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The matter particles

The fundamental interactions. Gravitation electromagnetism weak nuclear force strong nuclear force. The ‘ Standard Model ’. = Cosmic DNA. The matter particles. Where. do. the. masses. come from. ?. photon. 0. W. +. Z. 0. W. -. +. 1. 0. -. 1.

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The matter particles

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

  2. 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)

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

  4. -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

  5. 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

  6. 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

  7. When do graviton decouple? 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

  8. Solar System ? ? Tides/vertical force Rot. curves HSB/LSB Lensing by Ellip/Clusters Hubble Expansion/CMB ???? Update Scores LCDM TeVeS-MOND Stay Tuned!

  9. 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

  10. 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 !

  11. A future mission should: Achieve BLIP Observe longer (~2) ~2 for satellites John will discuss ground-based Use many more pixels To go much deeper, we must use arrays. How to go deeper

  12. The South Pole NSF NSF NSF NSF

  13. 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:

  14. 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)

  15. 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

  16. 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

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