1. IceCube Construction and Analysis Report
Martijn Duvoort
Sterrekundig Instituut Utrecht
Faculty of Science, Department of Physics and Astronomy, University of Utrecht
Princetonplein 5, NL-3584 CC Utrecht, The Netherlands

2. Neutrino Astronomy protons E>1019 eV (<30 Mpc) neutrinos
gammas < 50 Mpc for E<100 TeV
Cosmic
accelerator
1 pc ~ 3 ly ~ 1018 cm
Drs. M.R. Duvoort - University of Utrecht
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3. Introducing IceCube 18-1-2019
Drs. M.R. Duvoort - University of Utrecht
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4. IceTop InIce IceCube Three more deployment seasons to finish in 2011: 18 :
13 Strings
: 8 Strings
: 1 String
IceTop
total of 40 Strings
IceCube: 0.5 km3
AMANDA: km3
Air shower detetor
threshold ~ 300 TeV
InIce
first data 2005
upgoing muon 18. Juli 2005
70-80 Strings ,
60 Optical Modules
17 m between Modules
125 m between Strings
IceCube fügt sich ins Gesamtbild ein ->
AMANDA
19 Strings
677 Modules
Three more deployment seasons to finish in 2011
Drs. M.R. Duvoort - University of Utrecht
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5. IceCube 40 First km-scale detector 31 times AMANDA
Fully digital waveforms
In-ice timing calibration
degree resolution
(depending on track length)
Data since March 2008
Drs. M.R. Duvoort - University of Utrecht
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6. Drs. M.R. Duvoort - University of Utrecht
Drs. M.R. Duvoort - University of Utrecht
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7. IC22 Events ( Red hits = early; yellow/green/blue = later )
IceCube DOM locations blue, AMANDA OM locations red
Downward cosmic-ray event (“muon bundle”)
Upward candidate n event
Drs. M.R. Duvoort - University of Utrecht
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8. IceCube extensions – Deep Core
IceCube DOM technology
AMANDA has no veto coverage from top, (which is where the muons come from)
Ice below 2100m is exceptionally clear, significantly better even than current ice model.
Swedish proposal funded by Wallenberg Foundation
Drs. M.R. Duvoort - University of Utrecht
+31-(0)

9. γ - ν coincident analysis per GRB
Current GRB analyses
γ - ν coincident analysis per GRB
Fails in case of time difference
Rolling time window
Needs GRB with multiple ν detections
Only 1 – 10% of GRBs will induce signal ν
Halzen & Hooper 1999, Astrophys. J. 527 (1999) L93
Need new method
Should cope with time difference
Should allow for cumulative statistics
Drs. M.R. Duvoort - University of Utrecht
+31-(0)

10. Stacking T T T + Need to cut the background! T T+∆ T-∆ T T+∆ T-∆ T T+∆
time T
T+∆
T-∆ T
T+∆
T-∆ T
T+∆
T-∆
ν data
Need to cut the background! + T
T+∆
T-∆
Drs. M.R. Duvoort - University of Utrecht
+31-(0)

11. Stacking around the GRB
Bkg suppression by GRB location
5 deg area around GRB position
0.5 – 1 deg resolution → cut bkg keep signal
Used 100 GRBs
background determination → off-time sample
Signal +
Background
On-source
Background
Off-time
Drs. M.R. Duvoort - University of Utrecht
+31-(0)

12. Sensitivity of our method
Parameters determining sensitivity
Number of bursts in sample
Fraction f of GRBs which yield a signal ν
Detection in case of 5 σ effect
Minimal f as function of #GRBs for detection
Swift and GLAST nicely coincide with IceCube
Drs. M.R. Duvoort - University of Utrecht
+31-(0)

13. Conclusion 1 km3 ν detector: discovery in coming year(s)
Astropart. Phys 28 (2008) 540
f: the fraction of GRBs inducing a signal ν
1 km3 ν detector: discovery in coming year(s)
Drs. M.R. Duvoort - University of Utrecht
+31-(0)

14. Current Status Data reconstruction
4 years of full AMANDA data
2 years of IceCube data
Off-time bkg determination in process
(blind) sample used to settle final analysis cuts
Unblinding proposal expected this spring
Run final analysis on unblinded sample
Drs. M.R. Duvoort - University of Utrecht
+31-(0)