Summary Talk at VI Rencontre du Vietnam Challenges in ParticleAstroPhysics

1. Summary Talk atVI Rencontre du VietnamChallenges in ParticleAstroPhysics Hinrich Meyer Univ. of Wuppertal and DESY

2. Overview of talks UHECR 7 VHEGR 2 CMB 4 DE, DM 5 GRW 5 Neutrino 14 And 4 parallel sessions on one afternoon 37

3. Please accept my apologies if you do not find your beautiful and important work properly represented in my talk. There have been about 2000 pictures shown in the talks at this meeting. And, the results and presentations have been of such high quality that many (most) of us were keen not to miss one the talks.

4. In the last 10 years or so there have been several great advances in particle-astrophysics just when a rather complete picture of the Standard Model of particle physics was found. Keynote talk by John Ellis

5. The fundamental interactions Gravitation electromagnetism weak nuclear force strong nuclear force The ‘Standard Model’ = Cosmic DNA The matter particles

6. Where do the masses come from ? photon 0 W + Z 0 W - + 1 0 - 1 Some particles have mass, some do not Newton: Weight proportional to Mass Einstein: Energy related to Mass Neither explained origin of Mass Mass 0 Mass 80.419 91.188 80.419 Are masses due to Higgs boson? (yet another particle)

7. Neutrino oscillations have been discovered in studies of neutrinos from the SUN, the earth atmosphere,from reactors and particle accelerators. Extensive studies of the CMB have revealed a flat universe and supported by SN1A observations a content of the universe dominated by dark energy and dark matter, and not by ordinary baryonic matter.

8. CR-experiments have revealed more than 40 TeV gamma ray sources both of galactic and extragalactic origin of (at least) five different kinds. Searches for gravitational waves have reached a new quality with 3 LIGO, GEO600 and VIRGO taking data in a regular search mode. Searches for diffuse SN Neutrinos and for diffuse infrared photons have produced interesting limits also for astronomers

9. Further developments in the field is driven by these successes and most important by very basic questions and problems formulated long ago by great scientists of the past. To name a few….. Max Planck, 1899 Victor Hess, 1912 Albert Einstein, 1916 Wolfgang Pauli, 1930 Fritz Zwicky, 1933 Ettore Majorana,1937 Peter Higgs, 1962 Greisen, Zatsepin and Kuzmin, 1966 Andre Sakharov,1968 Bruno Pontecorvo, 1968

10. Upper end of the CR-spectrum

11. Is there a cutof in the all-particle CR-spectrum?? Protons? > 50 Mpc isotropically ?? Protons producing Pions colliding with the CMB photons Dip due pair production ? Rubakov at Moscow summary

12. Overview of detection methods for UHE showers

14. Fluorescence Detectors: 11000 PMTs Surface Detectors: 1600 Cherenkov tanks (spacing 1.5 km) • 3000 km2 covered The Pierre Auger Observatory

15. The radiowaves generated by particle showers in matter area new and very promising means to detect Cosmic Rays Askarian 1962!! Geo-synchrotron Effect in earth Mag.field

17. NuMoon Experiment @ WRST Use Westerbork radio observatory Using “Askarian” to detect Neutrino-showers emerging

18. High energy Neutrinos

19. The South Pole NSF NSF NSF NSF

20. Circum polar flights with balloons (40 days)

21. Flux of Neutrinos is dropping off faster than acceptance can be provided by the experiments

23. Dark Matter

24. Events rate comparison : Lensing Galactic-Galactic stars: gal-gal 2.0 10-6 Lensing LMC-Galactic stars: LMC-gal 0.01 10-6 Full Macho Halo: LMC 0.45 10-6 SMC 0.65 10-6 (MACHO 0.12 10-6) Self lensing: LMC-LMC 0.005 - 0.05 10-6 SMC-SMC 0.04 10-6

25. Final EROS combined limit (1990-2003) _3% at 10-2M Domain excluded from all EROS data _7% at 0.4 M _10% at 1 M ZOOM LMC data set / No event LMC + SMC data set with 1 SMC halo candidate

26. Alternative gravitational theories compared to cold dark matter LCDM TeVeS-MOND • Tides/vertical force • Rot. curves HSB/LSB • Lensing by Ellip/Cluster • Hubble Expansion/CMB Stay Tuned!

27. Dwarf spheroidal galaxies M/L ranges from 1 to 3000!! 12 have been analysed sofar, 5 more newly discovered But all seem to have 4x10e7 solar mass DM!!! No tidal effects apparent, no r-cut found sofar Very enigmatic MOND etc. fail

28. PMTs PEEK Supports Grids Waveshifter/Reflector Cathode Natural WIMP candidate: SUSY LSP neutralino • Stable if SUSY exists and R-parity is conserved • Direct detection: • WIMP scattering off nuclei gaugino fraction:

29. Gravitational Waves

30. Noise Sources in LIGO Ground motion couples into motion of mirrors Thermal excitations of mirror suspensions Counting statistics of photons at photodiode

31. -18 10 -19 10 -20 10 -21 10 -22 10 -23 10 -24 10 4 1 10 100 1000 10 Design sensitivity h (Hz-1/2) Credit: P.Rapagnani Pulsars hmax – 1 yr integration LIGO Virgo Resonant antennas GEO BH-BH Merger Oscillations @ 100 Mpc Core Collapse QNM from BH Collisions, @ 10 Mpc QNM from BH Collisions, 100 - 10 Msun, 150 Mpc 1000 - 100 Msun, z=1 BH-BH Inspiral, 100 Mpc NS-NS Merger Oscillations @ 100 Mpc BH-BH Inspiral, z = 0.4 -6 e NS, =10 , 10 kpc NS-NS Inspiral, 300 Mpc Hz

32. Measured sensitivity (7 W) (7 W) (7 W) (7 W) (0.7 W) (0.7 W) (0.7 W) C7 NS/NS maximum distance ~ 1.5 Mpc Design NS/NS maximum distance ~ 30 Mpc

33. Low energy neutrinos

34. Neutrinos will have (already) a very complicated phenomenology!!!! There is a problem of mass

35. 3 twin reactors 4 underground Tunnels Large multinational collaboration Great attack on theta 13

36. Recent Advances In BKG Reduction For 2beta decay Experiments About factor 100000!! Arrays are the future

37. Moore’s sensitivity law ? • Rapid evolution of sensitivity of discriminating experiments(CDMS, EDELWEISS, CRESST, WARP, XENON…) • But goals are still ≈3 orders of magnitude beyond present best performances (After Gaitskell)

38. TeV photons

39. MAGIC-II MAGIC-I • 5. MAGIC-II [Teshima] • New 17m telescope. • Possible high-QE camera. • 2007 schedule. 85m OG 2.7: New Experiments • 4. HESS-II [Vincent] • New 28m telescope. • 2048 pixel camera. • Lower energy 40-50 GeV. Cherenkov Telescopes

42. Field of view [π sr] Field of view [deg] Collecting Area [km2] Future ConceptsLarge Cherenkov Tel. Arrays Also, detailed work in Europe and Japan. Cherenkov Telescope Array (CTA) concept well underway. HE-ASTRO: 217 Telescopes (ø10m), 80m separation. 1.1 km2 collection area & 15o FOV !

43. Universal Photon Flux • HESS, Magic • Result • Using • Distant • BLASARS • At TeV

44. Early Universe

45. At t = 400 000 yrs, the Universe becomes transparent: photons no longer interact with matter Looking back to the primordial Universe BIG BANG Cosmological background T = 3 K = - 270 °C WMAP satellite

46. 4He synthesis Light element production , the first three minutes Since the baryon/photon ratio is so well fixed How about 4He, 3He, 2H, and 7Li ??? Diffusion plus turbulent mixture in old stars may solve the long standing 7Li problem!!

48. Max Planck

49. When do graviton decouple? (Binetruy) T5 Interaction rate ~ GN2 T5 ~ ---- MPl4 T2 Expansion rate H ~ ---- (radiation dominated era) MPl T3  ---- ~ ---- H MPl3 Gravitons decouple at the Planck era : fossile radiation

50. Natural units