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Using the Westerbork radio observatory to detect UHE cosmic particles interacting on the Moon

This paper discusses the use of the Westerbork Radio Observatory to detect ultra-high energy cosmic particles interacting on the Moon. The Askaryan effect, coherent Cherenkov emission, and transmission through Moon material are explored. The proposed experiment would utilize the observatory's 117-175 MHz band, 25-meter diameter dishes, and 5-degree field of view.

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Using the Westerbork radio observatory to detect UHE cosmic particles interacting on the Moon

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  1. Using the Westerbork radio observatory to detect UHE cosmic particles interacting on the Moon J. Bacelar (KVI) O. Scholten (KVI) G. de Bruyn (ASTRON) H. Falcke (ASTRON) Int. ARENA workshop, 17-19 May, Zeuthen

  2. UHE Cosmic-rays Int. ARENA workshop, 17-19 May, Zeuthen

  3. Experiments performed Satellite: FORTE Phys.Rev.D69(04)13008 Balloon: ANITA Astro-phys./411007(2004) Ground: RICE AstroP.Phys. 20(03)195 Moon: GLUE Phys.Rev.Lett. 93(04)41101 Int. ARENA workshop, 17-19 May, Zeuthen

  4. Askaryan effect: Coherent Cherenkov emission Experiment at SLAC with beams of 28.5 GeV electrons And 1010 e-/bunch: effective shower energies 0.06-1.10 1019 eV D. Saltzberg et al PRL 86 (2001) 2802 1 Jy = 10-20 W/m2/MHz Int. ARENA workshop, 17-19 May, Zeuthen

  5. Askaryan effect: Coherent Cherenkov emission Experiment at SLAC with beams of 28.5 GeV electrons And 1010 e-/bunch: effective shower energies 0.06-1.10 1019 eV D. Saltzberg et al PRL 86 (2001) 2802 1 Jy = 10-20 W/m2/MHz Int. ARENA workshop, 17-19 May, Zeuthen

  6. Vacuum Moon n=1.5-1.8 θc ≈ 560 Cosmic particle interaction • Particle hits Moon (radius=1700 km; area = 6π 106 km2): • Interacts: protons within meters, V • Askaryan effect -> Coherent Cherenkov emission • Shower development -> including LPM effect • Transmission through Moon material λr= 15[m] /  [GHz] = 7m (at 2.2 GHz) • Transmissivity across Moon surface – vacuum boundary 60 km @ 1021 eV 6 km @ 1024 eV Vacuum Moon n=1.5-1.8 Spread emitted power density in a gaussian of width Δθc≈λ/ℓ Hadronic component: Δθc= 2.5 (3/) = 3.50 (at 2.2 GHz) EM component Δθc= 2.5 (3/)(4.1014 / E)1/3 = 0.0250 θc ≈ 560 θc Int. ARENA workshop, 17-19 May, Zeuthen

  7. Vacuum Moon n=1.5-1.8 θc ≈ 560 Cosmic particle interaction • Particle hits Moon (radius=1700 km; area = 6π 106 km2): • Interacts: protons within meters, V • Askaryan effect -> Coherent Cherenkov emission • Shower development -> including LPM effect • Transmission through Moon material λr= 15[m] /  [GHz] = 150 m (at 0.1 GHz) • Transmissivity across Moon surface – vacuum boundary 60 km @ 1021 eV 6 km @ 1024 eV Spread emitted power density in a gaussian of width Δθc≈λ/ℓ Hadronic component: Δθc= 2.5 (3/) = 750 (at 0.1 GHz) EM component Δθc= 2.5 (3/)(4.1014 / E)1/3 = 0.50 θc Int. ARENA workshop, 17-19 May, Zeuthen

  8. Results of calculations for cosmic rays: Int. ARENA workshop, 17-19 May, Zeuthen

  9. Results of calculations for neutrinos: Int. ARENA workshop, 17-19 May, Zeuthen

  10. Proposed Experiment Use Westerbork radio observatory • Advantages: • 117-175 MHz band • 25 m diameter dishes • 5 degree field of view • 12-14 coincident receivers • 100 hour observation time • 40 M samples/sec (PuMa2) • Polarization information Int. ARENA workshop, 17-19 May, Zeuthen

  11. Proposed Experiment Use Westerbork radio observatory Int. ARENA workshop, 17-19 May, Zeuthen

  12. Int. ARENA workshop, 17-19 May, Zeuthen

  13. Calc. limits GLUE Published limits Rice,GLUE,FORTE Int. ARENA workshop, 17-19 May, Zeuthen

  14. Calc. limits GLUE Published limits Rice,GLUE,FORTE Theoretical predictions Active galactic nuclei Astro.Phys.3(96)295 GZK induced flux Phys.Rev.D64(04)93010 Topological defects AstroPhys. J. 479(97)547 Int. ARENA workshop, 17-19 May, Zeuthen

  15. Calc. limits GLUE Published limits Rice,GLUE,FORTE Predicted limits 45 days ANITA Theoretical predictions Active galactic nuclei Astro.Phys.3(96)295 GZK induced flux Phys.Rev.D64(04)93010 Topological defects AstroPhys. J. 479(97)547 Calc. limits 100 hours Westerbork Int. ARENA workshop, 17-19 May, Zeuthen

  16. Conclusions • Westerbork observatory: • 14 radio antennas • 117-175 MHz band • PuMa 2 data acquisition mode • Low background noise • Large field of view • Polarization information • Within 100 hours observation competitive sensitivity to both cosmic rays and neutrino fluxes • Energy threshold 1021 eV • Polarization determines plane of incidence of original particle Future:Experiment with LOFAR Int. ARENA workshop, 17-19 May, Zeuthen

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