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IceCube

IceCube. Christian Spiering, VLVNT Workshop Amsterdam, October 2003. IceCube Collaboration. Institutions: 11 US, 11 European, 1 Japanese and 1 Venezuelan Bartol Research Institute, University of Delaware BUGH Wuppertal, Germany Universite Libre de Bruxelles, Brussels, Belgium

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IceCube

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  1. IceCube Christian Spiering, VLVNT Workshop Amsterdam, October 2003

  2. IceCube Collaboration Institutions: 11 US, 11 European, 1 Japanese and 1 Venezuelan Bartol Research Institute, University of Delaware BUGH Wuppertal, Germany Universite Libre de Bruxelles, Brussels, Belgium CTSPS, Clark-Atlanta University, Atlanta, USA DESY-Zeuthen, Zeuthen, Germany Institute for Advanced Study, Princeton, USA 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 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 Dept. of Physics, Stockholm University, Stockholm, Sweden Dept. of Physics, University of Alabama, USA Vrije Universiteit Brussel, Brussel, Belgium Chiba University, Japan Dept. of Astrophysics, Imperial College, UK Dept. of Physics, University of Maryland, USA Universidad Simon Bolivar, Caracas, Venezuela NIKHEF, Utrecht, Netherlands

  3. Design and Technology C.Spiering, VLVNT Workshop

  4. IceTop AMANDA South Pole 1400 m 2400 m IceCube - 80 Strings - 4800 PMT • Instrumented volume: 1 km3 • Installation: 2004-2010 ~ 80.000 atm. per year C.Spiering, VLVNT Workshop

  5. South Pole Dark sector Skiway AMANDA Dome IceCube C.Spiering, VLVNT Workshop

  6. Drilling Hot water drilling C.Spiering, VLVNT Workshop

  7. Drilling: from Amanda to IceCube Amanda IceCube Heat (surface) 2 MW 5 MW Time to 2400 m 120-140 hours 35-40 hours Fuel (gal/hole) 10,000 - 12,000 7,000 - 8,000 Set-up Time 5-6 weeks 18-25 days C.Spiering, VLVNT Workshop

  8. Drilling Amanda (3-reel) and ICECUBE (1-reel) Drill C.Spiering, VLVNT Workshop

  9. Drilling ICECUBE C.Spiering, VLVNT Workshop

  10. Deployment now ... Deployment ... will be at room temperature C.Spiering, VLVNT Workshop

  11. Digital Optical Module - (DOM)  Captures waveforms with - 250 MHz first 500 ns - 40 MHz over 5000 ns  Time-stamps each pulse - r.m.s. < 5 nsec  Dynamic range - 200 PE over 15 ns - 2000 PE over 5000 ns  Dead time < 1 %  Noise rate < 500 Hz DOM 33 cm C.Spiering, VLVNT Workshop

  12. The New DOM Main Board Test Card - March 2003 DOM Main Board - March 2003 C.Spiering, VLVNT Workshop

  13. DOR PCI-Card Read-out of 8 DOMs (2 per twisted pair cable) C.Spiering, VLVNT Workshop

  14. String - Electronics in the ice DAQ Network Architecture Global Timing

  15. String 18 • Amanda DOM test string • timing 3.5 ns r.m.s. • cable length << 1 ns r.m.s. • gain drift << 0.2% per week • down going muons as expected • 15% of events have > 1 hit DOM board string 18

  16. Time Synchronization Surface DOM dt Dtdown =Dtup=1/2(Tround-trip- dt) C.Spiering, VLVNT Workshop

  17. Physics Capabilities C.Spiering, VLVNT Workshop

  18. Effective Area of IceCube Aeff / km2 cos  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)

  19. Angres 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 C.Spiering, VLVNT Workshop

  20. Energy Spectrum Point Source Search Blue: after downgoing muon rejection Red: after cut on Nhit to get ultimate sensitivity C.Spiering, VLVNT Workshop

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

  22. IceCube sensitivity vs time Diffuse Fluxes Point Sources C.Spiering, VLVNT Workshop

  23. DUMAND FREJUS  bound MACRO Muons in Amanda-B10 (1997) WB bound Expectation Amanda-II, 3 years Expectation IceCube, 3 years Search for diffuse excess of extra-terrestrial high energy muon neutrinos log E /GeV C.Spiering, VLVNT Workshop

  24. Limit on all neutrino flavors Cascades Cascades competitive with muons w.r.t. limit on diffuse fluxes !! Role will increase for IceCube. C.Spiering, VLVNT Workshop

  25. Count rates 0 5 10 sec Supernova Monitor Amanda-II B10: 60% of Galaxy A-II: 95% of Galaxy Amanda-B10 LMC IceCube C.Spiering, VLVNT Workshop

  26. IceTop C.Spiering, VLVNT Workshop

  27. 15 m IceTop Station Schematic Two Ice Tanks 3.6 m2 x 1 m To DAQ IceCube Drill Hole Two DOMs: 10” PMT C.Spiering, VLVNT Workshop

  28. Functions of IceTop • IceCube calibration with the help of downgoing muons (absolute pointing, angular resolution, detector geometry, ice atten.) • Anti-Shield (helps to reject downgoing muons from independent air showers) • Chemical Composition (IceTop measures electron component, IceCube muon component) C.Spiering, VLVNT Workshop

  29. spase-amanda 1 km 2 km SPASE air shower arrays  calibration of AMANDA angular resolution and pointing !  resolution Amanda-B10 ~ 3.5° results in ~ 3° for upward moving muons (Amanda-II: ~ 2°)

  30. Chem. Composition Iron 1 km Proton AMANDA (number of muons) log(E/PeV) 2 km Spase (number of electrons) Chemical Composition preliminary C.Spiering, VLVNT Workshop

  31. Cosmic rays CosmicRays Amanda/Spase IceCube/IceTop C.Spiering, VLVNT Workshop

  32. Schedule 03-04 drill equipment to Pole 04-05 first strings (proof that 16/season are feasible, prepare 6 full strings) 05-06 12 strings 06-07 16 strings 07-08 16 strings 08-09 16 strings 09-10 remaining strings C.Spiering, VLVNT Workshop

  33. Addendum on Lake Baikal C.Spiering, VLVNT Workshop

  34. The Baikal Collaboration Institute of Nuclear Research, Moscow Irkutsk State University, Irkutsk DESY Zeuthen, Zeuthen Moscow State University, Moscow Nishni Novgorod State Technical University State Marine Technical University, St.Petersburg Kurchatov Institute, Moscow JINR, Dubna C.Spiering, VLVNT Workshop

  35. Baikal History 93 94 95 96 97 98 99 00 01 02 03 04 > ----------------------------------------------------------------------- #OM 36 36 72 96 144 192 192 192 192 192 228 first 2 neutrino candidates NT-200+ NT-200 upgrade Baikal will stay largest H.E. neutrino telescope on northern hemisphere until Antares/Nestor will have installed arrays with 100-200 OMs and will nicely complement Amanda. One of the first neutrino events recorded with the 1996 four-string version of the Baikal Telescope

  36. Lake Baikal: The Detector C.Spiering, VLVNT Workshop

  37. NT-200 NT-200 140 m cascades Baikal Upgrade NT200+ 36 additional PMTs  4 times better sensitivity ! C.Spiering, VLVNT Workshop

  38. A lesson on electro-corrosion + -  40m  unexpected electro-corrosion after > 6 years C.Spiering, VLVNT Workshop

  39. points of problems + - Two out of four cables have broken during installation works in Spring 2003. Detector runs only with 5 strings in 2003. Two new cables in March 2004. C.Spiering, VLVNT Workshop

  40. End of Talk C.Spiering, VLVNT Workshop

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