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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 ...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 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 Z0hadrons
e:: =1:2:0 at sourcee:: =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
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 , !
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
Submarine cable Antares Erlangen: acoustic detection, reconstruction string based detector 0.01 km3 instrumented volume 40 km ~ 40 km -2400m
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
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
IceCube preparation Hot water drill wheel ready for shipment Water heating plant
IceCube preparation .... Assembly and cold room DESY-Zeuthen
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)
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
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)
RICE AGASA 2002 Amanda, Baikal AUGER nt Anita 2004 0.1 km3 2007 Auger/Salsa km3 2012 EUSO
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-
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
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 ...
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 !
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
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)]
Signature in ICECUBE … 1013 eV (10 TeV) 6x1015 eV (6 PeV) Multi-PeV B10 +N+... ± +hadrons signature of signature of