The matter particles
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Zur Anzeige wird der QuickTime™ Dekompressor „TIFF (LZW)“
benötigt.
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The matter particles
The ‘Standard Model’
The fundamental interactions
Gravitation electromagnetism weak nuclear force strong nuclear force
= Cosmic DNA
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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)
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Noise Sources in LIGOGround motion couplesinto motion of mirrors
Counting statistics ofphotons at photodiode
Thermal excitations ofmirror suspensions
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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
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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
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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
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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)
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Update Scores LCDM TeVeS-
MOND• Solar System ? ?
• Tides/vertical force
• Rot. curves HSB/LSB
• Lensing by Ellip/Clusters
• Hubble Expansion/CMB ????
Stay Tuned!
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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
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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.
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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.
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The South Pole
NSF NSFNSF
NSF
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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
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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)
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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)
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_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
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