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?



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Flyabout + SDSS movie

Fluctuation generator

Fluctuation amplifier

(Graphics from Gary Hinshaw/WMAP team)

Hot Dense SmoothCool Rarefied

Clumpy

Brief History of the Universe





Clumpy

To 0th order:

Cosmological functions

H(z)





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!



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Measuringclustering

(That’s where the neutrino signal is)



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History

CMBF

oreg

roun

d-cl

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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



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Boomzoom

z = 1000



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Boomzoom

z = 2.4

Mat

his,

Lem

son,

Spr

inge

l, K

auff

man

n, W

hite

& D

ekel

200

1



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Boomzoom

z = 0.8

Mat

his,

Lem

son,

Spr

inge

l, K

auff

man

n, W

hite

& D

ekel

200

1



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Boomzoom

Mat

his,

Lem

son,

Spr

inge

l, K

auff

man

n, W

hite

& D

ekel

200

1 z = 0



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1parmovies

Ly

LSS

Clusters

Lensing

Tegmark & Zaldarriaga, astro-ph/0207047 + updates

CMB



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Cmbgg OmOl



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1parmovies

Ly

LSS

Clusters

Lensing


CMB



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000619

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



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1parmovies

LSS



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1parmovies

LSS

Clusters




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1parmovies

LSS

ClustersCMB


History

(Figure from Wayne Hu)

(Figure from WMAP team)

History



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History

CMB

For

egro

und-

clea

ned

WM

AP

map

fro

m T

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ark,

de

Oli

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0249

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Boomzoom

Gut

h &

Kai

ser

2005

, Sci

ence



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1parmovies

LSS

ClustersCMB




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1parmovies

Ly

LSS

Clusters


CMB



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Boomzoom

Lyman Alpha Forest Simulation: Cen et al 2001

You

Quasar

LyF



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1parmovies

Ly

LSS

Clusters


CMB



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1parmovies

Ly

LSS

Clusters

Lensing


CMB



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



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distortion

Lensing



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1parmovies

Ly

LSS

Clusters

Lensing


CMB



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000619

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



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1parmovies

Ly

LSS

Clusters

Lensing


CMB



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Measuringcosmologicalparameters



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Neutrinos



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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.



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Cmbgg OmOl



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Cmbgg OmOl



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Cmbgg OmOl

CMB



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Cmbgg OmOl

CMB

+

P(k)



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Cmbgg OmOl

CMB

+

LyF

+P(k)

THE FUTUREIt's tough to make predictions, especially about the future. Yogi Berra



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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:



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Galaxy clustering progress



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Why are LRGs so useful?



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SDSS sphere anim



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History

CMB

For

egro

und-

clea

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WM

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map

fro

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ark,

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0249

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LSS Our observable universe



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LSS

Quasars



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LSS

LRG’s



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LSS

Common galaxies



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LSS

Common gals: too dense

Quasars: too sparse

LRG’s: just right!

Why LRG’s are “Goldilocks galaxies”:



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LSS

LRG’s

Also more strongly clustered



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LSS

Why LRG’s are “just right”:60000 LRG’s have more statistical power than 2 million regular gals

(Eisenstein et al 2005)

Documents

What can we learn about neutrinos from cosmology?