Neutrino physics imprinted in the Cosmic Microwave Background Manoj - - PowerPoint PPT Presentation

Neutrino physics imprinted in the Cosmic Microwave Background

Manoj Kaplinghat University of California Irvine

Massive Neutrinos and Cosmology: Overview

Masses, number, BSM ν scattering, large asymmetry … Cosmic shear Lensed CMB Galaxies Ly-α forest 21 cm Primary CMB BBN Early phase structure formation

Future of Laboratory Constraints

Tritium endpoint

Aim: mνe < 0.2 eV at 95% CL (KATRIN) 0νββ: Test if neutrinos are Majorana particles Next gen ~ 100 meV and lower in double beta decay mass

Mass schemes from measurement of neutrino oscillation

Sum of neutrino masses greater than about 60 meV Both double beta decay experiments and cosmology should be able to probe this regime. Sum of neutrino masses greater than about 100 meV

atmospheric solar solar atmospheric

Massive Neutrino and Primary CMB

1 x 0.8 eV neutrino (dashed)

• Expansion rate increases
• Changes: gravitational potential,

damping and angle subtended by sound horizon For a precision probe, we need the physics after last scattering.

600 800 1000 1200 1400 1600 1800 2000

• 5. ¥10-11
• 1. ¥10-10

1.5 ¥10-10

• 2. ¥10-10

2.5 ¥10-10

• 3. ¥10-10

3.5 ¥10-10 Multipole Temperature lHl+1LClêH2pL

Jeans Instability for Neutrinos

Neutrino perturbations on length scales larger than the Jeans length become unstable and collapse into dark matter potential wells.

Bond and Szalay, ApJ 274, 443 (1983) Hu and Eisenstein, ApJ 498, 497 (1998) Hu, Eisenstein and Tegmark, PRL 80, 5255 (1998)

kJ(z)-1

Effect of non-zero neutrino mass on the density perturbations

kJ(now) H0

ΔP/P ~ 4 Ωnu/ΩM ~ 4(Σm/94 eV)/(ΩMh2)

0.001 0.005 0.010 0.050 0.100 0.500 1.000 0.93 0.94 0.95 0.96 0.97 0.98 0.99 1.00 k HhêMpcL PS HSmn = 0.12 eV in 3 nL PS HSmn = 0L

z=100 10 2

Effect of Lensing on the CMB

z

Deflection ~ arcmin

Coherence of (CMB) Lensing Deflection

Coherence ~ 10 deg Peak sensitivity ~ z=2

Estimate d from CMB maps Hu and Okamoto, 2002

Effect of Lensing on galaxy shapes: Cosmic Shear

5 10 50 100 500 1000

• 0.04
• 0.02

0.00 0.02 Multipole Cl HSmn = 0.12 eV in 3 nL Cl HSmn = 0L

• 1

Effect of massive neutrino on CMB lensing

EE TT dd

Best CMB constraints from lensing deflection measure (dd)

The dominant effect is due to the change in the angle subtended by the sound horizon

Unlensed TT, EE not the way for precision Σmν.

5 10 50 100 500 1000

• 0.04
• 0.02

0.00 0.02 Multipole Cl HSmn = 0.12 eV in 3 nL Cl HSmn = 0L

• 1

Effect of massive neutrino on CMB lensing

EE TT dd

Best CMB constraints from lensing deflection measure (dd)

The dominant effect is due to the change in the angle subtended by the sound horizon

5 10 50 100 500 1000

• 0.06
• 0.04
• 0.02

0.00 0.02 0.04 Multipole Cl HSmn = 0.12 eV in 1 nL Cl HSmn = 0L

• 1

Unlensed TT, EE not the way for precision Σmν.

Effect of dynamical dark energy on the density perturbations

~mφ H0

0.001 0.005 0.010 0.050 0.100 0.500 1.000 0.93 0.94 0.95 0.96 0.97 0.98 0.99 1.00 1.01 k HhêMpcL PS Hw0 = -0.9L PS Hw0 = -1L

Depends on w(a) and matter density

Neutrino mass and dark energy: can we infer them separately?

Kaplinghat, Knox and Song, PRL (2003)

The answer is yes! **

• ** if DE is only important at

late times

Both ν mass and DE are unknown late-time effects.

Prospects: CMB Lensing

Kaplinghat, Knox and Song, PRL 2003

CMB lensing (by itself) can measure the effect of finite neutrino mass allowing for DE EOS and running at the level of ~ 40 meV (1σ).

Lesgourgues, Perroto, Pastor, Piat PRD 2006

Extra radiation parameterized as Neff

5 10 50 100 500 1000

• 0.4
• 0.2

0.0 0.2 0.4 0.6 Multipole Cl HNeff = 4.04L Cl HNeff = 3.04L -1

Not a late time effect, but since CMB lensing is an integrated effect, this is important.

EE TT dd

Phase shift: a way to measure Nefg precisely

Information in phase shift: Bashinsky and Seljak 2004 (separate from damping!)

Follin, Knox, Millea and Pan 2015

Future: σ(Nν) ~ 0.3 (Planck polarization), 0.1 (CMB-S4)

Baumann, Green, Meyers and Wallisch 2015 (very nice description of the physics)

Key caveat

Cosmological probes are sensitive to the energy density of neutrinos. While the Jeans length does depend on the mass, it does not seem that we will be able to exploit this scale dependence to measure the mass hierarchy directly.

Current limits: assuming base ΛCDM model

X mν < 0.72 eV Planck TT+lowP ; X mν < 0.21 eV Planck TT+lowP+BAO ; X mν < 0.49 eV Planck TT, TE, EE+lowP ; X mν < 0.17 eV Planck TT, TE, EE+lowP+BAO . 95% C.L. assuming ΛCDM (Planck 2015 results XIII)

WMAP+HST+CMASS (conservative): ∑mv<0.36 eV (95% C.L. De Putter et al 2012)

Current limits: effect of dark energy EOS

DE with constant EOS+CDM+flatness (wCDM) WMAP7+H0+BAO (SDSS): ∑mv<1.3 eV WMAP7+SNe (constitution)+BAO (SDSS): ∑mv<0.9 eV WMAP7+LRGs (SDSS)+H0: ∑mv<0.8 eV Previous+SNe (constitution): ∑mv<0.5 eV (95% C.L. WMAP collaboration)

• Planck (including lensing)+WMAPpol+SDSS DR9: ∑mv<0.48 eV

(95% C.L. Guisarma et al 2013)

Current limits: complementarity of data sets — the case of Ly-α forest + CMB data

Palanque-Delabrouille et al 2015 (BOSS + Planck 2015)

)

• 1

k (h Mpc

• 4

10

• 3

10

• 2

10

• 1

10 1

(massless)

k

(massive) / P

k

P

0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 1.1

Level from CMB Lyman-alpha

= 0.5 eV, z=4

ν

m Σ = 0.5 eV, z=2

ν

m Σ = 0.5 eV, z=0

ν

m Σ = 1.0 eV, z=4

ν

m Σ = 1.0 eV, z=2

ν

m Σ = 1.0 eV, z=0

ν

m Σ

• 1

k (km/s)

0.002 0.004 0.006 0.008 0.01 0.012 0.014 0.016 0.018 0.02

π P(k)*k/

• 2

10

• 1

10

z=2.2 z=2.4 z=2.6 z=2.8 z=3.0 z=3.2 z=3.4 z=3.6 z=3.8 z=4.0 z=4.2 z=4.4

Palanque-Delabrouille et al 2015

8

σ

0.65 0.7 0.75 0.8 0.85 0.9

s

n

0.91 0.92 0.93 0.94 0.95 0.96 0.97 0.98 0.99 1

Planck (TT+lowP) + H α Ly- + Planck (TT+lowP) α Ly-

m

Ω

0.26 0.28 0.3 0.32 0.34 0.36 0.38 0.4 0.42 0.44

ν

m Σ

0.2 0.4 0.6 0.8 1 1.2

Planck (TT+lowP) + H α Ly- + Planck (TT+lowP) α Ly- 8

σ

0.65 0.7 0.75 0.8 0.85 0.9

ν

m Σ

0.2 0.4 0.6 0.8 1 1.2 Planck (TT+lowP) + H α Ly- + Planck (TT+lowP) α Ly-

P P

/dlnk

s

dn

• 0.04 -0.03 -0.02 -0.01

0.01 0.02 0.03

ν

m Σ

0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8

Planck (TT+lowP) α Planck (TT+lowP) + Ly- α Planck (TT,TE,EE+lowP) + Ly- + BAO α Planck (TT,TE,EE+lowP) + Ly-

Σmν < 0.19 eV (95%CL) m 0 12 eV (95%CL)

Planck (TT, TE, EE + lowP) + Lyα Σmν < 0.12 eV (95%CL) Planck (TT, TE, EE + lowP) + BAO + Lyα

~ 3σ preference for negative running ~ 2σ with older Ly-α data (Minor and Kaplinghat 2014).

Current limits: complementarity of data sets — the case of Ly-α forest + CMB data

Near Term CMB Lensing Experiments

Atacama Cosmology Telescope Polarization (ACTPol) South Pole Telescope Polarization (SPTPol→SPT-3G)

Near: ACTPol and SPTPol: σ(Σmν) ~ 100 meV; σ(Neff) ~ 0.12 Mid: SPT-3G forecast to σ(Σmν) ~ 74 meV; σ(Neff) ~ 0.076 (Benson et al arXiv:1407.2973; CMB 2015 at U Minnesotta)

Key degeneracies for the future: spatial curvature of the universe

Degeneracy between neutrino mass and curvature in lensing measurements. Smith, Hu and Kaplinghat, PRD 2004; PRD

2006.

If neutrino mass measurement is known to 0.1 eV accuracy, then it helps in the determination of curvature (0.3%) and dark energy equation of state from next generation ground based CMB experiments, Planck and

• SNAP. Smith, Hu and Huterer, ApJL 2007

Key degeneracies for the future: unknown expansion history of the universe

Parameterizing our ignorance of H(z) in terms of early DE, we find this to be a significant source of degeneracy. (De

Putter, Zahn, Linder PRD 2009, Joudaki and Kaplinghat, PRD 2012)

This degeneracy can be tamed if other data sets are used. Specifically the cosmic shear and CMB lensing degeneracies are not aligned and the addition of these two data sets can extend the reach to the 40 meV level.

Complementarity of data sets: the future

Joudaki and Kaplinghat PRD 2012

(Planck) (Planck) lensing,

rted

• rmal

0.001 0.005 0.01 0.05 0.02 0.1 0.04 0.06 0.08 0.1 0.15 0.22 0.3

Neutrino mass forecasts

CMB lensing (Planck) CMB lensing (Planck) fixing Curvature and Early Dark Energy CMB lensing, Weak lensing, Galaxy power spectrum, SNe

Inverted Normal 0.001 0.005 0.01 0.05 0.02 0.1 0.04 0.06 0.08 0.1 0.16 0.2 0.3 Lightest Neutrino Mass HeVL Sum of neutrino masses HeVL

Abazajian et al 2013 (Snowmass) Wu et al 2014

CMB lensing, Weak lensing, Galaxy power spectrum, SNe CMB lensing (Planck) fixing Curvature and Early Dark Energy CMB lensing (Planck)

0.05 0.10 0.20 0.50 0.001 0.005 0.010 0.050 0.100 0.500 Sum of neutrino masses HeVL Double beta decay mass HeVL

Joudaki and Kaplinghat PRD 2012