1. Basic parameters (June, 2006):
RICE Status
Basic parameters (June, 2006):
17 dipole antennas, depths: m, 200m x 200m
3 dipoles on optical fiber (test channels)
5 transmitters for timing/amplitude calibration
Triggers:
4-fold in 1.25 microsecond
SPASE .or. AMANDA coincidence w/ 1 Rx (1.25 us)
also, fast rejection of noise
South Pole, co-located with AMANDA/IceCube expts.
Diffuse neutrino flux limits
GRB point source limits
Monopole comments

2. RICE receiver antennas (half-wave dipole; L~25 cm)

3. Things not to do in the future
Deploy in the firn
Variable index-of-refraction to depth of 160 m or so
(n.b: only 90 m at vostok)

4. ray Tracing thru varying n(z)
Radial distance (km)
DEPTH Rx
Source point

5. Data – surface reflections (03 data) – sample along trajectory of reflected waveform

6. Initiated radioglaciology studies 02-03 for Real(e); 03-04 for Im(e)

7. Transmitter Reconstruction (timing)
True (known) Tx Depth
Points=reconstructed depths from data

8. Single Channel Absolute Gain Calibration
TX….RX
antenna + amplifier calibrations
cable (TX, RX) and filter
relative geometry of TX/RX
MHz: +/- 3 dB (E)

9. Tx → Rx simulation vs. data
simulated
data

10. Bottom echo visible thru 5.6 km! (20 dB noise reduction [averaging])
Radio Echo using horn antennas directed downwards on surfaceAntarctic ice transparent to radiowaves!
Bottom echo visible thru 5.6 km! (20 dB noise reduction [averaging])
Bedrock/2850m
J. Glac. 2005

11. MC simulations: Angular Resolution; dE/E~1
+Energy resolution~50% for r<1 km

12. Effective Volume
Systematics:
Signal Strength
Transfer Function
Re(epsilon) (=n)
Im(epsilon) (=Latt)
Birefringence
System Total Gain
Livetime
Software Cuts

14. GZK nu models
No UHE neutrinos yet observed compare with theoretical predictions for how many neutrinos RICE should have observed, given sensitivity of experiment and radio transmission properties of ice
Two representative models: ESS/WB. Both bootstrap from observed charged CR spectrum and estimate neutrino flux (WB assumes all UHECR’s from GRB’s)
Diffuse GRB flux

15. Caution on presentation
RICE uses a 95% CL upper limit convention
(vs. conventional 90% CL upper limit convention)
ESS GZK-flux depends on several parameters
RICE upper limits based on most conservative (I.e., lowest flux – not typical)
Upper limits as a function of energy are a total fake

16. Volumosity? Voluminosity? Your model x our exposure

19. Note: Limits generally rather weak (preferentially z>1 sample)

20. Relativistic magnetic monopole generates photon swarm.
Search for highly ionizing magnetic monopoles in Antarctic ice (Daniel Hogan, KU UG)
Relativistic magnetic monopole generates photon swarm.
Weizsäcker-Williams energy spectrum:
Jackson, 1963, etc.

21. Energy Loss in Earth: ionization+brem+pair production+ photonuclear
Check total energy loss against mmc package (dima chirkin) and also seckel, weiler&wick calculation
Razzaque et al., 2002

22. θ r l r Energy Loss in Earth Chord Length through Earth:
Loses energy as z=1/(2α) electric charge θ r l r

23. Preliminary monopole flux limits

24. Unforseen Complication
4 typical channels show clear sine wavesimpossible to see transient pulser signals;
FFT to determine frequency content…
9 waves/20 ns

25. 10 dB above noise; AFTER 25 dB noise filtering
450 MHz LMR signal
10 dB above noise; AFTER 25 dB noise filtering