3. Large Magellanic Cloud, 1987 (51.4 kparsec) SN 1987a after before 2006 Hubble

4. Precursor of Superkamiokande H2OH2O

5. 8 more events in IMB

7. Crab, 1054 About 1 SN every 30 years in our galaxy Einstein satellite (X)

10. Where does the acceleration take place? Cosmic rays

11. Look for the neutrals, not deflected in B fields, to identify, the sites of acceleration HE gamma and neutrino astronomy  : created by synchrotronstrahlung, decay from decay: or very high energy charged particles Candidates: Fermi (SN remnants…) AGN, pulsars, …

12. From a presentation by: Paul Mantsch Auger Project Manger Building the Pierre Auger Observatory (Argentina)

13. Adventures in Cosmic Ray Physics

14. The Design

15. The Observatory Plan Surface Array 1600 detector stations 1.5 km spacing 3000 km 2 Fluorescence Detectors 4 Telescope enclosures 6 Telescopes per enclosure 24 Telescopes total

16. The Surface Array Detector Station Communications antenna Electronics enclosure 3 – nine inch photomultiplier tubes Solar panels Plastic tank with 12 tons of water Battery box GPS antenna

19. EGRET on Compton Gamma Ray Observatory (NASA) Galactic view

21. Active Galactic Nucleus (AGN) Matter accreting on supermassive black hole at center of galaxy

22. Gamma ray burst (GRB) must be « small » size sources

23. Microquasar: binary systems with a black hole

24. Ground based: look for electromagnetic shower induced in the upper atmosphere, measure Cerenkov light E>10 GeV HESS in Namibia (others: MAGIC in Mallorca, future (CTA))

25.  shower hadron shower

26. HESS, stereoscopic view

29. Look for upward going muons

30. Neutrino astronomy principles  

32. Antares Mediterranean, off Toulon, 3000 m deep, 0.1 km 2 Cerenkov light

34. t height Downward going muon

35. Antares, 0.1 km 2 at the bottom of the Mediterreanean (3000 m deep), Starting to take data But: needs 1 km 3 !!!