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

2. Upgrade and IceCube Neutrinos Cosmic rays 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. Neutrino source candidates Active Galaxy (optically dense, e.g. FRII) Black hole with 10 8 x mass of sun  10 6 LJ extra-galactic Supernova remnant Microquasar (SS433 etc.) Crab nebula Black hole with  mass of sun  1 LJ galactic

5. Importance of all flavor detection Extended source with e :  :  =1:2:0 production (e.g.   decay) : Expect for 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 !

6. Detection of e, ,  ~ 5 m Electromagnetic and hadronic cascadesO(km) long muon tracks direction determination by cherenkov light timing  15 m

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

8. Complementarity (point sources): E  < 100 TeV South Pole (ice) AMANDA, ICECUBE Mediterranean (ocean) Antares, Nestor, 1 km 3... dots: distribution of gamma ray bursts (GRBs) galactic center in middle

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

10. Amundsen-Scott Station South Pole Optical module 1996-2000 AMANDA II Detector

11. The AMANDA Collaboration Venezuela (1) Europe (10+1) Antarctica New Zealand USA (7+3) Japan 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  150 members + associated institutes e.g. Chiba University

12. South Pole AMANDA The laboratory

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

14. Two events... 200 TeV e candidate

15. 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   effective area (schematic):  E E 3 cm 2 -interaction in earth, cuts 2 -5m 2 100 GeV 100 TeV 100 PeV ¶  [log 10 (E/TeV)]

16. Atmospheric muons in AMANDA-II PRELIMINARY threshold energy ~ 40 GeV (zenith averaged) 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 poster 1-P-265

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

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

19. publication in preparation Composition change around „knee“ 1998 data 10 15 eV10 16 eV talk HE 1.1-25 A=30 A=6 confirms trend seen by other experiments... blue band: detector and model uncertainties red band: uncertainty due to low energy normalization

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

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

22. 2.5 ·10 6 – 5.6 ·10 8 GeV: E 2  (E) < 7.2  10 -7 GeV -1 cm -2 s -1 sr -1 3·10 3 – 10 6 GeV: E 2  (E) < 8  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 AMANDA II (with 3 years data): ~ 10 X higher Sensitivity Diffuse flux muon neutrinos Note that limits depend on assumed energy spectrum... prel. poster 1-P-257poster 1-P-256

23. Diffuse limit cascades Effective volume 80 TeV – 7 PeV  For E 2  (E) = 10 -6 GeV cm -2 s -1 sr -1 flux would expect: 9.3 e, 6.2 , 8.0  events 2 candidate events total observed E 2  all (E) < 9·10 - 7 GeV cm -2 s -1 sr -1 90% CL limit, assuming e :  :  =1:1:1 : PRELIMINARY talk HE 2.3-4

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

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

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

27. Sourcesdeclination1997 ¶ 2000 SS4335.0 o -0.7 M8712.4 o 17.01.0 Crab22.0 o 4.22.4 Mkn 42138.2 o 11.23.5 Mkn 50139.8 o 9.51.8 Cyg. X-341.0 o 4.93.5 Cas. A58.8 o 9.81.2 Selected point source flux limits sensitivity  flat above horizon - 4 times better than B10 ¶ ! declination averaged sensitivity:  lim  0.2310 -7 cm -2 s -1 @90% PRELIMINARY ¶ published Ap. J, 582 (2003) upper limits @ 90% CL in units of 10 -8 cm -2 s -1 talk HE 2.3-5

28. -90 0-45 9045 10 -15 10 -14 muons/cm 2 s 1 10 -17 10 -16 published data 1 km 3 detector, 3 years 1 km 3 Expected source sensitivity MACRO 8 years N AMANDA 137 days declination (degrees) S AMANDA+16 (2007) GX 339-4 Antares (2007+) preliminary 2000 data SS-433 Mark. 501 Crab

29. GRB n search in AMANDA Search for  candiates correlated with GRBs - background established from data  317 BATSE triggers (1997—2000)  effective  -area  50000 m 2 low background due to space- time coincidence  No excess observed! assuming WB spectrum 4 x 10 -8 GeV/s/cm 2 /sr analysis continues with non-triggered BATSE and IPN3 data …  <20° PRELIMINARY talk OG 2.4-7

30. Outlook... did not mention new improved search for WIMPs (HE 3.3-6)... supernova detection (1-P-258) etc. *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

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

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