The IceCube High Energy Telesope

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

3. The IceCube Collaboration Institutions: 11 US, 9 European institutions and1 Japanese institution; ≈150 people • Bartol Research Institute, University of Delaware, USA • BUGH Wuppertal, Germany • Dept. of Physics, Chiba University, JAPAN • Universite Libre de Bruxelles, Brussels, Belgium • CTSPS, Clark-Atlanta University, Atlanta USA • DESY-Zeuthen, Zeuthen, Germany • Institute for Advanced Study, Princeton, USA • Dept. of Technology, Kalmar University, Kalmar, Sweden • Lawrence Berkeley National Laboratory, Berkeley, USA • Department of Physics, Southern University and A\&M College, Baton Rouge, LA, USA • Dept. of Physics, UC Berkeley, USA • Institute of Physics, University of Mainz, Mainz, Germany • Department of Physics, University of Maryland, USA • University of Mons-Hainaut, Mons, Belgium • Dept. of Physics and Astronomy, University of Pennsylvania, Philadelphia, USA • Dept. of Astronomy, Dept. of Physics, SSEC, University of Wisconsin, Madison, USA • Physics Department, University of Wisconsin, River Falls, USA • Division of High Energy Physics, Uppsala University, Uppsala, Sweden • Fysikum, Stockholm University, Stockholm, Sweden • University of Alabama, USA • Vrije Universiteit Brussel, Brussel, Belgium

4. South Pole Dark sector Skiway AMANDA Dome IceCube

5. IceTop AMANDA South Pole Skiway 1400 m 2400 m IceCube • 80 Strings • 4800 PMT • Instrumented volume: 1 km3 (1 Gt) • IceCube is designed to detect neutrinos of all flavors at energies from 107 eV (SN) to 1020 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. ν Downward lepton γ γ ± π + + e e － － e e m １．４ｋｍ １ｋｍ Ice γ ν lepton １ｋｍ Rock ν Upward

8. How our events look like Eµ=10 TeV ≈ 90 hits Eµ=6 PeV ≈ 1000 hits 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. Design parameters: Time resolution:≤ 5 nsec (system level) Dynamic range: 200 photoelectrons/15 nsec (Integrated dynamic range: > 2000 photoelectrons) (1.p.e. /10ns ~ 160mA 10^7G ~8mV 50 W) 4V saturation500p.e. Digitization depth: 4 µsec. Noise rate in situ: ≤500 Hz Tube trig.rate by muons 20Hz DAQ design: Digital Optical Module- PMT pulses are digitized in the Ice DOM 33 cm

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

13. 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. Photomultiplier:HamamatsuR7081-02 (10”, 10-stage, 1E+08 gain)

14. Custom design: 5000 DOMs, 2500 copper pairs, 800 PCI cards (10 racks) DAQ Network architecture 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 CH2 CH1

18. The big reel for the hotwater drill

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

20. after trigger after cuts to reject atm. background (Level 2) • 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

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

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

23. Aeff / km2 cos  Effective area of IceCube 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)

24. ICRC 2003 In three years operation… • E2dNn/dE ~10-8 GeV/cm2 s sr (diffuse) • E2dNn/dE ~7x10-9 GeV/cm2 s (Point source) • 200 bursts in coincidence (GRBs – WB flux) For 5s detection

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

26. ICRC 2003 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.

27. 11000m 2800 m 1400 m Down-going events dominates… Up Down ICRC 2003

28. 1 km2 year Downward going!! ICRC 2003

29. Intensity of EHE m and t [cm-2 sec-1] ICRC 2003