1. Carlos de los Heros, Uppsala University results from neutrino telescopes COSMO05. Bonn, Aug. 28 – Sep. 1, 2005

2. Outlook.  as a framework : high energy neutrino astronomy  the world of neutrino telescopes: current projects  recent physics results from AMANDA and Baikal  ICECUBE: status and capabilities  summary

3. nature accelerates particles to ~10 7 times the CM energy of LHC!  acceleration sites must sit somewhere candidate sources: SNe remnants,  quasars active galactic nuclei gamma ray bursts neutrino astronomy ? proton accelerators guaranteed sources: atmospheric neutrinos (from  & K mesons decay) galactic plane: – CR interacting with ISM, concentrated on the disk CMB (diffuse):   – UHE p    +  n  + (p  0 ) T. Gaisser 2005

4. particle propagation in the Universe production: neutrino production at source: p+  or p+p collisions give pions:        e - +   e neutrino flavors: e :  :  1:2:~0 at source. Expect 1:1:1 at detector propagation: photons: can be absorbed on intervening matter or radiation; protons: deviated by magnetic fields at high-enough energies: p and g react with the CMB bckgr. n ’s will get to you however: n’s extremely difficult to detect! your favourite cosmic accelerator p g your favourite detector n

5. Outlook.  as a framework : high energy neutrino astronomy  the world of neutrino telescopes: current projects  recent physics results from AMANDA and Baikal  ICECUBE: status and capabilities  summary

6. current HE neutrino detection efforts OPTICALRADIOACOUSTIC @ extremely high energies (E>10 18 eV) AMANDA / ICECUBE NEMO NESTOR BAIKAL RICE, ANITA SALSA KAMCHATKA AUTEC GLUE ANTARES SADCO

7. neutrino detection in ice/water longer absorption length → larger effective volume longer scattering length → better pointing resolution event reconstruction by Cherenkov light timing: need array of PMTs with ~1ns resolution  optical properties of the medium of prime importance absorption lengthscattering length South Pole ice (AMANDA/IceCube) 110 m ( @ 400nm) 20 m ( @ 400nm) Lake Baikal 25 m (@ 480nm) 59 m (@ 480nm) Mediterranean (ANTARES/NESTOR) ~60 m (@ 470nm) 100-300 m (@ 470nm) neutrino astronomy possible since O(km) long muon tracks O(10m) cascades, e  neutral current signatures

8. the BAIKAL detector NT-200 - - 8 strings with 192 optical modules - - 72 m height, 1070 m depth - - m effective area >2000 m 2 (E  >1 TeV) - - Running since 1998 NT-200+ - - commisioned April 9, 2005. - 3 new strings, 200 m height - 1 new bright Laser for time calibration imitation of 20TeV-10PeV cascades, >10^12 photons/pulse w/ diffusor, - new DAQ - 2 new 4km cables to shore 4 Km to shore NT200+ is tailored to UHE n-induced cascades 5 Mton equipped volume; V_eff > 10 Mton at 10 PeV

9. PMT noise: ~1 kHz Optical Module the AMANDA detector AMANDA-B10 - - 10 strings with 302 optical modules - - 450 m height, 1500 m depth - - data years: 1997/99 AMANDA-II - 19 strings, 677 OMs - running since 2000 - new DAQ with FADC since 2003 since March 2005 we are called IceCube! (AMANDA and IceCube collaborations merged)

10. Amundsen-Scott South Pole station South Pole Station facilities AMANDA your daily commute to work 1500 m 2000 m the site [not to scale]

11. muons: directional error: 1.5° - 2.5°  ( log(E reco /E true ) ) : 0.3 – 0.4 coverage: 2  cascades: (e ±,  , neutral current ) zenith error: 30° - 40°  ( log(E reco /E true ) ) : 0.1 – 0.2 (5TeV < E < 5PeV) coverage: 4   effective area: >10000 m 2 for E  >1TeV AMANDA detector performance Average upper limit = sensitivity (δ>0°) (integrated above 10 GeV, E -2 signal) average flux upper limit [cm -2 s -1 ] sin  AMANDA-B10 AMANDA-II time

12. Outlook.  as a framework : high energy neutrino astronomy  the world of neutrino telescopes: current projects  recent physics results from AMANDA and Baikal  ICECUBE: status and capabilities  summary

13. in this talk: AMANDA (and Baikal when available) results from:  atmospheric neutrinos  searches for an extra-terrestrial flux:  galactic center  diffuse (anytime, anywhere)  point source (anytime, somewhere)  transient (known ‘flary’ objects & GRBs) (sometime, somewhere)  search for WIMPs: Excess from the center of the Sun/Earth agreed AMANDA collaboration strategy: analyses are done ‘blind’. cuts optimized on a % of data or on a time-scrambled data set.

14. E Hadron  E -2.7  0.02 cosmic ray muons test beams: atmospheric muons SPASE (scintillator array @ 3000m) e density @ surface shower core resolution: 0 (m) shower direction resolution: < 1.5 o AMANDA  ‘s @ >1500m (>300 GeV @ surface) use SPASE core position for combined fit combined SPASE-AMANDA ‘detector’:  probes hadronic (  ) and EM (e) component of the primary shower  (E) ~ 0.07 in log(E prim )  results compatible with composition change around the knee  sources of systematic uncertainties: (~30% in ln(A), not shown in the plot) -shower generation models -muon propagation atmospheric muons: - AMANDA test beam: I  vs depth, CR composition - background for other searches

15. set limit on cosmic neutrino flux:  how much E -2 cosmic ν - signal allowed within uncertainty of highest energy bins? limit on diffuse E -2 ν μ flux (100 -300 TeV): first spectrum > 1 TeV (up to 300 TeV) - matches lower energy Frejus data E 2  μ (E) < 2.6·10 –7 GeV cm -2 s -1 sr -1 test beams: atmospheric neutrinos vertical horizontal Frejus AMANDA ► reconstruct energy of up-going μ` s ► obtain energy spectrum from regularized unfolding atmospheric neutrinos: - guaranteed test beam - background for other searches

16. on-source region on-source events expected background 90% event upper limit line source limit GeV -1 cm -2 s -1 rad -1 diffuse limit GeV -1 cm -2 s -1 sr -1 gaussian limit GeV -1 cm -2 s -1 sr -1  2.0º 128129.419.8 6.3  10 - 5 6.6  10 - 4 —  4.4º 272283.320.0—— 4.8  10 - 4 - - - - - - - Gaus. limit model ’ s from the galactic plane location of AMANDA not optimal  reach only outer region of the galactic plane: 33 o <  <213 o three signal ansatz: line source, Gaussian source, diffuse source limits include systematic uncertainty of 30% on atm. flux energy range: 0.2 to 40 TeV data sample 2000-03: 3369 evts:

17. strategies in the search for point sources: diffuse flux with no time-space correlations. from high energy tail of atmospheric ν μ selection with emphasis on background(s) rejection spatial correlation with steady objects search for clusters of events (w. or w.o. catalogue) stacking of same-type of point source candidates space and/or time correlation with transient phenomena known active flary periods of TeV gamma sources coincidence with GRBs search for HE neutrinos from the cosmos UHE: E > PeV Earth opaque: search in the upper hemisphere and close to the horizon HE: TeV < E < PeV search confined to up-going tracks analyses optimized for  ( reduced sensitivity to e and  ) Cascades: TeV < E < PeV 4  sensitivity all-flavour energy regions:

18. diffuse flux search AMANDA 1: B10, 97, ↑μ 2: A-II, 2000, atmosph. 3: A-II, 2000, cascade 4: B10, 97, UHE 6: A-II, 2000, UHE sensit. 7: A-II, 2000-03 ↑μ sensit. Baikal 5: 98-03, cascades 8: NT200+ sensitivity to n e limits for other flux predictions: - cuts optimized for each case. - expected limit from a given model compared with observed limit. some AGN models excluded at 90% CL: Szabo-Protehoe 92. Proc. HE Neutr. Astrophys. Hawaii 1992. Stecker, Salamon. Space Sc. Rev. 75, 1996 Protheroe. ASP Conf series, 121, 1997 1:1:1 flavor flux ratio all-flavor limits 6 7 8

19. event selection optimized for both dN/dE ~ E -2 and E -3 spectra search for clusters of events in the northern sky source nr. of events (4 years) expected backgr. (4 years) flux upper limit  90% (E >10 GeV) [10 -8 cm -2 s -1 ] Markarian 42165.580.68 1ES1959+65053.710.38 SS43324.500.21 Cygnus X-365.040.77 Cygnus X-145.210.40 Crab Nebula105.361.25 data from 2000-2003 (807 days) 3369 from northern hemisphere 3438 expected from atmosphere search for excesses of events on: the full Northern Sky a set of selected candidate sources significance map … out of 33 Sources crab Mk421 Mk501 M87 Cyg-X3 SS433 1ES1959 Cyg-X1

20. neutrino sky from Baikal 1998-2002 data sample - 372 events - 385 evts expected - no indication of clustering

21. catalogues: BATSE+IPN3 bckg. Stability required within ±1 hour from burst several search techniques: coincidence with T90 precursor (110s before T90) cascades (all flavour, 4  ) -coincident with T90 -rolling time window (no catalogue) search for ’s correlated with GRBs low background analysis due to both space and time coincidence search! year # GRBs from preliminary 90%CL upper limit assuming WB spectrum (E B at 100 TeV and  = 300) '97 - '00312 BATSE triggered bursts E 2 d  /dE = 4 · 10 -8 GeV cm -2 s -1 sr -1 '00 - '03139 BATSE & IPN bursts E 2 d  /dE = 3 · 10 -8 GeV cm -2 s -1 sr -1 '01 - '0350IPN bursts (Assuming the Razzaque model) E 2 d  /dE = 5 · 10 -8 GeV cm -2 s -1 sr -1 '01(425) Rolling window E 2 d  /dE = 2.7 · 10 -6 GeV cm -2 s -1 sr -1 '0073 BATSE triggered bursts E 2 d  /dE = 9.5 · 10 -7 GeV cm -2 s -1 sr -1 10 min 1 hour 110 s T90 time Off-Time PrecursorOn Time Always Blind

22.  m  20%,  b  5%  non-baryonic matter  MSSM candidate: the neutralino, c c may exist as relic gas in the galactic halo gravitational accumulation in Sun/Earth makes ‘indirect’ searches with neutrino telescopes possible search for DM candidates in the Sun/Earth neutralino-induced neutrinos: qq  l + l -  W, Z, H signature: n excess from Sun/Earth’s center direction A lot of physics (ie. uncertainties) involved: - relic density calculations - DM distribution in the halo - velocity distribution - c properties (MSSM) - interaction of c with matter (capture)

23. 2001 Sun analysis possible due to improved reconstruction capability for horizontal tracks in AMANDA-II compared with B10. search for a neutralino signal from the Earth search for a neutralino signal from the Sun results from indirect DM searches

24. e.g. magnetic monopoles: Cherenkov-light  (n·g/e) 2 (1.33*137/2) 2  8300 times brighter than  ‘s! signature: ‘slowly‘ moving bright particles other particle searches 10 -16 10 -15 10 -14 10 -18 10 -17  = v/c 1.000.750.50 upper limit (cm -2 s -1 sr -1 ) KGF Soudan Baikal 2005 Amanda-B10 1 km 3  electrons MACRO Orito

25. Outlook.  as a framework : high energy neutrino astronomy  the world of neutrino telescopes: current projects  recent physics results from AMANDA and Baikal  ICECUBE: status and capabilities  summary

26. deep ice array: IceCube  digital readout technology (DOMs)  80 strings, 60 DOM’s each  17 m DOM spacing  125 m between strings  hexagonal pattern over 1 km 2 x1 km 1200 m the IceCube observatory: IceCube+IceTop IceTop IceCube surface array: IceTop  80 stations air shower array (one per IceCube string)  similar station concept as Auger  2 tanks (2 DOMs each) per station  125 m grid, 1 km 2 at 690 g/cm 2

27. E  =6 PeV IceCube: an all-flavor neutrino telescope IceCube will be able to identify -  tracks from  for E > 100 GeV - cascades from e for E > 10 TeV -  for E > 1 PeV background mainly downgoing  bundles (+ uncorrelated coincident  's) - exp. rate at trigger level ~1.7 kHz - atm.  rate at trigger level ~300/day    e  e  “cascade” E = 375 TeV ~300m @ E  = 1 PeV

28. Galactic center IceCube: A eff and resolution 1 year sensitivity E 2 ·d  /dE diffusepoint 8.1  10 -9 [cm -2 s -1 sr -1 GeV] 5.5  10 -9 [cm -2 s -1 GeV] E  < 1 PeV: focus on the Northern sky, E > 1 PeV: sensitive aperture increases with energy  full sky observations possible

29. IceTop Stations with DOMs – January 2004 digitized muon signals from DOMs Amplitude (ATWD counts) vs time (ns) power cable signal, freeze control, temperature control cables

30. 27.1, 10:08: Reached maximum depth of 2517 m, reversed direction, started to ream up 28.1, 7:00: drill head and return water pump are out of the hole, preparations for string installation start 7:52: Handover of hole for deployment 9:15: Started installation of the first DOM (DOM 60) 12:06: 10th DOM installed 22:36: 60th DOM installed Typical time for DOM installation:12 min 22:48: Start drop 29.1, 1:31: String secured at depth of 2450.80 m 20:40: First communication to DOM IceCube first string: january 2005

31. an IceCube-IceTop event deployed string AMANDA 4 IceTop stations

32. timing verification with flashers

33. Outlook.  as a framework : high energy neutrino astronomy  the world of neutrino telescopes: current projects  recent physics results from AMANDA and Baikal  ICECUBE: status and capabilities  summary

34. a wealth of physics results from the currently working neutrino telescopes on several topics sensitivity reaching the level of current predictions of production in AGN. Some models already excluded @ 90%CL first Km 3 project (IceCube) started at the South Pole: first events seen two projects + R&D efforts for a Km 3 detector in the Mediterranean summary

36. Absorption dust ice bubbles dust optical properties: data from calibration light sources deployed along the strings and from cosmic ray muons. absorption length @ 400 nm eff. Scattering length @ 400 nm 110 m20 m effective scattering length absorption length on average: detector medium: nice ice AMANDA depth

37. Preliminary source nr. of events (4 years) expected BG (4 years) time window Markarian 42165.5840 days 1ES 1959+65053.7140 days 3EG J1227+4302 64.3740 days QSO 0235+16465.0440 days Cygnus X-365.0420 days GRS 1915+10564.7620 days GRO J0422+3255.1220 days search for excesses in time-sliding windows: galactic objects: 20 days extra-galactic objects: 40 days … out of 12 Sources → no statistically significant effect observed time events sliding window search for neutrino flares without a-priori hypothesis on their time of occurrence search for neutrino flares

38. AMANDA: sensitive in very different energy regimes Energy range production site(s) MeVSupernovae GeV-TeV Atmosphere Dark matter from Sun/Earth Galactic center TeV-EeV  Quasars SN remnant AGN GRB galactic extra galactic

39. Transient Waveform Recorder system installed between the 2001 and 2004 campaigns Increased OM dynamic range x ~100 Increased 1pe detection efficiency Virtually dead-time free Manageable trigger rate: ~150 Hz (majority 18) Possibility of using software trigger Under evaluation Physics benefits: Improved angular resolution Improved energy resolution UHE/EHE physics TRANSIENT WAVEFORM RECODER UPGRADE

40. Up to 18 holes per season: Nov.: preparation Dec.: construction Jan.: construction Feb.: commissioning IceCube: time plan

41. Diffuse   sensitivityPoint source   sensitivity IceCube: sensitivities 1 year sensitivity E 2 ·d  /dE diffusepoint 8.1  10 -9 [cm -2 s -1 sr -1 GeV] 5.5  10 -9 [cm -2 s -1 GeV]

42. IceCube+AMANDA event verification of newly deployed string off-line synchronization of AMANDA and IceCube data

43. May '02 July '02June '02 Error bars: off-source background per 40 days sliding search window Preliminary Example: 1ES1959+650 “Orphan flare” (MJD 52429) POINT SOURCE SEARCH: TIME WINDOW EXCESS

44. Preliminary!... very rare - very high energy events many proposals for radio and acoustic detectors in ice, water, salt, from moon.. e.g. ice: >>km attenuation length sparse instrumentation 100-fold volume increase... or moon, ice radio emission >100 < 10 GZK neutrinos/year

45. RICEAGASA Amanda, Baikal 2002 2007 AUGER  Anita Amanda,Antares, Baikal, Nestor 2012 km 3 Auger + new techn. 2004 RICE GLUE