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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
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SEQUENCE:1
UID:UW-Physics-Event-9739
DTSTART:20260709T150000Z
DTEND:20260709T170000Z
DTSTAMP:20260624T045012Z
LAST-MODIFIED:20260619T134905Z
LOCATION:Chamberlin 5310
SUMMARY:Search for Neutrinos with Energy Greater than 10^17 eV Using A
 ll 5 Stations of the Askaryan Radio Array at the South Pole\, Graduate
  Program Event\, Abigal Bishop
DESCRIPTION:Ultra-high energy (UHE\, 10^17 eV) neutrinos are rare mess
 engers which are valuable for understanding the UHE cosmic ray flux\, 
 composition\, and origin. When UHE neutrinos interact in dielectric me
 dia\, they initiate particle cascades that emit optical-wavelength Che
 renkov and radio-wavelength Askaryan emission. The highest energy neut
 rino reported had an energy of ∼ 220 PeV and was detected by the KM3
 NeT Collaboration via Cherenkov Radiation in the Mediterranean Sea [Ai
 ello et al.\, 2025]. At higher energies\, neutrino interactions are ex
 pected to only occur once per year per square kilometer [Navas et al.\
 , 2024]. Monitoring ice for Askaryan Radiation is powerful due to long
  attenuation and scattering lengths for radio waves in ice\, allowing 
 a single detector to monitor for rare UHE neutrino interactions over m
 any cubic kilometers. This thesis presents the neutrino search through
  10.6 yrs of data taken by the Askaryan Radio Array at the South Pole.
  Many techniques for background rejection are presented and used along
  with updated detector simulations. This analysis finds 0 neutrino can
 didates and therefore establishes an upper limit on the 10^16 eV - 10^
 21 eV cosmic neutrino flux. This result is also the world-leading uppe
 r limit above 4 × 10^19 eV.
URL:https://www.physics.wisc.edu/events/?id=9739
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