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06/18/22 MASSIVE NEUTRINOS AND COSMOLOGY Sergio Pastor (IFIC) ν CuTAPP 2005, Ringberg Castle

MASSIVE NEUTRINOS AND COSMOLOGY

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MASSIVE NEUTRINOS AND COSMOLOGY. ν. Sergio Pastor (IFIC). CuTAPP 2005, Ringberg Castle. Outline. Neutrinos as DM. Effect of neutrino mass on cosmological observables. Current bounds and future sensitivities. Neutrinos decoupled at T~MeV, keeping a - PowerPoint PPT Presentation

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Page 1: MASSIVE NEUTRINOS  AND COSMOLOGY

04/22/23

MASSIVE NEUTRINOS AND COSMOLOGY

Sergio Pastor (IFIC)

ν

CuTAPP 2005,

Ringberg Castle

Page 2: MASSIVE NEUTRINOS  AND COSMOLOGY

Current bounds and future sensitivities

Effect of neutrino mass on cosmological observables

Outline

Neutrinos as DM

Page 3: MASSIVE NEUTRINOS  AND COSMOLOGY

The Cosmic Neutrino Background

• Number density

• Energy density

flavor per

cm )( 112

present at3- 3

23

3

11

3(6

11

3

2 CMBγννν Tπ

)ζn)(p,Tf

π)(

pdn

nm

T

)(p,Tfπ)(

pdmp

i

ii

CMB

νν

43/42

3

322

11

4

120

7

2

Massless

Massive mν>>T

Neutrinos decoupled at T~MeV, keeping a spectrum as that of a relativistic species 1e

1T)(p,f p/T

Page 4: MASSIVE NEUTRINOS  AND COSMOLOGY

04/22/23

Relic neutrinos influence several cosmological epochs

T < eVT ~ MeV

Formation of Large Scale Structures

LSS

Cosmic Microwave Background

CMB

Primordial

Nucleosynthesis

BBN

No flavor sensitivity Neff & mννevs νμ,τ Neff

Non-instantaneous ν decoupling (including oscillations)

3.045N eff T.Pinto et al, in preparation

Page 5: MASSIVE NEUTRINOS  AND COSMOLOGY

Neutrinos as Dark Matter

• Neutrinos are natural DM candidates

• They stream freely until non-relativistic (collisionless phase mixing) Neutrinos are HOT Dark Matter

• First structures to be formed when Universe became matter -dominated

• Ruled out by structure formation CDM

MpceV 30

m 41

-1

ν

Neutrino Free Streaming

b, cdm

eV 46 m 1 Ω eV 93.2

mhΩ

iiν

ii

Page 6: MASSIVE NEUTRINOS  AND COSMOLOGY

Neutrinos as Dark Matter

• Neutrinos are natural DM candidates

• They stream freely until non-relativistic (collisionless phase mixing) Neutrinos are HOT Dark Matter

• First structures to be formed when Universe became matter -dominated

• HDM ruled out by structure formation CDM

eV 46 m 1 Ω eV 93.2

mhΩ

iiν

ii

MpceV 30

m 41

-1

ν

Page 7: MASSIVE NEUTRINOS  AND COSMOLOGY

Neutrinos as Hot Dark Matter

• Effect of Massive Neutrinos: suppression of Power at small scales

Massive Neutrinos can still be subdominant DM: limits on mν from Structure Formation (combined with other cosmological data)

Page 8: MASSIVE NEUTRINOS  AND COSMOLOGY

CMB DATA: INCREASING PRECISION

Multipole Expansion

Angular Power SpectrumMap of CMBR temperature

Fluctuations

T

T-),T(),Δ(

Page 9: MASSIVE NEUTRINOS  AND COSMOLOGY

Galaxy Redshift Surveys

SDSS

2dFGRS

~ 1300 M

pc

Page 10: MASSIVE NEUTRINOS  AND COSMOLOGY

Power Spectrum of density fluctuations

Galaxy Surveys

CMB experiments

SDSS

Field of density Fluctuations

)(

)(x

x

Matter power spectrum is the Fourier transform of the

two-point correlation function

Page 11: MASSIVE NEUTRINOS  AND COSMOLOGY

Power spectrum of density fluctuations

Bias b2(k)=Pg(k)/Pm(k)

Non-linearity

2dFGRS

kmax

SDSS

Page 12: MASSIVE NEUTRINOS  AND COSMOLOGY

Neutrinos as Hot Dark Matter

W. Hu

• Effect of Massive Neutrinos: suppression of Power at small scales

Massive Neutrinos can still be subdominant DM: limits on mν from Structure Formation (combined with other cosmological data)

Page 13: MASSIVE NEUTRINOS  AND COSMOLOGY

Effect of massive neutrinos on the CMB and Matter Power

Spectra

Max Tegmark

www.hep.upenn.edu/~max/

Page 14: MASSIVE NEUTRINOS  AND COSMOLOGY

Cosmological bounds on neutrino mass(es)

A unique cosmological bound on mν DOES NOT exist !Different analyses have found upper bounds on neutrino masses, since they depend on

• The assumed cosmological model: number of parameters (problem of parameter degeneracies)

• The combination of cosmological data used

Page 15: MASSIVE NEUTRINOS  AND COSMOLOGY

Cosmological Parameters: example

SDSS Coll, PRD 69 (2004) 103501

Page 16: MASSIVE NEUTRINOS  AND COSMOLOGY

Cosmological Data

• CMB Temperature: WMAP plus data from other experiments at large multipoles (CBI, ACBAR, VSA…)

• CMB Polarization: WMAP

• Large Scale Structure:

* Galaxy Clustering (2dF,SDSS)

* Bias (Galaxy, …): Amplitude of the Matter P(k) (SDSS,σ8)

* Lyman-α forest: independent measurement of power on small scales

• Priors on parameters from other data: SNIa (Ωm), HST (h), …

Page 17: MASSIVE NEUTRINOS  AND COSMOLOGY

3 degenerate massive neutrinos Σmν = 3m0

Neutrino masses in 3-neutrino schemes

eV

From present evidences of atmospheric and solar neutrino oscillations

atmatm

solar

solar

eV 0.009 m

eV 0.05m

2sun

2atm

eV

m0

Page 18: MASSIVE NEUTRINOS  AND COSMOLOGY

Absolute mass scale searches

Cosmology < 0.42-2.0 eV

Neutrinoless double beta decay

< 0.3-1.6 eVi

ieiee mUm 2

Tritium decay < 2.3 eV

i

im~

2/1

22

iiei mUm

e

Page 19: MASSIVE NEUTRINOS  AND COSMOLOGY

Cosmological bounds on neutrino mass since 2003

390280640 . . .

Bound on Σmν (eV) at 95% CL

Data used

Ichikawa, Fukugita & KawasakiPRD 71 (2005) 043001

2.0 WMAP

SDSS Coll.PRD 69 (2004) 103501

1.7 WMAP, SDSS

HannestadJCAP 0305 (2003) 004

1.01 WMAP, other CMB, 2dF, HST

Crotty, Lesgourgues & SPPRD 69 (2004) 123007

1.0 [0.6] WMAP, other CMB, 2dF, SDSS [HST,SN]

Barger. Marfatia & TregrePLB 595 (2004) 55

0.75 WMAP, other CMB, 2dF, SDSS, HST

WMAP Coll.ApJ Suppl 148 (2003) 175

0.7

WMAP, other CMB,2dF (bias,galaxy clustering), Ly-α, HST

Fogli et al.PRD 70 (2004) 113003

0.47WMAP, other CMB, 2dF, SDSS (Ly-α),HST

Seljak et al.PRD (2005) [astro-ph/0407372]

0.42WMAP, SDSS (bias, galaxy clustering, Ly-α)

Page 20: MASSIVE NEUTRINOS  AND COSMOLOGY

Neutrino masses in 3-neutrino schemes

Fig from Strumia & Vissani, hep-ph/0503246

CMB + galaxy clustering

+ HST, SNI-a [σ8]

+ Ly-α [bias]

Page 21: MASSIVE NEUTRINOS  AND COSMOLOGY

Global analysis: oscillations + tritium decay + 02 + Cosmology

Fogli et al., PRD 70 (2004) 113003

CMB + 2dF

Page 22: MASSIVE NEUTRINOS  AND COSMOLOGY

390280640 . . .

Bound on Σmν (eV) at 95% CL

Data used

Ichikawa, Fukugita & KawasakiPRD 71 (2005) 043001

2.0 WMAP

SDSS Coll.PRD 69 (2004) 103501

1.7 WMAP, SDSS

HannestadJCAP 0305 (2003) 004

1.01 WMAP, other CMB, 2dF, HST

Crotty, Lesgourgues & SPPRD 69 (2004) 123007

1.0 [0.6] WMAP, other CMB, 2dF, SDSS [HST,SN]

Barger. Marfatia & TregrePLB 595 (2004) 55

0.75 WMAP, other CMB, 2dF, SDSS, HST

WMAP Coll.ApJ Suppl 148 (2003) 175

0.7

WMAP, other CMB,2dF (bias,galaxy clustering), Ly-α, HST

Fogli et al.PRD 70 (2004) 113003

0.47WMAP, other CMB, 2dF, SDSS (Ly-α),HST

Seljak et al.PRD (2005) [astro-ph/0407372]

0.42WMAP, SDSS (bias, galaxy clustering, Ly-α)

Allen, Smith & BridleMNRAS 346 (2003) 593

WMAP, other CMB, 2dF, X-ray galaxy cluster

390280640 . . .

Page 23: MASSIVE NEUTRINOS  AND COSMOLOGY

The bound depends on the number of neutrinos

• Example: in the 3+1 scenario, there are 4 neutrinos (including thermalized sterile)

• Calculate the bounds with Nν > 3

Abazajian 2002, di Bari 2002

Hannestad JCAP 0305 (2003) 004

(also Elgarøy & Lahav, JCAP 0304 (2003) 004)

3 ν4 ν

5 ν

Hannestad

95% CL

WMAP + Other CMB + 2dF + HST + SN-Ia

Page 24: MASSIVE NEUTRINOS  AND COSMOLOGY

Σmν and Neff degeneracy

(0 eV,3)

(0 eV,7)

(2.25 eV,7)(0 eV,3)

(0 eV,7)

(2.25 eV,7)

Page 25: MASSIVE NEUTRINOS  AND COSMOLOGY

Analysis with Σmν and Neff free

Hannestad & Raffelt, JCAP 0404 (2004) 008

Crotty, Lesgourgues & SP, PRD 69 (2004) 123007

2σ upper bound on Σmν (eV)

WMAP + ACBAR + SDSS + 2dF Previous + priors (HST + SN-Ia)

Page 26: MASSIVE NEUTRINOS  AND COSMOLOGY

Non-thermal relic neutrinos

The spectrum could be distorted after neutrino decoupling

Example: decay of a

light scalar after BBN

Cuoco, Lesgourgues, Mangano & SP, astro-ph/0502465

Thermal FD spectrum

Distortion from decay

CMB + LSS data still compatible with large deviations from a thermal neutrino spectrum (degeneracy NT distortion – Neff)

* Better expectations for future CMB + LSS data, but model degeneracy NT- Neff remains

/T p

Page 27: MASSIVE NEUTRINOS  AND COSMOLOGY

Future sensitivities to Σmν

• Next CMB data from WMAP and PLANCK (+ other CMB experiments on large l’s) temperature and polarization spectra

• SDSS galaxy survey: 106 galaxies (250,000 for 2dF)

• Fisher matrix analysis: expected sensitivities assuming a fiducial cosmological model

• Forecast analysis for

WMAP and ΩΛ=0 models Hu et al, PRL 80 (1998) 5255

Sensitivity to

With current best-fit values

eV 0.1N

hΩ 0.65 Σm

0.82m

νν

eV0.37 Σm

Recent update: Lesgourgues, SP & Perotto, PRD 70 (2004) 045016

Fiducial cosmological model:(Ωbh2 , Ωmh2 , h , ns , τ, Σmν ) = (0.0245 , 0.148 , 0.70 , 0.98 , 0.12, Σmν )

Page 28: MASSIVE NEUTRINOS  AND COSMOLOGY

PLANCK+SDSS

Lesgourgues, SP & Perotto, PRD 70 (2004) 045016

Ideal CMB+40xSDSS

Σm detectable at 2σ if larger than

0.21 eV (PLANCK+SDSS)

0.13 eV (CMBpol+SDSS)

Σm Σm

Fiducial value

2 sensitivity

Page 29: MASSIVE NEUTRINOS  AND COSMOLOGY

Future sensitivities to Σmν: new ideas

galaxy weak lensing and CMB lensing

no bias uncertaintysmall scales in linear regime

makes CMB sensitive to much smaller masses

Page 30: MASSIVE NEUTRINOS  AND COSMOLOGY

Future sensitivities to Σmν: new ideas

galaxy weak lensing and CMB lensing

sensitivity of future weak lensing survey(4000º)2 to mν

σ(mν) ~ 0.1 eV

Abazajian & DodelsonPRL 91 (2003) 041301

sensitivity of CMB(primary + lensing) to mν

σ(mν) = 0.15 eV (Planck)

σ(mν) = 0.044 eV (CMBpol)

Kaplinghat, Knox & SongPRL 91 (2003) 241301

Page 31: MASSIVE NEUTRINOS  AND COSMOLOGY

Neutrino masses in 3-neutrino schemes

Fig from Strumia & Vissani, hep-ph/0503246

CMB + galaxy clustering

+ HST, SNI-a [σ8]

+ Ly-α [bias]

PLANCK + SDSS

CMBpol + SDSS

CMBpol (including CMB lensing)

KATRIN

Page 32: MASSIVE NEUTRINOS  AND COSMOLOGY

Bounds on the sum of neutrino masses from CMB + 2dFGRS or SDSS, and other

cosmological data (best Σmν<0.42 eV, conservative Σmν<1 eV)

Conclusions

Sub-eV sensitivity in the next future (0.1-0.2 eV and better) Test degenerate

mass region and eventually the IH case

ν

Cosmological observables efficiently constrain some properties of (relic) neutrinos