The matter particles The ‘ Standard Model ’ The fundamental interactions Gravitationelectromagnetism weak nuclear force strong nuclear force = Cosmic DNA

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

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

h (Hz -1/2 ) Virgo LIGO Resonant antennas Hz GEO Core 10 Mpc BH-BH Merger 100 Mpc Pulsars h max – 1 yr integration BH-BH Inspiral, z = 0.4 BH-BH Inspiral, 100 Mpc QNM from BH Collisions, Msun, z=1 NS,  =10 -6, 10 kpc QNM from BH Collisions, Msun, 150 Mpc NS-NS Inspiral, 300 Mpc NS-NS Merger 100 Mpc Credit: P.Rapagnani Design sensitivity

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

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

When do graviton decouple? Interaction rate  ~ G N 2 T 5 ~ ---- T5T5 M Pl 4 Expansion rateH ~ ~ ---- T2T2 T3T3 M Pl M Pl 3  H Gravitons decouple at the Planck era : fossile radiation (radiation dominated era)

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

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

Future Concepts Large Cherenkov Tel. Arrays HE-ASTRO: 217 Telescopes (ø10m), 80m separation. 1.1 km 2 collection area & 15 o FOV ! Field of view [π sr] Field of view [deg] Collecting Area [km 2 ] Also, detailed work in Europe and Japan. Cherenkov Telescope Array (CTA) concept well underway.

How to go deeper 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.

The South Pole NSF

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

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)

Full Macho Halo:  LMC   SMC  Self lensing:  LMC-LMC   SMC-SMC  Lensing LMC-Galactic stars:  LMC-gal  Lensing Galactic-Galactic stars:  gal-gal  Events rate comparison : (  MACHO  )

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