WIN 02 Francis Halzen

1. WIN 02Francis Halzen the sky > 10 GeV photon energy < 10-14 cm wavelength > 108 TeV particles exist Fly’s Eye/Hires they should not more/better data arrays of air Cherenkov telescopes 104 km2 air shower arrays ~ km3 neutrino detectors

2. Energy (eV) 1 TeV CMB Radio Visible GeV g-rays Flux

3. With103 TeV energy, photons do not reach us from the edge of our galaxy because of their small mean free path in the microwave background. g + gCMB e++ e-

4. n / / / / / / / / / / / / / / / / / TeV sources! cosmic rays

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

8. fluorescence from atmospheric nitrogen + _ cosmic ray + _ oe  fluorescent light electromagnetic shower

11. Acceleration to 1021eV? ~102 Joules ~ 0.01 MGUT • 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

12. Cosmic Accelerators E ~ GcBR R ~ GM/c2 magnetic field energy E ~GBM mass boost factor

13. Supernova shocks expanding in interstellar medium Crab nebula

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

15. Gamma Ray Burst

16. E > 1019 eV ? E ~ GB M > ~ quasars G@ 1 B @ 103G M @109 Msun blasars 10 neutron stars G@ 1 B @ 1012G M @ Msun black holes . . grb  102 > ~ emit highest energy g’s!

17. Particles > 1020 eV ? • not protons • cannot reach us from cosmic accelerators • lint < 50 Mpc • no diffusion in magnetic fields • doublets, triplet • not photons • g + Bearth e+ + e- not seen • showers not muon-poor • not neutrinos • snp 10-5spp no air showers

18. Interaction length of protons in microwave backgroundp + gCMBp + …. lgp =(nCMBs  ) -1 @10 Mpc p+gCMB GZK cutoff

19. Particles > 1020 eV ? new astrophysics? • not protons • cannot reach us from cosmic accelerators • lint < 50 Mpc • no diffusion in magnetic fields • doublets, triplet • not photons • g+ Bearth e+ + e- not seen • showers not muon-poor • not neutrinos • snp 10-5spp no air showers trouble for top-down scenarios snpspp with TeV - gravity unitarity?

20. _ 1024 eV = 1015 GeV ~ MGUT are cosmic rays the decay product of • topological defects? • (vibrating string, annihilating monopoles) • heavy relics? Top. Def.  X,Y  W,Z  quark + leptons  >> p  >> g • top-down spectrum • hierarchy n >>  g >> p

21. TeV-Scale Gravity Modifies PeV Neutrino Cross Sections! 103 TeV

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

23. black hole radiation enveloping black hole

26. Radiation field: Ask astronomers Produces cosmic ray beam

27. cosmic ray puzzle neutrinos protons TeV g - rays ~ 1 km3 high energy detectors ~ 104 km2 air shower arrays • atmospheric Cherenkov • space-based • AMANDA / Ice Cube • Antares, Nestor, • NEMO • Veritas, Hess, Magic … • GLAST… • Hi Res, Auger, • Airwatch, • OWL, TA… e.g. • particle physics • and cosmology • dark matter search • discovery • short-wavelength • study of supernova • remnants and galaxies also

29. 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 Cherenkov light cone muon interaction Detector • The muon radiates blue light in its wake • Optical sensors capture (and map) the light neutrino

30. Optical Module Photomultiplier: 10 inch Hamamatsu Active PMT base Glass sphere: Nautillus Mu metal magnetic shield

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

32. 3600 m 1366 m Lake Baikal, NT-200: The Site

33. Lake Baikal: atmospheric neutrinos Gold plated neutrino event, 4-string stage (1996) NT-200: zenith angle distribution 234 days in 1998/99 19 hits

34. 40Km SE Toulon Depth 2400m Shore Base La Seyne-sur-Mer ANTARES SITE 40 km Submarine cable -2400m

35. ANTARES Deployment Sites Thetys Marseille La Seyne sur Mer Toulon Existing Cable Marseille-Corsica Demonstrator Line Nov 1999- Jun 2000 42°59 N, 5°17 E Depth 1200 m New Cable (2001) La Seyne-ANTARES ANTARES 0.1km2 Site 42°50 N, 6°10 E Depth 2400 m ~ 40 deployments and recoveries of test lines for site exploration 0.1 km2 Detector with 900 Optical Modules , deployment 2002- 2004

36. ANTARES 0.1km2 Detector Shore station Optical module hydrophone Compass, tilt meter 2400m float ~60m Electro-optic submarine cable ~40km 300m active Electronics containers Readout cables ~100m Junction box anchor Acoustic beacon

37. ANTARES 0.1km2 detector

38. 1.5 km

43. Amundsen-Scott South Pole Station South Pole

44. Optical sensor The Counting House

48. AMANDA NEUTRINO SKY

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

50. Atmospheric Muons and Neutrinos