NEUTRINO-LIKE COSMOLOGY · ΛCDM+N eff+ Ω k+fν+n s ΛCDM+N eff ... Single temperature: Density:...

NEUTRINO-LIKE COSMOLOGY Signe Riemer-Sørensen University of Queensland Review in PASA arXiv:1301.7102 (Riemer-Sørensen, Parkinson, Davis)

Measurements

ΛCDM+Neff+Ωk+fν+ns ΛCDM+Neff+Ωk+fν+w ΛCDM+Neff+fν+w ΛCDM+Neff+Ωk+fν ΛCDM+Neff+Ωk ΛCDM+Neff+Yp

ΛCDM+Neff+fν

ΛCDM+Neff

2

3

4

5

6

7

Neff

W7+SPT+BAO

+H0+Union2 1

W7+CM

B+LRG+SN+H0 2

W7+CM

B+BAO+SN+H0 3

W7+CM

B+LRG+H0 4

W7+CM

B+BAO+H0 5

W7+H0+W

L+BAO+H(z)+Union2 6

W7+SPT+W

iggleZ+H(z)+BAO+SNLS

7

W9+SPT+W


8

W7+SPT+BAO

+H0 9W7+SPT+BAO

+H0+Union2 10

W7+ACT+SPT+BAO

+H0 11

W7+ACT+SPT+BAO

+H0 12

W7+BAO

+H0 13W7+ACT

14W7+ACT+BAO

+H0 15W7+SPT+W


16

W7+CM

B+LRG+H0 17

W7+CM

B+BAO+H0 18

W7+ACT+SPT+LRG

+H0 19

W7+SPTSZ+BAO

+H0 20

W7+SDSS+H0 21

W7+SDSS+H0+Union2 22

W7+SDSS+H0+Union2+

4He+D/H23

W7+H0+W

L+BAO+H(z)+Union2 24

W7+SPT+BAO

+H0 25W7+SNLS+BAO

+BOSS

26

W7+SPT+BAO

+H0 274He 28D/H

29D/H+

4He 30W7+D/H

31W7+SPT(agnostic) 32

W7+SPT

33W7+ACT+SPT+BAO

+H0 34

W7+ACT+SPT+LRG

+H0 35

W7+SPT+BAO

+H0 36W7+SPT

37W7+ACT+BAO

+H0 38W7+ACT

39W7+LRG

+H0 40W7+BAO

+H0 41W5+LRG

+maxBG

C+H0 42

W5+CM

B+BAO+fgas+H0 43

W5+LRG

+H0 44W5+BAO

+SN+H0 45W7+H0+SDSS+SN+CHFTLS

46

W7+SPT+H(z)+H0 47

W7+H0+W


W7+ACBAR+BAO

+H0+ACT49

W7+ACBAR+ACT+SPT+SDSS+H0 50

W7+ACBAR+ACT+SPT+SDSS+M

SH0 51

W7+SPT+BAO

+H0 52W7+SPT

53W7+H0 54

W7+SPT+BAO

+H0 55W7+SPT

56W7+SPT+BAO

+H0 57W9+ACT+SPT+BAO

+H0 58

Early Universe and cosmology

str.llnl.gov

Neutrino decoupling

str.llnl.gov

Neutrino decoupling (MeV)

Fermi-Dirac phase space Single temperature: Density: Ultra relativistic if mν< 1eV

Tν =411!

"#

$

%&1/3

Tγ

ρν = Neff7π 2

120T 4ν

energy density in one family with temp T

Dark radiation effects Expansion Nuclear Structure

Changing weak interaction rates

Suppressing structure formation

CMB Galaxies

Abundances (D, He, Li) Galaxies

CMB experiments Galaxy surveys

CMB experiments Galactic abundances Inter galactic absorption in quasar spectra

Galaxy surveys Lyman alpha forest

H 2 (z) ≈ 8πG3

ργ + ρν( )

Nucleosynthesis (BBN)

str.llnl.gov

Nucleosynthesis (0.8 MeV)

Formation of D (n+p) and He (2n+2p) Increase expansion rate: More D, He Sterile neutrinos change electron neutrino spectrum?

Electron re-combination

str.llnl.gov

Photon re-heating (0.2 MeV)

e-+e+ -> γγ Photon re-heating Absorbed in so Neff = 3.046

ρν = Neff7π 2

120T 4ν

Matter-radiation equality

str.llnl.gov

Matter-radiation equality (0.8 eV)

Determines when structures can grow

aeqa0

=1

1− fνΩr

Ωm

Recombination and photon decoupling

str.llnl.gov

Recombination (e++p) Photon decoupling (CMB) (0.25 eV)

map.gsfc.nasa.gov

francisthemulenews.wordpress.com

Hinshaw, 2013

Cosmic microwave background

Temperature fluctuations in the Cosmic Microwave Background

Tem

per

ature

flu

ctuat

ions

[μK

2]

Amplitude (matter-radiation equality)

Damping tail (expansion, diffusion,

anisotropic stress)

Peak positions (expansion)

Increase Neff

• Change positions and amplitudes

Increase Σmν

• Very little effect

Structure formation

str.llnl.gov

Neutrinos become non-relativistic Remove “matter” Structures form slower

Structure formation

znr ≈ 2×103 mν ,i

eV

Neutrinos wipe out structure

ilovephilosophy.com

Galaxy surveys

Hubblesite.org

num

ber

of

gala

xy p

airs

per

vol

um

e

Large scales Small scales

faint wiggles = acoustic

oscillations

Increase Neff • Suppress power on small scales

Increase Σmν

• Suppress power on small scales

Degeneracies

Complicating factors •  Oscillation experiments prefer ~eV

mass – ruled out by cosmology unless

•  non-thermal velocity distribution •  can change nucleosynthesis •  can avoid mass bounds from structure

formation

•  non-equilibrium

•  lepton asymmetry •  suppress oscillation to sterile states

via matter-like effects •  enhance production via resonances

Saviano et al. 2013

Results

ΛCDM+Neff+Ωk+fν+ns ΛCDM+Neff+Ωk+fν+w ΛCDM+Neff+fν+w ΛCDM+Neff+Ωk+fν ΛCDM+Neff+Ωk ΛCDM+Neff+Yp

ΛCDM+Neff+fν

ΛCDM+Neff

2

3

4

5

6

7

Neff

W7+SPT+BAO

+H0+Union2 1

W7+CM

B+LRG+SN+H0 2

W7+CM

B+BAO+SN+H0 3

W7+CM

B+LRG+H0 4

W7+CM

B+BAO+H0 5

W7+H0+W

L+BAO+H(z)+Union2 6

W7+SPT+W


7

W9+SPT+W


8

W7+SPT+BAO

+H0 9W7+SPT+BAO

+H0+Union2 10

W7+ACT+SPT+BAO

+H0 11

W7+ACT+SPT+BAO

+H0 12

W7+BAO

+H0 13W7+ACT

14W7+ACT+BAO

+H0 15W7+SPT+W


16

W7+CM

B+LRG+H0 17

W7+CM

B+BAO+H0 18

W7+ACT+SPT+LRG

+H0 19

W7+SPTSZ+BAO

+H0 20

W7+SDSS+H0 21

W7+SDSS+H0+Union2 22

W7+SDSS+H0+Union2+

4He+D/H23

W7+H0+W


W7+SPT+BAO

+H0 25W7+SNLS+BAO

+BOSS

26

W7+SPT+BAO

+H0 274He 28D/H

29D/H+

4He 30W7+D/H

31W7+SPT(agnostic) 32

W7+SPT

33W7+ACT+SPT+BAO

+H0 34

W7+ACT+SPT+LRG

+H0 35

W7+SPT+BAO

+H0 36W7+SPT

37W7+ACT+BAO

+H0 38W7+ACT

39W7+LRG

+H0 40W7+BAO

+H0 41W5+LRG

+maxBG

C+H0 42

W5+CM

B+BAO+fgas+H0 43

W5+LRG

+H0 44W5+BAO

+SN+H0 45W7+H0+SDSS+SN+CHFTLS

46

W7+SPT+H(z)+H0 47

W7+H0+W


W7+ACBAR+BAO

+H0+ACT49

W7+ACBAR+ACT+SPT+SDSS+H0 50

W7+ACBAR+ACT+SPT+SDSS+M

SH0 51

W7+SPT+BAO

+H0 52W7+SPT

53W7+H0 54

W7+SPT+BAO

+H0 55W7+SPT

56W7+SPT+BAO

+H0 57W9+ACT+SPT+BAO

+H0 58

Neff summary •  Effects of relativistic species •  Change nucleosynthesis -> increased abundances •  Increase expansion rate -> dampen structure •  Matter redistribution -> dampen structure

•  Parametrised as effective number of neutrinos

•  APPLIES TO ALL RELATIVISTIC SPECIES AND CHANGES TO GRAVITY

•  Planck expected to measure ΔNeff with an uncertainty of

0.1

•  If Neff ≠ 3: precise measurements of primordial nuclear abundances break degeneracies

Sterile neutrino dark matter •  eV scale dark matter ruled out by phase-space constraints • νMSM •  neutrino mass generation and flavour oscillations •  baryon asymmetry •  dark matter, keV mass -> non-relativistic before CMB •  resonantly produced, non-thermal, require lepton asymmetry •  keV emission

1 10ms [keV]

10-14

10-12

10-10

10-8

10-6

sin

2(2!)

Sterile neutrino dark matter Emission line searches: Bullet Cluster, Milky Way, M31, Ursa Minor (Boyarsky et al., Watson et al. Loewenstein et al., Abazajian et al., Yüksel et al.)

Too much dark matter, Ων>Ω

DM

L > 2.5×10-3 violating BBN

Phas

e sp

ace

const

rain

ts

1 10ms [keV]

10-14

10-12

10-10

10-8

10-6

sin

2(2!)

Sterile neutrino dark matter Emission line searches: Bullet Cluster, Milky Way, M31, Ursa Minor (Boyarsky et al., Watson et al. Loewenstein et al., Abazajian et al., Yüksel et al.)

Too much dark matter, Ων>Ω

DM

L > 2.5×10-3 violating BBN

Phas

e sp

ace

const

rain

ts

Lyman alpha (Viel et al., Seljak et al., Boyarsky et al.)

Majoron dark matter •  Seesaw mechanism

to generate neutrino masses

•  Break lepton symmetry -> massive Nambu-Goldstone boson: Majoron

•  keV-GeV mass dark matter

•  J -> νν, J -> γγ

100 102 104 106 108

Ea [keV]

10−40

10−35

10−30

10−25

KJaa [

s−1 ]

A4 symmetry with u6 = 100 MeVA4 symmetry with u6 = 10 MeVA4 symmetry with u6 = 1 MeVA4 symmetry with u6 = 10 keVA4 symmetry with u6 = 100 eV

Observational constraints

`=1 `=0.1

v 3 = 5

GeV

v 3 = 1

GeV

v 3 = 0

.1 G

eVv 3 =

0.0

1 Ge

V

Bazzocchi et al. 2008, Esteves et al. 2010, Lattanzi, SRS et al. in prep

PRELIMINARY

Neutrino dark matter summary • Models for neutrino mass generation can provide dark matter • Some models can be constrained observationally • Relevant because no SUSY needed

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