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The matter particles

The ‘Standard Model’

The fundamental interactions

Gravitation electromagnetism weak nuclear force strong nuclear force

= Cosmic DNA

Some particles have mass, some do not

+1 0 -1

W + Z 0 W -

Mass 80.419 91.188 80.419

0photon

Mass 0

Where do the masses 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 LIGOGround motion couplesinto motion of mirrors

Counting statistics ofphotons at photodiode

Thermal excitations ofmirror suspensions

10-24

10-23

10-22

10-21

10-20

10-19

10-18

1 10 100 1000 104

h (

Hz-1

/2)

Virgo

LIGO

Resonantantennas

Hz

GEO

Core Collapse@ 10 Mpc

BH-BH MergerOscillations@ 100 Mpc

Pulsars hmax – 1 yr integration

BH-BH Inspiral,z = 0.4

BH-BH Inspiral, 100 Mpc

QNM from BH Collisions, 1000 - 100 Msun, z=1

NS, =10-6 , 10 kpc

QNM from BH Collisions, 100 - 10 Msun, 150 Mpc

NS-NS Inspiral, 300 Mpc

NS-NS MergerOscillations@ 100 Mpc

Credit: P.Rapagnani

Design sensitivity

Measured sensitivity

C7 NS/NS maximum distance ~ 1.5 Mpc

(7 W)(7 W)(7 W)(7 W)(0.7 W)(0.7 W)(0.7 W)

Design NS/NS maximum distance ~ 30 Mpc

WMAP satellite

At t = 400 000 yrs, the Universe becomes transparent: photons no longer interact with

matterBIG BANG

Cosmological background T = 3 K = - 270 °C

Looking back to the primordial Universe

When do graviton decouple?

Interaction rate ~ GN2 T5 ~ ----T5

MPl4

Expansion rate H ~ ----

---- ~ ----

T2

T3

MPl

MPl3

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 ExperimentsCherenkov TelescopesCherenkov Telescopes

4. HESS-II [Vincent]

• New 28m telescope.• 2048 pixel camera.• Lower energy 40-50

GeV.

5. MAGIC-II [Teshima]

• New 17m telescope.• Possible high-QE

camera.• 2007 schedule.

MAGIC-IMAGIC-I MAGIC-IIMAGIC-II

85m

Future ConceptsLarge Cherenkov Tel. Arrays

HE-ASTRO: 217 Telescopes (ø10m), 80m separation.1.1 km2 collection area & 15o FOV !

Fie

ld o

f vi

ew [

π s

r] Field

of view

[deg

]

Collecting Area [km2]

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 NSFNSF

NSF

Natural WIMP candidate:SUSY LSP neutralino

Stable if SUSY exists and R-parity is conserved

• Direct detection:– WIMP scattering off nuclei

˜ χ 10 =N11

˜ B +N12˜ W 3 +N13

˜ H 10 +N14

˜ H 20

Zg = N11

2+ N12

2gaugino fraction:

PMTsPMTs

PEEK SupportsPEEK Supports

CathodeCathode

GridsGrids

Waveshifter/ReflectorWaveshifter/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

0.45 10-6

SMC

0.65 10-6

Self lensing:

LMC-LMC

0.005 - 0.05 10-6

SMC-SMC

0.04 10-6

Lensing LMC-Galactic stars:

LMC-gal

0.01 10-6

Lensing Galactic-Galactic stars:

gal-gal

2.0 10-6

Events rate comparison :

(MACHO 0.12 10-6)

_3% at 10-2 M

Final EROS combined limit (1990-2003)

_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

ZOOMZOOM