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Neutrino Telescopes

Neutrino Telescopes. ...existing activities for future projects in Germany.  motivation - particle physics aspects  detectors - principles - capabilities - time-lines  (particle) physics examples. Lutz Köpke Workshop on Neutrino Physics DESY Hamburg, 7.10.03. Physics motivation.

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Neutrino Telescopes

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  1. Neutrino Telescopes ...existing activities for future projects in Germany motivation - particle physics aspects  detectors - principles - capabilities - time-lines  (particle) physics examples Lutz Köpke Workshop on Neutrino Physics DESY Hamburg, 7.10.03

  2. Physics motivation origin and acceleration of cosmic rays  understand cosmic cataclysms  find new kind of objects?  neutrino properties  , cross sections, oscillations (ANTARES) mass hierarchy from SN (ICECUBE)  dark matter (neutralino annihilation)  new (rare) particles tests of relativitiy .. effects of extra dimension etc. . Neutrino background radiation Z0hadrons

  3. e:: =1:2:0 at sourcee:: =1:1:1 at Earth ! O(km) long muon tracks  15 m ~ 5 m direction determination by Cherenkov light timing Detection of e , , Electromagnetic and hadronic cascades

  4. Mediterranean (ocean) Antares, Nestor, 1 km3 ... Complementarity needed Need earth as shielding agains cosmic rays for  (if E< 100 TeV) South Pole (ice) AMANDA, ICECUBE galactic center in middle 4  coverage for e ,  !

  5. Antares Nestor March 17, 2003 2 strings connected 2400 m deep completion: 2006 Erlangen March 29, 2003 1 of 12 floors deployed 4000 m deep completion: 2006 Kiel Northern hemisphere detectors Baikal NT200 1100 m deep data taking since 1998 new: 3 distant strings DESY-Zeuthen

  6. Submarine cable Antares Erlangen: acoustic detection, reconstruction string based detector 0.01 km3 instrumented volume 40 km ~ 40 km -2400m

  7. 0 m (IceTop) IceCube 80 Strings 4800 PMTs 1km3 1400 m Optical module (677) 2400 m  80000 atmospheric ‘s /year AMANDA and IceCube DESY-Zeuthen, Wuppertal, Mainz 1996-2000  1000 atmospheric ‘s /year

  8. Status km3-detector in Mediterranean  decision by Antares, Nemo and Nestor (late 2002): cooperate in preparing future km3-telescope  EU application to fund design study -> TDR 2007?  ApPEC site recommendation 2003/2004 (difficult ...)  8 -10 years of R&D and construction? km3 - detectors Status of IceCube  NSF funding 2002, 2003  European funding from Sweden, Belgium, DESY  complete cost in presidential budget for 2004 mid-may earliest time for final funding  first Strings 04/05 season  80 string detector finished 2010 IceCube 10 TeV  Antares Nestor Nemo

  9. IceCube preparation Hot water drill wheel ready for shipment Water heating plant

  10. IceCube preparation .... Assembly and cold room DESY-Zeuthen

  11. N Antares (2007+) SS-433 AMANDA+16 (2007) -45 0 45 90 -90 1 km3 1 km3 detectors, 3 years Expected source sensitivity muons/cm2 s1 AMANDA 137 days 10-14 S MACRO 8 years Crab published data Mark. 501 10-15 year 2000 data GX 339-4 10-16 10-17 declination (degrees)

  12. Very high energy neutrinos Karlsruhe, Wuppertal Pierre Auger Observatory 3000 m2 horizontal high energy neutrinos... e.g GZK-neutrinos: 0.6 x 10-27 cm2 High energy neutrinos! Detection capability similar to 1 km3 neutrino telescope

  13. Even higher energies .... Zeuthen (Mainz),Erlangen R&D acoustic detection (absorption length O(km) in ice, water) radio detection (RICE/AMANDA, Anita, Lopez/Kaskade Grande etc) MPI-Munich space based detection (e.g. EUSO)

  14. RICE AGASA 2002 Amanda, Baikal AUGER nt Anita 2004 0.1 km3 2007 Auger/Salsa km3 2012 EUSO

  15. e.g.:  +   b + b c + - +  Indirect search for dark matter neutralino is best particle physics candidate for dark matter  stable if R-parity conserved (for most parameters)  can self-annihilate (Majorana particle) and produce neutrinos  gravitationally trapped in center of earth, sun or center of galaxy  ; W+W-

  16. Edelweiss excluded Edelweiss excluded Sun Antares 3 years AMANDA 1y 1km3 (IceCube) 1km3 (IceCube) Limits:  flux from the Earth/Sun Earth prel. AMANDA 1y mSUGRA parameter scan in cosmological interesting region

  17. Future direct detection limits Sun Future direct detection experiments 1 km3 detector (IceCube) If neutralinos found at LHC: - really source of dark matter? - learn about dark matter distribution ... Direct searches, neutrino telescopes and LHC are complementary ...

  18. 10-14 Soudan KGF Baikal 10-15 MACRO Orito upper limit (cm-2 s-1 sr-1) Amanda 10-16  electrons 10-17 1 km3 10-18 0.50 0.75 1.00  = v/c New particles high sensitivity to rare new particles if signature unambigous .... ... (slowly) moving bright particles ... e.g magnetic monopoles: Cherenkov-light  (n·g/e)2 (1.33*137/2)2 8300 times stronger than for !

  19. Summary  neutrino telescopes clue to understand cosmic accelerators  with some luck also important results for particle physics  with very much luck extremely interesting .... Very important contributions by DESY to AMANDA and IceCube

  20.  effective area (schematic): -interaction in earth, cuts 2 -5m2 En 2 3 cm2 100 GeV 100 TeV 100 PeV Detector capabilities •  muons: • directional error: 2.0 - 2.5° • energy resolution:¶0.3 – 0.4 • coverage: 2 •  „cascades“: (e±,  , neutral current) • zenith error: 30 - 40° • energy resolution:¶ 0.1 – 0.2 • coverage: 4 Noise: 500 Hz, 50000 Hz ¶[log10(E/TeV)]

  21. Signature in ICECUBE … 1013 eV (10 TeV) 6x1015 eV (6 PeV) Multi-PeV  B10 +N+... ±  +hadrons signature of signature of

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