1. D. Seckel, Univ. of Delaware

2. Overview Expectations for extraterrestrial neutrinos Detector options
Ultra-High-Energy (UHE): 1018 eV
Detector options
Scale ( km3)
Technology: Radio, Acoustic (~10 units per km3)
Strawman timeline
Smooth transition at SP from optical to radio

3. Cosmic Rays ?? ?
Galactic
SN shock
Extra Galactic

4. + Gamma ray observations (TeV)

5. => Pion production => Neutrino production
Neutrinos
High energy hadrons
+ g-rays
=> Pion production => Neutrino production
E+D < 18-P 15 18
IceCube P=3
IceTop P=0

6. Typical summary of UHE models
1.9 15 18
IceCube P=3
RICE III P=3

7. Detector Scale
~ 1000 km3 sr
> 100 km2
Ethr < 1 EeV (109 GeV)
Bigger and Sparser than IceCube

8. RF Detection (RICE version)
600 m
~ 10 PeV event
~ 10 EeV event
5 km

9. Spectrum & Frequency Response
Minimum Bandwidth > 1 GHz

10. Attenuation & horizontal spacing
leff includes temperature profile to bottom. Data from Barwick et. al.
Maximum Spacing < 2 km

11. Cerenkov cone & vertical spacing
10 deg * 2 km = 200m
3 deg width for hadronic or EHE e-showers
LPM effect for UHE e-showers
Maximum separation < 300 m

12. Ray tracing & Depth
Minimum Depth > 200 m

13. Timing & vertex reconstruction
Don’t have illustration, but 10 ns relative timing across array is probably adequate. 100 ns is probably not.

14. Waveforms & event reconstruction
This is actually a simulation of the
radio signal from an air shower core
impacting the ice above RICE
Arrival time distribution
Antenna
RF Pulse at antenna
sample time <1 ns
“snips” > 100 ns

15. 10 year goals Completed Detector 100 events/yr from GZK 1000 km3 sr
Ethr < 1 EeV (109 GeV)
100 events/yr from GZK
Full sky spectrum above 1 EeV
Event/Flavor ID
Measure snN
Point source, GRB detection …

16. Transition IceCube construction from optical to radio (& acoustic?)
5 year goals
Transition IceCube construction from optical to radio (& acoustic?)
Funded Proposal (100M ?)
Array design
Drill
m deep
10 km from SP (300 holes ?)
Instrumentation
Antennas
Optical Fiber
High speed/low power (GHz, 1W) digitizers
Multilevel triggering
Power/DAQ: central vs. distributed

17. RICE-II deployed on IceCube footprint
3 year goals
RICE-II deployed on IceCube footprint
Antenna clusters on 4-6 strings
Cooperative relationship with IceCube
Engineering studies for RICE-III
Drilling
Power
Proposal submitted for RICE-III

18. Engineering studies for prototype array
2 year goals
Season Goals
Demonstration of key technologies
Working antenna cluster
RF/OF/RF analog link
GHz/ xW Digitizer
Closer integration of operations with IceCube
Improved ice properties in situ (1 km baseline)
Engineering studies for prototype array

19. 1 Year goals Season Goals Annual Goals Pressure Vessel survives
Fiber freeze-in
RF/OF/RF channel demonstration
Annual Goals
Design studies for prototype array
DAQ hardware finalized
Increased participation by IceCube institutions (KU, UD, UW, PSU, UMd, Christchurch)

20. Summary Wide range of models for UHE neutrino production
GZK neutrinos are robust prediction – provide “guaranteed” baseline flux
1000 km3 sr, EeV threshold
Radio technique feasible
Development timeline commensurate with IceCube construction

21. Blank

22. Other Physics/Astrophysics/Cosmology
Top down scenarios
Strings/monopoles…
Dark Matter, WIMPs, SUSY particles
Neutrino physics
oscillations, decay…
Cross-sections (exotic)
Hadronic physics
Cross-sections (standard)
Non-neutrino physics w/neutrino detector
Cosmic ray physics (upper end of galactic spectrum
Charm production

23. UHE Production: Acceleration
AGASA, HiRes
1. Acceleration predictions depend on scenario – could be “no n’s”.
2. “GZK” neutrinos are guaranteed – a guide for experiment design.
3. Still some model dependence.
4. Constraints from EGRET & UHECR
5. En ~ .05 Ep

24. Estimated Rate at PeV (crude)

25. GZK cosmic cascade codes
propagation & dE/dx
adiabatic (cosmic expansion)
photonuclear: g+p ® B+X (ESS use SOPHIA)
pair production: g+p ® pe+e-
source characteristics
injection spectrum dN/dE ~ E-(1+g)
source cutoff Ec
luminosity (ESS – normalize to UHECR, KKSS limit from EGRET)
homogenous
cosmology
integrate over red-shift
source evolution: (1+z)m, zmax
H0, L…

26. dE/dx (g+p ® B+X (SOPHIA))
More to life than the D-resonance
En / Ep
En / Eem

27. ESS result for a “reasonable” model
zmax = 1.9, flat to 2.7, rolloff for z > 2.7.
Log Ec = 21.5
Norm. (19 < Log Ecr < 21)
L = 0.0, 0.7
Flux “grazes” WB
nm ~ 2ne
n-decay for anti-ne

28. Reasonable landmark – but…
What are limits?
Simple scaling with m, g for matter dominated
q = 1 + z
Change magnitude of yield
with epoch
Shift energy of yield
with epoch

29. Simple scaling of GZK Spectrum: (Ep)-(1+g) Evolution (1+z)m
Matter dominated cosmology (1+z)-5/2
Spacing D(ln q) = 1 dB
Consider effects of zmax, L
Shape of Y changes with g

30. Discussion: Degeneracy of UHECR models
Flat spectrum, evolution, galactic contribution
Steep spectrum, no evolution, no galaxy
DeMarco: Steep
w/evolution is OK

31. Neutrinos break degeneracy
a) Flat spectrum, evolution, galactic contribution
b) Steep spectrum, no evolution, no galaxy
c) Cutoffs, Lambda…

32. Range of GZK possibilities

33. Long term view of UHE neutrino experiments
100 GZK events/yr requires ~ 1000 km3 (1 Eg) (~ 2.5 p 102)
LPM
ANITA
Auger: tau
e, mu
IceCube/NEMO
LPM
AMANDA/ANTARES
RICE: LPM no LPM