The field of radio detection of high-energy cosmic particles has been growing rapidly over the past decade. Radio Neutrino Observatory (RNO-G) capitalizes on the success and combined expertise of the ARA, ARIANNA, ANITA and RICE experiments, for a design that will deliver world-leading measurements of the high-energy neutrino flux, with the pointing and energy resolution required for multi-messenger astronomy, aligned with the Astro2020 Science whitepapers.
Within RNO-G, we will also develop critical hardware for the radio component of IceCube-Gen2.
We foresee 35 stations to be deployed at Summit Station in Greenland. Each station will have a surface component and a deep component (100 m below the surface of the ice) that together enable the detection and detailed reconstruction of neutrino events.
The Radio Neutrino Observatory Greenland (RNO-G)
With the discovery of a diffuse flux of astrophysical neutrinos and the identification of a multi-messenger source candidate, the success of IceCube has established neutrinos as a powerful messenger in the exploration of the high-energy universe. RNO-G will extend multi-messenger neutrino astronomy to energies above 10 PeV. RNO-G is designed around a broad multi-messenger astrophysics program to be an instrument that measures of order ten neutrinos at the highest energies, possibly including the first discovery. The RNO-G collaboration will develop the techniques required to rapidly produce and respond to alerts of astrophysical transients.
A Pathfinder for IceCube-Gen2 Radio
RNO-G Science: the Highest Energy Neutrinos
Neutrinos are unique messengers. They point back to their sources and can reach us from the most distant corners of the universe because they travel undeflected by magnetic fields and unimpeded by interactions with matter or radiation. Unlike γ-rays, which can be explained by inverse Compton scattering, the observation of high-energy neutrinos from these objects provides incontrovertible evidence for cosmic-ray acceleration, since both neutrinos and γ-rays are produced when cosmic rays interact with ambient photons or matter within their source. Resolving the sources of cosmic rays and the acceleration mechanisms will require a comprehensive multi-messenger program involving observations of cosmic rays, γ-rays, and neutrinos across many decades of energy.