2010/02/26 by S. Buitink, O. Scholten, O. Schölten +10 · 43 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Cherenkov radiation #Cosmic ray #Detector #Flux (metallurgy) #Gamma-ray bursts and supernovae #LOFAR #Narrowband #Neutrino #Optics #Physics #Radio Astronomy Observations and Technology #Radio frequency #Radio telescope #Telecommunications #Telescope #astro-ph.HE #hep-ex
paper · pdf · doi:10.1051/0004-6361/201014104
published in Astronomy and Astrophysics 521, A47 (EDP Sciences) · 13 pages, 17 figures, accepted for publication in Astronomy & Astrophysics
openalex publication_date 2010/02/26 · arxiv created 2010/04/02 · arxiv updated 2015/05/18 · openalex created_date 2020/11/23 · openalex updated_date 2026/08/05
<i>Context. <i/>Ultra-high energy (UHE) neutrinos and cosmic rays initiate particle cascades underneath the Moon's surface. These cascades have a negative charge excess and radiate Cherenkov radio emission in a process known as the Askaryan effect. The optimal frequency window for observation of these pulses with radio telescopes on the Earth is around 150 MHz. <i>Aims. <i/>By observing the Moon with the Westerbork Synthesis Radio Telescope array we are able to set a new limit on the UHE neutrino flux. <i>Methods. <i/>The PuMa II backend is used to monitor the Moon in 4 frequency bands between 113 and 175 MHz with a sampling frequency of 40 MHz. The narrowband radio interference is digitally filtered out and the dispersive effect of the Earth's ionosphere is compensated for. A trigger system is implemented to search for short pulses. By inserting simulated pulses in the raw data, the detection efficiency for pulses of various strength is calculated. <i>Results. <i/>With 47.6 hours of observation time, we are able to set a limit on the UHE neutrino flux. This new limit is an order of magnitude lower than existing limits. In the near future, the digital radio array LOFAR will be used to achieve an even lower limit.