Recent Results Lutz Köpke University of Mainz, Germany July 31,

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

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....

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

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 !

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

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)

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

Northern hemisphere detectors Nestor March 29, of 12 floors deployed 4000 m deep completion: 2006 Antares March 17, strings connected 2400 m deep completion: start 2006 Baikal NT m deep data taking since 1998 new: 3 distant strings

Amundsen-Scott Station South Pole Optical module AMANDA II Detector

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

South Pole AMANDA The laboratory

The Dome The new station operating at least until 2035

Two events TeV e candidate

Detector capabilities  muons: directional error: ° energy resolution: ¶ 0.3 – 0.4 coverage: 2   primary cosmic rays: (+ SPASE) energy resolution: ¶ 0.07 – 0.10  „cascades“: (e ±,  , neutral current) zenith error: ° energy resolution: ¶ 0.1 – 0.2 coverage: 4   effective area (schematic):  E E 3 cm 2 -interaction in earth, cuts 2 -5m GeV 100 TeV 100 PeV ¶  [log 10 (E/TeV)]

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 ( 400nm) absorption 400nm)  20% optical module sensitivity  10% refreezing of ice in hole poster 1-P-265

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

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

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

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 TeV In future, spectrum will be used to study excess due to cosmic ‘s PRELIMINARY talk HE 2.3-6

Excess of cosmic neutrinos? Not yet... cascades (2000 data) „ AGN“ with 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

2.5 ·10 6 – 5.6 ·10 8 GeV: E 2  (E) < 7.2  GeV -1 cm -2 s -1 sr -1 3·10 3 – 10 6 GeV: E 2  (E) < 8  GeV -1 cm -2 s -1 sr -1 Expected sensitivity 2000 data: ~ 3  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

Diffuse limit cascades Effective volume 80 TeV – 7 PeV  For E 2  (E) = 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· GeV cm -2 s -1 sr -1 90% CL limit, assuming e :  :  =1:1:1 : PRELIMINARY talk HE 2.3-4

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

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

 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 no clustering observed - no evidence for extraterrestrial neutrinos...

Sourcesdeclination1997 ¶ 2000 SS o -0.7 M o Crab22.0 o Mkn o Mkn o Cyg. X o Cas. A58.8 o Selected point source flux limits sensitivity  flat above horizon - 4 times better than B10 ¶ ! declination averaged sensitivity:  lim  cm -2 s PRELIMINARY ¶ published Ap. J, 582 (2003) upper 90% CL in units of cm -2 s -1 talk HE 2.3-5

muons/cm 2 s 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 Antares (2007+) preliminary 2000 data SS-433 Mark. 501 Crab

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

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

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

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