Exploring Cosmic Accelerators and High-Energy Phenomena in the Universe

1. Collisions: Cosmic Accelerators the sky > 10 GeV photon energy < 10-14 cm wavelength > 108 TeV particles exist they should not more/better data arrays of air Cherenkov telescopes 104 km2 air shower arrays ~ km3 neutrino detectors f.halzen

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

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

4. 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 + g e++ e-

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

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

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

14. 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

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

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. Supernova shocks expanding in interstellar medium Crab nebula

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

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

21. Gamma Ray Burst

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

23. 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

24. Interaction length of protons in microwave backgroundp + gCMBp + …. lgp = (nCMBs  ) -1 @10 Mpc p+gCMB 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! • Are the highest energy cosmic rays Fe? GKZ cutoff at ~2 1020 eV ?

27. 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?

28. _ 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

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. black hole radiation enveloping black hole

33. 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

34. Array => Very large effective area (105 m2) => 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 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

39. Another example:velocity muon > velocity light

40. 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

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