1. Lepton - Photon 01 Francis Halzen the sky 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

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.

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

12. 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

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

14. 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. 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

19. 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 AMANDA II will probe this flux for Flux (>1 TeV) < 2 – 30 x 10 -7 cm -2 s -1 @ 90% However,  spectrum probably softer due to reprocessing (core) and absorption in photon BG /  = 1 /  = 1

20. 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

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

23. 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 ?

24. 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

25. 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 _

26. radiation enveloping black hole

29. 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…

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

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

41. e + e W  +  6400 TeV

43. PeV  (300m)    decays

44. 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

45. Lepton - Photon 01 Francis Halzen the sky 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

46. TeV sources! cosmic rays //////////////////////////////////