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Vrije Universiteit Brussel, Belgium

6 th Cracow Epiphany Conference. http://amanda.uci.edu. http://icecube.wisc.edu. The AMANDA – IceCube telescopes & Dark Matter searches. B. Baret on behalf of the IceCube collaboration. Vrije Universiteit Brussel, Belgium. bruny.baret@vub.ac.be. Physics Motivations and Goals. AMANDA.

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Vrije Universiteit Brussel, Belgium

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  1. 6th Cracow Epiphany Conference http://amanda.uci.edu http://icecube.wisc.edu The AMANDA – IceCube telescopes & Dark Matter searches B. Baret on behalf of the IceCube collaboration Vrije Universiteit Brussel, Belgium bruny.baret@vub.ac.be

  2. Physics Motivations and Goals AMANDA IceCube Attractive astronomical messengers: • Transparent Universe (≠g) • Travel in straight line (≠p) • Produced in hadronic accelerators ? Study of: • Sources: AGNs, SNRs, GRBs... • n-physics (atmospheric production): Oscillations, cross-sections.. • “new” physics: WIMPS, decoherence, monopoles...

  3. The IceCube collaboration Sweden: Uppsala Universitet Stockholm Universitet USA: Bartol Research Institute, Delaware Univ. of Alabama Pennsylvania State University UC Berkeley UC Irvine Clark-Atlanta University Univ. of Maryland IAS, Princeton University of Wisconsin-Madison University of Wisconsin-River Falls LBNL, Berkeley University of Kansas Southern University and A&M College, Baton Rouge Germany: Universität Mainz DESY-Zeuthen Universität Dortmund Universität Wuppertal Humboldt Universität, Berlin UK: Imperial College, London Oxford University Belgium: Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut Netherlands: Utrecht University Japan: Chiba University New Zealand: University of Canterbury

  4. Where are we ? Amundsen-Scott South Pole Station IceCube North Amanda Here! (South pole) Technically North also

  5. Detection principle O(km) long tracksnm O(10m) cascadesne, nt South Pole Ice properties (@400nm): • Scattering:~20m Pointing res. (m~2° , casc. ~35°) • Absorption:~110m Effective volume atm. n E.T. n Background (x E.T. n events/year): atmospheric m O(109) atmospheric n O(103) p m

  6. Layout Amanda: • Ø=200m, h=500m (0.02 km³) • Amanda B-10: 302 Optical Modules (OMs) on 10 strings (97-99) • Amanda II: 677 OMs on 19 strings (00->) IceCube: • 1km x1 km² instrumented volume • 4800 Digital Optical Modules (DOMs) on 80 strings IceTop(air shower array): • 1km² instrumented area • 160 surface water tanks with 2 DOMs each

  7. IceCube Deployment Hot water drilling: 2450 m deep straight within 1m 35-40 hrs per hole Deployment: 2 more strings up to now Expected completion in 2010 January 2005: First string deployed 60 DOMs installed (and working!)

  8. IceCube First Events! IceTop – IceCube IceTop tanks Down going m String 21

  9. Sensitivity and limits νe (cascades B10 1yr) νμ (B10 1yr) all-flavor limits νe+νμ+ντ (UHE B10 1yr) νμ (A-II 1yr) νe+νμ+ντ(cascades A-II 1yr) νμ (A-II 4yr) νe+νμ+ντ (UHE A-II 1yr) Icecube (1yr) AMANDA-B10 average flux upper limit [cm-2s-1] AMANDA-II IceCube 1/2 year sin Diffuse search E-2 flux hypothesis Steady point sources sensitivity: WB bound * Limit Sensitivity

  10. Point sources Sky map (00'-03') 3329n Significance maps real sky scrambled sky no source No point source detected so far...

  11. Neutralino as dark matter candidate Cosmological observations m ~ 0.30 b ~ 0.05 Minimal Supersymmetric Standard Model PR conserved  LSP stable = neutralino interacts weakly  = GeV-TeV mass = dark matter??? stable $ dark, non-baryonic matter

  12. Neutralino capture by Sun and Earth Sun – direct capture from galactic DM halo Earth – capture by gravitational diffusion and weak scattering

  13. Which WIMP signal Neutralino-induced neutrinos qq l+l-    W,Z,H Atmospheric background • atm. : absorbed by the Earth • atm. : compare on/off source angular regions “up” “down”

  14. Data and Monte Carlo used Data 1997-1999: 5.0x109 events 536.6 days eff. livetime 2001: 8.7x108 events 143.7 days eff. livetime Monte Carlo neutralino: 50 GeV < M< 5000 GeV [DARKSUSY] hard (W+W-) and soft (bb) ann. channel 90° << 113° (Sun) ~ 180° (Earth) atm.: Sun: 32 days Earth: 128 days[CORSIKA] 600 GeV < Ep< 1011 GeV0° <p< 90° atm.: Sun: 2.104 evts Earth: 2.108 evts[ NUSIM ] 10 GeV < E< 108 GeV 80° << 180°

  15. Rejection of signal & background Sun 2001 (submitted to Astrop. Phys.) Earth 1997-1999 (paper in preparation)

  16. No excess of neutralino-induced neutrinos signal region signal region Sun 2001 (submitted to Astrop. Phys.) Earth 1997-1999 (paper in preparation)

  17. Muon flux limits – Earth ’97-’99 Improvements (wrt. ’97) separate filter for each neutralino model more statistics Outlook 2001-2003 data set improved reconstructions new trigger lowers Ethresh PAPER IN PREPARATION

  18. AMANDA results submitted for publication Muon flux limits - Sun 2001 1st AMANDA solar neutralino results 200m diameter enables robust reconstruction of horizontal tracks Outlook 2000-2003 data set improved reconstructions new trigger lowers Ethresh

  19. Conclusion & outlook AMANDA & IceCube: • Amanda • provided very useful information (ice, drilling, detection strategy, bkgd, ...) • providing tighter and tighter constraints on models • IceCube • all flavour detection, ~30x more sensitive almost guaranteed discoveries • Is being deployed and takes data WIMPs search: • No statistically significant excess of neutralino-induced neutrinos from the center of the Earth or the Sun observed • Upper limits on the muon flux competitive with other indirect searches • Additional data are being analysed with improved techniques

  20. Technically Amanda IceCube Optical Module Digital Optical Module 10” PMT +Main Board +flasher 8” PMT Trigger, Digitization, HV Surface DOM single p.e. time res. <2ns 400ns and 6.4µs range 3 gains noise ~700Hz time res. ~4-8 ns 32 µs range noise: ~1kHz Digitized Waveform

  21. Plan... Season planning: Nov.: preparation Dec.: construction Jan.: construction Feb.: commissioning This austral summer : 8 to 12 strings deployed By 2010 : 1km³ instrumented

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