1. The IceCube High Energy Telesope The detector elements Expected Sensitivity Project Status Shigeru Yoshida Dept. of Physics CHIBA Univ. ICRC 2003

3. The IceCube Collaboration Institutions: 11 US, 9 European institutions and 1 Japanese institution; ≈150 people 1. Bartol Research Institute, University of Delaware, USA 2. BUGH Wuppertal, Germany 3. Dept. of Physics, Chiba University, JAPAN 4. Universite Libre de Bruxelles, Brussels, Belgium 5. CTSPS, Clark-Atlanta University, Atlanta USA 6. DESY-Zeuthen, Zeuthen, Germany 7. Institute for Advanced Study, Princeton, USA 8. Dept. of Technology, Kalmar University, Kalmar, Sweden 9. Lawrence Berkeley National Laboratory, Berkeley, USA 10. Department of Physics, Southern University and A\&M College, Baton Rouge, LA, USA 11. Dept. of Physics, UC Berkeley, USA 12. Institute of Physics, University of Mainz, Mainz, Germany 13. Department of Physics, University of Maryland, USA 14. University of Mons-Hainaut, Mons, Belgium 15. Dept. of Physics and Astronomy, University of Pennsylvania, Philadelphia, USA 16. Dept. of Astronomy, Dept. of Physics, SSEC, University of Wisconsin, Madison, USA 17. Physics Department, University of Wisconsin, River Falls, USA 18. Division of High Energy Physics, Uppsala University, Uppsala, Sweden 19. Fysikum, Stockholm University, Stockholm, Sweden 20. University of Alabama, USA 21. Vrije Universiteit Brussel, Brussel, Belgium

4. South Pole Dark sector AMANDA IceCube Dome Skiway

5. IceCube 1400 m 2400 m AMANDA South Pole IceTop Skiway 80 Strings 4800 PMT Instrumented volume: 1 km3 (1 Gt) IceCube is designed to detect neutrinos of all flavors at energies from 10 7 eV (SN) to 10 20 eV

6. Design goals IceCube was designed to detect to neutrinos over a wider range of energies and all flavors. If one would wish to build a detector to detect primarily PeV or EeV neutrinos, one would obviously end up with a different detector.

7. １．４ ｋｍ １ｋｍ Upward Ice Rock ν ± π γ ν + e － e １ｋｍ Downward ν γ γ + e － e lepton 

8. E µ =10 TeV ≈ 90 hitsE µ =6 PeV ≈ 1000 hits How our events look like The typical light cylinder generated by a muon of 100 GeV is 20 m, 1PeV 400 m, 1EeV it is about 600 to 700 m.

9. Assembled DOM

11. DAQ design: Digital Optical Module - PMT pulses are digitized in the Ice Design parameters: Time resolution:≤ 5 nsec (system level) Dynamic range: 200 photoelectrons/15 nsec (Integrated dynamic range: > 2000 photoelectrons) (1.p.e. /10ns ~  10^7G ~8mV 50  4V saturation  500p.e. Digitization depth: 4 µ sec. Noise rate in situ: ≤500 Hz Tube trig.rate by muons 20Hz 33 cm DOM

12. Capture Waveform information (MC) ATWD 300MHz 14 bits. 3 different gains (x15 x3 x0.5) Capture inter. 426nsec 10 bits FADC for long duration pulse. E=10 PeV 0 - 4 µsec Events / 10 nsec String 1 String 2 String 3 String 4 String 5

13. Photomultiplier: Hamamatsu R7081-02 (10 ”, 10-stage, 1E+08 gain) Selection criteria (@ -40 °C) Noise < 300 Hz (SN, bandwidth) Gain > 5E7 at 2kV (nom. 1E7 + margin) P/V > 2.0 (Charge res.; in-situ gain calibration) Notes: Only Hamamatsu PMT meets excellent low noise rates! Tested three flavors of R7081.

14. DAQ Network architecture Custom design: 5000 DOMs, 2500 copper pairs, 800 PCI cards (10 racks) Off the shelf IT infrastructure, Computers, switches, disks DAQ Software Datahandling software

15. Digital Optical Module (DOM) Main Board Test Card

16. SPE Discriminator Scan – PMT Pulses Input (71DB)

17. SPE Waveforms CH0 CH1 CH2

18. The big reel for the hotwater drill

19. Angular resolution as a function of zenith angle  above 1 TeV, resolution ~ 0.6 - 0.8 degrees for most zenith angles 0.8° 0.6° Waveform information not used. Will improve resolution for high energies !

20. Event rates for -atmospheric - AGN (E -2 flux 10 times below MPR bound and present exp. limits) - atm.  from 1 EAS - atm.  from 2 EAS after trigger after cuts to reject atm.  background (Level 2)

21. Energy Spectrum Diffuse Search Blue: after downgoing muon rejection Red: after cut on N hit to get ultimate sensitivity

22. Energy Spectrum Point Source Search Blue: after downgoing muon rejection Red: after cut on N hit to get ultimate sensitivity

23. cos  A eff / km 2 Effective area vs. zenith angle after rejection of background from downgoing atmospheric muons Effective area vs. muon energy - after trigger - after rejection of atm  - after cuts to get the ultimate sensitivity for point sources (optimized for 2 benchmark spectra) Effective area of IceCube

24. E 2 dN /dE ~10 -8 GeV/cm 2 s sr (diffuse) E 2 dN /dE ~7x10 -9 GeV/cm 2 s (Point source) 200 bursts in coincidence (GRBs – WB flux) In three years operation … ICRC 2003 For 5  detection

25. Construction: 11/2004-01/2009 AMANDA SPASE-2 South Pole Dome Skiway 100 m Grid North Next season: Buildup of the Drill and IceTop prototypes

26. Project status Approved by U.S. the National Science Board Startup funding is allocated. 100 DOMs are produced and being tested this year. Assembling of the drill/IceTop prototypes is carried out at the pole this season. Full Construction start in 04/05; takes 6 years to complete. Then 16 strings per season, increased rate may be possible. ICRC 2003

27. Down-going events dominates… 1400 m 2800 m 11000m UpDown

28. ICRC 2003 Downward going!! 1 km 2 year

29. ICRC 2003 Intensity of EHE  and  GZK model I  (E>10PeV)I  (E>10PeV) RATE [/yr/ km 2 ] m=4 Z max =4 Down 5.90 10 -19 5.97 10 -19 0.37 Up 3.91 10 -20 6.63 10 -20 0.03 m=7 Z max =5 Down 8.88 10 -17 9.10 10 -17 53.4 Up 5.72 10 -19 9.73 10 -18 4.64 [cm -2 sec -1 ]