2. Sept. 2010CRIS, Catania Olaf Scholten KVI, Groningen Physics Radio pulse NuMoon@WSRT, results NuMoon@LOFAR, plans

3. Physics of Cosmic rays Spectrum is power law Flux ~ E -3 Non thermal spectrum! There must be sources! Where? What? End point? This talk: Measurement at highest E (NuMoon) F(E) [ m 2 sr s GeV ] -1 E [eV ] 10 -28 10 4 10 9 10 21 ← 32 orders of magnitude  ← 12 orders of magnitude  ← 1 [m -2 s -1 ] 1 [km -2 y -1 ] UHECR E -2.7 

4. Use the Moon!! Area = 2 10 7 km 2 ≈ 1 / km 2 / sr / century above 10 20 eV! Think Large

5. Sept. 2010CRIS, Catania Cosmic ray 100MHz Radio waves Detection: Westerbork antennas Principle of the measurement 10 7 km 2

6. Goldstone Lunar UHE Neutrino Search (GLUE) P. Gorham et al., PRL 93, 041101 (2004) Two antennas at JPL’s Goldstone, Calif. Tracking Station @ 2.2 GHz: l limits on >10 20 eV ’s l ~123 hours livetime Earlier experiment: 12 hrs using single Parkes 64m dish in Australia: T. Hankins et al., MNRAS 283, 1027 (1996) Detection off the Moon

7. Askaryan effect -1: Coherent Cherenkov emission ~10 cm ~2 m Cosmic ray shower Wave front Experiment at SLAC with beams of photons And 10 10 e-/bunch: effective shower energies 0.06-1.10 10 19 eV D. Saltzberg et al PRL 86 (2001) 2802 Basic emission mechanism

8. Askaryan effect -2: Coherent Cherenkov emission in air ~10 cm ~2 m Cosmic ray shower Wave front ----- 4000 m Recent evidence: Askaryan effect in CR airshowers K.D. de Vries, AstroParticle Physics & arXiv:1008.3308 H. Schoorlemmer for PAO, ARENA 2010 Polarization radio signal: Transverse current, Geomagnetic : Charge excess, Askaryan: Wave front

9. Askaryan effect -3: Coherent Cherenkov emission Leading cloud of electrons, v  c Typical size of order 10cm Coherent Čerenkov for ν  2-5 GHz cos θ c =1/n, θ c =56 o for ∞ shower length Length of shower, L  few m Important for angular spreading ~10 cm ~2 m Cosmic ray shower Wave front Important magnitudes:

10. Cosmic rays, Position on Moon Calculations for E cr =4 10 21 eV With decreasing ν increasing probability: ∫ over surface Moon D  ν -3 3 GHz 100 MHz O.S. et al, Astropart.Phys. 26 (2006) 219 3 GHz 100 MHz riminside

11. Sept. 2010CRIS, Catania Use Westerbork radio observatory NuMoon Experiment @ WSRT 2 bands over Moon 11 dishes of 25 m diameter, 110-175 MHz band

12. Trigger: 4σ pulse in all four frequency bands + dedispersion dispersed pulse pulse visible after dedispersion time  frequency 

13. Pulse Power Spectrum Effect successive steps in analysis Timer signal Wide pulses Anti coincidence

14. Simulations fraction pulses recovered with S>77 Dispersed pulses of different strength added to experimental background Pulse limit: 120 σ 2 =240kJy DE=87.5% 1 Jy = 10 -26 W/m 2 /Hz

15. Results No pulse of 240kJy seen in 46.7 h data  90% confidence limit on neutrino flux O.S. et al, PRL 103(2009)191301 Buitink, et al., http://arxiv.org/abs/1004.0274http://arxiv.org/abs/1004.0274

16. Detecting cosmic rays - 1 Sept. 2010CRIS, Catania The question: Will showers, just below the lunar surface, emit Askaryan radiation? Is there a ‘formation zone’ ? S. ter Veen et al, submitted for publication Full solution wave equation with transmission In medium Passing through to vacuum

17. Detecting cosmic rays - 2 Sept. 2010CRIS, Catania The answer: No ‘formation zone’ ! S. ter Veen et al, submitted for publication Present limit from WSRT observation 1 week bservation limits LOFAR-core Full E-LOFAR

18. Sept. 2010CRIS, Catania Total collecting area 0.5 km 2 Cover whole moon, Sensitivity 25 times better than WSRT. Band: 115-240 MHz NuMoon Experiment @ LOFAR New generation of radio-telescopes, many (3000) simple wire antennas

19. New generation telescopes: software beamforming Coherently add signal of antennas Delay determines viewing direction Multiple beams per station possible

20. Sept. 2010CRIS, Catania

21. Sept. 2010CRIS, Catania elofar

22. Neutrinos LOFAR, 30 days Theoretical predictions: Waxman-Bahcall limit GZK induced flux Phys.Rev.D64(04)93010 Topological defects AstroPhys. J. 479(97)547

23. Future: SKA LOFAR-core: 1 month SKA: 3 month observation, LFB: 100-300 MHz MFB: 300-500 MHz

24. Sept. 2010CRIS, Catania Conclusions NuMoon @ WSRT: New limit for E > 10 23 eV Future: NuMoon @ LOFAR NuMoon @ SKA Extend limit to lower E Improve Flux limit NuMoon collaboration: O.S., Stijn Buitink, Heino Falcke, Clancy James, Maaijke Mevius, Ben Stappers, Kalpana Singh, Richard Strom, Sander ter Veen

25. Sept. 2010CRIS, Catania Askaryan effect: confirmation in sand Experiment at SLAC with beams of photons And 10 10 e-/bunch: effective shower energies 0.06-1.10 10 19 eV 1 Jy = 10 -26 W/m 2 /Hz Angular spread Z 0 ~ λ /L D. Saltzberg et al PRL 86 (2001) 2802 Evidence in CR induced airshowers K.D. de Vries, AstroParticle Physics arXiv:1008.3308arXiv:1008.3308 H. Schoorlemmer, (PAO) ARENA 2010 1 Jy = 10 -26 W/m 2 /Hz

26. Tau-neutrinos @ Pierre Auger Pierre Auger, PRD79(2009)102001 NuMoon@WSRT, PRL103(2009)191301