1 / 25

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

calix
Télécharger la présentation

The ICE 3 Experiment

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related