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Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques). David Saltzberg (UCLA) David Waters (UCL) [Summary by Justin Vandenbrouke (UCB)] Panel Discussion Leader: Albrecht Karle (UW) TeV Astrophysics Workshop, II August 31, 2006. Gurgen Askaryan (1928-1997). Many Ideas:

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Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

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  1. WG7 summary, 1 of 11 Working Group Summary:New Techniques(Really, Just Askarayan’s Techniques) David Saltzberg (UCLA) David Waters (UCL) [Summary by Justin Vandenbrouke (UCB)] Panel Discussion Leader: Albrecht Karle (UW) TeV Astrophysics Workshop, II August 31, 2006

  2. WG7 summary, 2 of 11 Gurgen Askaryan(1928-1997) Many Ideas: Radio Detection of UHE  Acoustic Detection of UHE  Laser Ablation Bubble Chamber Yesterday’s topics

  3. WG7 summary, 3 of 11 UHE Neutrinos are Here(we just have to find them) • GZK with protons: • GZK with nuclei: (NOT a typo) ~1019 eV neutrinos +

  4. WG7 summary, 4 of 11 More Particle Physics:z=1 is a VERY long baseline One experimental parameter: (L/E)|lab-frame/ ~tproper-time determines (largely) the sensitivity to m2, decays, decoherence… available ? • Decays alter flavor ratios: Beacom,Bell,Hooper,Pakvasa,Weiler, PRL 90,181301 (2003) Recent review: Pakvasa, Phys. Atom. Nucl., 67, 1154 (2004)

  5. WG7 summary, 5 of 11 Predgrag Miocinovic:Frequency + Phase  Reconstruct time domain pulse • Reconstructed signal is a brief, unresolved, bipolar pulse of radiation • Details of analysis in PRD 74, 043002 (2006) • Even more data from June 2006 ice run

  6. WG7 summary, 6 of 11 Steve Barwick:ARIANNA“span the energy gap” ARIANNA rates (6 month) ESS Fe-only ~40 few

  7. WG7 summary, 7 of 11 Gary VarnerAURA How does radio-array sensitivity compare to ARIANNA?

  8. WG7 summary, 8 of 11 Westerbork Experiment 4 freq.bands 4 freq.bands Westerbork Synthesis Radio Telescope

  9. WG7 summary, 9 of 11 Neutrinos TDs GZK ν´s WRST Expected Sensitivity Cosmic Rays Scholten et al. (NuMoon Collab.) 2006, Astropart. Phys., in press

  10. WG7 summary, 10 of 11 Fabrice Feinstein & Gary VarnerAdvanced Front-End Electronics Design • Specfications: • High bandwidth (>1 GHz) • Low noise (thermal) • Fast (> GSa/s) • Low Power • High dynamic range: 12-16 bits • <1% cross talk • Deep digital buffers • Self-Triggering capability • But need them cheap Fabrice will put a full comparison in the proceedings

  11. WG7 summary, 11 of 11 Conclusions • GZK neutrinos are a beam for particle physics as • well as astronomers • In 1-5 years, we may have a handful of events, but • we need ~50-100 for science • Next generation plans await attenuation length • measurements, emission strengths, background • surveys---many this upcoming season • Meanwhile, work on detector technology, especially front-end hardware proceeds apace.

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