Could the H0 Tension be Pointing Toward the Neutrino Mass Mechanism?
Miguel Escudero Abenza [email protected]
based on ArXiv:1909.04044 with Sam Witte PALS Paris 27/09/19 H0 H0
⌫ ⌫ e ! µ m =0 ⌫ 6 H0
⌫
⌫e ⌫µ ⌫¯ ! m =0 ⌫ 6 Outline
1) The Hubble Tension
2) The Scenario
3) Cosmology with a light Majoron
4) Conclusions
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 3 The Hubble Tension
Taken from Wendy Freedman, see 1706.02739
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 4 The Hubble Tension
Taken from Wendy Freedman, see 1706.02739 Riess et al 1903.07603
1 1 H = 74.03 1.42 km s Mpc 0 ± 4.4 σ tension within ΛCDM!
1 1 H = 67.36 0.54 km s Mpc 0 ± Planck 2018 1807.06209
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 4 The Hubble Tension
Taken from Wendy Freedman, see 1706.02739 Riess et al 1903.07603
1 1 H = 74.03 1.42 km s Mpc 0 ± 4.4 σ tension within ΛCDM!
1 1 H = 67.36 0.54 km s Mpc 0 ± Planck 2018 1807.06209
Tension very unlikely generated by CMB systematics see e.g. Spergel et al 1312.3313, Addison et al 1511.00055, Verde et al 1601.01701, Planck 1608.02487
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 4 The Hubble Tension
Taken from Wendy Freedman, see 1706.02739 Riess et al 1903.07603
1 1 H = 74.03 1.42 km s Mpc 0 ± 4.4 σ tension within ΛCDM!
1 1 H = 67.36 0.54 km s Mpc 0 ± Planck 2018 1807.06209
Tension very unlikely generated by CMB systematics see e.g. Spergel et al 1312.3313, Addison et al 1511.00055, Verde et al 1601.01701, Planck 1608.02487 Local measurements have also been checked against systematics see e.g. Efstathiou 1311.3461, Cardona et al 1611.06088, Zhang et al 1706.07573, Follin & Knox 1707.01175
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 4 The Hubble Tension
Taken from Wendy Freedman, see 1706.02739 Riess et al 1903.07603
1 1 H = 74.03 1.42 km s Mpc 0 ± 4.4 σ tension within ΛCDM!
1 1 H = 67.36 0.54 km s Mpc 0 ± Planck 2018 1807.06209
Tension very unlikely generated by CMB systematics see e.g. Spergel et al 1312.3313, Addison et al 1511.00055, Verde et al 1601.01701, Planck 1608.02487 Local measurements have also been checked against systematics see e.g. Efstathiou 1311.3461, Cardona et al 1611.06088, Zhang et al 1706.07573, Follin & Knox 1707.01175 Although other calibrations lead to different results see Freedman et. al. 1907.05922 but also see Riess et. al. 1908.00993
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 4 The Hubble Tension
Taken from Wendy Freedman, see 1706.02739 Riess et al 1903.07603
1 1 H = 74.03 1.42 km s Mpc 0 ± 4.4 σ tension within ΛCDM!
1 1 H = 67.36 0.54 km s Mpc 0 ± Planck 2018 1807.06209
Tension very unlikely generated by CMB systematics see e.g. Spergel et al 1312.3313, Addison et al 1511.00055, Verde et al 1601.01701, Planck 1608.02487 Local measurements have also been checked against systematics see e.g. Efstathiou 1311.3461, Cardona et al 1611.06088, Zhang et al 1706.07573, Follin & Knox 1707.01175 Although other calibrations lead to different results see Freedman et. al. 1907.05922 but also see Riess et. al. 1908.00993
Tension between H0 local and BAO is also present see Addison et al 1707.06547, Font-Ribera et al 1906.11628, Schöneberg et al 1907.11594
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 4 The Hubble Tension Beyond ΛCDM possibilities:
Early Dark Energy Poulin, Smith, Karwal, Kamionkowski 1811.04083 Agrawal, Cyr-Racine, Pinner, Randall 1904.01016 Decaying Dark Matter Bringmann, Kahlhoefer, Schmidt-Hoberg, Walia 1803.03644
Increasing Neff e.g. Weinberg 1305.1971
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 5 The Hubble Tension Beyond ΛCDM possibilities:
Early Dark Energy Poulin, Smith, Karwal, Kamionkowski 1811.04083 Agrawal, Cyr-Racine, Pinner, Randall 1904.01016 Decaying Dark Matter Bringmann, Kahlhoefer, Schmidt-Hoberg, Walia 1803.03644
Increasing Neff e.g. Weinberg 1305.1971
Perhaps the simplest one is to increase Neff:
0.84 75 CMB+BAO Riess et al. (2018) 0.83 N =2.99 0.17 ] e↵ 1 ± 0.82 70 Mpc
0.81 1
8 CMB+BAO+H0 N =3.27 0.15 0.80 e↵ 65 ± [km s
0 0.79 H BBN Pitrou et al 1801.08023 0.78 Ne↵ < 3.4 60 Planck 2018 0.77
2.0 2.5 3.0 3.5 4.0
Ne↵
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 5 The Physics
CMB BBN 1) 380.000 yr 3 min
T =0.26 eV T =0.07 MeV
The Universe has expanded by a factor of 105!
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 6 The Physics
CMB BBN 1) 380.000 yr 3 min
T =0.26 eV T =0.07 MeV
The Universe has expanded by a factor of 105!
2) Photons 40 % Neutrinos 60 %
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 6 The Seesaw Mechanism
Minkowski, Yanagida, Gell-Mann, Ramond, Slansky, Glashow, Mohapatra, Senjanovic, Schechter, Valle
m⌫ yDvH Type-I seesaw
mN
Neutrinos are very light Majorana particles:
2 yD TeV m⌫ 0.03 eV 6 ' 10 MN ⇣ ⌘
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 7 The Scenario
Global U(1)L Spontaneously Broken Symmetry Chikashige, Mohapatra, Peccei (1981)
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 8 The Scenario
Global U(1)L Spontaneously Broken Symmetry Chikashige, Mohapatra, Peccei (1981)
The Majoron: int = i ⌫ ¯ 5 ⌫ L
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 8 The Scenario
Global U(1)L Spontaneously Broken Symmetry Chikashige, Mohapatra, Peccei (1981)
The Majoron: int = i ⌫ ¯ 5 ⌫ L
13 m⌫ 246 GeV Extremely feebly interacting: 10 (type-I seesaw) ' 0.05 eV vL
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 8 The Scenario
Global U(1)L Spontaneously Broken Symmetry Chikashige, Mohapatra, Peccei (1981)
The Majoron: int = i ⌫ ¯ 5 ⌫ L
13 m⌫ 246 GeV Extremely feebly interacting: 10 (type-I seesaw) ' 0.05 eV vL
20 Extremely feebly interacting with matter: 10 ee ⇠
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 8 The Scenario
Global U(1)L Spontaneously Broken Symmetry Chikashige, Mohapatra, Peccei (1981)
The Majoron: int = i ⌫ ¯ 5 ⌫ L
13 m⌫ 246 GeV Extremely feebly interacting: 10 (type-I seesaw) ' 0.05 eV vL
20 Extremely feebly interacting with matter: 10 ee ⇠
vL Dimension-5 Planck suppressed operators: m vL . keV Rothstein, Babu, Seckel hep-ph/9301213 ' MPl Akhmedov, Berezhiani, Mohapatra, Senjanovic hep-ph/9209285 r
Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 8 The Scenario
Global U(1)L Spontaneously Broken Symmetry Chikashige, Mohapatra, Peccei (1981)
The Majoron: int = i ⌫ ¯ 5 ⌫ L
13 m⌫ 246 GeV Extremely feebly interacting: 10 (type-I seesaw) ' 0.05 eV vL
20 Extremely feebly interacting with matter: 10 ee ⇠
vL Dimension-5 Planck suppressed operators: m vL . keV Rothstein, Babu, Seckel hep-ph/9301213 ' MPl Akhmedov, Berezhiani, Mohapatra, Senjanovic hep-ph/9209285 r
15 3 Parameter Space: 10 < < 10 0.1 eV Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 8 Cosmological Implications Only Relevant Process: ⌫ provided H(T = m /3) ⌫ ⌫¯ Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 9 Cosmological Implications Only Relevant Process: ⌫ provided H(T = m /3) ⌫ ⌫¯ Non-standard expansion history Two main effects: Chacko, Hall, Okui, Erase the neutrino anisotropic stress Oliver hep-ph/0312267 Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 9 Cosmological Implications Only Relevant Process: ⌫ provided H(T = m /3) ⌫ ⌫¯ Non-standard expansion history Two main effects: Chacko, Hall, Okui, Erase the neutrino anisotropic stress Oliver hep-ph/0312267 We solve the Boltzmann equation for the background Escudero 1812.05605, 1910.XXXXX We include the full neutrino-majoron Boltzmann hierarchy in CLASS Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 9 Cosmological Implications T m Production Equilibrium Decay Final State T m /3 ⇠ ⌫⌫¯ ⌫⌫¯ ! ! Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 10 Cosmological Implications T m Production Equilibrium Decay Final State T m /3 ⇠ ⌫⌫¯ ⌫⌫¯ ! ! H(T⌫ = m /3) 0.20 ' ⌫ 0.15 4 T 0.10 ⇢ / 0.05 0.00 10 7 5 3 2 1 0.7 0.5 0.3 0.1 T /m Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 10 Cosmological Implications T m Production Equilibrium Decay Final State T m /3 ⇠ ⌫⌫¯ ⌫⌫¯ ! ! H(T⌫ = m /3) 0.20 ' N =0.11 ⌫ e↵ 0.15 4 Ne↵ ⇢⌫ /⇢ T 0.10 / ⇢ / 0.05 0.00 10 7 5 3 2 1 0.7 0.5 0.3 0.1 T /m Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 10 Effects on the CMB 2 1 keV = e↵ 4 10 12 m ✓ ⇥ ◆ ✓ ◆ Ne↵ =0.11 SM Ne↵ =3.045 Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 11 Effects on the CMB 2 1 keV see Bashinsky and Seljak astro-ph/0310198 = e↵ 4 10 12 m 0 ✓ ◆ ✓ ◆ ⌫ ! ⇥ Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 12 Parameter Space Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 13 Parameter Space Excluded m v3/2/M 1/2 ⇠ L Pl Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 13 Parameter Space Ne↵ =0.11 Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 14 Parameter Space Full MCMC to Planck 2018 data Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 15 Parameter Space 1σ preference when including H0 in the fit and an additional ΔNeff Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 16 Parameter Space for H0 Planck2018+BAO+H 0 Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 17 Parameter Space for H0 Planck2018+BAO+H 0 Requires a positive ΔNeff ~ 0.5 H0 Planck 2018 fit is not degraded wrt ΛCDM Very close to the electroweak scale v (0.1 1) TeV L ⇠ Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 17 Conclusions The H0 tension: Beyond ΛCDM? Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 18 Conclusions The H0 tension: Beyond ΛCDM? The specific case of the Majoron: Compelling extension of the SM Couplings from seesaw and mass from gravity Planck sets very stringent constraints Ameliorates H0 tension via Ne↵ =0.11 m (0.1 1) eV ⇠ May solve the tension for: v (0.1 1) TeV L ⇠ N 0.5 e↵ ⇠ Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 18 Questions and Comments? Thank you for your attention! ⌫ ⌫¯ Check ArXiv:1909.04044 with Sam Witte! Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 19 Back Up Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 20 Neff and BBN Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 21 The Physics: Interaction Strength Decay m =1keVRatevsHubble 102 φ λ 3 × 10−11 10 1 × 10−11 6 × 10−12 3 × 10−12 1 1 × 10−12 5 × 10−13 10−1 1 × 10−13 H / −2 Γ 10 10−3 10−4 10−5 Relativistic factor 102 101 100 10−1 10−2 Tν/mφ Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 22 H0 Plots 1.0 ⇤CDM Planck18+BAO ⇤CDM+ N Planck18+BAO+SH ES 0.8 eff 0 Majoron+ Neff SH0ES 0.6 Posterior 0.4 0.2 0.0 66 68 70 72 74 76 H0 (km/s/Mpc) Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 23 H0 Plots 1.0 ⇤CDM Planck18+BAO ⇤CDM+ N Planck18+BAO+SH ES 0.8 eff 0 Majoron+ Neff Planck18+BAO, Neff > 0 SH ES 0.6 0 Posterior 0.4 0.2 0.0 66 68 70 72 74 76 H0 (km/s/Mpc) Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 24 The Physics: Neutrino Perturbations see Bashinsky and Seljak astro-ph/0310198 Neutrino-Majoron Interactions impact Neutrinos and hence and hence Photons Dark Matter Metric Thompson Scattering Electrons Protons Coulomb Scattering Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 25 The Physics: Neutrino Perturbations i i i i f(x ,p ,t)=f0(p) 1+ (x ,p ,t) ` = 1( i) (2⇥` + 1) P (µ)⇤ 0 ` ` P 4 2 ˙ = ✓ h,˙ ⌫ 3 ⌫ 3 1 ✓˙ = k2 , ⌫ 4 ⌫ ⌫ ✓ ◆ 8 3 4 8 F˙ =2˙ = ✓ kF + h˙ + ⌘˙ 2a , ⌫ 2 ⌫ 15 ⌫ 5 ⌫ 3 15 5 ⌫ ˙ k F⌫ ` = ` F⌫ (` 1) (` + 1)F⌫ (`+1) a F⌫ ` , ` 3 . 2` +1 ⇥ ⇤ 2 1 n⌫ m µ⌫ m = e T⌫ K ⌘ n t 2 T 2 1 T ⌫ forward ⌫ ✓ ⌫ ◆ Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 26 The Physics: Neutrino Perturbations Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 27 The Physics: Power Spectrum Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 28 Primordial Abundance Neff 1 0.5 0.16 eff 0.11 N 0.05 Simons Observatory 0.03 CMB Stage-IV 0.01 4 3 2 1 0 1 2 10 10 10 10 10 10 10 eff Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 29 Hubble Constant from the CMB CMB measurements provide a H0 prediction from: ✓ r /D (z ) s ⌘ s M ? 1 cs r = dz0 Comoving sound horizon s H(z ) Zz? 0 z 1 D (z)= dz0 Comoving angular diameter distance M H(z ) Z0 0 Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 30 Hubble Constant from the CMB CMB measurements provide a H0 prediction from: ✓ r /D (z ) s ⌘ s M ? 1 cs r = dz0 Comoving sound horizon s H(z ) Zz? 0 z 1 D (z)= dz0 Comoving angular diameter distance M H(z ) Z0 0 Comoving sound horizon is the easiest thing to modify Enhance the expansion prior to recombination Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 30 The Hubble Tension as of today 1908.00993 Riess et. al. Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 31 Neutrino Masses At least two neutrinos are massive 1806.11051, de Salas et. al. m2 0.05 eV m2 0.01 eV | 31| ' 21 ' q q Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 32 Future Measurements 1% local determination of H0 in the next decade Future CMB missions, Simons, Stage-IV experiments Expansion History in the next decade: ] 1 - SH0ES 2019 from 1904.07868 by Julian Muñoz Mpc 70 1 - 60 ms km [ BOSS DR12 2 / 3 50 ) z BOSS DR14 + DESI HERA VAOs 1 (this work) )/( 40 z ( H 1 3 BOSS LyA 10 1+z Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 33 The Hubble Tension Tension is also present in BAO Addison et al 1707.06547 Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 34 The Hubble Tension Tension is also present when compared with BAO and SNIa (Parthenon) using Ωbh2 from BBN 76 Riess et al. (2018) ] 1 72 Mpc 1 68 [km s 0 64 H BAO+Pantheon+D/H BBN BAO+Pantheon+D/H BBN+lensing BAO+Pantheon+D/H BBN+✓ 60 MC Planck TT,TE,EE+lowE 0.24 0.28 0.32 0.36 0.40 ⌦m Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 35 ⇤CDM SH0ES (Riess et al. (2018)) 0.88 Ne↵ 5 . 0 n =2 3) . 0.86 0 / m 0.84 ( ⌦ 8 0.82 = 8 S 0.80 HSC (Hikage et al. (2018)) 0.78 66.0 67.5 69.0 70.5 72.0 73.5 75.0 H0 [km/s/Mpc] from 1904.01016 Agrawal, Cyr-Racine, Pinner, Randall Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 36 Neutrino Decoupling 8 11 4/3 ⇢ ⇢ Definition: N rad e↵ ⌘ 7 4 ⇢ ✓ ◆ ✓ ◆ SM 1606.06986 de Salas & Pastor SM prediction: Ne↵ =3.045 hep-ph/0506164 Mangano et. al. Why is it not 3? for an excellent review see hep-ph/0202122 by Dolgov 1) Neutrino Decoupling not instantaneous G2 E2 ⇠ F ⌫ 2) Weak Interactions freeze out at T = 2-3 MeV n v G2 T 5 H hence, some heating from e+e- annihilation h i' F ' 2 2 3) Finite Temperature QED corrections me(T ), m (T ) 4) Neutrino oscillations are active at T < 3 MeV Simplified approach: Escudero arXiv:1812.05605, JCAP 1902 (2019) 007 Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 37 Beyond ΛCDM Early Universe or late Universe modifications? Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 38 Beyond ΛCDM Early Universe or late Universe modifications? 1904.03400 de Sainte Agathe et al BAO measurements point toward an early Universe effect Miguel Escudero (KCL) H0 and the Majoron PALS 27-09-19 38