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Development of Telescopes for Extremely Energetic Neutrinos

Development of Telescopes for Extremely Energetic Neutrinos. ~1 km. Steven W. Barwick, UC-Irvine. Neutrino Telescopes: Agenda. 10 years of progress with optical Cherenkov Detectors Extremely Energetic Neutrinos - New Technologies Radio Cherenkov: ARIANNA. Teraton -Petaton.

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Development of Telescopes for Extremely Energetic Neutrinos

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  1. Development of Telescopes for Extremely Energetic Neutrinos ~1 km Steven W. Barwick, UC-Irvine

  2. Neutrino Telescopes: Agenda • 10 years of progress with optical Cherenkov Detectors • Extremely Energetic Neutrinos - New Technologies • Radio Cherenkov: ARIANNA Teraton -Petaton

  3. PHOTONS: not deflected, but: reprocessed in sources, absorbed in IR (100 TeV), and CBR PROTONS: deflection in magnetic fields, GZK cutoff NEUTRINOS: not absorbed or deflected, hard to see

  4. 1997: Unlimited Opportunity A. Silvestri, PhD Dissertation, 2008 E2 dN/dE (GeVcm-2s-1sr-1) WB Log10(E[GeV])

  5. 13 Years of Diffuse  Progress 2010 ~100x improvement A. Silvestri, PhD Dissertation, 2008 E2 dN/dE (GeVcm-2s-1sr-1) Auger x3 ANITA AMANDA-UHE WB Log10(E[GeV])

  6. Excluding AGN Model Predictions for Diffuse Flux Excluded Normalization to x-ray or 1-1000 MeV ’s overproduces neutrino flux

  7. GZK neutrinios[ one of the the most secure predictions in the field ] New Technologies

  8. Cosmogenic (or GZK) Neutrinos Predictions are secure: p + cmb  ->  -> n + + n -> lower energy protons  ->  • However, -Flux Calculations depend on: • Elemental composition (p, Fe, mixed) • Cosmology (=0.7) • Injection Spectra, E- and Emax • Evolution of sources with redshift, (1+z)m • Star formation, QSO, GRB, little or no

  9. GZK Model-Specific limits Log10(E[GeV]) all) E dN/dE (cm-2s-1sr-1) ANITA-08 109 GeV

  10. Why Big Detectors? • GZK  Flux,  (E~1018 eV): 100 /km2/yr •  Interaction Length, : 500 km • Event Rate/km3/yr = [/] ~ 0.2 • Efficiency, livetime, nice if more than one So GZK  detection requires > 10 km3 (aperture > 60 km3sr) Note: ARIANNA has ~ 2400 km3sr

  11. ARIANNA Sensitivity Greatly increases sensitivity to GZK  in E=1018-1019 eV ARIANNA + ESS Flux: 40 events/yr ARIANNA Energy Res: dE/E~1, Angular Res: ~1 deg

  12. EHE Neutrinos Explore Higher Dimensions ~100sm For GZK E ARIANNA-GZK CC: sm (Anchordoqui, et al, hep-ph/0307228)

  13. Neutrino Cross-Section A. Connolly, 2006 ARIANNA - 10 years [] = 0.24 If Nev = 400 If  =0.5o If =2GQRS GQRS 2 parameter fit: Normalization cross-section

  14. New Techniques to Observe Cosmogenic Neutrinos

  15. Askaryan Radio Emission from SLAC beam in Ice Gorham, Barwick, et al., astro-ph/0611008 Absolute RF power and frequency dependence confirmed Width of cherenkov cone and frequency dependence confirmed

  16. ARIANNA 31 x 31 array [30 km x 30 km] 1 km 600 m UCI, LBL, OSU, WashU, KU,UC-London, S.Korea Barwick, astro-ph/0610631

  17. Satellite Image of Victoria Land and Ross Ice Shelf Ross Island Dry Valleys wireless internet (2009) ~120 km Minna Bluff ARIANNA 30x30 km2 Ice Thickness ~600m south

  18. ARIANNA Advantages • Straightforward logistics • not far (~120 km) from main US science station • surface deployment (no drilling) • Excellent site properties • Protected from man-made noise • Remarkable attenuation length and reflectivity from bottom • Lightweight, robust technologies (so low $$) • Internet access 24/7 • Array is reconfigurable to follow science

  19. ARIANNA Characteristics log(E) eV Zenith Angle Nearly uniform response over the entire sky Peak response at “sweet spot” of GZK spectrum

  20. Optimal Antenna Gain = 7 higher gain restricts viewing of reflected events but accesses lower energy cascades LPDA

  21. Impact of firn ice on LPDA Antenna(not much, except at f<100MHz) L. Gerhardt, et al, NIMA, 2010

  22. Time(ns) Time(ns) 10 10 -10 -10 Time-domain is rich in information on-cone off-cone J. Alvarez-Muniz, A. Romero-Wolf, and E. Zas, arXiv:1002.3873v1

  23. Modification by antenna+amp Interesting structure, well suited to pattern trigger Similar pulse structure for on-cone and off-cone Time(ns)

  24. Camping at Moore’s Bay Site David Saltzberg

  25. Preliminary Value assumed prior to this work ARIANNA Site Studies T. Barrella, et al, J. Glaciology, 2010, submitted Arbitrary amplitude scaling Amazing fidelity of reflected pulse from sea-water bottom -behaves as nearly flawless mirror 1-way attenuation length, averaged over depth and temperature And Radio Quiet!

  26. L. Gerhardt, et al, NIMA, 2010 ARIANNA Prototype Station(deployed Dec. 2009) Wireless Power Tower “lab”

  27. Housekeeping Data Outside Temp windy Wind speed Power Supply Voltage Jan 1, 2010 Feb 4, 2010

  28. Trigger rates ~ 10-2 s-1 Randomly distributed in time Trigger: 2 of 3 majority, 5*Vrms

  29. Prelim. Event Analysis(Jan 5 -Feb 4, 2010) No events in signal region

  30. ARIANNA Visualization

  31. Outlook • To probe the GZK neutrinofluxes and particle physics at highest energies, new techniques are being developed based on radio cherenkov , air shower and acoustic detection. • ARIANNA has the right combination of size and simplicity of deployment to keep costs down • Ice studies in Nov’ 06 astonishingly good • Recent protostation studies show low Anthropogenic noise over 1 month periods • 7-station engineering array approved by NSF in April 2010

  32. Air Shower vs Ice Shower(time profiles quite different!) 100MHz-1 GHz

  33. Electronic Module Schematics L. Gerhardt, et al, NIMA, 2010

  34. Solar Panel Power Electronic Module

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