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Recent Results

Recent Results. Lutz Köpke University of Mainz, Germany July 31, 2003. http://amanda.uci.edu. Cosmic rays. Neutrinos. Upgrade and IceCube. Contributed papers to ICRC.  Response of AMANDA to cosmic ray muons  Cosmic ray flux measurement

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Recent Results

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  1. Recent Results Lutz Köpke University of Mainz, Germany July 31, 2003 http://amanda.uci.edu

  2. Cosmic rays Neutrinos Upgrade and IceCube Contributed papers to ICRC Response of AMANDA to cosmic ray muons  Cosmic ray flux measurement  Cosmic ray composition at the knee with SPASE and AMANDA  Atmospheric neutrino and muon spectra Search for diffuse fluxes of extraterrestrial muon neutrinos  AMANDA-B10 limit on UHE-Neutrinos  Search for high energy neutrinos of all flavours  Search for extraterrestrial point sources of neutrinos  Search for muons from WIMP annihilation in center of earth  Search for high energy neutrinos from GRBs Online search for neutrino bursts from Supernovae New capabilities of the AMANDA detector  The IceCube high energy neutrino telescope  IceTop: the surface component of IceCube Simulation of ice Cherenkov detectors for IceTop + 3 individual contributions black: parallel talk

  3. Physics motivation • origin and acceleration of cosmic rays •  understand cosmic cataclysms •  find new kind of objects? •  neutrino properties ( , cross sections ..) •  dark matter (neutralino annihilation) • tests of relativitiy .... • search for big bang relics ... • effects of extra dimension etc. ...

  4. Supernova remnant Microquasar (SS433 etc.) Active Galaxy (optically dense, e.g. FRII)  1 LJ  106 LJ Crab nebula Black hole with  mass of sun Black hole with 108 x mass of sun extra-galactic galactic Neutrino source candidates

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

  6. Above O(PeV): significant  absorption: O(10 PeV) O(PeV): use horizontal events O(10 PeV): use events from above Detection of muon neutrinos cosmic radiation  (e)  (e) atmospheric muons Earth acts as shield

  7. Mediterranean (ocean) Antares, Nestor, 1 km3 ... Complementarity (point sources): E < 100 TeV South Pole (ice) AMANDA, ICECUBE galactic center in middle dots: distribution of gamma ray bursts (GRBs)

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

  9. Optical module (677) 1996-2000 AMANDA II Detector Amundsen-Scott Station South Pole

  10.  150 members The AMANDA Collaboration Bartol Research Institute UC Berkeley UC Iivine Pennsylvania State UW Madison UW River Falls LBL Berkeley U. Simón Bolivar, Caracas VUB, Brussel ULB-IHEE, Bruxelles U. de Mons-Hainaut Imperial College, London DESY, Zeuthen Mainz Universität Wuppertal Universität Stockholm Universitet Uppsala Universitet Kalmar Universitet South Pole Station Antarctica Antarctica New Zealand Venezuela (1) USA (7+3) Europe (10+1) Japan + associated institutes e.g. Chiba University

  11. South Pole AMANDA The laboratory

  12. The new station operating at least until 2035 The Dome

  13. 200 TeV e candidate Two events ...

  14.  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 •  primary cosmic rays:(+ SPASE) • energy resolution:¶0.07 – 0.10 •  „cascades“: (e±,  , neutral current) • zenith error: 30 - 40° • energy resolution:¶ 0.1 – 0.2 • coverage: 4 ¶[log10(E/TeV)]

  15. poster 1-P-265 Atmospheric muons in AMANDA-II Atmospheric muons and neutrinos: AMANDA‘s test beams much improved simulation ...but data 30% higher than MC ...  normalize to most vertical bin Systematic errors: 10% scattering ( 20m @ 400nm) absorption (110m @ 400nm) 20% optical module sensitivity 10% refreezing of ice in hole PRELIMINARY threshold energy ~ 40 GeV (zenith averaged)

  16. talk HE2.1-13 for QGSJET generator: (H) = 2.70 ± 0.02 0 (H) = 0.106(7) m-2s-1sr-1TeV-1 Spectral index  compatible with direct measurements, error competivie Cosmic Ray flux measurement In some cases ice and OM-sensitivity effect can be circumvented ... (E)=0E- empirical separation of ice and OM sensitivity effects PRELIMINARY

  17. talk HE 1.1-25 iron AMANDA (correlate to #muons) proton log(E/GeV) SPASE-2 (correlated to #electrons) cosmic ray composition studies SPASE-2 (electronic component) - AMANDA B10 (muonic component) - unique combination! AMANDA II robust evidence for composition change around knee ...

  18. talk HE 1.1-25 blue band: detector and model uncertainties red band: uncertainty due to low energy normalization confirms trend seen by other experiments ... publication in preparation (1998 data) Composition change around „knee“ 1015 eV 1016 eV A=30 A=6

  19. talk HE 2.3-6 Atmospheric n's in AMANDA-II neural network energy reconstruction regularized unfolding PRELIMINARY measured atmospheric neutrino spectrum  spectrum up to 100 TeV  compatible with Frejus data presently no sensitivity to LSND/Nunokawa prediction of dip structures between 0.4-3 TeV 1 sigma energy error In future, spectrum will be used to study excess due to cosmic ‘s

  20. poster HE talk HE 2.3-4 cascades (2000 data) Excess of cosmic neutrinos? Not yet ... .. for now use number of optical modules hit as energy variable ... muon neutrinos (1997 B10-data) accepted by PRL „AGN“ with 10-5 E-2 GeV-1 cm-2 s-1 sr-1 cuts determined by MC – blind analyses !

  21. poster 1-P-256 poster 1-P-257 2.5 ·106 – 5.6 ·108 GeV: E2(E) < 7.2 10-7 GeV-1 cm-2 s-1 sr-1 Expected sensitivity 2000 data: ~ 310-7 GeV-1 cm-2 s-1 sr-1 Diffuse flux muon neutrinos Note that limits depend on assumed energy spectrum ... 3·103 – 106 GeV: E2(E) < 8 10-7 GeV-1 cm-2 s-1 sr-1 prel. AMANDA II (with 3 years data): ~ 10 X higher Sensitivity

  22. talk HE 2.3-4 after acceptance expect: e :  :  1 : 0.67 : 0.41 events  2 candidate events total observed 90% CL upper limit: E2all (E) < 9·10 - 7 GeV cm-2s-1sr-1 Diffuse limit cascades 80 TeV – 7 PeV effective volume PRELIMINARY

  23. talk HE 2.3-4 Flux results summary (all flavors) assuming e:: =1:1:1 ratio: special analysis for resonant production (6.3 PeV)  multiplicative factor 3 applied for single e , channels … ...can combine analyses ! 2000  analysis will yield comparable result ...

  24. talk HE 2.3-5 Point source search in AMANDA II Search for excess events in sky bins for up-going tracks PRELIMINARY 697 events observed above horizon 3% non-neutrino background for  > 5°  cuts optimized in each declination band above horizon: mostly atmospheric ‘s below horizon:mostly fake events  sky subdivided into 300 bins (~7°x7°) no clustering observed - no evidence for extraterrestrial neutrinos ...

  25. talk HE 2.3-5 Selected point source flux limits sensitivity  flat above horizon - 4 times better than B10 ¶! PRELIMINARY declination averaged sensitivity: lim  2.3•10-8 cm-2s-1 @90% upper limits @ 90% CL in units of 10-8cm-2s-1 ¶published Ap. J, 582 (2003)

  26. 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 preliminary 2000 data GX 339-4 10-16 10-17 declination (degrees)

  27. talk OG 2.4-7 317 BATSE triggers (1997—2000) effective -area  50000 m2 low background due to space- time coincidence No excess observed! assuming WB spectrum 4 x 10-8GeV/s/cm2/sr analysis continues with non-triggered BATSE and IPN3 data … GRB n search in AMANDA Search for  candiates correlated with GRBs - background established from data <20° 10 min PRELIMINARY

  28. Outlook ... did not mention new improved search for WIMPs (HE 3.3-6) ... supernova detection (1-P-258) etc. ..no extraterrestrial neutrinos found yet ...but: • combined analysis 1997-2003: 8 x more days ! •  improved selection and analysis methods ... •  new transition waveform based readout installed 02/03 • improved performance in particular at high energies (1-P-264) •  first IceCube strings 2004/05 – combined analysis with AMANDA

  29. Is there a signal at higher energies? no indication of clustering also at higher energies ! increasing energy deposition

  30. Sun Crab Nebula Cassiopeia. A LMC Cygnus-X1 SMC Approximate AMANDA horizon 90 000 light years

  31. Importance of all flavor detection Extended source with e:: =1:2:0 production (e.g.  decay): E.g.: Maki-Nakagawa-Sakato mixing matrix with 12=30°, 23=45°, 13=0°: e:: =1:1:1 on earth O(10) x less background for e – but you don’t profit from long -range  Regeneration of  - no absorption in earth even at very high energies !

  32. DUMAND test string NT-200 FREJUS AMANDA-97 NT-200+ AMANDA-II IceCube AMANDA-00 MACRO Theoretical bounds and future opaque for neutrons MPR neutrons can escape atmospheric  W&B Mannheim, Protheroe and Rachen (2000) – Waxman, Bahcall (1999) derived from known limits on extragalactic protons + -ray flux

  33. talk HE 2.3-4 For E2(E) =10-6GeV cm-2s-1sr-1 flux would expect: 9.3 e , 6.2  , 3.8  events 2 candidate events total observed 90% CL limit, assuming e:: =1:1:1 : E2all (E) < 9·10 - 7 GeV cm-2s-1sr-1 Diffuse limit cascades Effective volume 80 TeV – 7 PeV PRELIMINARY

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