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Cosmic collisions: dark matter, dark energy & inflation
Max Tegmark, Penn/MITMax Tegmark, Penn/MIT
100dpi
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Smorgasbord
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Measuringclustering
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
exp9911
CMB 1992-94
2004
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
105dpi
CMB
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
De Bernardis et al 2000, Lange et al 2000
CMB
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Tegmark, Jr., 2001
CMB
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
History
CMB
For
egro
und-
clea
ned
WM
AP
map
fro
m T
egm
ark,
de
Oli
veir
a-C
osta
& H
amil
ton,
ast
ro-p
h/03
0249
6
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
CMB FRONTIERS:• Polarization• Small scales (AKBAR, CBI, Planck,
APEX, ACT, SPT, …)
Atacama Cosmology Telescope (ACT):
150 GHz
SZ Simulation MBAC on ACT 1.7’ beam w/ 2X
noise
PLANCK
1.4°
= 145, 225 & 265 GHz.
Ground based experiment at Atacama desert, Chile.
Sensitivity/pixel ~ 2, 8 & 16mK (64 nights of quality data).
FWHM=1.7, 1.1 & 0.93’.
Scans only in azimuth with the ability to cross-link elevations.
More info at http://www.physics.upenn.edu/act
Team:
D. Benford, S. Boughn, J. Chervenak, A. de Oliveira-Costa, M. Devlin, R. Doriese, L. Ferrarese, J. Fowler, M. Halpern, D. Hughes, J. Hughes, K. Irwin, B. Jain, N. Jarosik, R. Jimenez, J. Klein, A. Kosowsky, R. Lupton, A. Miller, H.Moseley, B. Netterfield, L. Page (P.I.), B. Partridge, H. Quintana, A. Reiseneggar, U. Seljak, D. Spergel, M. Spergel, S. Staggs, C. Stahle, M. Tegmark, L. Verde, T. Williams, G. Wilson, E. Wollack.
Atacama Cosmology Telescope (ACT):
150 GHz
SZ Simulation MBAC on ACT 1.7’ beam w/ 2X
noise
PLANCK
1.4°
Measure the primary anisotropy beyond the WMAP & Planck resolution limits.
Measure the amplitude of the CMB gravitational lensing, and therefore probe the mass power spectrum at 1Mpc scales at z~1-2.
Find galaxy clusters at z<1 through SZ effect.
Detect signature of reonization at z~15 through Vishniac effect.
Find all extragalactic mm-wave point sources in 100(o)2 to a sensitivity of 1mJy.
= 145, 225 & 265 GHz.
Ground based experiment at Atacama desert, Chile.
Sensitivity/pixel ~ 2, 8 & 16mK (64 nights of quality data).
FWHM=1.7, 1.1 & 0.93’.
Scans only in azimuth with the ability to cross-link elevations.
More info at http://www.physics.upenn.edu/act
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
z = 1000
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Mat
his,
Lem
son,
Spr
inge
l, K
auff
man
n, W
hite
& D
ekel
200
1
z = 2.4
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Mat
his,
Lem
son,
Spr
inge
l, K
auff
man
n, W
hite
& D
ekel
200
1
z = 0.8
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Mat
his,
Lem
son,
Spr
inge
l, K
auff
man
n, W
hite
& D
ekel
200
1
z = 0
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
000619
Galaxy power spectrum measurements 1999(Based on compilation by Michael Vogeley)
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
1parmovies
LSS
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
1parmovies
LSS
Clusters
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
1parmovies
LSS
ClustersCMB
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
1parmovies
Ly
LSS
Clusters
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Lyman Alpha Forest Simulation: Cen et al 2001
You
Quasar
LyF
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
1parmovies
Ly
LSS
Clusters
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
1parmovies
Ly
LSS
Clusters
Lensing
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Lensing
Gravitational lensing
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Lensing
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Lensing
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Lensing
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Lensing
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
distortion
Lensing
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
1parmovies
Ly
LSS
Clusters
Lensing
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
000619
Galaxy power spectrum measurements 1999(Based on compilation by Michael Vogeley)
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
1parmovies
Ly
LSS
Clusters
Lensing
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
QuickTime™ and aAnimation decompressor
are needed to see this picture.
Mark Whittle 2004
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
LSS frontiers/SDSS
propaganda
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
APO
SDSS
100dpi
Cmbgg OmOl
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
100dpi
100dpi
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
LSS
Cool new/imminent LSS-measurements:
•P(k) from full 2dF data set (~250k gals)
•SDSS DR3 goes public this fall
•P(k) from SDSS DR3 (>300k gals)
•P(k) from SDSS LRG’s (Eisenstein et al)
•Angular galaxy clustering from SDSS
•Clustering dependence on SDSS galaxy properties (Zehavi et al)
•SDSS LyF analysis (McDonald et al, Seljak et al)
•See also Pope et al (2003), Budavari et (2004)
Cmbgg OmOl
LSS
Data & image processing by Robert Lupton & David Schlegel
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
LSS
Angular clustering
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
LSS
Angular clustering
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Tegmark et al 2002, for SDSS collab.Dodelson et al 2002, for SDSS collab.
This was from just 400 square degrees:
Now we have an order of magnitude more, and photometric redshifts.
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
1parmovies
Ly
LSS
Clusters
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Measuringparameters
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
+CMB
LSS
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
+CMB
LSS
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
Cmbgg OmOl
Cmbgg OmOl
CMB
+
LSS
Cmbgg OmOl
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
What’s theMatter?
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
How much dark matter is there?
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
How much dark matter is there?
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
+
LSS
How much dark matter is there?
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
• No direct detection
• No accelerator detection
• No bulge annihilation detection
• No astrophysically observed departures from vanilla CDM
DARK MATTER:
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
DARK MATTER:
Redshift z0 1 2
Gro
wth
fac
tor
(obs
/the
o)
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Darkenergy
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
How much dark energy is there?
flat
closedopen
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMBflat
closedopen
How much dark energy is there?
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
+
LSS
How much dark energy is there?
WMAP + SDSS: lots
flat
closedopen
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
+
LSS
How much dark energy is there?
flat
closedopen
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
+
LSS
How much dark energy is there?
flat
closedopen
• Late Integrated Sachs-Wolfe effect detected by Boughn & Crittenden 2003, Nolta et al 2003, Fosalba et al 2003, Scranton et al 2003, Afshordi et al 2003, Padmanabhan et al in prep
• Illustration by Albert Stebbins
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Equation of state?
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Nature of the dark energy
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
Nature of the dark energy
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
+
LSS
Nature of the dark energy
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
+
LSS
Nature of the dark energy
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
Fro
m S
aul P
erlm
utte
r’s
web
site
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
THE NATURE OF DARK ENERGY:
Den
sity
rel
ativ
e to
now
(Yun Wang & MT, astro-ph/0403292, PRL, in press)
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
THE NATURE OF DARK ENERGY:
Den
sity
rel
ativ
e to
now
(Using SN Ia “gold” data from Riess et al 2004)
(Yun Wang & MT, astro-ph/0403292, PRL 2004)
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
THE NATURE OF DARK ENERGY:
Den
sity
rel
ativ
e to
now
(Using SN Ia “gold” data from Riess et al 2004)
(Yun Wang & MT, astro-ph/0403292, PRL, in press)
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
THE NATURE OF DARK ENERGY:
Den
sity
rel
ativ
e to
now
(Using SN Ia “gold” data from Riess et al 2004)
(Yun Wang & MT, astro-ph/0403292, PRL, in press)
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
THE NATURE OF DARK ENERGY:
Den
sity
rel
ativ
e to
now
(Using SN Ia “gold” data from Riess et al 2004)
(Yun Wang & MT, astro-ph/0403292, PRL, in press)
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
• w(z) =-1, w’=w’’=…=0
• No dark energy clustering
DARK ENERGY:
Redshift z0 1 2
Dar
k en
ergy
den
sity
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Inflation
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Testing inflation I:
How flat is space?
Predictiontot=1.000000.00001
Observationtot=1.010.02 (WMAP+SDSS)
SN Ia+CMB+LSS constraints
CMB polarization missions
Dark Energy missions
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Testing inflation II:
SDSS collaboration, astro-ph/0310723, PRD 68, 193591
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Testing inflation II:
SDSS collaboration, astro-ph/0310723, PRD 68, 193591
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
Testing inflation II:
SDSS collaboration, astro-ph/0310723, PRD 68, 193591
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
CMB
+
LSS
Testing inflation II:
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Planck + SDSS: n=0.008, r=0.012
ns=0.96
r=0.15
SDSS collaboration, astro-ph/0310723, PRD 68, 193591
+
LSS
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Planck + SDSS: n=0.008, r=0.012
ns=0.96
r=0.15
SDSS collaboration, astro-ph/0310723, PRD 68, 193591
+
LSS
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Planck + SDSS: n=0.008, r=0.012
ns=1
r=0
SDSS collaboration, astro-ph/0310723, PRD 68, 193591
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Boomzoom
• n=1, dn/dlnk=d^2ndlnk = … = 0
•No gravity waves detected
INFLATION:
Wavenumber k [1/Mpc]
Prim
ordi
al p
ower
spe
ctru
m P
*(k)
/k
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
Cmbgg OmOl
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
My wish list: get at the underlying physics by measuring four cosmologicalfunctions:
1) cosmic expansion history H(z) ==> Nature of dark energy 2) linear growth factor g(z,k) ==> Nature of dark energy, dark matter, neutrinos 3) primordial scalar power spectrum P*(k) ==> Inflation 4) primordial tensor power spectrum P*
T(k) ==> Inflation
Note that 1 predicts 4 and (for most inflation models) 3
Max TegmarkUniv. of Pennsylvania/MIT
max@physics.upenn.eduPhysics in Collision
June 29, 2004
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