The History of the Universe in 60 Minutes

General

The History of the Universe in 60 Minutes
Max Tegmark, MIT

Max TegmarkDept. of Physics, [email protected] 15, 2005

100dpi

Cosmology timeline:
Overduin & Priester 2001, astro-ph/0101484

Cosmology timeline:
Cosmic Microwave Background detected (Penzias & Wilson)
1st quasar discovered (Schmidt)
Weak lensing detected (4 teams)
Derision cosmology
Precision cosmology
Galaxy redshift surveys
Cosmic microwave backgroud anisotropies
Supernova cosmology
Weak gravitational lensing
Lyman a forest cosmology
21 cm cosmology
2dF galaxy clustering
CMB polarization detected (DASI)
Cosmic Microwave Background predicted (Alpher & Herman)


Flyabout + SDSS movie


(Graphics from Gary Hinshaw/WMAP team)


Fluctuation generator
Fluctuation amplifier
Hot Dense Smooth
Cool Rarefied Clumpy
Brief History of the Universe


Hot Dense Smooth
What do we want to measure?
Cosmological functions
(z), G(z,k), Ps(k), Pt(k)


Hot Dense Smooth
To 0th order:
H(z)


Hot Dense Smooth
H(z)
P(k,z)
To 1st order:


MATTER BUDGET
INITIAL CONDITIONS
(Q)


OUR TOOLS


Smorgasbord


Measuringexpansion


Alexander Friedmann1888-1925(Russian; 1922 paper)
George Lematre 1894-1936(Belgian; indep. 1927 paper)
Arthur Geoffrey Walker 1909-?(British; 1935 paper with H P Robertson showed that F(L)RW metric is only homogeneous & isotropic metric)


Robertson
Wigner
Weyl
Gdel
Rabi
Ladenburg
Oppenheimer
Clemence


Cosmic scale factor a(t)
t [Gigayears]


The Universe is expanding:H>0 todayvHr for vc



Edwin Hubble 1889-(American; 1930 paper)
Mt. Wilson Observatory 1931


Hubble 1929:H550 km/s/Mpc
Riess et al 1996:H70 km/s/Mpc
How measure distance & redshift?



Cosmic scale factor a(t)
t [Gigayears]


Boomzoom
Standardizable candles
(From Saul Perlmutters web site)


Boomzoom
Using galaxy correlations as a standardizable ruler:
Easiest to understand in real space (Bashinsky & Bertschinger, PRL, 87, 1301, 2001; PRD 123008, 2002)
(Eisenstein, Hu & MT 1998; Eisenstein et al 2005; Cole et al 2005)


Boomzoom
Weve measured distance to z=0.35 to 5% accuracy
(Eisenstein et al 2005, for the SDSS collaboration astro-ph/050112)


Tytler et al 2000, astro-ph/0001318
Big Bang nucleosynthesis as a standardizable clock:


SN Ia+CMB+LSS constraints
Yun Wang & MT 2004, PRL 92, 241302
H = dlna/dt, H2
Assumes k=0


Measuringclustering


History
CMB
Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496


Boomzoom
z = 1000


Boomzoom
z = 2.4
Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001


Boomzoom
z = 0.8


Boomzoom
z = 0


Nbody_fluct_growth.mpg


1parmovies
Lya
LSS
Clusters
Lensing
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB


Cmbgg OmOl


1parmovies
Lya
LSS
Clusters
Lensing
CMB


000619
Galaxy power spectrum measurements 1999(Based on compilation by Michael Vogeley)


1parmovies
LSS


1parmovies
LSS
Clusters


1parmovies
LSS
Clusters
CMB


History
(Figure from Wayne Hu)
(Figure from WMAP team)


History


History
CMB
Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496


Boomzoom
Guth & Kaiser 2005, Science


1parmovies
LSS
Clusters
CMB


1parmovies
Ly
LSS
Clusters
CMB


Boomzoom
You
Quasar
LyF


1parmovies
Ly
LSS
Clusters
CMB


1parmovies
Ly
LSS
Clusters
Lensing
CMB


GRAVITATIONAL LENSING:A1689 imaged by Hubble ACS, Broadhurst et al 2004


distortion
Lensing


1parmovies
Ly
LSS
Clusters
Lensing
CMB


000619
Galaxy power spectrum measurements 1999(Based on compilation by Michael Vogeley)


1parmovies
Lya
LSS
Clusters
Lensing
CMB


But the best is yet to come


DATAINTERPRETATION


Measuringcosmologicalparameters


Cosmological parameter movies available athttp://space.mit.edu/home/tegmark/movies.html


Cmbgg OmOl
How much dark matter is there?
Why are we cosmologists so excited?
=d /(1.878810-26 kg m3)
b /(1.878810-26 kg m3)


Cmbgg OmOl
=d /(1.878810-26 kg m3)
b /(1.878810-26 kg m3)


Cmbgg OmOl
Ruled out by CMB 2000(COBE, Boomerang, MAXIMA, etc)
=d /(1.878810-26 kg m3)
b /(1.878810-26 kg m3)


Cmbgg OmOl
CMB
=d /(1.878810-26 kg m3)
b /(1.878810-26 kg m3)


Cmbgg OmOl
CMB
+
P(k)
=d /(1.878810-26 kg m3)
b /(1.878810-26 kg m3)


Cmbgg OmOl
CMB
+
LyF
+
P(k)
SDSS LyaF analysis lead by Pat McDonald, Uros Seljak, Scott Burles & co
b /(1.878810-26 kg m3)


Cmbgg OmOl
CMB


Cmbgg OmOl


Cmbgg OmOl
CMB
+
LSS


Cmbgg OmOl


THEORY


MATTER BUDGET
INITIAL CONDITIONS
(Q)

Cosmological data
Cosmological Parameters

Cosmological data
ARE WE DONE?

Cosmological data
Fundamental theory
Nature of dark matter?
Nature of dark energy?
Nature of early Universe?
Why these particular values?


MATTER BUDGET
INITIAL CONDITIONS
(Q)


WHY?
(Q)


Why these values?
Standard model parameters:

Cosmological data
All vanilla?
H(z), P(k,z), ClT , ClX , ClE , ClB ,

Cosmological data
Clues about Dark matter Dark energy Inflation
All vanilla?
Non-scale invariance?Gravitational waves?Non-Gaussianity?Isocurvature modes?Non-flatness?
Non-vanilla clustering?Make at LHC?Detect directly? Indirectly?
Non-constant density?Clustering?

Cosmological data
Clues about Dark matter Dark energy Inflation
All vanilla?
Non-scale invariance?Gravitational waves?Non-Gaussianity?Isocurvature modes?Non-flatness?
Non-vanilla clustering?Make at LHC?Detect directly? Indirectly?
Non-constant density?Clustering?
c, Q


Boomzoom
w(z) =-1, w=w==0 No dark energy clustering
DARK ENERGY:
Redshift z
0 1 2
Dark energy density


Boomzoom
DARK MATTER:
Redshift z
0 1 2
Growth factor (obs/theo)
No direct detection No indirect detection No accelerator detection No astrophysically observed departures from vanilla CDM


Boomzoom
No departures from scale invariance detected (n=1, dn/dlnk=0, etc) No gravity waves detected No non-Gaussianity detected No isocurvature detected
INFLATION:
Wavenumber k [1/Mpc]
Primordial power spectrum P*(k)/k


The History of the Universe in 60 Minutes

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