The History of the Universe in 60 Minutes
Max Tegmark, MIT 100dpi Cosmology timeline:
500 BC
2000 AD
Overduin & Priester 2001, astro-ph/0101484 1900 Cosmology timeline: 1910 s e
Einstein’s theory of gravity i
1920 p o
Expanding Universe theoretically possible (Friedmann) r t o s
Universe is expanding (Hubble) i
y 1930 n g a o l d o s u
1940 y m o e s r v o g r
c Big Bang Nucleosynthesis (Gamow) k
g u y c n s
1950 n
Cosmic Microwave Background predicted (Alpher & Herman) g a i o t i s o y f b l s
i n g i o e h r e o l v l s e
1960 m a l o y d s
D 1st quasar discovered (Schmidt) a e g o w m r n o c o
s l
Cosmic Microwave Background detected (Penzias & Wilson) o r t y o i o s c t c x
1970 i
e a m a a r t l s m i v
o a o v f c o c y
i
a G n g a r 1980 r
r m o
Inflation invented (Guth, Linde, Albrecht & Steinhardt) e g l e n s
t o s a o p CfA Galaxy Redshift Survey k u u a C m l m e S 1990 s y C CMB anisotropies detected (COBE) o L W c
m y Dark energy discovered with supernovae (2 teams), CMB peaks detected c
g 2000
Weak lensing detected (4 teams) o 1 l WMAP CMB, SDSS galaxy clustering 2dF galaxy clustering 2 o Planck CMB satellite CMB polarization detected (DASI) m 2010 s o c CMBPOL satellite? JDEM? JWST? LSST? SKA? n o 2020 i s i c e r P Flyabout + SDSS movie
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 (Graphics from Gary Hinshaw/WMAP team) Brief History of Fluctuation generator the Universe Fluctuation amplifier
H o D t en Sm se oo th
Co ol Ra re Cl fi um ed py (Graphics from Gary Hinshaw/WMAP team) What do we want Fluctuation generator to measure? Fluctuation amplifier
H o D t en Sm se oo th
Co ol Ra re Cl fi um ed py (Graphics from Gary Hinshaw/WMAP team) Cosmological ρ (z), G(z,k), P (k), P (k) functions Λ s t Fluctuation generator To 0th order: Fluctuation amplifier
H o D t en Sm se oo H th (z) Co ol Ra re Cl fi um ed py (Graphics from Gary Hinshaw/WMAP team) Cosmological ρ (z), G(z,k), P (k), P (k) functions Λ s t Fluctuation generator To 1st order: Fluctuation amplifier
H o D t en Sm se oo H th (z) P( C k, o z) ol Ra re Cl fi um ed py (Graphics from Gary Hinshaw/WMAP team) Cosmological functions MATTER BUDGET
(Q)
INITIAL CONDITIONS OUR TOOLS
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 Smorga sbord
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 Measuring expansion
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 Arthur Geoffrey Walker 1909-? (British; 1935 paper with H P Robertson Alexander showed that F(L)RW Friedmann metric is only 1888-1925 homogeneous & George Lemaître 1894-1936 isotropic metric) (Russian; 1922 paper) (Belgian; indep. 1927 paper) Robertson Weyl Ladenburg Clemence Wigner Gödel Rabi
Oppenheimer Cosmic scale factor a(t)
t
[ G i g a y e a r s ] The Universe is expanding: •H>0 today •v≈Hr for v«c
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005
Edwin Hubble 1889- (American; 1930 paper)
Max Tegmark Dept. of Physics, MIT [email protected] Mt. Wilson Observatory 1931 NEPPSR August 15, 2005 Hubble 1929: Riess et al 1996: H≈550 km/s/Mpc H≈70 km/s/Mpc
How measure distance & redshift?
Cosmic scale factor a(t)
t
[ G i g a y e a r s ] Standardizable candles (From Saul Perlmutter’s web site)
Boom zoom Using galaxy correlations as a standardizable ruler: (Eisenstein, Hu & MT 1998; Eisenstein et al 2005; Cole et al 2005)
Boom zoom
Max Tegmark Dept. of Physics, MIT [email protected] Easiest to understand in real space NEPPSR August 15, 2005 (Bashinsky & Bertschinger, PRL, 87, 1301, 2001; PRD 123008, 2002) (Eisenstein et al 2005, for the SDSS collaboration astro-ph/050112)
Boom zoom
We’ve measured distance to z=0.35 to 5% accuracy
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 B i g
B a n g
nu c l e o s y n t h e s i s
as
a
s t a n d a r d i z a b l e
Tytler et al 2000, astro-ph/0001318 c l o c k : H = dlna/dt, H2 ∝ ρ,
Assumes k=0
SN Ia+CMB+LSS constraints Yun Wang & MT 2004, PRL 92, 241302 Measuring clustering
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 0302496 h/ ro-p t s
CMBa
on, t l i m a H & a t -Cos ra i ve i l O
History rk, de a m g e T from p a m P A M d W ne a e l round-c g Max Tegmark ore
Dept. of PhF ysics, MIT [email protected] NEPPSR August 15, 2005 z = 1000
Boom zoom
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 1 0
0 z = 2.4 2
l e k e D
&
e t i h W
, n n a m
Boom f f u
zoom a K
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Dept. of Physics, MIT t [email protected] a
NEPPSR M August 15, 2005 1 0
0 z = 0.8 2
l e k e D
&
e t i h W
, n n a m
Boom f f u
zoom a K
, l e g n i r p S
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Dept. of Physics, MIT t [email protected] a
NEPPSR M August 15, 2005 1 0
0 z = 0 2
l e k e D
&
e t i h W
, n n a m
Boom f f u
zoom a K
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Dept. of Physics, MIT t [email protected] a
NEPPSR M August 15, 2005 CMB Clusters
1par LSS Lensing movies
Lyα
Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 Cmbgg OmOl
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 CMB Clusters
1par LSS Lensing movies
Lyα
Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 000619
Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley)
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 1par LSS movies
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 Clusters
1par LSS movies
Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 CMB Clusters
1par LSS movies
Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 (Figure from Wayne Hu)
History (Figure from WMAP team) History 0302496 h/ ro-p t s a
on, t l CMBi m a H & a t -Cos ra i ve i l O rk, de a m g History e T from p a m P A M d W ne a e l round-c g ore F
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 e c n e i c S
, 5 0 0 2
Boom r e s zoom i a K
&
h t u G
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 CMB Clusters
1par LSS movies
Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 CMB Clusters
1par LSS movies
Lyα
Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 Lyman Alpha Forest Simulation: Cen et al 2001
LyαF Quasar
Boom zoom You
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 CMB Clusters
1par LSS movies
Lyα
Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 CMB Clusters
1par LSS Lensing movies
Lyα
Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 GRAVITATIONAL LENSING: A1689 imaged by Hubble ACS, Broadhurst et al 2004
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 Lensing
distorti on
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 CMB Clusters
1par LSS Lensing movies
Lyα
Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 000619
Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley)
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 CMB Clusters
1par LSS Lensing movies
Lyα
Tegmark & Zaldarriaga, astro-ph/0207047 + updates Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 But the best is yet to come…
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 Measuring cosmological parameters Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 Cosmological parameter movies available at http://space.mit.edu/home/tegmark/movies.html
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 How much dark matter is there? ) 3 kg m
6 2 − 0 1
Cmbgg × OmOl Why are we /(1.8788
b
ρ cosmologists so excited?
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR −26 3 August 15, 2005 =ρd /(1.8788×10 kg m ) How much dark matter is there? ) 3 kg m
6 2 − 0 1
Cmbgg × OmOl /(1.8788
b ρ
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR −26 3 August 15, 2005 =ρd /(1.8788×10 kg m ) How much dark matter is there? ) 3 kg m
6 2 − 0 1
Cmbgg × OmOl /(1.8788
b
ρ Ruled out by CMB 2000 (COBE, Boomerang, MAXIMA, etc)
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR −26 3 August 15, 2005 =ρd /(1.8788×10 kg m ) How much dark matter is there?
CMB ) 3 kg m
6 2 − 0 1
Cmbgg × OmOl /(1.8788
b ρ
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR −26 3 August 15, 2005 =ρd /(1.8788×10 kg m ) How much dark matter is there?
CMB ) + 3 kg m
6 2 − 0 1
Cmbgg × OmOl P(k) /(1.8788
b ρ
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR −26 3 August 15, 2005 =ρd /(1.8788×10 kg m ) How much dark matter is there?
CMB ) + 3 kg m
6 2 − 0 1
Cmbgg × OmOl P(k) /(1.8788
+ b ρ
LyαF Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR SDSS LyaF analysis lead by Pat McDonald, Uros August 15, 2005 Seljak, Scott Burles & co CMB
Cmbgg OmOl
Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005 Cmbgg OmOl CMB +
Cmbgg OmOl LSS Cmbgg OmOl MATTER BUDGET
(Q)
INITIAL CONDITIONS Cosmological data
Cosmological Parameters Cosmological data
Cosmological Parameters
ARE WE DONE? Cosmological data
Cosmological Parameters
Why these particular values?
Nature of dark matter?
Fundamental Nature of dark energy? theory ? Nature of early Universe? MATTER BUDGET
(Q)
INITIAL CONDITIONS (Q) Inflation!
Baryogenesis SUSY? ν-physics WHY? Standard model Why these values? parameters: Cosmological T X E B data H(z), P(k,z), Cl , Cl , Cl , Cl ,…
Cosmological ρ (z), G(z,k), P (k), P (k) functions Λ s t All vanilla? Cosmological T X E B data H(z), P(k,z), Cl , Cl , Cl , Cl ,…
Cosmological ρ (z), G(z,k), P (k), P (k) functions Λ s t All vanilla? Non-vanilla clustering? Make at LHC? Detect directly? Indirectly?
Non-constant density? Clues about Clustering?
• Dark matter Non-scale invariance? • Dark energy Gravitational waves? Non-Gaussianity? • Inflation Isocurvature modes? Non-flatness? Cosmological T X E B data H(z), P(k,z), Cl , Cl , Cl , Cl ,…
Cosmological ρ (z), G(z,k), P (k), P (k) functions Λ s t All vanilla? Non-vanilla clustering? Make at LHC? Detect directly? Indirectly?
Non-constant density? Clues about Clustering?
• Dark matter Non-scale invariance? • Dark energy Gravitational waves? Non-Gaussianity? • Inflation Isocurvature modes? Non-flatness? ξc, ρΛ, Q DARK ENERGY: • w(z) =-1, w’=w’’=…=0 • No dark energy clustering y t i Boom s n zoom e d
y g r e n e
k r a D
Max Tegmark 0 1 2 Dept. of Physics, MIT [email protected] NEPPSR Redshift z August 15, 2005 DARK MATTER: • No direct detection • No indirect detection • No accelerator detection • No astrophysically observed departures from vanilla CDM
Boom zoom Growth factor (obs/theo)
Max Tegmark 0 1 2 Dept. of Physics, MIT [email protected] NEPPSR Redshift z August 15, 2005 INFLATION: • No departures from scale invariance detected (n=1, dn/dlnk=0, etc) • No gravity waves detected • No non-Gaussianity detected • No isocurvature detected *(k)/k Boom P zoom Primordial power spectrum
Max Tegmark Dept. of Physics, MIT Wavenumber k [1/Mpc] [email protected] NEPPSR August 15, 2005 Max Tegmark Dept. of Physics, MIT [email protected] NEPPSR August 15, 2005