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The ICE 3 Experiment

The ICE 3 Experiment. Thanks to O. Botner (Neutrino-2004). Acceleration up to 10 21 eV ?. ~10 2 Joules ~0.01 M GUT. Ultra high energy n ’s are associated with the sources of high energy cosmic rays. p + p(  )      e ,  . Dense regions with exceptional

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The ICE 3 Experiment

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  1. The ICE3 Experiment Thanks to O. Botner (Neutrino-2004)

  2. Acceleration up to 1021 eV ? ~102 Joules ~0.01 MGUT Ultra high energy n’s are associated with the sources of high energy cosmic rays p+ p()    e , • Dense regions with exceptional • gravitational force creating relativistic • flows of charged particles, e.g. • coalescing black holes/neutron stars • dense cores of exploding stars • supermassive black holes D. Bertrand

  3. Supernova Remnant in X-rays Shock fronts Fermiacceleration D. Bertrand

  4. Black Hole Accretion Disk Active Galactic Nucleus (Artist impression) Shock fronts Jets Fermiacceleration D. Bertrand

  5. IceCube – a ”next generation” n observatory kilometer-scale successor to AMANDA A 1 kilometer squared area is needed to see the potential energetic sources Candidates for 10 events/year/km² (n ~ g) D. Bertrand

  6. ICE3 Planned Location 1 km “west” South Pole “North” Dark sector Skiway AMANDA Dome D. Bertrand

  7. The ICE3 detector • 160 frozen water tanks (2/string) • Ice cylinder (2 m diameter; 0.9 m height) • 2 OM’s each • 80 strings • 17 m OM spacing • 125 m between strings • Geometry optimized for a detection range [TeV-PeV(EeV)] D. Bertrand

  8. AMANDA integration • AMANDA now runs with TWR • Data similar in structure to ICE3 • Work on a combined trigger • Position of 1st ICE3 strings • As close to AMANDA as possible • But … logistics and safety requirements • AMANDA • Calib. device for 1st ICE3 strings • + 20 ICE3 strings = powerful combined detector • Fully integrated low threshold subdetector of ICE3 D. Bertrand

  9. IceTop+ICE3: 1/3 km².sr (for coincident tracks) Energy range 1015 eV - 1018 eV VETO against • All downward events E > 300 TeV with trajectories inside IceTop • Larger events falling outside CALIBRATION • of angular response with tagged µ • Measure • Energy spectrum • Chemical composition Expect ~100 tagged air showers/day with multi-TeV µ’s in Ice3 • Muon survey of Ice3 D. Bertrand

  10. Showers triggering 4 stations give ~300 TeV threshold Large showers with E ~ 100-1000 PeV will clarify transition from galactic to extra-galactic cosmic rays Small showers (2-10 TeV) associated with the dominantm background detected as 2-tank coincidences at a station. Cosmic ray physics IceCube - Icetop coincidences D. Bertrand

  11. Digital Optical Module (DOM) Optical sensor : 10 inch Hamamatsu R-7081 Local digitization : • Time stamp • Wave form • Buffer • Digital transmission to surface on request Sampling at 300 MHz over 0.5 µs at 40 MHz over 5 µs Dynamic range 200 p.e./15 ns 2000 p.e./ 5µs penetrator HV board flasher board pressure sphere DOM main board • Local Controls : • HV • Discriminators • Global synchronization delay board PMT optical gel mu metal cage D. Bertrand

  12. Enhanced hot water drill AMANDA (3-reel) and ICE3 (1-reel) drill AMANDA system ICE3 • Goals • 18 holes/season • 2450 m deep • straight within 1m • quality logged AMANDA ICE3 Power consum. 2 MW 5 MW Time to 2400 m 120-140 h 35-40 h Fuel (gal/hole) 10000-12000 7000-8000 Set-up time 5 – 6 weeks 18-25 d D. Bertrand

  13. ICE3 DAQ architecture • DOM hub : • Industrial PC • Dual 1 GHz PIII processor • 2 GB memory • 250 GB hard-drive • dual 400W power supply for DOM’s 5 DOM hubs for ICETOP 80 DOM hubs for the in ice devices D. Bertrand

  14. ICE3 physics performance ICE3 will be able to identify •  tracks from for E>1011 eV • cascades from efor E> 1013 eV •  for E> 1015 eV Eµ=10 TeV • Background • mainly downgoing cosmic ray’s • (+ time coinc. ’s from uncorrelated air showers) • exp. rate at trigger level ~1.7 kHz • atm.  rate at trigger level ~300/day Rejected  using direction/energy/flavor id  temporal/spatial coincidence w. source for E< 1 PeV focus on the Northern sky for E> 1 PeV sensitive aperture increases w. energy  full sky observationspossible D. Bertrand

  15. Galactic center ICE3 effective area & angular resolution (µ) Further improvement expected using waveform info Median angular reconstruction uncertainty ~ 0.8 • E-2nmspectrum • After quality cuts and bgr suppression (atm µ reduction by ~106) D. Bertrand

  16. Eµ= 6 PeV, 1000 hits Eµ= 10 TeV, 90 hits Diffuse  hard Eµ cut Eµ > 100 TeV Point sources  softer Eµ cut + spatial correlation Diffuse nµ flux & Point sources • Objective (after removal of atm µ background): • Reject the steep energy spectrum of atm n • Retain as much signal as possible from a (generic) E-2 spectrum Use optimized energy cut Eµ number of hit OM’s D. Bertrand

  17. atm v signal Diffuse nµ flux Assume generic flux dN/dE = 10 –7 E-2 (cm-2s-1sr-1GeV) Expect ~ 103 events/year after atm µ rejection ~ 75 events/year after energy cut cf background 8 atm n blue: after atm µ rejection red: after Eµ cut Sensitivity (1 y):8.110-9 E-2 (cm-2s-1sr-1GeV) D. Bertrand

  18. Steady point sources Sensitivity point sources (1 y): 5.510-9 E-2 (cm-2s-1GeV) Search cone 1 opening half-angle + ”soft” energy cut (< 1 TeV) Transient point sources – ex GRB Essentially background-free search : Energy, spatial and temporal correlation with independent observation • For ~1000 GRB’s observed/year expect (looking in Northern sky only) • Signal: 12 n • Background (atm n): 0.1 Sensitivity GRB (1 y): ~0.2 fWB D. Bertrand

  19. e  e E = 375 TeV nt  “double bang” E = 1PeV ~300m IceTop veto on cosmics C.O.G. inside array E << 1 PeV 2 cascades coincide E  1 PeV ”double bang” E >> 1 PeV ”lollipop” (partial containment, reconstruct t track + 1 cascade) • Lcascade ~10 m small cf sensor spacing • ”spherical” energy deposition •  at 1 PeV, Øcascade ~ 500 m Cascades  ~10% in log(E/TeV) • sensitivity to all flavors • 4p coverage For diffuse flux expect similar sensitivity in the cascade channel as in the muon channel  Considerable improvement of overall sensitivity D. Bertrand

  20. Neutralino dark matter astro-ph/0401113 (Lundberg/Edsjö) WIMP orbits in the solar system perturbed Rates from the Sun less affected Rates from the Earth affected Direct and indirect searches might not be directly comparable • Past/present history of solar syst. • Low/high energy tail of  vel. distr. D. Bertrand Sun

  21. Status of ICE3 • Many reviews – international and within the U.S. - strongly emphasize the exciting science which can be performed with ICE3 • In Jan 2004, the U.S. Congress approved the NSF budget including the full ICE3 MRE • Significant funding approved also in Belgium, Germany and Sweden • In Feb 2004, NSF conducted a baseline review  “go ahead” • However … revised baseline preserving original scientific goals preserving current detector design straightforward upgrade path ICE3 strings IceTop tanks 4 8 Jan 2005 16 32 Jan 2006 32 64 Jan 2007 50 100 Jan 2008 68 136 Jan 2009 70+n 140+2n Jan 2010 D. Bertrand

  22. Summary • ICE3 is for real ! - and moving ahead at full speed • AMANDA experience provides for huge benefits • - both logistics-wise and for simulations/reconstruction • ICE3 is expected to be • Considerably more sensitive than AMANDA • Provide new opportunities for discovery • With IceTop – a unique tool for cosmic ray physics Decision on total number of strings summer 2006 1st challenge – successful deployment of strings 2004/2005 • Data taking during construction • First data augment AMANDA data • Later AMANDA an integral part of ICE3 D. Bertrand

  23. Transmission of nµ through the earth TeV: use upward going muons PeV: use horizontal events EeV: use events from above AMANDA-II D. Bertrand

  24. Status of ICE3 • Drill development on schedule for operation at Pole in Jan 2005 • Instrumentation • Production for the 4 string first season starts this summer • 50% PMTs delivered – on schedule • 3 DOM production sites • Wisconsin 290 1st season • DESY 60 1st season • Sweden 50 1st season • Spheres ordered – 40K depleted Benthos (dark noise ~0.8 kHz) • DOM mainboard – designed @ LBNL tests OK • DAQ S/W developed • Data transfer DOM  DOM Hub  Data Collection prog tested • Implementation for first season’s DAQ • Cables – Ericsson, Sweden / JDR, Netherlands • Preparing for analysis of early data (calibration, testing) • 4 DOM’s are collecting IceTop data using test s/w D. Bertrand

  25. IceTop tank with hood at the South Pole – Nov 2003 View of DOMs D. Bertrand

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