An experiment to search for ultra high energy γ-ray sources from the south pole

1989 ◽  
Vol 276 (3) ◽  
pp. 622-627 ◽  
Author(s):  
N.J.T. Smith ◽  
J.C. Perrett ◽  
M.A. Pomerantz ◽  
A.M. Hillas ◽  
P.A. Ogden ◽  
...  
Keyword(s):  
High Energy ◽  
South Pole ◽  
Ultra High Energy ◽  
The South ◽  
Γ Ray

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 Gamma-ray counterparts of 2WHSP high-synchrotron-peaked BL Lac objects as possible signatures of ultra-high-energy cosmic ray emission

2020 ◽  
Vol 497 (2) ◽  
pp. 2455-2468
Author(s):  
Michael W Toomey ◽  
Foteini Oikonomou ◽  
Kohta Murase
Keyword(s):  
Energy Range ◽  
Gamma Ray ◽  
Cosmic Ray ◽  
High Energy ◽  
Potential Candidate ◽  
Ultra High Energy ◽  
Bl Lac Objects ◽  
Cherenkov Telescopes ◽  
Bl Lac ◽  
Γ Ray

ABSTRACT We present a search for high-energy γ-ray emission from 566 Active Galactic Nuclei at redshift z > 0.2, from the 2WHSP catalogue of high-synchrotron peaked BL Lac objects with 8 yr of Fermi-LAT data. We focus on a redshift range where electromagnetic cascade emission induced by ultra-high-energy cosmic rays can be distinguished from leptonic emission based on the spectral properties of the sources. Our analysis leads to the detection of 160 sources above ≈5σ (TS ≥25) in the 1–300 GeV energy range. By discriminating significant sources based on their γ-ray fluxes, variability properties, and photon index in the Fermi-LAT energy range, and modelling the expected hadronic signal in the TeV regime, we select a list of promising sources as potential candidate ultra-high-energy cosmic ray emitters for follow-up observations by Imaging Atmospheric Cherenkov Telescopes.

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 ULTRA HIGH ENERGY COSMIC RAYS: PROPAGATION IN THE GALAXY AND ANISOTROPY

2001 ◽  
Vol 16 (39) ◽  
pp. 2505-2515 ◽  
Author(s):  
O. E. KALASHEV ◽  
V. A. KUZMIN ◽  
D. V. SEMIKOZ
Keyword(s):  
Cosmic Rays ◽  
Cold Dark Matter ◽  
High Energy ◽  
Ultra High Energy ◽  
Galactic Magnetic Field ◽  
High Energy Cosmic Rays ◽  
Self Consistent ◽  
The Galaxy ◽  
Γ Ray ◽  
Electron And Photon

We considered propagation of Ultra High Energy Cosmic Rays (UHECR) through the galaxy. We investigated models with sources of UHECR distributed in the same way as Cold Dark Matter (CDM) in a self-consistent way, taking into account both extra-galactic and Galactic contributions. Using a very simple toy model of galactic magnetic field we showed that in the case of galactic origin of UHECRs the anisotropy can reach considerable values. In the case of extragalactic UHECRs origin, the anisotropy appears to be nonvanishing only for electron and photon components due to synchrotron losses, but it can hardly be reassured. The reason is an extremely low flux of UHE electrons and a too low level of γ-ray anisotropy.

scholarly journals A STUDY ON ANISOTROPY IN THE ARRIVAL DIRECTIONS OF ULTRA-HIGH-ENERGY COSMIC RAYS OBSERVED BY PIERRE AUGER OBSERVATORY

2013 ◽  
Vol 28 (18) ◽  
pp. 1350075
Author(s):  
HANG BAE KIM
Keyword(s):  
Cosmic Rays ◽  
High Energy ◽  
Angular Distance ◽  
Pierre Auger Observatory ◽  
South Pole ◽  
Ultra High Energy ◽  
Background Contribution ◽  
High Energy Cosmic Rays ◽  
Centaurus A ◽  
Arrival Directions

We study the anisotropy in the arrival directions of Pierre Auger Observatory (PAO) ultra-high-energy cosmic rays (UHECRs), using the point source correlational angular distance distribution (CADD). The result shows that the anisotropy is characterized by one prominent excess region and one void region. The excess region is located near the Centaurus A direction, supporting that the Centaurus A is a promising UHECR source. The void region near the south pole direction may be used to limit the diffuse isotropic background contribution.

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 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%.

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