working group summary: new techniques (really, just askarayan’s techniques)
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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: - PowerPoint PPT PresentationTRANSCRIPT
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
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Gurgen Askaryan (1928-1997)
Many Ideas:
Radio Detection of UHE Acoustic Detection of UHE
Laser Ablation
Bubble Chamber
Yesterday’s topics
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UHE Neutrinos are Here (we just have to find them)
● GZK with protons:
● GZK with nuclei:
neutrinos
+
(NOT a typo)~1019 eV
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More Particle Physics:z=1 is a VERY long baseline
One experimental parameter: (L/E)|lab-frame / ~tproper-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)
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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
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Steve Barwick:ARIANNA
“span the energy gap”
ARIANNA rates(6 month)
ESS Fe-only~40 few
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Gary VarnerAURA
How does radio-array sensitivity compare to ARIANNA?
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Westerbork Synthesis Radio Telescope
Westerbork Experiment
4 freq.bands
4 freq.bands
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WRST Expected Sensitivity
Scholten et al. (NuMoon Collab.) 2006, Astropart. Phys., in press
Neutrinos
GZK ν´s
TDs
Cosmic Rays
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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
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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.