1. first-generation neutrino telescopes

2. neutrino muon or tau Cerenkov light cone Detector interaction Infrequently, a cosmic neutrino is captured in the ice, i.e. the neutrino interacts with an ice nucleus The muon radiates blue light in its wake In the crash a muon (or electron, or tau) is produced Optical sensors capture (and map) the light

3. Optical Module

4. size perspective 50 m

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

6. South Pole AMANDA– 1 mile deep

7. Building AMANDA Drilling Holes with Hot Water The Optical Module

8. Christchurch, New Zealand Christchurch, New Zealand International Antarctic Center

9. Logistics simple!

10. thedome the dome the new station

11. Hot water drilling

13. McMurdo, Antarctica

15. LC-130 Hercules

19. Building AMANDA

24. AMANDA II up-going muon up-going muon 61 modules hit 61 modules hit ti ttiimemettiimeme size ~ size ~ number of photons number of photons > 4 neutrinos/day on-line on-line

25. AMANDA Event Signatures: Muons  + N   +X  + N   + X CC muon neutrino Interaction  track  track

26. two events 200 TeV e

27. event reconstruction Maximum Likelihood methodMaximum Likelihood method Take into account time profiles of expected photon flight timesTake into account time profiles of expected photon flight times Bayesian approach - use prior knowledge of expected backgrounds and signalsBayesian approach - use prior knowledge of expected backgrounds and signals

28. Quality parameters: Example 1: The track length Short track length = more likely to be background

29. Quality parameters: Example 2: The smoothness The smoothness is a measure of how regular the photon density is distributed along the track. A well reconstructed muon track is more likely to have a high smoothness. High Low

30. Quality parameters: Example 3: The angular difference between 2 fits A well reconstructed event has better agreement between a simple fit and a full likelihood reconstruction.

31. Quality Parameters LikelihoodLikelihood Zenith angle mismatch between two types of fits.Zenith angle mismatch between two types of fits. Sphericity of Hits (Brem?)Sphericity of Hits (Brem?) Track Length (is an energy cut, too)Track Length (is an energy cut, too) Smoothness of hits along the trackSmoothness of hits along the track Number of unscattered photonsNumber of unscattered photons Combine 6 to a single event quality parameter.Combine 6 to a single event quality parameter. Only 3 for completed detector!Only 3 for completed detector!

32. quality cut

33. Atmospheric muons and neutrinos Atm. Neutrinos (  ): 60/day Atm. Muons: 8.6*10 6 /day Lifetime: 135 days Observed DataPred. Neutrinos Triggered1,200,000,0004574 Reconstructed upgoing 5000571 Pass Cuts (Q ≥ 7)204273

34. Atmospheric Neutrinos, 97 data vertically uphorizontally  AMANDA sensitivity understood down to normalization factor of ~ 40% (modeling of ice...) ~ 300 events

35. Understanding Ice and Calibrating AMANDA In situ light sourcesIn situ light sources –Ice properties –Relative PMT timing, gain –Response to electromagnetic showers –crosstalk Downgoing cosmic-ray muonsDowngoing cosmic-ray muons –Relative PMT timing, gain AMANDA-SPASE coincidencesAMANDA-SPASE coincidences –Directionality –Ice properties Atmospheric neutrinosAtmospheric neutrinos –Full detector response

36. Amanda: time delay due to scattering 3 50 200 400 700 6 m 17 m d=32 m delay, nsec d muon 

37. Ice Properties Most challenging initial problems now understood using in situ lasers and LEDsMost challenging initial problems now understood using in situ lasers and LEDs –Disappearance of bubbles –Mapping of dust layers scatter : 6 m - 52 m scatter : 6 m - 52 m abs : 9 m - 240 m abs : 9 m - 240 m

41. AMANDA Is Working Well: 4 nus per day! Sensitivity to up-going muons demonstrated with CC atm. n m interactions: Sensitivity to cascades demonstrated with in-situ sources (see figs.) & down- going muon brems. In-situ light sourceSimulated light source AMANDA also works well with SPASE: AMANDA also works well with SPASE: Calibrate AMANDA angular response Calibrate AMANDA angular response Do cosmic ray composition studies. Do cosmic ray composition studies. HorizontalUp-going MC Data 290 atm.  candidates (2000 data) Zenith

42. 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)]

43. AMANDA-II Antarctic Muon And Neutrino Detector Array Construction began in 1995 (4 strings)Construction began in 1995 (4 strings) AMANDA-II completed in 2000 (19 strings total)AMANDA-II completed in 2000 (19 strings total) 677 optical modules677 optical modules 200 m across200 m across ~500 m tall (most densely instrumented volume)~500 m tall (most densely instrumented volume)

44. The AMANDA detector Construction began in 1995 (4 strings)Construction began in 1995 (4 strings) AMANDA-II completed in 2000 (19 strings total)AMANDA-II completed in 2000 (19 strings total) 677 optical modules677 optical modules 200 m across200 m across ~500 m tall (most densely instrumented volume)~500 m tall (most densely instrumented volume)

45. Slant Depth 1730m 8650m 1 2 3 4 5 6 7 8 Slant Depth Binning  zenith angle cos θ

46. Required background rejection Signature Signature Neutrino signal / Neutrino signal / cosmic muon bkg cosmic muon bkg Diffuse flux Diffuse flux ~10 -8 ~10 -8 Point source Point source > 10 -6 > 10 -6 Gamma ray burst Gamma ray burst > 10 -4 > 10 -4

47. 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

48. Down-going Muon Flux Down-going Muon Flux zenith angle zenith angle depth depth

49. Atmospheric  ’s as Test Beam Neutrino energy in GeV

50. 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

51. Atmospheric  ’s as Test Beam Selection Criteria:Selection Criteria: –(N hit < 50 only) –Zenith > 110 o –High fit quality –Uniform light deposition along track Excellent shape agreement!Excellent shape agreement! –Less work to obtain than with A-B10 a. b. c.d. Gradual tightening of cuts extracts atm. signal MCData 290 events 2 cuts only! 2 cuts only! > 4 nus per day

52. Log neutrino energy in GeV AMANDA Energy Measurement from muon’s catastrophic energy loss: 0.3 log E

53. 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

54. South Pole Dark sector AMANDA IceCube Dome Skiway South Pole Air Shower Experiment (SPASE) AMANDA-II: 200 x 500 cylinder + 3 1km strings, running since 2000

55. 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)

56. 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

57. 1 km 2 km SPASE air shower array Cosmic ray composition preliminary

58. Relativistic Magnetic Monopoles 10 -16 10 -15 10 -14 10 -18 10 -17  = v/c 1.000.750.50 upper limit (cm -2 s -1 sr -1 ) C - light output  n 2 ·(g/e) 2 n 2 ·(g/e) 2 n = 1.33 (g/e) = 137 / 2  8300 KGF Soudan MACRO Orito Baikal Amanda IceCube  electrons

59. Excess of cosmic neutrinos? Electron + tau (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) cuts determined by MC – blind analyses !

60. 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) cuts determined by MC – blind analyses !

61. 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.

62. Effective Volume for e,  and 

63. 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

64. 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!

65. neutrinos associated with the source of the cosmic rays? AMANDA II sensitivity (00-03) sensitivity (00-03)

66. theoretical bounds and future atmospheric  W&B MPR DUMAND test string FREJUS NT-200 MACRO  NT-200+ AMANDA-II 5 years IceCube AMANDA-97 AMANDA-00 100 days opaque for neutrons Mannheim, Protheroe and Rachen (2000) – Waxman, Bahcall (1999)  derived from known limits on extragalactic protons +  -ray flux neutrons can escape

67. Excess of cosmic neutrinos? Electron + tau (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) cuts determined by MC – blind analyses !

68. Ultra High Energy Neutrinos in AMANDA Energy > 10 PeV Energy > 10 PeV All sky All sky Large neutrino cross sections Large neutrino cross sections Large muon range (> 10 km)Large muon range (> 10 km) Competitive with radio, acoustic and air shower experiments

69. diffuse EHE neutrino flux limits a)Stecker & Salamon (AGN) b)Protheroe (AGN) c)Mannheim (AGN) d)Protheroe & Stanev (TD) e)Engel, Seckel & Stanev Ranges are central 80% AMANDA AMANDA Sensitivity (00-03)

70. Raffelt astro-ph/0303210 ! Supernova Monitor Amanda-II Amanda-B10 IceCube B10: 60% of Galaxy A-II: 95% of Galaxy IceCube: up to LMC 0 5 10 sec Count rates

71.  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 Search for excess events in sky bins for up-going tracks talk HE 2.3-5 no clustering observed - no evidence for extraterrestrial neutrinos...

72. 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

73. -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

74. GRB 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

77. 90% upper limits calculated using background levels predicted from data “neutrino = gamma” sensitivity 0.04 km 2 area above 10 TeV 3.12.5Cygnus X-3 0.8SS 433 1.00.7Cas-A 2.1 Crab 1.51.3Markarian 501 3.02.6Markarian 421  (10 -8 GeVcm -2 s -1 ) muon (  10 -15 cm -2 s -1) Source\90% limit Point Sources Amanda II (2000) 0.6

78. Point source search 2000 AMANDA-II Cuts optimized for each declination bandCuts optimized for each declination band Analysis developed with azimuth- scrambled data for blindnessAnalysis developed with azimuth- scrambled data for blindness 40,000 m 2 area above 10 TeV40,000 m 2 area above 10 TeV 2000 data: Contamination by cosmic ray muons: <10% (above 110 degrees)

79. AMANDA II 2000

81. Declination RA(hours) 64 21 64 21 40 21 40 21 20 9 20 9

82. increasing energy

84. AMANDA II

85. 

86.  -rays from  0 decay? E N (E ) =  E  N  (E  ) 1 <  < 8 transparentsource  0 =  + =   0 =  + =  - accelerator beam dump (hidden source) flux predictedObserved  -ray flux flux predictedObserved  -ray flux 20 km -2 yr -1 Crab sn remnant 35 km -2 in 97Markarian 501 (9 for p  )

87.  ~ 

88. -90 0-45 9045 10 -15 10 -14 muons/cm 2 s 1 10 -17 10 -16 published data preliminary 2000 data Integrated AMANDA + IceCube fluency ~2007 Integrated AMANDA + IceCube fluency ~2007 All sky > PeV All sky > PeV 1 km 3 Expected source sensitivity GX 339-4 SS-433 MACRO (8 year) N Antares (2007) AMANDA 137 days declination (degrees) S Mark. 501 Crab

89. AMANDA II Antares

90. AMANDA-IIANTARES ICEWATER # OF PMTS 600 / 8 INCH 900 / 10 INCH TRANSMISSIONANALOGEDIGITAL HE POINT- SOURCE AREA *40,000 m 2 After all cuts * After all cuts

91. AMANDA-IIANTARES ICEWATER # OF PMTS 600 / 8 INCH 900 / 10 INCH point source Sensitivity* 2.3** in 200 days 1.2** in 1 year diffuse limit*** 3 in 100 days 1.0 in 1 year *After all cuts and including angular resolution:   lim (10 -15 cm -2 s -1 )   lim (10 -15 cm -2 s -1 ) ** averaged over declination *** units 10 -7 GeV cm -2 s -1 sr -1 (~2 x Waxman-Bahcall)

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

93. Optical Cerenkov Neutrino Telescope Projects NESTOR Pylos, Greece ANTARES La-Seyne-sur-Mer, France BAIKAL Russia DUMAND Hawaii Hawaii (cancelled 1995) (cancelled 1995) AMANDA, South Pole, Antarctica NEMO Catania, Italy