1. Collisions: Cosmic Accelerators the sky > 10 GeV photon energy the sky > 10 GeV photon energy < 10 -14 cm wavelength > 10 8 TeV particles exist > 10 8 TeV particles exist they should not they should not more/better data more/better data arrays of air Cherenkov telescopes 10 4 km 2 air shower arrays ~ km 3 neutrino detectors f.halzen

2. Energy (eV ) Radio CMB Visibe GeV  -rays 1 TeV Flux

3. TeV sources! cosmic rays //////////////////////////////////

4.  +    e + + e - With 10 3 TeV energy, photons do not reach us from the edge of our galaxy because of their small mean free path in the microwave background.

5. Cosmic Ray spectrum Atmospheric neutrinos Extragalactic flux sets scale for many Accelerator models

6. Telescope = Earth’s Atmosphere Particle initiates electromagnetic + hadronic cascade detected by: Electron/photon shower Muon component Cerenkov radiation Nitrogen fluorescence Neutrinos

9. fluorescence from atmospheric nitrogen cosmic ray fluorescent light electromagnetic shower  o     +_+_ +_+_

14. Acceleration to 10 21 eV? ~10 2 Joules ~ 0.01 M GUT dense regions with exceptional gravitational force creating relativistic flows of charged particles, e.g. annihilating black holes/neutron stars dense cores of exploding stars supermassive black holes

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

16. 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! >~ >~

17. Supernova shocks expanding in interstellar medium Crab nebula

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

19. Profile of Gamma Ray Bursts Total energy: one solar massTotal energy: one solar mass Photon energy: 0.1 MeV to TeVPhoton energy: 0.1 MeV to TeV Duration: 0.1 secs -- 20 minDuration: 0.1 secs -- 20 min Several per daySeveral per day Brightest object in the skyBrightest object in the sky Complicated temporal structure:Complicated temporal structure: no ‘typical’ burst profile

21. Gamma Ray Burst

22. Two Puzzles or One? Gamma ray burstsGamma ray bursts Source of the highest energy cosmic raysSource of the highest energy cosmic rays

23. Particles > 10 20 eV ? not protons cannot reach us from cosmic accelerators cannot reach us from cosmic accelerators int < 50 Mpc int < 50 Mpc no diffusion in magnetic fields no diffusion in magnetic fields doublets, triplet not photons  + B earth e + + e - not seen  + B earth e + + e - not seen showers not muon-poor showers not muon-poor not neutrinos  p  10 -5  pp  no air showers  p  10 -5  pp  no air showers

24. Interaction length of protons in microwave background p +  CMB  + ….   p = ( n CMB   ) -1  10 Mpc  10 Mpc p +  CMB GZK cutoff

26. Forthcoming AGASA Results The highest energy cosmic rays do come from point sources: 5 sigma correlation between directions of pairs of particles. Birth of proton astronomy!The highest energy cosmic rays do come from point sources: 5 sigma correlation between directions of pairs of particles. Birth of proton astronomy! Are the highest energy cosmic rays Fe?Are the highest energy cosmic rays Fe? GKZ cutoff at ~2 10 20 eV ? GKZ cutoff at ~2 10 20 eV ?

27. new astrophysics? trouble for top-down scenarios  p @  pp with TeV - gravity unitarity? Particles > 10 20 eV ? not protons cannot reach us from cosmic accelerators int < 50 Mpc no diffusion in magnetic fields doublets, triplet not photons  + B earth e + + e - not seen showers not muon-poor not neutrinos  p  10 -5  pp   no air showers

28. 10 24 eV = 10 15 GeV ~ M GUT topological defects (vibrating string, annihilating monopoles) heavy relics? Top. Def.  X,Y  W,Z  quark + leptons   >> p    top-down spectrum hierarchy       p are cosmic rays the decay product of _

29. The Oldest Problem in Astronomy: No accelerator No particle candidate (worse than dark matter!) Not photons (excludes extravagant particle physics ideas) What Now?

30. radiation enveloping black hole

33. cosmic ray puzzle protons TeV  - rays neutrinos ~ 10 4 km 2 air shower air shower arrays arrays e.g. also atmospheric Cherenkovatmospheric Cherenkov space-basedspace-based short-wavelengthshort-wavelength study of supernova remnants and galaxies ~ 1 km 3 high energy detectors particle physicsparticle physics and cosmology and cosmology dark matter searchdark matter search discoverydiscovery AMANDA / Ice CubeAMANDA / Ice Cube Antares, Nestor, NEMO Hi Res, Auger,Hi Res, Auger,Airwatch, OWL, TA… Veritas, Hess, Magic …Veritas, Hess, Magic … GLAST…GLAST…

34. Array => Very large effective area (10 5 m 2 ) => 3-dim shower reconstruction => Dramatic improvements in - Energy Resolution - Background Rejection

35. STACEE Solar Tower Atmospheric Cherenkov Effect Experiment Gamma-ray Astrophysics between 50-500 GeV

38. Infrequently, a cosmic neutrino is captured in the ice, i.e. the neutrino interacts with an ice nucleusInfrequently, a cosmic neutrino is captured in the ice, i.e. the neutrino interacts with an ice nucleus In the crash a muonIn the crash a muon (or electron, or tau) is produced is produced The muon radiates blue light in its wakeThe muon radiates blue light in its wake Optical sensors capture (and map) the lightOptical sensors capture (and map) the light

39. Another example: velocity muon > velocity light

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

41. ANTARES SITE 40Km SE Toulon Depth 2400m Shore Base La Seyne-sur-Mer -2400m 40 km Submarine cable

71. Atmospheric Muons and Neutrinos Lifetime: 135 days Observed Data Predicted Neutrinos Triggered1,200,000,0004574 Reconstructed upgoing 5000571 Pass Quality Cuts (Q ≥ 7) 204273

72. ...online 2001 analysis 2 recent events: October 7, 2001 October 10, 2001

73. ...online 2001 analysis  real-time filtering at Pole  real-time processing (Mainz) Left plot:  20 days (Sept/Oct 2001)  90  candidates above 100° 4.5  candidates / day atmospheric muons (data/MC normalized above 100°) atmospheric ‘s Zenith angle comparison with signal MC

75. IceCube 1400 m 2400 m AMANDA South Pole IceTop Skiway 80 Strings 4800 PMT Instrumented volume: 1 km3 (1 Gt) IceCube is designed to detect neutrinos of all flavors at energies from 10 7 eV (SN) to 10 20 eV

76. South Pole

77. Dark sector AMANDA IceCube Planned Location 1 km east Dome Skiway

78. South Pole Dark sector AMANDA IceCube Dome Skiway

79. The IceCube Collaboration Institutions: 11 US and 9 European institutions (most of them are also AMANDA member institutions) 1.Bartol Research Institute, University of Delaware 2.BUGH Wuppertal, Germany 3.Universite Libre de Bruxelles, Brussels, Belgium 4.CTSPS, Clark-Atlanta University, Atlanta USA 5.DESY-Zeuthen, Zeuthen, Germany 6.Institute for Advanced Study, Princeton, USA 7.Dept. of Technology, Kalmar University, Kalmar, Sweden 8.Lawrence Berkeley National Laboratory, Berkeley, USA 9.Department of Physics, Southern University and A\&M College, Baton Rouge, LA, USA 10.Dept. of Physics, UC Berkeley, USA 11.Institute of Physics, University of Mainz, Mainz, Germany 12.Dept. of Physics, University of Maryland, USA 13.University of Mons-Hainaut, Mons, Belgium 14.Dept. of Physics and Astronomy, University of Pennsylvania, Philadelphia, USA 15.Dept. of Astronomy, Dept. of Physics, SSEC, PSL, University of Wisconsin, Madison, USA 16.Physics Department, University of Wisconsin, River Falls, USA 17.Division of High Energy Physics, Uppsala University, Uppsala, Sweden 18.Fysikum, Stockholm University, Stockholm, Sweden 19.University of Alabama, Tuscaloosa, USA 20.Vrije Universiteit Brussel, Brussel, Belgium

81. 1 km AMANDA-II µ-event in IceCube Low Noise: ≈ 2 photoelectrons / (5000 PMT x µsec)

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

83. e + e W  +  6400 TeV

85. PeV  (300m)    decays

86. Why is Searching for ’s from GRBs of Interest? Search for vacuum oscillations (    ):Search for vacuum oscillations (    ):  m 2  10 -17 eV 2  m 2  10 -17 eV 2 Test weak equivalence principle: 10 -6Test weak equivalence principle: 10 -6 Test : 10 -16Test : 10 -16 >~ C photon - C C photon - C C C

87. the sky > 10 GeV photon energy the sky > 10 GeV photon energy < 10 -14 cm wavelength > 10 8 TeV particles exist > 10 8 TeV particles exist Fly’s Eye/Hires they should not they should not more/better data more/better data arrays of air Cherenkov telescopes 10 4 km 2 air shower arrays ~ km 3 neutrino detectors Summary

88. TeV sources! cosmic rays //////////////////////////////////

91. A few more results … Gamma Ray Bursts (GRBs) –Observation of single 3  excess (GRB 970417a) within 1997 BATSE trigger. Flux limit for unidentified TeV point sources –For E spectrum Flux (>1 TeV) < 2 – 30 x 10 -7 cm -2 s -1 @ 90% /  = 1 However,  spectrum probably softer due to reprocessing (core) and absorption in photon BG AMANDA II will probe this flux for