working group summary: new techniques (really, just askarayan’s techniques)

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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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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 Presentation

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Page 1: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

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

Page 2: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

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

Page 3: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

WG7 summary, 3 of 11

UHE Neutrinos are Here (we just have to find them)

● GZK with protons:

● GZK with nuclei:

neutrinos

+

(NOT a typo)~1019 eV

Page 4: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

WG7 summary, 4 of 11

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)

Page 5: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

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

Page 6: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

WG7 summary, 6 of 11

Steve Barwick:ARIANNA

“span the energy gap”

ARIANNA rates(6 month)

ESS Fe-only~40 few

Page 7: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

WG7 summary, 7 of 11

Gary VarnerAURA

How does radio-array sensitivity compare to ARIANNA?

Page 8: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

WG7 summary, 8 of 11

Westerbork Synthesis Radio Telescope

Westerbork Experiment

4 freq.bands

4 freq.bands

Page 9: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

WG7 summary, 9 of 11

WRST Expected Sensitivity

Scholten et al. (NuMoon Collab.) 2006, Astropart. Phys., in press

Neutrinos

GZK ν´s

TDs

Cosmic Rays

Page 10: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

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

Page 11: Working Group Summary: New Techniques (Really, Just Askarayan’s Techniques)

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.