the 1995-96 season, as many as six more strings will be deployed at greater depths. Provided absorption, scattering and refraction of visible light are sufficiently small, the trajectory of a muon into which a neutrino converts can be determined by using the array of phototubes to measure the arrival times of Cherenkov light emitted by the muon. To help in deciding on the depth for implantation of the six new strings, we discuss models of age vs depth for South Pole ice, we estimate mean free paths for scattering from bubbles and dust as a function of depth and we assess distortion of light paths due to refraction at crystal boundaries and interfaces between air-hydrate inclusions and normal ice. We conclude that the interval 1600-2100 m will be suitably transparent for a future 1 km3 observatory except possibly in a region a few tens of meters thick at a depth corresponding to a peak in the dust concentration at 60 k year BP.

scholarly journals Modeling ice birefringence and oblique radio wave propagation for neutrino detection at the South Pole

2020 ◽  
Vol 61 (81) ◽  
pp. 84-91 ◽  
Author(s):  
T. M. Jordan ◽  
D. Z. Besson ◽  
I. Kravchenko ◽  
U. Latif ◽  
B. Madison ◽  
...  
Keyword(s):  
Time Delays ◽  
Ice Core ◽  
High Energy ◽  
Propagation Model ◽  
Neutrino Interaction ◽  
Crystallographic Axis ◽  
South Pole ◽  
The South ◽  
Range Estimation ◽  
Ice Flow

AbstractThe Askaryan Radio Array (ARA) experiment at the South Pole is designed to detect high-energy neutrinos which, via in-ice interactions, produce coherent radiation at frequencies up to 1000 MHz. Characterization of ice birefringence, and its effect upon wave polarization, is proposed to enable range estimation to a neutrino interaction and hence aid in neutrino energy reconstruction. Using radio transmitter calibration sources, the ARA collaboration recently measured polarization-dependent time delay variations and reported significant time delays for trajectories perpendicular to ice flow, but not parallel. To explain these observations, and assess the capability for range estimation, we use fabric data from the SPICE ice core to model ice birefringence and construct a bounding radio propagation model that predicts polarization time delays. We compare the model with new data from December 2018 and demonstrate that the measurements are consistent with the prevailing horizontal crystallographic axis aligned near-perpendicular to ice flow. The study supports the notion that range estimation can be performed for near flow-perpendicular trajectories, although tighter constraints on fabric orientation are desirable for improving the accuracy of estimates.

scholarly journals IceCube — the next generation neutrino telescope at the South Pole

2003 ◽  
Vol 118 ◽  
pp. 388-395 ◽  
Author(s):  
A. Karle ◽  
J. Ahrens ◽  
J.N. Bahcall ◽  
X. Bai ◽  
T. Becka ◽  
...  
Keyword(s):  
Neutrino Telescope ◽  
South Pole ◽  
Next Generation ◽  
The South

ULTRA HIGH ENERGY NEUTRINO TELESCOPES

2006 ◽  
Vol 21 (08n09) ◽  
pp. 1914-1924
Author(s):  
PER OLOF HULTH
Keyword(s):  
Lake Baikal ◽  
High Energy ◽  
Atmospheric Neutrinos ◽  
South Pole ◽  
Ultra High Energy ◽  
The South ◽  
High Energy Neutrino ◽  
Neutrino Telescopes ◽  
Energy Neutrino ◽  
Neutrino Astronomy

The Neutrino Telescopes NT-200 in Lake Baikal, Russia and AMANDA at the South Pole, Antarctica have now opened the field of High Energy Neutrino Astronomy. Several other Neutrino telescopes are in the process of being constructed or very near realization. Several thousands of atmospheric neutrinos have been observed with energies up to several 100 TeV but so far no evidence for extraterrestrial neutrinos has been found.

scholarly journals Receiver development for BICEP Array, a next-generation CMB polarimeter at the South Pole

2020 ◽  
Author(s):  
Lorenzo Moncelsi ◽  
Peter A. Ade ◽  
Zeeshan Ahmed ◽  
Mandana Amiri ◽  
Denis Barkats ◽  
...  
Keyword(s):  
South Pole ◽  
Next Generation ◽  
The South

scholarly journals Observation of radio emissions from electron beams using an ice target

2019 ◽  
Vol 216 ◽  
pp. 02010
Author(s):  
Keiichi Mase ◽  
Daisuke Ikeda ◽  
Aya Ishihara ◽  
Hiroyuki Sagawa ◽  
Tatsunobu Shibata ◽  
...  
Keyword(s):  
Light Source ◽  
Electron Beams ◽  
High Energy ◽  
Neutrino Telescope ◽  
South Pole ◽  
The South ◽  
Telescope Array ◽  
Radio Emissions ◽  
Systematic Uncertainties ◽  
Radio Signals

To observe high energy cosmogenic neutrinos above 50 PeV, the large neutrino telescope ARA is being built at the South Pole. The ARA telescope detects neutrinos by observing radio signals by the Askaryan effect. We performed an experiment using 40 MeV electron beams of the Telescope Array Electron Light Source to verify the understanding of the Askaryan emission as well as the detector responses used in the ARA experiment. Clear coherent polarized radio signals were observed with and without an ice target. We found that the observed radio signals are consistent with simulation, showing that our understanding of the radio emissions and the detector responses are within the systematic uncertainties of the ARAcalTA experiment which is at the level of 30%.

scholarly journals IceCube: A Kilometer-Scale Neutrino Observatory at the South Pole

2005 ◽  
Vol 13 ◽  
pp. 949-950
Author(s):  
Francis Halzen
Keyword(s):  
Cosmic Rays ◽  
Particle Physics ◽  
High Energy ◽  
Neutrino Telescope ◽  
South Pole ◽  
Neutrino Detector ◽  
The South ◽  
High Energy Neutrino ◽  
Neutrino Telescopes ◽  
Diversity Of Science

AbstractSolving the century-old puzzle of how and where cosmic rays are accelerated mostly drives the design of high-energy neutrino telescopes. It calls, along with a diversity of science goals reaching particle physics, astrophysics and cosmology, for the construction of a kilometer-scale neutrino detector. This led to the IceCube concept to transform a kilometer cube of transparent Antarctic Ice, one mile below the South Pole, into a neutrino telescope.

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