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Tension between Planck constraints and local
Universe measurements?
• Planck found quite large changes in some parameters of the base ΛCDM
model when compared with those from other astrophysical measurements:
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Riess et al (2011)
Friedmann et al. (2012)
Planck+WP+highL :
1
H0  67.3  1.2 km s Mpc
1
H0  74.08  2.25 km s1 Mpc1
Heymans et al. (2013)
Planck+WP+highL :
CFHTLenS:
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σ8 (Ωm /0.27)0.46  0.89  0.03
(68% errors)
σ8 (Ωm /0.27)0.460.02  0.744  0.04
Lucia A. Popa
March 22-29, 2014
Planck+WP+highL+BAO
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Possible interpretation of the existing tension
• Some sources of systematic error in cosmological measurements are not
completely understood – Planck Collaboration (2013), Spergel et al. (2013)
• Existing tension between different data-sets -Hou et al. (2013)
• Extrapolation of CMB measurements (z~1000) to z=0 within the base ΛCMB
model that can be inadequate or incomplete.
Extensions of the based ΛCMB model
 massive neutrinos with  mυ  0.15 eV
 extra radiation energy density:
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Verde et al. (2013)
Neff  3.6  3.8
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 sterile neutrino with eV-mass scale required by the SBL data
Gariazzo et al. (2013); Wyman et al. (2013)
 phantom values of dark energy equation of state (w ∼ −1.2)
or small positive curvature
3
2
Verde,Protopapas,Jimenez (2013)
 7 10
 ΩK  1.5 10

No single parameter extension to the baseline ΛCDM
model helps to alleviate the tension
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March 22-29, 2014
Lepton Asymmetric Universe ?
• Affleck-Dine mechanism during or after reheating
• Active-sterile neutrino oscillations after the electroweak phase
transition
• Large lepton asymmetry can postpone symmetry restoration in nonsupersymmetric or supersymmetric models.
chemical potential
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LSS - delay of matter-radiation equality shifts the power spectrum turnover
position toward larger scales, suppressing the power at small scales.
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YP
sensitive to expansion rate
Neutrino freeze out earlier with direct effect
on n-p interactions:
υ  n  p  e e  n  p  ~
υ
e
e
YP sensitive to ξ e
BBN
~
ξ e  0 more e than 
e
Aver et al. (2012)
n/p goes down
Y goes down
P
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Degenerate massive neutrinos
Planck + WP + highL +BAO
 mυ  0.25 eV ;
 mυ  0.35 eV ;
Neff  3.33  0.19
Neff  3.40  0.22
(68% CL)
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eff
 m  0.28 eV; ms  0.43 eV ; Neff  3.40  0.22
eff
 m  0.23 eV; ms  0.21 eV ; Neff  3.22  0.13
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(Vikhlinin et al. 2009)
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Non-degenerate massive neutrinos
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Global fit of neutrino mixing parameters (Maltoni et al. 2013):
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(68% error)
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Conclusions:
• For all cosmological asymmetric models we find a preference of
cosmological data for smaller values of active and sterile neutrino masses
when compared with base ΛCDM case.
• An increased tension between cosmological asymmetric models and
short baseline neutrino oscillation data that favors a sterile neutrino with
the mass of ∼ 1 eV.
• For the case of degenerate massive neutrinos , tensions between direct
determination of Hubble constant and cluster abundance are alleviated (at
about 1.3 σ level)
• Preference of cosmological data (at ~2 σ statistical significance) for
normal neutrino hierarchy.
Cosmological data favor the leptonic asymmetric extension of the base
ΛCDM model and normal neutrino mass hierarchy over the models with
additional sterile neutrino species and/or inverted neutrino mass
hierarchy.
49th Rencontres de Moriond
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March 22-29, 2014