Abstract
The ARIANNA experiment is currently taking data in its pilot-phase on the Ross ice-shelf. Fully autonomous stations measure radio signals in the frequency range from 100 MHz to 1 GHz. The seven station HRA was completed in December 2014, and augmented by two special purpose stations with unique configurations. In its full extent ARIANNA is targeted at detecting interactions of cosmogenic neutrinos (> 1016eV) in the ice-shelf. Downward-pointing antennas installed at the surface will record the radio emission created by neutrino-induced showers in the ice and exploit the fact that the ice- water surface acts as a mirror for radio emission. ARIANNA stations are independent, low-powered, easy to install and equipped with real-time communication via satellite modems. We report on the current status of the HRA, as well as air shower detections that have been made over the past year. Furthermore, we will discuss the search for neutrino emission, future plans and the energy-dependent sensitivity of the experiment.
Highlights
The ARIANNA detector is aimed at detecting neutrinos from an energy just below 1016 eV [1]
The detector profits from the fact that the water-ice interface at the bottom of the shelf-ice acts as a mirror for the radio emission and the antennas can be installed on top of the ice, which has the advantage that the antenna dimensions are not restricted by borehole geometry
The ARIANNA Collaboration is currently developing an eight-channel alternative, which will allow for the full combination of down-and upward facing antennas in one station
Summary
The ARIANNA detector is aimed at detecting neutrinos from an energy just below 1016 eV [1] Whenever these neutrinos produce an electromagnetic cascade after interacting in the ice of Moore’s Bay on the Ross Ice-shelf in Antarctica, the ensuing radio emission will be strong enough to be detectable. A trigger in a station is formed, if a combination of low-and-high threshold crossings is found in a window of 5 ns This allows for the HRA stations to run on very low threshold values of between three and four times the noise level and still maintain a very low trigger rate. The regular stations are affected less by the Galactic noise due to the directivity of the antennas
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