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 WB A. Silvestri, PhD Dissertation, 2008 Log 10 (E [GeV]) E 2 dN/dE (GeVcm -2 s -1 sr -1 )

5. 13 Years of Diffuse Progress WB ~100x improvement A. Silvestri, PhD Dissertation, 2008 Log 10 (E [GeV]) E 2 dN/dE (GeVcm -2 s -1 sr -1 ) 2010 AMANDA-UHE ANITA Auger x3

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: 1.Elemental composition (p, Fe, mixed) 2.Cosmology (  =0.7) 3.Injection Spectra, E -  and E max 4.Evolution of sources with redshift, (1+z) m  Star formation, QSO, GRB, little or no

9. GZK Model-Specific limits  all ) Log 10 (E [GeV]) E dN/dE (cm -2 s -1 sr -1 ) ANITA-08 10 9 GeV

10. Why Big Detectors? GZK Flux,  (E~10 18 eV): 100 /km 2 /yr  Interaction Length, : 500 km Event Rate/km 3 /yr = [  ] ~ 0.2 Efficiency, livetime, nice if more than one So GZK detection requires > 10 km 3 (aperture > 60 km 3 sr) Note: ARIANNA has ~ 2400 km 3 sr

11. ARIANNA Sensitivity Greatly increases sensitivity to GZK in E=10 18 -10 19 eV ARIANNA + ESS Flux: 40 events/yr Energy Res: dE/E~1, Angular Res:   ~1 deg

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

13. Neutrino Cross-Section   ] = 0.24 If N ev = 400 If  =0.5 o If  =   2 parameter fit: Normalization cross-section ARIANNA - 10 years GQR S A. Connolly, 2006

14. New Techniques to Observe Cosmogenic Neutrinos CurrentUnder Development Radio RICE, ANITAARIANNA, ARA, IceRay, SALSA, etc Air Shower HiRes, AugerTA, Auger N, OWL Acoustic SPATS, AMADEUS

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

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

17. Satellite Image of Victoria Land and Ross Ice Shelf Ross Island Dry Valleys ARIANNA south Minna Bluff ~120 km 30x30 km 2 Ice Thickness ~600m wireless internet (2009)

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

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

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

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

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

25. Camping at Moore’s Bay Site David Saltzberg

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

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

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

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

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

31. ARIANNA Visualization

32. Outlook To probe the GZK neutrino fluxes 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

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

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

36. Solar Panel Power Electronic Module