Title: THE STANDARD MODEL OF COSMOLOGY: PAST, PRESENT AND FUTURE
1THE STANDARD MODEL OF COSMOLOGY PAST, PRESENT
AND FUTURE
- Joe Silk
-
- University of Oxford
- (visiting APC, IAP)
-
XLIth Rencontres de Moriond, La Thuile
March 22, 2006
2WE HAVE ENTERED A NEW ERA OF PRECISION COSMOLOGY
THAT HAS LEFT US WITH SOME OF THE GREATEST
PUZZLES IN PHYSICS
WHAT IS THE DARK ENERGY ?
WHAT IS THE DARK
MATTER?
3 - A BRIEF HISTORY OF COSMOLOGY
FRIEDMANN(1923) AND LEMAITRE (1927) PROPOSED THE
EXPANDING UNIVERSE
4WHERE DARK ENERGY ORIGINATED
- WHERE DARK MATTER ORIGINATED
5A BRIEF HISTORY OF COSMOLOGY, CTD
brightest cluster galaxies
6 - A BRIEF HISTORY OF COSMOLOGY, CTD
RELIC RADIATION DISCOVERED BY PENZIAS AND WILSON
(1964)
These are 400 sigma error bars! COBE 1990
7FROM EXPANSION TO INFLATION (1980)
Alan Guth
Andrei Linde
The Big Bang? Believe me, it was very, very,
very, very, very, very big
8THE ONSET OF INFLATION AT 10-35 sec
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10THE INFLATIONARY UNIVERSE
11COSMOLOGICAL CONSTANT OR DARK ENERGY?
In general, pw??with w-1 for the cosmological
constant ?
12A SPACE-TIME DIAGRAM OF THE UNIVERSE
FIRST LIGHT
THE DARK AGES
- ON ANGULAR SCALES ABOVE A DEGREE, WE ARE
- VIEWING QUANTUM FLUCTUATIONS IN THE SKY!
13SOME MORE PREHISTORY
ACOUSTIC RADIATION OSCILLATIONS
- BARYON ACOUSTIC OSCILLATIONS
Silk 1967
Peebles and Yu 1970
Sunyaev and Zeldovich 1970
Silk and Wilson 1981
Doroshkevich, Zeldovich and Sunyaev 1977
14THE MILKY WAY
distance from centre of galaxy
rotation velocity
Sofue and Rubin
NON-BARYONIC DARK MATTER DOMINATES!
15THE BARYON DENSITY IS KNOWN..AND VERY
SUBDOMINANT
HELIUM
LIGHT ELEMENTNUCLEOSYNTHESIS IN THE BIG BANG
OmegaB measures the density of baryons
DEUTERIUM
LITHIUM
16PRIMORDIAL SOUND WAVES IN THE PHOTON-BARYON
PLASMA
NON-BARYONIC WEAKLY INTERACTING DARK MATTER
BOOSTS FLUCTUATION GROWTH
density fluctuation strength
time
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18FROM COBE TO WMAP
1992
2006
19 TEMPERATURE VARIATIONS IN THE SKY
WL Wm 1 is measured by cosmic microwave
background peak SPACE IS APPROXIMATELY
EUCLIDEAN!
THEORY
DATA as of March 2006
BECAUSE OF PARAMETER DEGENERACIES WE NEED TO DO
BETTER THAN CMB ALONE
20BARYON OSCILLATIONS
21SUCCESS OF LARGE-SCALE STRUCTURE
THE DARK SIDE OF GALAXY FORMATION
MPA Millennium simulation 2005
dark matter
luminous matter
22MILLENNIUM SIMULATION
23WHERE IS THE HALO SUBSTRUCTURE?
Diemand and Madau 2006
and the dark matter concentration?
24THE MILKY WAY HALO DWARF GALAXIES
- DWARF GALAXY ROTATION CURVE
orbital velocity
vp gt13 km/s
distance from centre of galaxy
J. Taylor 2005
25RESURRECTION OF DARK MATTER VIA NEW PHYSICS ?
- OR RESURRECTION VIA MESSY ASTROPHYSICS ?
26THE EFFECTS OF SUPERNOVA-DRIVEN WINDS
vp gt 43 km/s
orbital velocity
J. Taylor 2005
distance from centre of galaxy in kpc
27SHEDDING LIGHT ON COLD DARK MATTER
MOTIVATED CANDIDATE LIGHTEST SUPERSYMMETRIC
PARTICLE IS EXPECTED TO BE IN MASS RANGE 100-1000
GeV
THERMAL FREEZE-OUT AT kTm?/20 IMPLIES RELIC
DENSITY ?weak/?annihilation
PENDING SUCCESS OF DIRECT DETECTION ATTEMPTS,
THE MILKY WAY HALO PROVIDES A LABORATORY FOR
INDIRECT SEARCHES VIA ANNIHILATIONS INTOHIGH
ENERGY PHOTONS, POSITRONS, NEUTRINOS, ANTIPROTONS
28COSMIC RAY POSITRON SPECTRUM
Baltz and Edsjo
PAMELA launch in 2006
positron energy (GeV)
29EGRET GAMMA RAY FLUXFROM GALACTIC CENTRE
photon energy (GeV)
PREDICTIONS
Nezri et al. 2004
GLAST 2007
30PROBING DARK ENERGY WITH SUPERNOVAE
a high redshift SN
flux
observed wavelength
I.Hook et al 2005
31WL - Wm is measured by SN1a
acceleration inferred, hence WL or dark
energy since r3plt0
magnitude
WL
SN are fainter at high z
Wm
32Investigating dark energy
- The equation of state parameter w(z) p/?
- w -1
- w const ? -1
- w(z)
-
- Theoretical explanations are guided by
observations
Spergel et al 2006
Seljak et al 2005
33THE FUTURE FOR DARK ENERGY
- Dark Energy Survey (2009)
- 4-5 bands in visible band (4m)
- 10,000 sq deg to z gt 1
- Pan-STARRS (2006-2009)
- US Air Force, 4 1.8m telescopes
- 3,000 sq deg in 5 bands
- Spectrographs
- AAOmega, 1,000 sq deg (4m) (2006/9)
- GWFMOS/HyperSuprime z 1-3 (8m) (2013)
- The ultimate surveys
- LSST 20,000 sq deg to z 3 (2015)
- SKA 20,000 sq deg redshifts (2020)
darkCAM
DES
GWFMOS
gt 1 billion euros worth of proposals until 2015
ULTIMATE AIM MEASURE w TO A PERCENT
R. Trotta 2006
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35A NEW ERA OF PRECISION COSMOLOGY
FUNDAMENTAL ISSUES FOR PARTICLE ASTROPHYSICS
WHAT IS THE NON-BARYONIC DARK
MATTER? WHY IS THE DARK ENERGY SO
SMALL TODAY? WHY DOES IT DOMINATE
THE UNIVERSE SO RECENTLY? IS THE
UNIVERSE FINITE OR INFINITE? (W1/-e)
DID INFLATION OCCUR? HOW DID
GALAXIES FORM? ??????????????????
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