1. Icefishing for… Icefishing for… Neutrinos Neutrinos Francis Halzen University of Wisconsin http://icecube.wisc.edu

2. seeing

3. Seeing: Cosmic Messengers light ( Alhassan 1000 )light ( Alhassan 1000 ) light of other wavelengths:light of other wavelengths: blue, red, infrared, X-rays, radiowaves,…. blue, red, infrared, X-rays, radiowaves,….

4. Supernova shocks expanding in interstellar medium Crab nebula

5. X-ray picture Infrared picture

7. Cosmic Accelerators High Energy large magnetic field large magnetic field over large distances over large distances cfr Fermilab requires many Tesla (~10 Tesla) many kilometers (~4 km)

8. Cosmic Accelerators E ~  BM energy magnetic field boost factor mass E ~  cBR R ~ GM/c 2

9. E ~  B M quasars   1 B  10 3 G M  10 9 M sunquasars   1 B  10 3 G M  10 9 M sun blasars 10blasars 10 neutron stars   1 B  10 12 G M  M sunneutron stars   1 B  10 12 G M  M sun black holes black holes.. grb  10 2grb  10 2 E > 10 19 eV ? emit highest energy  ’s! >~ >~

10. Crab nebula Supernova shocks expanding in interstellar medium

11. Active Galaxies: Jets VLA image of Cygnus A 20 TeV gamma rays Higher energies obscured by IR light

12. GammaRayBurst

14. 1 pc ~ 3 ly ~ 10 18 cm 1000 Mpc 100 Mpc 10 Mpc 1 Mpc 100 kpc 10 kpc 1 kpc 0.1 kpc gamma ray bursts closest active galaxies local supecluster Virgo halo center of galaxy galaxy (scale height)

15. Seeing: Cosmic Messengers light ( Alhassan 1000 )light ( Alhassan 1000 ) light of other wavelengths:light of other wavelengths: blue, red, infrared, X-rays, radiowaves… blue, red, infrared, X-rays, radiowaves… Neutrinos instead of photons (particles of light)Neutrinos instead of photons (particles of light)

18. New Window on Universe? Expect Surprises New Window on Universe? Expect Surprises

19. the science: a sampler Source(s) of cosmic rays Source(s) of cosmic rays: gamma-ray bursts, active galaxies, cosmological remnants…? Dark matter More

20. A particle that is almost nothing may tell us everything about the Universe. Christine Sutton, in Spaceship Neutrino

21. You can see a lot by looking. Yogi Berra

22. How large a neutrino telescope?

23. Kilometer-scale neutrino detectors? How? How?

24. I have done a terrible thing, I have invented a particle that cannot be detected. Wolfgang Pauli

25. 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

26. Optical Module

27. How to build a detector Use the phenomenon of Cherenkov light

28. Copyright © 2001 Purdue University

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

30. South Pole AMANDA– 1 mile deep

31. Size perspective 50 m

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

33. A real event in AMANDA Recorded on May 1, 2003 (demonstrating “daily nu” realtime filtering)Recorded on May 1, 2003 (demonstrating “daily nu” realtime filtering) time time

34. seeing with neutrinos

35. Neutrino sky seen by AMANDA Monte Carlo methods verified on dataMonte Carlo methods verified on data ~ 300 neutrinos from 130 days of B-10 operation (~ 300 neutrinos from 130 days of B-10 operation ( Nature 410, 441, 2001) Cos  events

36. AMANDA II 2000 1555 events

37. AMANDA II 2000 1555 events

38. The Challenge is Technological Needle in a haystack: have to find each neutrino in a background of more than one million background eventsNeedle in a haystack: have to find each neutrino in a background of more than one million background events Do this at a rate of 100 muons per secondDo this at a rate of 100 muons per second Deploy a particle physics detector in a hostile environmentDeploy a particle physics detector in a hostile environment Solutions demonstrated with AMANDASolutions demonstrated with AMANDA

39. We were lucky! Light travels more than 100 meters in the ultra-pure, sterile iceLight travels more than 100 meters in the ultra-pure, sterile ice Scattering of the light is manageableScattering of the light is manageable We use the existing infrastructure of the National Science Foundation’s South Pole Research StationWe use the existing infrastructure of the National Science Foundation’s South Pole Research Station Makes the construction of the ultimate kilometer - scale neutrino observatory possibleMakes the construction of the ultimate kilometer - scale neutrino observatory possible

40. Ignorance and luck represent a powerful mix fostering original research. Wisconsin Research Profiles in Discovery Yes, it was me.

42. Science!

43. 1 km 2 km 1 km deep and shallow ice for future IceCube for future IceCube IceCube 0.02 0.1 0.5Scatteringcoefficient(1/m) vs. depth

44. Education and Outreach Astronomy in the Ice Astronomy in the Ice to Science in the Ice – Partner with NSF MSP SCALE project to bring Polar Science to nearly 1 million mostly underrepresented K-12 students LA Denver Madison Providence One time events to multi-media resources One time events to multi-media resources – Use Exploratorium “Origins” project, NSF’s eTeach & National Science Digital Library to produce & distribute interactive, engaging resources Math Science Partnership Collaborative Proposal Math Science Partnership Collaborative Proposal – Build on Hands-on Universe model to provide student access to high energy cosmic ray and neutrino data

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

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

48. McMurdo, Antarctica

50. LC-130 Hercules

51. thedome the dome the new station

56. Building AMANDA

62. Is ice the solution, really…?

64. Assessment: The planned IceCube experiment can open a new window on the Universe by detecting very high energy neutrinos from objects across the Universe. The science is well motivated and exciting, the detection technique is proven, and the experiment appears ready for construction. Neutrinos and Beyond: New Windows on Nature

65. South Pole Dark sector AMANDA IceCube Planned Location 1 km east Dome Skiway

66. South Pole Dark sector AMANDA IceCube Dome Skiway

67. Assembled DOM

69. The IceCube Collaboration (1) Bartol Research Institute, University of Delaware, Newark, DE 19716, USA (2) Fachbereich 8 Physik, BUGH Wuppertal, D-42097 Wuppertal, Germany (3) Universite Libre de Bruxelles, Science Faculty CP230, Boulevard du Triomphe, B-1050 Brussels, Belgium (4) CTSPS, Clark-Atlanta University, Atlanta, GA 30314, USA (5) Dept. of Physics, Chiba University, Chiba 263-8522 Japan (6) DESY-Zeuthen, D-15738 Zeuthen, Germany (7) Blackett Laboratory, Imperial College, London SW7 2BW, UK (8) Institute for Advanced Study, Princeton, NJ 08540, USA (9) Dept. of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USA (10) Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA (11) Dept. of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802, USA (12) Dept. of Physics, Pennsylvania State University, University Park, PA 16802, USA (13) Dept. of Physics, Southern University, Baton Rouge, LA 70813, USA (14) Dept. of Physics, University of California, Berkeley, CA 94720, USA (15) Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany (16) Dept. of Physics, University of Maryland, College Park, MD 20742, USA (17) University of Mons-Hainaut, 7000 Mons, Belgium (18) Departamento de Fisica, Universidad Simon Bolvar, Caracas, 1080, Venezuela (19) Dept. of Astronomy, University of Wisconsin, Madison, WI 53706, USA (20) Dept. of Physics, University of Wisconsin, Madison, WI 53706, USA (21) SSEC and PSL, University of Wisconsin, Madison, WI 53706, USA (22) Physics Dept., University of Wisconsin, River Falls, WI 54022, USA (23) Division of High Energy Physics, Uppsala University, S-75121 Uppsala, Sweden (24) Faculty of Physics and Astronomy, Utrecht University, NL-3584 CC Utrecht, The Netherlands (25) Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden (26) Vrije Universiteit Brussel, Dienst ELEM, B-1050 Brussels, Belgium

70. The scientists are naïve and arrogant. They can get tangled up in their own underwear faster than anybody. Anthoni Fragomeni COBE observatory manager

71. AMANDA Drilling education

72. IceCube start 02 start 02 first strings 04 first strings 04 completed <09 completed <09

73. first 8 strings

74. The sole purpose of human existence is to kindle a light in the darkness of mere being. Carl Gustav Young

75. The End

76. Aurora Australis

77. IceCube 1400 m 2400 m AMANDA South Pole IceTopRunway 80 Strings80 Strings 4800 PMT4800 PMT Instrumented volume: 1 km3Instrumented volume: 1 km3 (1 Gton) (1 Gton) IceCube is designed to detect neutrinos of all flavors at energies from 10 7 eV (SN) to 10 20 eVIceCube is designed to detect neutrinos of all flavors at energies from 10 7 eV (SN) to 10 20 eV

78. 1 km AMANDA II µ-event in IceCube 300 atmospheric neutrinos per day IceCube : -> Larger telescope -> Larger telescope -> Superior detector -> Superior detector

79. E µ = 10 TeVE µ = 6 PeV Muon Events Measure energy by counting the number of fired PMT. (This is a very simple but robust method)

80. The effort to understand the Universe is one of the very few things that lifts human life above the level of farce and gives it some of the grace of tragedy Steve Weinberg

81. 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)

82. The effort to understand the Universe is one of the very few things that lifts human life above the level of farce and gives it some of the grace of tragedy Steve Weinberg

83. Blue glow of the particle (produced by the neutrino at locations removed by up to 10 kilometers) lights up the (produced by the neutrino at locations removed by up to 10 kilometers) lights up the sensors in the ice sensors in the ice

84. DAQ, Online filter Raw: ~4 MB/s Reconstructed: 100 GB/day  Tape Filtered: 10GB/day  Satellite Data Rates

85. How large a neutrino telescope? 1 neutrino per lifetime (30,000 days) in our body (100 kg or 0.1 m 3 ) means1 neutrino per lifetime (30,000 days) in our body (100 kg or 0.1 m 3 ) means 0.00003 per day in 0.1 m 3 or 0.00003 per day in 0.1 m 3 or 3 per day in 100,000 m 3 ( roughly SuperK with 3 per day in 100,000 m 3 ( roughly SuperK with 40x40x40 m 3 ) or 40x40x40 m 3 ) or 300,000 per day in 10 9 m 3 or 1 km 3 300,000 per day in 10 9 m 3 or 1 km 3

86. IceCube

87. Classroom visits – sharing the excitement, technology, and science

88. IceCube is part of the HEPAP “Roadmap to Particle Physics”. “Roadmap to Particle Physics”. It is the only university based project. project.

89. AMANDA II upgoing muonupgoing muon 61 modules 61 modules ti ttiimemettiimeme size ~ size ~ number of photons number of photons 4~5 neutrinos/day on-line on-line

90. AMANDA II upgoing muonupgoing muon 61 modules 61 modules ti ttiimemettiimeme size ~ size ~ number of photons number of photons 4~5 neutrinos/day on-line on-line

91. Neutrino Event Neutrino Event detected detected October 26, 02 October 26, 02

92. 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 25,000 m 2 area above 10 TeV25,000 m 2 area above 10 TeV 2000 data: Contamination by cosmic ray muons: <10% (above 110 degrees)

93. AMANDA, South Pole

95. ENGINEERING AND INSTRUMENTATION - UNIVERSITY OF WISCONSIN MADISON Hose Winch for the Ice Cube Project

96. Receiving drum weldment

97. How to build a neutrino detector Look for the neutrino’s interaction product (e, ,  )Look for the neutrino’s interaction product (e, ,  ) Use the earth as a filterUse the earth as a filter 1:10,000,0001:10,000,000 background rejection! EarthDetector cosmic ray 