Cosmological Aspects of Neutrino Physics (III)

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Cosmological Aspects of Neutrino Physics (III)
?

• Sergio Pastor (IFIC)
• 61st SUSSP
• St Andrews, August 2006

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Neutrino Physics and Cosmology
3rd lecture
Bounds on m? from CMB, LSS and other data
Bounds on the radiation content (Neff)
Future sensitivities on m? from cosmology
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Effect of massive neutrinos on the CMB and Matter
Power Spectra
Max Tegmark www.hep.upenn.edu/max/
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Neutrinos as Hot Dark Matter
Massive Neutrinos can still be subdominant DM
limits on m? from Structure Formation (combined
with other cosmological data)
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How to get a bound (measurement) of neutrino
masses from Cosmology
Fiducial cosmological model (Obh2 , Omh2 , h ,
ns , t, Sm? )
PARAMETER ESTIMATES
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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,s8)
• Lyman-a forest independent measurement of
  power on small scales
• Baryon acoustic oscillations (SDSS)
• Bounds on parameters from other data SNIa (Om),
  HST (h),

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Cosmological Parameters example
SDSS Coll, PRD 69 (2004) 103501
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Cosmological bounds on neutrino mass(es)
A unique cosmological bound on m? DOES NOT exist !
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Cosmological bounds on neutrino mass(es)
A unique cosmological bound on m? 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

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Cosmological bounds on neutrino masses using WMAP1
Bound on Sm? (eV) 95 CL Data used
Ichikawa et al, PRD 71 (2005) 043001 Sánchez et al, MNRAS 366 (2006) 189 MacTavish et al, astro-ph/0507503 1.6 - 3.1 CMB only
Hannestad, JCAP 0305 (2003) 004 SDSS Coll., PRD 69 (2004) 103501 Barger et al, PLB 595 (2004) 55 Crotty et al, PRD 69 (2004) 123007 Rebolo et al, MNRAS 353 (2004) 747 Fogli et al. PRD 70 (2004) 113003 Seljak et al, PRD 71 (2005) 103515 Sánchez et al, MNRAS 366 (2006) 189 MacTavish 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) 175 Fogli et al. PRD 70 (2004) 113003 Seljak et al, PRD 71 (2005) 103515 MacTavish et al, astro-ph/0507503 Hannestad, hep-ph/0409108 0.42-0.68 WMAP1, other CMB, 2dF/SDSS-gal, 2dF/SDSS-bias and/or Ly-a
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Cosmological bounds on neutrino masses using WMAP3
Bound on Sm? (eV) 95 CL Data used
WMAP Coll., astro-ph/0603449 Fukugita et al, astro-ph/0605362 Kristiansen et al, astro-ph/0608017 1.7 2.3 CMB only
WMAP Coll., astro-ph/0603449 Goobar et al, astro-ph/0602155 0.68 0.91 WMAP3, other CMB, 2dF/SDSS-gal, SNIa
Goobar et al, astro-ph/0602155 Seljak et al, astro-ph/0604335 Kristiansen et al, astro-ph/0608017 0.17-0.48 WMAP3, other CMB, 2dF/SDSS-gal, SDSS-BAO and/or Ly-a
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Neutrino masses in 3-neutrino schemes
CMB galaxy clustering
Fig from Strumia Vissani, NPB726(2005)294
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Tritium ? decay, 0?2? and Cosmology
Fogli et al., hep-ph/0608060
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0?2? and Cosmology
Fogli et al., hep-ph/0608060
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Parameter degeneracy Neutrino mass and w
In cosmological models with more parameters the
neutrino mass bounds can be relaxed. Ex
quintessence-like dark energy with ?DEw pDE
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Relativistic particles in the Universe
At Tltme, the radiation content of the Universe
is Effective number of relativistic neutrino
species Traditional parametrization of the energy
density stored in relativistic particles
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Extra relativistic particles

• Extra radiation can be
• scalars, pseudoscalars, sterile neutrinos
  (totally or partially
• thermalized, bulk), neutrinos in very low-energy
  reheating
• scenarios, relativistic decay products of heavy
  particles
• Particular case relic neutrino asymmetries

Constraints on Neff from BBN and from CMBLSS
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Effect of Neff at later epochs

• Neff modifies the radiation content
• Changes the epoch of matter-radiation equivalence

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CMBLSS allowed ranges for Neff

• Set of parameters ( Obh2 , Ocdmh2 , h , ns , A
  , b , Neff )
• DATA WMAP other CMB LSS HST ( SN-Ia)
• Flat Models
• Non-flat Models
• Recent result

Hannestad Raffelt, astro-ph/0607101
95 CL
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Future bounds on Neff

• Next CMB data from WMAP and PLANCK (other CMB
  experiments on large ls) temperature and
  polarization spectra
• Forecast analysis in O?0 models

Lopez et al, PRL 82 (1999) 3952
PLANCK
WMAP
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Future bounds on Neff
Updated analysis Larger errors
?Neff 3 (WMAP) ?Neff 0.2 (Planck)
Bowen et al 2002
Bashinsky Seljak 2003
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The bound on Sm? depends on the number of
neutrinos

• Example in the 31 scenario, there are 4
  neutrinos (including thermalized sterile)
• Calculate the bounds with N? gt 3

Abazajian 2002, di Bari 2002
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Sm? and Neff degeneracy
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Analysis with Sm? and Neff free
WMAP ACBAR SDSS 2dF
Previous priors (HST SN-Ia)
2s upper bound on Sm? (eV)
Hannestad Raffelt, JCAP 0404 (2004) 008 Crotty,
Lesgourgues SP, PRD 69 (2004) 123007
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Analysis with Sm? and Neff free
WMAP ACBAR SDSS 2dF
Hannestad Raffelt, astro-ph/0607101
Crotty, Lesgourgues SP, PRD 69 (2004) 123007
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Non-standard relic neutrinos
The cosmological bounds on neutrino masses are
modified if relic neutrinos have non-standard
properties (or for non-standard models)

• Two examples where the cosmological bounds do not
  apply
• Massive neutrinos strongly coupled to a light
  scalar field they could annihilate when becoming
  NR
• Neutrinos coupled to the dark energy the DE
  density is a function of the neutrino mass
  (mass-varying neutrinos)

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Non-thermal relic neutrinos
The spectrum could be distorted after neutrino
decoupling Example decay of a light scalar
after BBN

• 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

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Future sensitivities to Sm?
When future cosmological data will be available

• CMB (TP) galaxy redshift surveys
• CMB (TP) and CMB lensing
• Weak lensing surveys
• Weak lensing surveys CMB lensing

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PLANCKSDSS

• Fisher matrix analysis expected sensitivities
  assuming a fiducial cosmological model, for
  future experiments with known specifications

Fiducial cosmological model (Obh2 , Omh2 , h ,
ns , t, Sm? ) (0.0245 , 0.148 , 0.70 , 0.98 ,
0.12, Sm? )
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Future sensitivities to Sm? new ideas
weak gravitational and
CMB lensing lensing
No bias uncertainty Small scales much closer to
linear regime Tomography 3D reconstruction
Makes CMB sensitive to smaller neutrino masses
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Future sensitivities to Sm? new ideas
weak gravitational and
CMB lensing lensing
sensitivity of future weak lensing
survey (4000º)2 to m? s(m?) 0.1 eV Abazajian
Dodelson PRL 91 (2003) 041301
sensitivity of CMB (primary lensing) to
m? s(m?) 0.15 eV (Planck) s(m?) 0.044 eV
(CMBpol) Kaplinghat, Knox Song PRL 91 (2003)
241301
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CMB lensing recent analysis
s(M?) in eV for future CMB experiments alone
Lesgourgues et al, PRD 73 (2006) 045021
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Summary of future sensitivities
Lesgourgues SP, Phys. Rep. 429 (2006) 307
Future cosmic shear surveys
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End of 3rd lecture