Neutrino Masses in Cosmology Carlos Peña Garay IFIC, Valencia Jimenez et al, 1003.5918 Villaescusa et al, 1104.4770, 1106.2543 Nov 18th, 2011 GDR meeting, Annecy

Neutrino and impact on observables ~ 1s ~ 0.3 Myr ~ 1-10 Gyr Neutrino Photon LSS Decoupling Influence in background and growth of structure

Neutrinos in the early universe: Radiation density after neutrino decoupling and BBN (T< me): At present 112 per flavour

Extra light states Blue: CMB+HST+SDSS Red: CMB+HST+SDSS +SN-Ia Giusarma et al., 1102.4774

Evolution of background density photons neutrinos cdm baryons Λ Ωi= ρi/ρcrit m=1 eV m=0.05 eV m=0.009 eV m≈ 0 eV Lesgourgues-Pastor

Neutrino mass influence in linear P(k) - Change in matter-radiation equality - Suppression of power on scales smaller than the free-streaming scale 0.05 eV 0.5 eV

Linear and non Linear P(k)

Cosmological probes of neutrino mass 95%

Cosmological probes of neutrino mass 95% arXiv: 1103:5083

n mass and the Weakest force Impact of single neutrino masses ? Can we see the neutrino hierarchy in the sky ?

Parameterization: S, D, sgn(D) Solar splitting can be safely neglected ( < 1%)

P(k) dependence on D Numerical with CAMB

NH-IH quasi-degeneracy No distinguishable NH-IH Delta could be measured ! Handle to identify neutrinos

Can we see n-hierarchy in the sky? Full sky, variance-dominated Gal survey, 600 Gpc3 (z<2) WL survey (<z> < 3) 21cm HI, 2000 Gpc3 (z<5) 50 gal / sq-arcmin

n mass and the Weakest force Beyond linear order: Nonlinear effects of neutrinos in the dark matter power spectrum Observable effects in the deepest and shallowest DM potential wells

Facing the tiniest and the biggest (mass) mn ~ 9 10-38 kg MCOMA ~ 4 1045 kg

Dark matter profile: NFW + EL Zhao et al, AJ’09 Mvir (Msun) Rvir (Mpc) rhoc Rs (Mpc) z=5 1.1e12 0.057 3.8e16 0.014 z=1 2.0e14 0.905 1.7e15 0.223 z=0 1.4e15 2.856 4.3e14 0.664

n overdensity M=1015 Msun Large neutrino overdensity (~linear with cluster mass) Interesting region around Mpc scale Best observable: Convergence measured by Weak Lensing

Convergence Observable proportional to column density

Relative convergence due to n z=1 z=0.4 0.3 eV - 10^4 clusters to obtain a 5-s result Expected in a full-sky weak lensing survey N-body simulation (in progress): needed to confirm signal and study systematics

Facing the tiniest and the emptiest Voids : Underdense regions (z=0: from ~ 0 to ~ 0.3 times the mean density at 10 Mpc) Neutrinos make them smaller and denser : delay the rate at which DM is evacuated Density contrast decreases by 10% for S = 1eV Statistics of voids depends on S and s8 Observable: Lyman-a signature (quasar at z=2.2, z=4) of low density regions

High Transmission regions if the Ly-a forest N-body simulations 4500 random line of sight Compute transmitted flux Count weak absorption region

Sensitivity to neutrino mass PDF for the number of regions (100/h Mpc) above threshold Degeneracy could be broken by using several redshift quasar Study of systematics: calibrating the flux at weak absorption

Conclusions Cosmological neutrinos expected to be indirectly seen in cosmological data: Relativistic energy seeen in CMB, and total mass by CMB & LSS. Linear growth will be sensitive to the atmospheric splitting: handle to verify neutrino nature of the total mass effect. Difficult to distinguish NH from IH unless total mass < 0.1 eV. Study nonlinear effects: N-body simulations Neutrinos in clusters: Clean (mostly DM) but high precision needed ( < 1 %) Impact of neutrinos in voids: Not clean (baryons) but larger signal (~ 10%)

Extra light states Blue: WMAP-7 Red: w7+SN+Bao+H0 Green: w7+CMBsuborb+SN+LRG+H0 [eV]

Neutrino mass by the Weak Force Normal Hierarchy Inverted Hierarchy Degenerate

Neutrino mass by the Weak Force If q13=0 NH~IH Gonzalez-Garcia et al 2010 Different pattern for leptons and quarks

Neutrinoless double beta decay Are neutrinos Dirac or Majorana? 0nbb: nn  ppe–e– without neutrinos me |<mnee>| = (T1/2 FN )1/2 FN = G0n |M0nf – (gA/ gV)2 M0nGT |2

Mass scale onbb: predictions Present experiments aim at IH scale NH may lead to negligible signal j |<mnee>| = |S mj Uej2 | = |S mj | Uej | 2 eif |

Mass scale searches: beta decay 0nbb decay cosmology If Majorana neutrinos Reid et al 2010, …