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A Comprehensive Diffuse Neutrino Search Using the Full Askaryan Radio Array

Pawan Giri

Abstract

The Askaryan Radio Array (ARA) is a neutrino experiment at the South Pole, designed to detect radio-frequency emissions produced by interactions of ultra-high energy (UHE) neutrinos with the Antarctic ice. The array consists of five autonomous stations, each equipped with deep in-ice antennas sensitive to both vertically and horizontally polarized radio signals. With nearly 30 station-years of livetime accumulated, ARA is now conducting its first comprehensive array-wide search for diffuse UHE neutrinos. This analysis is expected to deliver the most stringent constraints from any in-ice radio-based detector up to 1~ZeV and is capable of probing flux levels suggested by KM3NeT around 220~PeV. The results from this analysis marks a critical step toward establishing scalable techniques for next-generation detectors.

A Comprehensive Diffuse Neutrino Search Using the Full Askaryan Radio Array

Abstract

The Askaryan Radio Array (ARA) is a neutrino experiment at the South Pole, designed to detect radio-frequency emissions produced by interactions of ultra-high energy (UHE) neutrinos with the Antarctic ice. The array consists of five autonomous stations, each equipped with deep in-ice antennas sensitive to both vertically and horizontally polarized radio signals. With nearly 30 station-years of livetime accumulated, ARA is now conducting its first comprehensive array-wide search for diffuse UHE neutrinos. This analysis is expected to deliver the most stringent constraints from any in-ice radio-based detector up to 1~ZeV and is capable of probing flux levels suggested by KM3NeT around 220~PeV. The results from this analysis marks a critical step toward establishing scalable techniques for next-generation detectors.
Paper Structure (8 sections, 1 equation, 2 figures)

This paper contains 8 sections, 1 equation, 2 figures.

Table of Contents

  1. Ultra-high energy neutrinos: origin and motivation
  2. Askaryan Radio Array
  3. First array-wide neutrino search
  4. Data cleaning strategy
  5. Detector modeling and noise simulation
  6. Neutrino simulation and effective volume estimation
  7. Event selection optimization
  8. Conclusion

Figures (2)

  • Figure 1: (a) Schematic diagram of a traditional ARA station (Stations 1–5), showing antenna geometry and deployment depth. (b) Cumulative data volume collected by all ARA stations during 2013–2023.
  • Figure 2: (a) Effective volume of the full array compared with individual stations. (b) Projected 90% C.L. upper limit (solid) and single-event sensitivity (dashed) 5SASim.