1. Large Area Telescopes Cosmic Rays – Gamma Rays – Neutrinos P.Kooijman

2. What do we want to learn? High energy Cosmic Rays A.What are they? B.Where are they accelerated? C.How are they accelerated?

3. How do we try to answer the questions? Measurements of Cosmic rays themselves – What are they Measurements of the interaction products – Whence do they come Gamma Rays Neutrinos

4. Possible sources Up to 1000 TeV sources are expected to be Galactic SuperNova Remnants Above 10 6 TeV Active Galactic Nuclei Gamma Ray Bursts SNR AGN GRB

5. Shockwave acceleration Acceleration by transfer of energy from large clouds of plasma to a few particles Matter is required for the acceleration  interactions Hadronic interaction Photo-hadron interaction Inverse Compton scattering Of course: Linked by isospin rules

6. Present status CR  PA Accelerators running out of steam? Steepening of spectrum Heavier Nuclei in spectrum GZK?? At highest energies the 1 nT Galactic fields give about 3-5 degrees smearing

7. Present status Gamma-Rays  HESS, FermiLAT Many Sources of high energy gammas now identified (mostly in Galaxy) SNR and PWN Some sources look hadronic others IC most undecided

8. Neutrinos  IceCube No Sources but IceCube looks away from Galaxy TeV gammas not likely  pointing speed

9. Where to go from here? Have to increase sensitivity Neutrinos Gamma Rays HESS, Magic  CTA, HAWC, TAA IceCube  KM3NeT Enlarge size  higher energy Change size of mirror  energy threshold Stay Southern Hemisphere  Galaxy HAWC  All sky search Enlarge size  4-5 times IceCube Seawater  2 times better resolution Northern Hemisphere  close by gamma sources that are good candidates

10. Expectation CTA: 1000 high energy sources Higher counting rate per source Lower threshold gives better discrimination hadronic/leptonic Systematic studies KM3NeT: First observation of neutrino source (5  in 5 years) Start of neutrino astronomy

11. What about Extra-Galactic? GC – 8.5 kpc Andromeda – 0.7 Mpc Virgo – 20 Mpc (2000 Galaxies) Same signal  Source more intense by 10 6

12. What about Extra-Galactic? Neutrinos concentrate on higher energies: Background low Resolution factor 5 better  25 times more sensitive Need high intensity (AGN) Gamma Ray Bursts (super high intensity; no background; need some luck i.e. close but not too)

13. Times CTA start construction 2015-2016 finished 2020 KM3NeT start construction 2013 finished 2018 HAWC being built

14. KM3NeT

15. KM3NeT first halfheight “IceCubes” 1250m

16. CTA Go high or make large area mirrors low energi Large area high energi Many pixels Better angular resolution

17. HAWC High altitude Water Cherenkov detector MILAGRO (Pre-HAWC)

18. Other Physics Dark Matter annihilation Gamma Neutrino GZK Cosmic Rays Neutrinos Supernovas Neutrinos – IceCube upgrade