Could the H0 Tension be Pointing Toward the Neutrino Mass ...€¦ · Miguel Escudero (KCL) H0 and the Majoron Beyond19 01-07-19 The Hubble Tension 4 Taken from Wendy Freedman, see

Could the H0 Tension be Pointing Toward the Neutrino Mass Mechanism?

Beyond 2019Warsaw

Miguel Escudero [email protected]

based on ArXiv:1907.XXXXX with Sam Witte

mailto:[email protected]

m⌫ 6= 0

⌫e ! ⌫µ

H0

m⌫ 6= 0

⌫e ! ⌫µ⌫̄

⌫

�

H0

H0 and the Majoron Beyond19 01-07-19Miguel Escudero (KCL)

Outline

3

1) The Hubble Tension

2) The Scenario

3) Cosmology with a light Majoron

4) Conclusions


The Hubble Tension

4

Taken from Wendy Freedman, see 1706.02739


The Hubble Tension

4


H0 = 67.36± 0.54 km s�1 Mpc�1

4.4 σ tension within ΛCDM!

Planck 2018 1807.06209

Riess et al 1903.07603

H0 = 74.03± 1.42 km s�1 Mpc�1


The Hubble Tension

4


Tension very unlikely generated by CMB systematicssee e.g. Spergel et al 1312.3313, Addison et al 1511.00055, Verde et al 1601.01701, Planck 1608.02487

H0 = 67.36± 0.54 km s�1 Mpc�1


Planck 2018 1807.06209


H0 = 74.03± 1.42 km s�1 Mpc�1


The Hubble Tension

4



Local measurements have also been checked against systematicssee e.g. Efstathiou 1311.3461, Cardona et al 1611.06088, Zhang et al 1706.07573, Follin & Knox 1707.01175

H0 = 67.36± 0.54 km s�1 Mpc�1


Planck 2018 1807.06209


H0 = 74.03± 1.42 km s�1 Mpc�1


The Hubble Tension

4




Tension between H0 local and BAO is also presentsee Addison et al 1707.06547, Font-Ribera et al 1906.11628

H0 = 67.36± 0.54 km s�1 Mpc�1


Planck 2018 1807.06209


H0 = 74.03± 1.42 km s�1 Mpc�1


The Hubble Tension

4




Tension between H0 local and BAO is also presentsee Addison et al 1707.06547, Font-Ribera et al 1906.11628

H0 = 67.36± 0.54 km s�1 Mpc�1


Planck 2018 1807.06209


H0 = 74.03± 1.42 km s�1 Mpc�1

Future measurements from BAO, local, lensing, GW ...


The Hubble Tension

5

Beyond ΛCDM possibilities: Early Dark Energy

Decaying Dark Matter Bringmann, Kahlhoefer, Schmidt-Hoberg, Walia 1803.03644

Increasing Neff e.g. Weinberg 1305.1971

Agrawal, Cyr-Racine, Pinner, Randall 1904.01016Poulin, Smith, Karwal, Kamionkowski 1811.04083


The Hubble Tension

5

Beyond ΛCDM possibilities: Early Dark Energy

Decaying Dark Matter Bringmann, Kahlhoefer, Schmidt-Hoberg, Walia 1803.03644

Increasing Neff e.g. Weinberg 1305.1971

Agrawal, Cyr-Racine, Pinner, Randall 1904.01016Poulin, Smith, Karwal, Kamionkowski 1811.04083

Perhaps the simplest one is to increase Neff:

2.0 2.5 3.0 3.5 4.0

Ne↵

60

65

70

75

H0[k

ms�

1M

pc�

1]

Riess et al. (2018)

0.77

0.78

0.79

0.80

0.81

0.82

0.83

0.84

�8

Planck 2018

NCMB+BAO+H0e↵ = 3.27± 0.15

NCMB+BAOe↵ = 2.99± 0.17

Pitrou et al 1801.08023NBBNe↵ < 3.4


The Scenario

6

Chikashige, Mohapatra, Peccei (1981)Global U(1)L Spontaneously Broken Symmetry


The Scenario

6

Chikashige, Mohapatra, Peccei (1981)

The Majoron: Lint = i�� ⌫̄ �5 ⌫�

Global U(1)L Spontaneously Broken Symmetry


The Scenario

6




� ' 10�13 m⌫0.05 eV

246GeV

vLExtremely feebly interacting: (type-I seesaw)


The Scenario

6




� ' 10�13 m⌫0.05 eV

246GeV


Dimension-5 Planck suppressed operators: m� ' vLr

vLMPl

. keVRothstein, Babu, Seckel, hep-ph/9301213Akhmedov, Berezhiani, Mohapatra, Senjanovic hep-ph/9209285


The Scenario

6




� ' 10�13 m⌫0.05 eV

246GeV


Dimension-5 Planck suppressed operators: m� ' vLr

vLMPl

. keVRothstein, Babu, Seckel, hep-ph/9301213Akhmedov, Berezhiani, Mohapatra, Senjanovic hep-ph/9209285

Parameter Space: 10�15 < � < 10�3

0.1 eV < m� < MeV


Cosmological Implications

7

⌫̄

⌫

�

Only Relevant Process:

�� H(T⌫ = m�/3)provided



7

⌫̄

⌫

�



Chacko, Hall, Okui, Oliver hep-ph/0312267

Non-standard expansion history

Erase the neutrino anisotropic stressTwo main effects:



7

⌫̄

⌫

�



Chacko, Hall, Okui, Oliver hep-ph/0312267

Non-standard expansion history

Erase the neutrino anisotropic stressTwo main effects:

We solve the full Boltzmann/Liouville equation for the background We include the full neutrino-majoron Boltzmann hierarchy in CLASS



8

Production Equilibrium Final StateDecay

� ! ⌫̄⌫⌫̄⌫ ! �T ⇠ m�/3

T � m�



8

Production Equilibrium Final StateDecay

� ! ⌫̄⌫⌫̄⌫ ! �T ⇠ m�/3

T � m�

�� ' H(T⌫ = m�/3)

�Ne↵ = 0.11

10 7 5 3 2 1 0.7 0.5 0.3 0.1T�/m�

0.00

0.05

0.10

0.15

0.20

⇢/T

4 �

⌫

�


Effects on the CMB

9

�e↵ =

✓�

4⇥ 10�12

◆2 ✓1 keVm�

◆

NSMe↵ = 3.045

�Ne↵ = 0.11


Effects on the CMB

10

�e↵ =

✓�

4⇥ 10�12

◆2 ✓1 keVm�

◆

�⌫ ! 0


Parameter Space

11


Parameter Space

11

Excluded

m� ⇠ v3/2L /M1/2Pl


Parameter Space

12

�Ne↵ = 0.11


Parameter Space

13


Parameter Space

14

PRELIMINARY


Couplings from seesaw and mass from gravity

Conclusions

15

The H0 tension: Beyond ΛCDM?

Ameliorates H0 tension via

The specific case of the Majoron:

Compelling extension of the SM

vL ⇠ 0.1� 1TeVMay solve the tension for:

m� ⇠ 0.1� 1 eV�Ne↵ = 0.11

Planck sets stringent constraints


Questions and Comments?

16

Thank you for your attention!

⌫̄

⌫

�

Stay tuned for: 1907.XXXXX with Sam Witte!


Back Up

17


The Physics: Interaction Strength

18

Relativistic factor

Decay

10−210−1100101102

Tν/mφ

10−5

10−4

10−3

10−2

10−1

1

10

102

Γ/H

λ3 × 10−11

1 × 10−11

6 × 10−12

3 × 10−12

1 × 10−12

5 × 10−13

1 × 10−13

mφ = 1 keV Rate vs Hubble


The Physics: Neutrino Perturbations

19


The Physics: Power Spectrum

20


Hubble Constant from the CMB

21

CMB measurements provide a H0 prediction from:

✓s ⌘ rs/DM (z?)

rs =

Z 1

z?

csH(z0)

dz0

DM (z) =

Z z

0

1

H(z0)dz0

Comoving sound horizon

Comoving angular diameter distance


Hubble Constant from the CMB

21

CMB measurements provide a H0 prediction from:

✓s ⌘ rs/DM (z?)

rs =

Z 1

z?

csH(z0)

dz0

DM (z) =

Z z

0

1

H(z0)dz0

Comoving sound horizon

Comoving angular diameter distance

Comoving sound horizon is the easiest thing to modify

Enhance the expansion prior to recombination


Neutrino Masses

22

At least two neutrinos are massive

q|�m231| ' 0.05 eV

q�m221 ' 0.01 eV1806.11051, de Salas et. al.


Future Measurements

23

Expansion History in the next decade:

1 3 10

40

50

60

70

1+z

H(z)

/(1+z)3

/2[kms-1Mpc

-1 ]

BOSS DR12

BOSS DR14 HERA VAOs(this work)

DESI

SH0ES 2019

BOSS LyA

from 1904.07868 by Julian Muñoz

1% local determination of H0 in the next decadeFuture CMB missions, Simons, Stage-IV experiments


The Hubble Tension

24

Tension is also present in BAO

Addison et al 1707.06547


The Hubble Tension

25

Tension is also present when compared with BAO and SNIa (Parthenon) using Ωbh2 from BBN

0.24 0.28 0.32 0.36 0.40

⌦m

60

64

68

72

76

H0[k

ms�

1M

pc�

1] Riess et al. (2018)

BAO+Pantheon+D/H BBN

BAO+Pantheon+D/H BBN+lensing

BAO+Pantheon+D/H BBN+✓MC

Planck TT,TE,EE+lowE

H0 and the Majoron Beyond19 01-07-19Miguel Escudero (KCL) 26

66.0 67.5 69.0 70.5 72.0 73.5 75.0

H0 [km/s/Mpc]

0.78

0.80

0.82

0.84

0.86

0.88

S8

=�

8(⌦

m/0

.3)0

.5⇤CDMNe↵

n = 2

HSC (Hikage et al. (2018))

SH0ES(Riess et al. (2018))

from 1904.01016 Agrawal, Cyr-Racine, Pinner, Randall


Neutrino Decoupling

27

Why is it not 3?1) Neutrino Decoupling not instantaneous

3) Finite Temperature QED corrections �m2e(T ), �m2�(T )

2) Weak Interactions freeze out at T = 2-3 MeV  hence, some heating from e+e- annihilation

4) Neutrino oscillations are active at T < 3 MeV

n h�vi ' G2FT 5 ' H

for an excellent review see hep-ph/0202122 by Dolgov

Ne↵ ⌘8

7

✓11

4

◆4/3 ✓⇢rad � ⇢�⇢�

◆Definition:

SM prediction: 1606.06986 de Salas & Pastor  hep-ph/0506164 Mangano et. al. NSMe↵ = 3.045

� ⇠ G2FE2⌫

Simplified approach: Escudero arXiv:1812.05605, JCAP 1902 (2019) 007

http://arxiv.org/abs/arXiv:1812.05605


Beyond ΛCDM

28

Early Universe or late Universe modifications?


Beyond ΛCDM

28

1904.03400 de Sainte Agathe et al

BAO measurements point toward an early Universe effect

Early Universe or late Universe modifications?

Documents

Could the H0 Tension be Pointing Toward the Neutrino Mass ...€¦ · Miguel Escudero (KCL) H0 and the Majoron Beyond19 01-07-19 The Hubble Tension 4 Taken from Wendy Freedman, see