2015/04/30 by A. G. Vieregg, A.G. Vieregg, K. Bechtol +1 · 2 citations
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Cherenkov detector #Cherenkov radiation #Detector #Energy (signal processing) #Flux (metallurgy) #Neutrino #Neutrino detector #Phased array #Radio Astronomy Observations and Technology #Superconducting and THz Device Technology #astro-ph.IM #hep-ex
paper · pdf · doi:10.1088/1475-7516/2016/02/005
published as JCAP 2 (2016) 005 · 21 pages, 10 figures
arxiv created 2016/01/07 · openalex publication_date 2016/02/02 · arxiv updated 2016/05/12 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The detection of high energy neutrinos (10 15 –10 20 eV) is an important step toward understanding the most energetic cosmic accelerators and would enable tests of fundamental physics at energy scales that cannot easily be achieved on Earth. In this energy range, there are two expected populations of neutrinos: the astrophysical flux observed with IceCube at lower energies (∼1 PeV) and the predicted cosmogenic flux at higher energies (∼10 18 eV) . Radio detector arrays such as RICE, ANITA, ARA, and ARIANNA exploit the Askaryan effect and the radio transparency of glacial ice, which together enable enormous volumes of ice to be monitored with sparse instrumentation. We describe here the design for a phased radio array that would lower the energy threshold of radio techniques to the PeV scale, allowing measurement of the astrophysical flux observed with IceCube over an extended energy range. Meaningful energy overlap with optical Cherenkov telescopes could be used for energy calibration. The phased radio array design would also provide more efficient coverage of the large effective volume required to discover cosmogenic neutrinos.