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Olaf Scholten KVI, Groningen

Ultra-High Energy Cosmic ray and Neutrino Physics using the Moon. Olaf Scholten KVI, Groningen. Large Area ??. Area = 2 10 7 km 2. Use the Moon!!. Principle of the measurement. Cosmic ray. Detection: Westerbork antennas. 10 7 km 2. 100MHz Radio waves. Detection off the Moon.

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Olaf Scholten KVI, Groningen

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  1. Ultra-High Energy Cosmic ray and Neutrino Physics using the Moon Olaf Scholten KVI, Groningen ARENA 2008

  2. Large Area ?? Area = 2 107 km2 Use the Moon!! ARENA 2008

  3. Principle of the measurement Cosmic ray Detection: Westerbork antennas 107 km2 100MHz Radio waves ARENA 2008

  4. Detection off the Moon Goldstone Lunar UHE Neutrino Search (GLUE) P. Gorham et al., PRL 93, 041101 (2004) First experiment: 12 hrs using single Parkes 64m dish in Australia: T. Hankins et al., MNRAS 283, 1027 (1996) Two antennas at JPL’s Goldstone, Calif. Tracking Station @ 2.2 GHz, 123 hours ARENA 2008

  5. ~2 m Cosmic ray ~10 cm shower Wave front Askaryan effect: Coherent Cherenkov emission • Leading cloud of electrons, v  c Typical size of order 10cm Coherent Čerenkov for ν 2-5 GHz cos θc =1/n , θc=56o for ∞ shower length • Length of shower, L  few m Important for angular spreading ARENA 2008

  6. Angular spread Z0~Δc~λ/L=1/Lν D. Saltzberg et al PRL 86 (2001) 2802 Askaryan effect: confirmation in sand Experiment at SLAC with beams of photons And 1010 e-/bunch: effective shower energies 0.06-1.10 1019 eV 1 Jy = 10-26 W/m2/Hz ARENA 2008

  7. Based on physics principles Old parametrization Spreading around Cherenkov-cone n=1.8 GHz Sine profile L=1.7 m , E=1020 O.S. etal., Astropart.Phys. 2006 ARENA 2008

  8. Reflection Spreading is diminishing internal reflection 3 GHz 100 MHz ARENA 2008

  9. Cosmic rays, Position on Moon Calculations for Ecr=4 1021 eV 100 MHz 3 GHz Partial Detection probability With decreasing ν : - increasing area - increasing probability ∫over surface Moon D ν-3 Normalized distance from center ARENA 2008

  10. Detection Limits, Cosmic rays Minimum Flux for detecting 1 count/100h Detection threshold = 500Jy Decreasing ν: • Increasing threshold like ν-1 • Increase sensitivity like ν-3 ARENA 2008

  11. NuMoon Experiment @ WSRT Use Westerbork radio observatory • Advantages: • 117-175 MHz band • 25 m diameter dishes • 5 degree field of view • 12-14 coincident receivers • 500 hour observation time • 40 M samples/sec (PuMa2) • Polarization information ARENA 2008

  12. NuMoon Experiment @ WSRT Use Westerbork radio observatory 4 frequencies ARENA 2008

  13. Processing Pipeline • 18 TB raw data per 6 hr slot • Excision of narrow-band interference • De-Dispersion of ionosphere with GPS TEC values • Indentification of peaks in time spectrum • Data reduction 100:1 to 180 GB ARENA 2008

  14. + dedispersion ARENA 2008 Trigger: 4σ pulse in all four frequency bands

  15. ARENA 2008

  16. Trigger Power Spectrum Effect successive steps in analysis Gaussian noise ARENA 2008

  17. Prelimenary Results Analysis of 10 h 40 min data Additional observation time: 7 June +10h ARENA 2008

  18. NuMoon Experiment @ LOFAR • Total collecting area 0.5 km2 • Cover whole moon, • Sensitivity 25 times better than WSRT. • Bands: • 30-80 MHz (600 Jy) • 115-240 MHz (20 Jy) ARENA 2008

  19. Neutrinos WSRT, 100 hours 0 counts LOFAR, 30 days ~60 counts Theoretical predictions: Waxman-Bahcall limit GZK induced flux Phys.Rev.D64(04)93010 ARENA 2008

  20. Future: SKA,LORD 1 year observation, LFB: 100-300 MHz MFB: 300-500 MHz From: O.S., SKA Design Study report ARENA 2008

  21. SKA-Hadrons ARENA 2008

  22. z=5 z=20 z=50 Resonant neutrino absorption 30 day Neutrinos are absorbed on relic neutrino background by forming Z-boson A. Ringwald, L. Schrempp, JCAP 0610 (2006) 012 Measured pulse-height spectrum can distinguish sources at various distances OS& A. van Vliet,JCAP06(2008)015 ARENA 2008

  23. Conclusions NuMoon @ WSRT Future: NuMoon @ LOFAR NuMoon @ SKA Competitive Sensitivity for cosmic rays and neutrinos NuMoon NuMoon collaboration: O.S., Stijn Buitink, Heino Falcke, Ben Stappers, Kalpana Singh, Richard Strom ARENA 2008

  24. LORD efficiency for neutrinos ARENA 2008

  25. The observed Universe ARENA 2008

  26. Some distance scales • Nearest star, Proxima Centauri – 4 LY • Diameter of our galaxy – 100,000 LY • Distance to nearest galaxy – the Sagittarius dwarf galaxy, which • is being “eaten” by the Milky Way – 80,000 LY • Size of our “Local Group” – a collection of at least 30 galaxies, • including Andromeda – 3 Million LY • Size of our “Local Supercluster” which contains our Local Group, • the Virgo Cluster, and others – 100 Million LY • 1pc = 3.26 LY ARENA 2008

  27. Case: Shower @ 2.50 with surface Calculations for Ecr=4 1021 eV Influence of frequency Simulations for Moon Minimal signal = 3000Jy 0.1 GHz 85% of area 2.2 GHz 0.8% of area ARENA 2008 Intensity v.s. cos θ, φ

  28. Shock wave acceleration Colliding galaxies “Fermi shock acceleration” proton passes several times through shock front due to magnetic field. Spectrum  E -2 Active galactic nucleus Need large scale magnetic fields ARENA 2008

  29. Short-range particle astronomy • Larmor radius for a charged particle (charge Z) and energy E (1020 eV) in a magnetic field with strength B(nG): ρ(Mpc)=108·(E/1020eV)·(1/BnG)·(1/Z). • Galaxy about 1000 nG; proton escapes; iron wanders around From: M. Teshima 2006 ARENA 2008

  30. ARENA 2008

  31. Greisen – Zatsepin - K’uzmin (GZK) Transport Energetic protons loose energy through Interactions with the cosmic microwave background ARENA 2008

  32. Possible Sources within 1.5 MpcLocal Group ARENA 2008

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