neutrino masses from cosmological observables
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ν. Neutrino masses from cosmological observables. Sergio Pastor (IFIC) Benasque Cosmology workshop 15 / 08 / 2006. Outline. Introduction: the Cosmic Neutrino Background. Relic Neutrinos as DM. Neutrino masses from cosmological observables. Effect of neutrino masses - PowerPoint PPT PresentationTRANSCRIPT
04/21/23
Neutrino masses from cosmological observables
Sergio Pastor (IFIC)
Benasque Cosmology workshop
15 / 08 / 2006
ν
Outline
Relic Neutrinos as DM
Effect of neutrino masses on cosmological observables
Current bounds and future sensitivities
Neutrino masses from cosmological
observables
Introduction: the Cosmic Neutrino Background
This is a neutrino!
T~MeVt~sec
Free-streaming neutrinos
(decoupled)Cosmic Neutrino
Background
Neutrinos coupled by weak
interactions(in equilibrium)
Neutrinos keep the energy spectrum of a relativistic
fermion with eq form
1e1
T)(p,f p/T
Primordial
Nucleosynthesis
At least 2
species are
NR today
Relativistic neutrinos
T~
eV
Neutrino cosmology is interesting because Relic neutrinos are very abundant:
• The CNB contributes to radiation at early times and to matter at late times (info on the number of neutrinos and their masses)
• Cosmological observables can be used to test non-standard neutrino properties
04/21/23
Evolution of the background densities: 1 MeV → now
photons
neutrinos
cdm
baryons
Λ
m3=0.05 eV
m2=0.009 eV
m1≈ 0 eV
Ωi= ρi/ρcrit
The Cosmic Neutrino Background
• Number density
• Energy density
323
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
At present 112 per flavour cm )( -3
Contribution to the energy density of the Universe
eV 93.2
mh Ω i
i2
ν
52 101.7h Ω ν
We know that flavour neutrino oscillations exist
From present evidences of oscillations from experiments measuring atmospheric, solar, reactor and accelerator neutrinos
Evidence of Particle Physics beyond the Standard Model !
),,(),(e, 321 ννντμ
Mixing Parameters...From present evidences of oscillations from experiments measuring
atmospheric, solar, reactor and accelerator neutrinos
Mixing matrix U
Maltoni, Schwetz, Tórtola, Valle, NJP 6 (2004) 122
Mixing Parameters...From present evidences of oscillations from experiments measuring
atmospheric, solar, reactor and accelerator neutrinos
Mixing matrix U
Maltoni, Schwetz, Tórtola, Valle, NJP 6 (2004) 122
... and neutrino masses
eV
Data on flavour oscillations do not fix the absolute scale of neutrino masses
atmatm
solar
solar
eV 0.009 Δm
eV 0.05Δm
2sun
2atm
NO
RM
AL
INV
ER
TE
D
eV
m0
What is the value of m0 ?
Direct laboratory bounds on mν
Searching for non-zero neutrino mass in laboratory experiments
• Tritium beta decay: measurements of endpoint energy
m(νe) < 2.2 eV (95% CL) Mainz-Troitsk
Future experiments (KATRIN) m(νe) ~ 0.3 eV
• Neutrinoless double beta decay: if Majorana neutrinos
76Ge experiments: ImeeI < 0.4hN eV
e -33 eHe H
-2e2)Z(A, Z)(A,
Absolute mass scale searches
Neutrinoless double beta decay
< 0.4-1.6 eV
Tritium decay < 2.2 eV
2/1
22
iiei mUm
e
< 0.3-2.0 eVCosmology i
im~
i
ieiee mUm 2
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 15 m 0.3Ω Ω
eV 46 m 1 Ω eV 93.2
mhΩ
iimν
iiν
ii
2ν
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
eV 15 m 0.3Ω Ω
eV 46 m 1 Ω eV 93.2
mhΩ
iimν
iiν
ii
2ν
Neutrinos as Hot Dark Matter
Massive Neutrinos can still be subdominant DM: limits on mν from Structure Formation (combined with other cosmological data)
Power Spectrum of density fluctuations
Matter power spectrum is the Fourier transform of the
two-point correlation function
Field of density Fluctuations
)(
)(x
x
Neutrinos as Hot Dark Matter: effect on P(k)
• 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)
ffν
Structure formation after equality
baryon and CDM
experiencegravitational
clustering
Structure formation after equality
baryon and CDM
experiencegravitational
clustering
Structure formation after equality
baryon and CDM
experiencegravitational
clustering
growth of /(k,t) fixed by
« gravity vs. expansion » balance
a
Structure formation after equality
baryon and CDM
experiencegravitational
clustering
neutrinosexperience
free-streamingwith
v = c or <p>/m
Structure formation after equality
baryon and CDM
experiencegravitational
clustering
Structure formation after equality
baryon and CDM
experiencegravitational
clustering
baryon and CDM
experiencegravitational
clustering
neutrinosexperience
free-streamingwith
v = c or <p>/m
neutrinos cannot cluster below a diffusion length
= ∫ v dt < ∫ c dt
Structure formation after equality
baryon and CDM
experiencegravitational
clustering
baryon and CDM
experiencegravitational
clustering
neutrinosexperience
free-streamingwith
v = c or <p>/m
o neutrinos cannot cluster below a diffusion length
= ∫ v dt < ∫ c dt
for (2/k) < ,free-streaming supresses growth of structures during MD
a1-3/5 f with f = /m ≈ (m)/(15 eV)
Structure formation after equality
baryon and CDM
experiencegravitational
clustering
baryon and CDM
experiencegravitational
clustering
neutrinosexperience
free-streamingwith
v = c or <p>/m
J.Lesgourgues & SP, Phys Rep 429 (2006) 307 [astro-ph/0603494]
Structure formation after equality
cdm
b
metric
a
Massless neutrinos
J.Lesgourgues & SP, Phys Rep 429 (2006) 307 [astro-ph/0603494]
Structure formation after equality
cdm
b
metric
a
1-3/5fa
Massive neutrinos
fν=0.1
Effect of massive neutrinos on P(k)
Observable signature of the total mass on Observable signature of the total mass on P(k) :P(k) :P(k) massiveP(k) massive
P(k) masslessP(k) massless
variousvariousffν
Lesgourgues & SP, Phys. Rep. 429 (2006) 307
DATA on CMB temperature /polarization anisotropies
Multipole Expansion
Map of CMBR temperature Fluctuations
T
T-),T(),Δ(
Angular Power Spectrum
Effect of massive neutrinos on the CMB spectra
1) Direct effect of sub-eV massive neutrinos on the evolution of the baryon-photon coupling is very small
2) Impact on CMB spectra is indirect: non-zero Ων today implies a change in the spatial curvature or other Ωi . The background evolution is modified
Ex: in a flat universe,
keep ΩΛ+Ωcdm+Ωb+Ων=1
constant
Crotty, Lesgourgues & SP, PRD 67 (2003)
3.32.1eff 3.5N
Effect of massive neutrinos on the CMB spectra
Problem with parameter degeneracies: change in other cosmological parameters can mimic the effect of nu masses
Effect of massive neutrinos on the CMB and Matter Power
Spectra
Max Tegmark
www.hep.upenn.edu/~max/
How to get a bound (measurement) of neutrino masses from Cosmology
DATA
Fiducial cosmological model:(Ωbh2 , Ωmh2 , h , ns , τ, Σmν )
PARAMETERESTIMATES
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
* Baryon acoustic oscillations (SDSS)
Bounds on parameters from other data: SNIa (Ωm), HST (h), …
Cosmological Parameters: example
SDSS Coll, PRD 69 (2004) 103501
Cosmological bounds on neutrino mass(es)
A unique cosmological bound on mν DOES NOT exist !
ν
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 combination of cosmological data used
• The assumed cosmological model: number of parameters (problem of parameter degeneracies)
• The properties of relic neutrinos
Cosmological bounds on neutrino masses using WMAP1
390280640 . . .
Bound on Σmν (eV) [95% CL]
Data used
Ichikawa et al, PRD 71 (2005) 043001Sánchez et al, MNRAS 366 (2006) 189MacTavish et al, astro-ph/0507503
1.6 - 3.1 CMB only
Hannestad, JCAP 0305 (2003) 004 SDSS Coll., PRD 69 (2004) 103501Barger et al, PLB 595 (2004) 55Crotty et al, PRD 69 (2004) 123007Rebolo et al, MNRAS 353 (2004) 747Fogli et al. PRD 70 (2004) 113003Seljak et al, PRD 71 (2005) 103515Sánchez et al, MNRAS 366 (2006) 189MacTavish et al, astro-ph/0507503
1.0 - 1.7 [0.6-1.2]
WMAP1, other CMB, 2dF/SDSS-gal [HST,SNIa]
WMAP Coll., ApJ Suppl 148 (2003) 175Fogli et al. PRD 70 (2004) 113003 Seljak et al, PRD 71 (2005) 103515MacTavish et al, astro-ph/0507503Hannestad, hep-ph/0409108
0.42-0.68
WMAP1, other CMB, 2dF/SDSS-gal, 2dF/SDSS-bias and/or Ly-α
Cosmological bounds on neutrino masses using WMAP3
390280640 . . .
Bound on Σmν (eV) [95% CL] Data used
WMAP Coll., astro-ph/0603449Fukugita et al, astro-ph/0605362Kristiansen et al, astro-ph/0608017
1.7 – 2.3 CMB only
WMAP Coll., astro-ph/0603449Goobar et al, astro-ph/0602155
0.68 – 0.91WMAP3, other CMB, 2dF/SDSS-gal, SNIa
Goobar et al, astro-ph/0602155Seljak et al, astro-ph/0604335Kristiansen et al, astro-ph/0608017
0.17-0.48
WMAP3, other CMB, 2dF/SDSS-gal, SDSS-BAO and/or Ly-α
Fogli et al., hep-ph/0608060
Neutrino masses in 3-neutrino schemes
Fig from Strumia & Vissani, NPB726(2005)294
CMB + galaxy clustering
+ HST, SNI-a…
+ BAO and/or bias
+ including Ly-α
02 and Cosmology
Fogli et al., hep-ph/0608060
Future sensitivities to Σmν
1. CMB (T+P) + galaxy redshift surveys
2. CMB (T+P) and CMB lensing
3. Weak lensing surveys
4. Weak lensing surveys + CMB lensing
When future cosmological data will be available
PLANCK+SDSS
Lesgourgues, SP & Perotto, PRD 70 (2004) 045016
Σm detectable at 2σ if larger than
0.21 eV (PLANCK+SDSS)
0.13 eV (CMBpol+SDSS)
Fiducial cosmological model:(Ωbh2 , Ωmh2 , h , ns , τ, Σmν ) =
(0.0245 , 0.148 , 0.70 , 0.98 , 0.12, Σmν )
• Fisher matrix analysis: expected sensitivities assuming a fiducial cosmological model, for future experiments with known specifications
Future sensitivities to Σmν: new ideas
weak gravitational and CMB lensing
lensing
No bias uncertaintySmall scales much closer
to linear regimeTomography:
3D reconstruction
Makes CMB sensitive to smaller neutrino masses
Future sensitivities to Σmν: new ideas
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
Lesgourgues, Perotto, SP & PiatPRD 73 (2006) 045021
weak gravitational and CMB lensing
lensing
CMB lensing: recent analysis
σ(Mν) in eV for future CMB experiments alone : Lesgourgues et al, PRD 73 (2006) 045021
Perotto et al, astro-ph/06062271
CMB lensing: recent analysis
Summary of future sensitivities
Lesgourgues & SP, Phys. Rep. 429 (2006) 307
Future cosmic shear surveys
Physics Reports 429 (2006) 307-379 [astro-ph/0603494]
For more details see
Current bounds on the sum of neutrino masses from cosmological data
(best Σmν<0.2-0.4 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 can be used to bound (or measure) the absolute scale of
neutrino masses. Information complementary
to laboratory results