NEUTRINOS IN COSMOLOGY STEEN HANNESTAD UNIVERSITY OF AARHUS ERICE, 17 SEPTEMBER 2005 e
What can we learn about neutrinos from cosmology?
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Transcript of What can we learn about neutrinos from cosmology?
What can we learn about neutrinos from cosmology?
Credit: SDSS team, Andrew Hamilton Blame: Max TegmarkCredit: SDSS team, Andrew Hamilton Blame: Max Tegmark
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
What have we learned
so far?
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Flyabout + SDSS movie
Fluctuation generator
Fluctuation amplifier
(Graphics from Gary Hinshaw/WMAP team)
Hot Dense SmoothCool Rarefied
Clumpy
Brief History of the Universe
Fluctuation generator
Fluctuation amplifier
(Graphics from Gary Hinshaw/WMAP team)
Hot Dense SmoothCool Rarefied
Clumpy
To 0th order:
Cosmological functions
H(z)
Fluctuation generator
Fluctuation amplifier
(Graphics from Gary Hinshaw/WMAP team)
Hot Dense SmoothCool Rarefied
Clumpy
Cosmological functions
H(z)P(k,z)
To 1st order:
SN Ia+CMB+LSS constraintsYun Wang & MT 2004, PRL 92, 241302
H = dlna/dt, H2
Assumes k=0
Vanilla rules OK!
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Measuringclustering
(That’s where the neutrino signal is)
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
History
CMBF
oreg
roun
d-cl
eane
d W
MA
P m
ap f
rom
Teg
mar
k, d
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live
ira-
Cos
ta &
Ham
ilto
n, a
stro
-ph/
0302
496
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Boomzoom
z = 2.4
Mat
his,
Lem
son,
Spr
inge
l, K
auff
man
n, W
hite
& D
ekel
200
1
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Boomzoom
z = 0.8
Mat
his,
Lem
son,
Spr
inge
l, K
auff
man
n, W
hite
& D
ekel
200
1
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Boomzoom
Mat
his,
Lem
son,
Spr
inge
l, K
auff
man
n, W
hite
& D
ekel
200
1 z = 0
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
1parmovies
Ly
LSS
Clusters
Lensing
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
1parmovies
Ly
LSS
Clusters
Lensing
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
000619
Galaxy power spectrum measurements 1999(Based on compilation by Michael Vogeley)
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
1parmovies
LSS
Clusters
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
1parmovies
LSS
ClustersCMB
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
History
(Figure from Wayne Hu)
(Figure from WMAP team)
History
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
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 TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Boomzoom
Gut
h &
Kai
ser
2005
, Sci
ence
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
1parmovies
LSS
ClustersCMB
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
1parmovies
Ly
LSS
Clusters
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Boomzoom
Lyman Alpha Forest Simulation: Cen et al 2001
You
Quasar
LyF
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
1parmovies
Ly
LSS
Clusters
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
1parmovies
Ly
LSS
Clusters
Lensing
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
GRAVITATIONAL LENSING:A1689 imaged by Hubble ACS, Broadhurst et al 2004
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
1parmovies
Ly
LSS
Clusters
Lensing
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
000619
Galaxy power spectrum measurements 1999(Based on compilation by Michael Vogeley)
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
1parmovies
Ly
LSS
Clusters
Lensing
Tegmark & Zaldarriaga, astro-ph/0207047 + updates
CMB
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Measuringcosmologicalparameters
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Boomzoom
How neutrinos suppress cosmic fluctuation growth
•If all the matter can cluster: a
Net growth until today: atoday/aprimordial ≈ 4700p ≈ 4700 e-4f
Power suppression: P(k)/P(k)primordial ≈ e-8f
f≈ ∑ mi /94.4 eV dm ≈ ∑ m
i /12 eV,So 1 eV cuts power in half.
•If only a fraction * can cluster: ap, where
p=[(1+24 *)-1]/4≈ *3/5 ≈ (1-f)3/5
(Bond, Efstathiou & Silk 1980)
Distinguish neutrinos from dark energy by time and scale dependence.
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Cmbgg OmOl
CMB
+
P(k)
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Cmbgg OmOl
CMB
+
LyF
+P(k)
THE FUTUREIt's tough to make predictions, especially about the future. Yogi Berra
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Boomzoom
Now:
• WMAP CMB + SDSS gals & LyF: ∑ mi < 0.4 eV
E.g., Hu & Tegmark astro-ph/9811168,
Hu astro-ph/9904153,
Hannestad et al, astro-ph/0603019
• Planck CMB + LSST lensing: (∑ mi) ~ 0.04 eV
Seljak et al, astro-ph/0407372,
Goobar et al astro-ph/0602155
Future:
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Galaxy clustering progress
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
Why are LRGs so useful?
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
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
LSS Our observable universe
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
LSS
Common galaxies
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
LSS
Common gals: too dense
Quasars: too sparse
LRG’s: just right!
Why LRG’s are “Goldilocks galaxies”:
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
LSS
LRG’s
Also more strongly clustered
Max TegmarkDept. of Physics, MIT
[email protected] ISSworkshop
BU, March 8, 2006
LSS
Why LRG’s are “just right”:60000 LRG’s have more statistical power than 2 million regular gals
(Eisenstein et al 2005)