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Lunar Radio Cerenkov Observations of UHE Neutrinos

Lunar Radio Cerenkov Observations of UHE Neutrinos. Ron Ekers, Clancy James, Justin Bray, Ray Protheroe, John Reynolds, Paul Roberts, Chris Phillips Curtin 15 April 2009. Lunar Cherenkov emission. neutrino. photon. shower. We know what this pulse is like. This is part of SKA development

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Lunar Radio Cerenkov Observations of UHE Neutrinos

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  1. Lunar Radio Cerenkov Observations of UHE Neutrinos Ron Ekers, Clancy James, Justin Bray, Ray Protheroe, John Reynolds, Paul Roberts, Chris Phillips Curtin 15 April 2009

  2. Lunar Cherenkov emission neutrino photon shower

  3. We know what this pulse is like • This is part of SKA development • Not to design out • Broadband • Freq 0.5 to 2 GHz • Max bandwidth possible • Δt  1/ Δν • Incoherent will not work • Never possible if Δt ~ 1/ ν • From all limb of moon • Ionospheric dispersion • Linear polarization

  4. Detecting the pulse • Minimum neutrino energy • Determined by pulse detection threshold, hence radio telescope sensitivity • GHz frequencies better • Moves curve to left • Neutrino flux limit determined by • Volume of neutrino detector • Acceptance solid angle • Lower frequency better • Observing time • Moves curve down

  5. 30’ 64m dish 20m dish array Seeing all the moon • Event rates highest at the limb • Noise contribution from all moon • We want to observe the entire lunar limb

  6. SKA configuration Trigger off core Inner core Keep long baselines in a buffer Station Combine high and low frequency triggers

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