neutrino cosmology in 2020: where do we stand? · 2020. 1. 28. · choudhury & hannestad...
TRANSCRIPT
![Page 2: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/2.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
New Laboratory Neutrino Mass Bound
2
3H ! 3He+ + e� + ⌫̄eKATRIN experiment
![Page 3: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/3.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
New Laboratory Neutrino Mass Bound
2
3H ! 3He+ + e� + ⌫̄eKATRIN experiment
Mainz and Troitsk (2001) : m⌫e < 2.2 eV (95 % CL)
![Page 4: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/4.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
New Laboratory Neutrino Mass Bound
2
3H ! 3He+ + e� + ⌫̄eKATRIN experiment
Mainz and Troitsk (2001) : m⌫e < 2.2 eV (95 % CL)
(90 % CL)(PRL 2019, 1909.06048)
m⌫e < 1.1 eVCurrent laboratory bound:
![Page 5: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/5.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
New Laboratory Neutrino Mass Bound
2
3H ! 3He+ + e� + ⌫̄eKATRIN experiment
Mainz and Troitsk (2001) : m⌫e < 2.2 eV (95 % CL)
(90 % CL)(PRL 2019, 1909.06048)
m⌫e < 1.1 eVCurrent laboratory bound:
(95 % CL)X
m⌫ < 3.9 eV
![Page 6: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/6.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
New Laboratory Neutrino Mass Bound
2
3H ! 3He+ + e� + ⌫̄eKATRIN experiment
KATRIN expected reach Xm⌫ < 0.6 eV
(90 % CL)m⌫e < 0.2 eV(in ~3-years)
Mainz and Troitsk (2001) : m⌫e < 2.2 eV (95 % CL)
(90 % CL)(PRL 2019, 1909.06048)
m⌫e < 1.1 eVCurrent laboratory bound:
(95 % CL)X
m⌫ < 3.9 eV
![Page 7: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/7.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Planck Legacy Data is now Public
3
Planck Likelihoods 1907.12875
CLASS/CAMB MontePython/CosmoMC
![Page 8: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/8.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
The Hubble Tension Increases
4
From Verde et. al. 1907.10625
![Page 9: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/9.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Outline
5
1) Neutrinos and ΛCDM2) Neutrino Masses
Cosmological Constraints within ΛCDM Non-standard Cosmologies
3) NeffBBN and the CMB Constraints on BSM Physics
4) Neutrinos and the Hubble Tension
5) Conclusions and Outlook
![Page 10: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/10.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Decoupling
6
e+e� $ ⌫̄i⌫ie±⌫i $ e±⌫i
ElectronsNeutrinos Z-W (off-shell)Photons
![Page 11: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/11.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Decoupling
7
Ne↵ ⌘ 8
7
✓11
4
◆4/3 ✓⇢rad � ⇢�⇢�
◆
![Page 12: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/12.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Decoupling
7
Ne↵ ⌘ 8
7
✓11
4
◆4/3 ✓⇢rad � ⇢�⇢�
◆Ne↵ = 3
✓1.4T⌫
T�
◆4
![Page 13: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/13.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Decoupling
7
Ne↵ ⌘ 8
7
✓11
4
◆4/3 ✓⇢rad � ⇢�⇢�
◆
de Salas & Pastor 1606.06986Escudero 2001.04466NSM
e↵ = 3.045
Ne↵ = 3
✓1.4T⌫
T�
◆4
![Page 14: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/14.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Decoupling
7
Ne↵ ⌘ 8
7
✓11
4
◆4/3 ✓⇢rad � ⇢�⇢�
◆
de Salas & Pastor 1606.06986Escudero 2001.04466NSM
e↵ = 3.045
Why is it not 3?Some e+e- heatingNon-instantaneous decouplingQED thermal correctionsNeutrino Oscillations
Excellent reviewby Dolgov 0202122
T⌫µ/⌫⌧⇠ 3.5MeV
T⌫e ⇠ 2MeV
Relic Neutrino Decouplingt ⇠ 0.1 s
Ne↵ = 3
✓1.4T⌫
T�
◆4
![Page 15: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/15.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Evolution
8
Xm⌫ = 1 eV
Neutrinos are always a relevant species in the Universe evolution
γ ν
Hot DM: ⌦⌫h2 ' 0.01
Xm⌫/eVNon-Rel: znon�rel
⌫ ' 600m⌫
0.3 eV
![Page 16: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/16.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
q�m2
sol
q�m2
atm
q�m2
sol
' 0.01 eV
q�m2
atm ' 0.05 eV
Neutrino Properties
9
InvertedNormal
Figure from de Salas et. al. 1806.11051
![Page 17: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/17.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
q�m2
sol
q�m2
atm
q�m2
sol
' 0.01 eV
q�m2
atm ' 0.05 eV
Neutrino Properties
9
InvertedNormal
Figure from de Salas et. al. 1806.11051
Xm⌫ & 0.06 eV
Xm⌫ & 0.10 eV
![Page 18: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/18.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
q�m2
sol
q�m2
atm
q�m2
sol
' 0.01 eV
q�m2
atm ' 0.05 eV
Neutrino Properties
9
InvertedNormal
Figure from de Salas et. al. 1806.11051
Xm⌫ & 0.06 eV
Xm⌫ & 0.10 eV
Mass differences and mixings measured with high precision
![Page 19: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/19.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
q�m2
sol
q�m2
atm
q�m2
sol
' 0.01 eV
q�m2
atm ' 0.05 eV
Neutrino Properties
9
InvertedNormal
Figure from de Salas et. al. 1806.11051
Xm⌫ & 0.06 eV
Xm⌫ & 0.10 eV
Mass differences and mixings measured with high precision
What is Delta CP and what is the mass ordering?(see Sophie's talk)
![Page 20: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/20.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
q�m2
sol
q�m2
atm
q�m2
sol
' 0.01 eV
q�m2
atm ' 0.05 eV
Neutrino Properties
9
InvertedNormal
Figure from de Salas et. al. 1806.11051
Xm⌫ & 0.06 eV
Xm⌫ & 0.10 eV
Mass differences and mixings measured with high precision
What is mmin? The lightest neutrino could still be massless!
What is Delta CP and what is the mass ordering?(see Sophie's talk)
![Page 21: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/21.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
10
Planck 2018 (1807.06209)X
m⌫ < 0.54 eVX
m⌫ < 0.26 eV
Xm⌫ < 0.12 eV
(95 % CL, TT+lowE)
(95 % CL, TTTEEE+lowE)
(95 % CL, TTTEEE+lowE+lensing+BAO)
(95 % CL, TTTEEE+lowE+lensing)X
m⌫ < 0.24 eV
![Page 22: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/22.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
10
Planck 2018 (1807.06209)X
m⌫ < 0.54 eVX
m⌫ < 0.26 eV
Xm⌫ < 0.12 eV
(95 % CL, TT+lowE)
(95 % CL, TTTEEE+lowE)
(95 % CL, TTTEEE+lowE+lensing+BAO)
(95 % CL, TTTEEE+lowE+lensing)X
m⌫ < 0.24 eV
1) Prior dependent bounds (see next talk by Constance)
2) Dependence upon the Cosmological Model
3) Other not that linear data sets?
Very robust bounds from linear Cosmology
![Page 23: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/23.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
11
Cosmological Model DependencePlanck+BAO and 3 degenerate neutrinosX
m⌫ < 0.12 eV ΛCDM+mνPlanck 1807.06209
Standard Case
![Page 24: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/24.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
11
Cosmological Model DependencePlanck+BAO and 3 degenerate neutrinos
Choudhury & Hannestad 19'CDM+mν+ωa+ω
Xm⌫ < 0.25 eV Dark Energy dynamics
Xm⌫ < 0.12 eV ΛCDM+mν
Planck 1807.06209Standard Case
![Page 25: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/25.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
11
Cosmological Model DependencePlanck+BAO and 3 degenerate neutrinos
Choudhury & Hannestad 19'CDM+mν+ωa+ω
Xm⌫ < 0.25 eV Dark Energy dynamics
Varying CurvatureX
m⌫ < 0.15 eV ΛCDM+mν+Ωk Choudhury & Hannestad 19'
Xm⌫ < 0.12 eV ΛCDM+mν
Planck 1807.06209Standard Case
![Page 26: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/26.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
11
Cosmological Model DependencePlanck+BAO and 3 degenerate neutrinos
Choudhury & Hannestad 19'CDM+mν+ωa+ω
Xm⌫ < 0.25 eV Dark Energy dynamics
Varying CurvatureX
m⌫ < 0.15 eV ΛCDM+mν+Ωk Choudhury & Hannestad 19'
Varying Neff ΛCDM+mν+Neff
Xm⌫ < 0.23 eV
Planck 1807.06209
Xm⌫ < 0.12 eV ΛCDM+mν
Planck 1807.06209Standard Case
![Page 27: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/27.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
11
Cosmological Model DependencePlanck+BAO and 3 degenerate neutrinos
Choudhury & Hannestad 19'CDM+mν+ωa+ω
Xm⌫ < 0.25 eV Dark Energy dynamics
Varying CurvatureX
m⌫ < 0.15 eV ΛCDM+mν+Ωk Choudhury & Hannestad 19'
Varying Neff ΛCDM+mν+Neff
Xm⌫ < 0.23 eV
Planck 1807.06209
Xm⌫ < 0.12 eV ΛCDM+mν
Planck 1807.06209Standard Case
Varying Neff+ω+αs+mνdi Valentino et al. 1908.01391
Xm⌫ < 0.17 eV CDM+mν+Neff+ω+αs+mν
![Page 28: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/28.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
11
Cosmological Model DependencePlanck+BAO and 3 degenerate neutrinos
Choudhury & Hannestad 19'CDM+mν+ωa+ω
Xm⌫ < 0.25 eV Dark Energy dynamics
Varying CurvatureX
m⌫ < 0.15 eV ΛCDM+mν+Ωk Choudhury & Hannestad 19'
Varying Neff ΛCDM+mν+Neff
Xm⌫ < 0.23 eV
Planck 1807.06209
Xm⌫ < 0.12 eV ΛCDM+mν
Planck 1807.06209Standard Case
Varying Neff+ω+αs+mνdi Valentino et al. 1908.01391
Xm⌫ < 0.17 eV CDM+mν+Neff+ω+αs+mν
Constraints are robust upon standard modifications of ΛCDM
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
12
Cosmological Model DependenceMore exotic scenarios:
![Page 30: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/30.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
12
Cosmological Model DependenceMore exotic scenarios:
⌫i
⌫j
�
relaxed by 0.1 eVEscudero & Fairbairn 1907.05425
Xm⌫
Invisible Neutrino Decay
![Page 31: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/31.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
12
Cosmological Model DependenceMore exotic scenarios:
⌫i
⌫j
�
relaxed by 0.1 eVEscudero & Fairbairn 1907.05425
Xm⌫
Invisible Neutrino Decay
Xm⌫ . 1 eV
⌫i
⌫4
�
Chacko et. al. 1909.05275
Invisible Neutrino Decay
![Page 32: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/32.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
12
Cosmological Model DependenceMore exotic scenarios:
⌫i
⌫j
�
relaxed by 0.1 eVEscudero & Fairbairn 1907.05425
Xm⌫
Invisible Neutrino Decay
Lorenz et. al. 1811.01991
Time dependent Neutrino Masses
Xm⌫ < 4.8 eV
m⌫(t)
Xm⌫ . 1 eV
⌫i
⌫4
�
Chacko et. al. 1909.05275
Invisible Neutrino Decay
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
12
Cosmological Model DependenceMore exotic scenarios:
⌫i
⌫j
�
relaxed by 0.1 eVEscudero & Fairbairn 1907.05425
Xm⌫
Invisible Neutrino Decay
Lorenz et. al. 1811.01991
Time dependent Neutrino Masses
Xm⌫ < 4.8 eV
m⌫(t)
Xm⌫ . 1 eV
⌫i
⌫4
�
Chacko et. al. 1909.05275
Invisible Neutrino Decay
Bounds can be significantly loosen in some extensions of ΛCDM. They typically require modifications to the neutrino sector.
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
13
Data beyond Planck and BAO within ΛCDMPlanck Planck 1807.06209
Xm⌫ < 0.26 eV
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
13
Data beyond Planck and BAO within ΛCDMPlanck Planck 1807.06209X
m⌫ < 0.12 eV Planck 1807.06209Planck+BAO
Xm⌫ < 0.26 eV
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
13
Data beyond Planck and BAO within ΛCDMPlanck Planck 1807.06209X
m⌫ < 0.12 eV Planck 1807.06209Planck+BAO
Xm⌫ < 0.26 eV
Ivanov et. al. 1909.05277BOSS P(k)X
m⌫ < 0.86 eV
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
13
Data beyond Planck and BAO within ΛCDMPlanck Planck 1807.06209X
m⌫ < 0.12 eV Planck 1807.06209Planck+BAO
Xm⌫ < 0.26 eV
Ivanov et. al. 1912.08208Planck+BOSS P(k)X
m⌫ < 0.16 eV
Ivanov et. al. 1909.05277BOSS P(k)X
m⌫ < 0.86 eV
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
13
Data beyond Planck and BAO within ΛCDMPlanck Planck 1807.06209X
m⌫ < 0.12 eV Planck 1807.06209Planck+BAO
Xm⌫ < 0.26 eV
Ivanov et. al. 1912.08208Planck+BOSS P(k)X
m⌫ < 0.16 eV
Palanque-Delabrouilleet. al. 1911.09073
Lyman-α+H0prior X
m⌫ < 0.58 eV
Ivanov et. al. 1909.05277BOSS P(k)X
m⌫ < 0.86 eV
![Page 39: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/39.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
13
Data beyond Planck and BAO within ΛCDMPlanck Planck 1807.06209X
m⌫ < 0.12 eV Planck 1807.06209Planck+BAO
Xm⌫ < 0.26 eV
Ivanov et. al. 1912.08208Planck+BOSS P(k)X
m⌫ < 0.16 eV
Planck+Lyman-α X
m⌫ < 0.10 eVPalanque-Delabrouilleet. al. 1911.09073
Lyman-α+H0prior X
m⌫ < 0.58 eV
Ivanov et. al. 1909.05277BOSS P(k)X
m⌫ < 0.86 eV
![Page 40: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/40.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
13
Data beyond Planck and BAO within ΛCDMPlanck Planck 1807.06209X
m⌫ < 0.12 eV Planck 1807.06209Planck+BAO
Xm⌫ < 0.26 eV
Ivanov et. al. 1912.08208Planck+BOSS P(k)X
m⌫ < 0.16 eV
Planck+Lyman-α X
m⌫ < 0.10 eV
Choudhury & Hannestad 19'Planck+BAO+H0X
m⌫ < 0.08 eV
Palanque-Delabrouilleet. al. 1911.09073
Lyman-α+H0prior X
m⌫ < 0.58 eV
Ivanov et. al. 1909.05277BOSS P(k)X
m⌫ < 0.86 eV
![Page 41: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/41.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
13
Data beyond Planck and BAO within ΛCDMPlanck Planck 1807.06209X
m⌫ < 0.12 eV Planck 1807.06209Planck+BAO
Xm⌫ < 0.26 eV
Ivanov et. al. 1912.08208Planck+BOSS P(k)X
m⌫ < 0.16 eV
Planck+Lyman-α X
m⌫ < 0.10 eV
Choudhury & Hannestad 19'Planck+BAO+H0X
m⌫ < 0.08 eV
Palanque-Delabrouilleet. al. 1911.09073
Lyman-α+H0prior X
m⌫ < 0.58 eV
Ivanov et. al. 1909.05277BOSS P(k)X
m⌫ < 0.86 eV
Planck is driving current cosmological constraints
Non-linear or mildly non-linear data sets break degeneracies in the fit
The larger H0 is, the stronger the constraint on areX
m⌫
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Current Constraints on Neff
14
Ne↵ = 2.99± 0.17 Planck 2018, 1807.06209
Current Constraints
Fields et. al. 1912.01132Ne↵ = 2.88± 0.28
Ne↵ = 3.27± 0.15
BBN
Planck+BAO
Planck+BAO+H0 Planck 2018, 1807.06209
![Page 43: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/43.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Current Constraints on Neff
14
Ne↵ = 2.99± 0.17 Planck 2018, 1807.06209
Current Constraints
Fields et. al. 1912.01132Ne↵ = 2.88± 0.28
Ne↵ = 3.27± 0.15
BBN
Planck+BAO
Planck+BAO+H0 Planck 2018, 1807.06209
Data is in excellent agreement with the Standard Model prediction
Standard Model Prediction: NSMe↵ = 3.045
![Page 44: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/44.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Constraints from Neff
15
Sterile NeutrinoGoldstone BosonsOther sterile long-lived particles Gravitino, axino, hidden sector particles ...
mN ⇠ eV �Ne↵ = 1
Weinberg 1305.1971
(e.g. Gariazzo, de Salas, Pastor 1905.11290)
![Page 45: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/45.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Constraints from Neff
15
Sterile NeutrinoGoldstone BosonsOther sterile long-lived particles Gravitino, axino, hidden sector particles ...
mN ⇠ eV �Ne↵ = 1
Weinberg 1305.1971
(e.g. Gariazzo, de Salas, Pastor 1905.11290)
![Page 46: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/46.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Constraints from Neff
15
Sterile NeutrinoGoldstone BosonsOther sterile long-lived particles Gravitino, axino, hidden sector particles ...
mN ⇠ eV �Ne↵ = 1
Weinberg 1305.1971
(e.g. Gariazzo, de Salas, Pastor 1905.11290)
Constraints are relevant in many other BSM settings (see James' talk)
![Page 47: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/47.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
The Hubble Tension
16
The Hubble Tension:
H0 = 67.36± 0.54 km s�1 Mpc�1
4.4 σ tension within ΛCDM! Planck 2018 1807.06209
Riess et. al. 1903.07603H0 = 74.03± 1.42 km s�1 Mpc�1
![Page 48: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/48.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
The Hubble Tension
16
The Hubble Tension:
H0 = 67.36± 0.54 km s�1 Mpc�1
4.4 σ tension within ΛCDM! Planck 2018 1807.06209
Riess et. al. 1903.07603H0 = 74.03± 1.42 km s�1 Mpc�1
Possible resolutions:1) Systematics in the CMB data very unlikely2) Systematics in local measurements none so far3) New feature of ΛCDM
![Page 49: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/49.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
The Hubble Tension
16
The Hubble Tension:
H0 = 67.36± 0.54 km s�1 Mpc�1
4.4 σ tension within ΛCDM! Planck 2018 1807.06209
Riess et. al. 1903.07603H0 = 74.03± 1.42 km s�1 Mpc�1
Possible resolutions:1) Systematics in the CMB data very unlikely2) Systematics in local measurements none so far3) New feature of ΛCDM
Possibilities Beyond ΛCDM (Knox and Millea 1908.03663):1) Late Universe Modifications very unlikely2) Early Universe Modifications hard but doable
![Page 50: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/50.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
The Hubble Tension: Theory
17
Way to Resolve the Hubble Tension (Knox and Millea 1908.03663):
![Page 51: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/51.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
The Hubble Tension: Theory
17
Way to Resolve the Hubble Tension (Knox and Millea 1908.03663):
Enhance the expansion history of the Universe prior and close to recombination!
![Page 52: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/52.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
The Hubble Tension: Theory
17
Most Popular Scenario: Early Dark EnergyPoulin, Smith, Karwal, Kamionkowski 1811.04083. Smith, Poulin, Amin 1908.06995 Agrawal, Cyr-Racine, Pinner, Randall 1904.01016.
V (�) ⇠ �2n
M2n�4Pl
n = 2� 3 z� ⇠ 3000 f� ⇠ 10%
Way to Resolve the Hubble Tension (Knox and Millea 1908.03663):
Enhance the expansion history of the Universe prior and close to recombination!
![Page 53: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/53.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
The Hubble Tension: Theory
17
Most Popular Scenario: Early Dark EnergyPoulin, Smith, Karwal, Kamionkowski 1811.04083. Smith, Poulin, Amin 1908.06995 Agrawal, Cyr-Racine, Pinner, Randall 1904.01016.
V (�) ⇠ �2n
M2n�4Pl
n = 2� 3 z� ⇠ 3000 f� ⇠ 10%
Way to Resolve the Hubble Tension (Knox and Millea 1908.03663):
Enhance the expansion history of the Universe prior and close to recombination!
Resolve the tension 4.4σ to ~1σ
Theoretical Interpretation is not simple ... m� ⇠ 10�27 eV
So far, only Planck 2015 analysesThere are some discrepancies between these analyses
f� ⇠ 10% z� ⇠ 3000
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
18
Why Neutrinos?
![Page 55: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/55.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
18
1) Neutrinos are always a relevant species in the Universe evolution
Why Neutrinos?
![Page 56: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/56.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
18
1) Neutrinos are always a relevant species in the Universe evolution
2) Neutrino masses are the only Laboratory evidence of Physics Beyond the Standard Model
Why Neutrinos?
![Page 57: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/57.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
19
Dark Radiation
(68 % CL, Planck+BAO+H0)
�Ne↵ = 0.23± 0.15
![Page 58: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/58.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
19
Dark Radiation
(68 % CL, Planck+BAO+H0)
�Ne↵ = 0.23± 0.15 H0 tension from 4.4σ to 3σCMB fit is degraded
Clear Interpretation 😃😐☹
![Page 59: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/59.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
19
Dark Radiation
(68 % CL, Planck+BAO+H0)
�Ne↵ = 0.23± 0.15 H0 tension from 4.4σ to 3σCMB fit is degraded
Clear Interpretation 😃😐☹
Strong Neutrino Scattering + Dark Radiation Kreisch, Cyr-Racine, Doré 1902.00543
⌫
⌫
⌫
⌫
![Page 60: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/60.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
19
Dark Radiation
(68 % CL, Planck+BAO+H0)
�Ne↵ = 0.23± 0.15 H0 tension from 4.4σ to 3σCMB fit is degraded
Clear Interpretation 😃😐☹
Strong Neutrino Scattering + Dark Radiation Kreisch, Cyr-Racine, Doré 1902.00543
⌫
⌫
⌫
⌫
H0 tension solved if TEEE data is ignored 😃
Almost excluded by Lab data (Blinov++1905.02727)☹If pol data is included no solution for H0 😐
![Page 61: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/61.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
19
Dark Radiation
(68 % CL, Planck+BAO+H0)
�Ne↵ = 0.23± 0.15 H0 tension from 4.4σ to 3σCMB fit is degraded
Clear Interpretation 😃😐☹
Light Neutrinophilic Scalar + Dark Radiation Escudero & Witte 1909.04044
⌫̄
⌫
�
Strong Neutrino Scattering + Dark Radiation Kreisch, Cyr-Racine, Doré 1902.00543
⌫
⌫
⌫
⌫
H0 tension solved if TEEE data is ignored 😃
Almost excluded by Lab data (Blinov++1905.02727)☹If pol data is included no solution for H0 😐
![Page 62: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/62.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
19
Dark Radiation
(68 % CL, Planck+BAO+H0)
�Ne↵ = 0.23± 0.15 H0 tension from 4.4σ to 3σCMB fit is degraded
Clear Interpretation 😃😐☹
Light Neutrinophilic Scalar + Dark Radiation Escudero & Witte 1909.04044
⌫̄
⌫
�H0 tension from 4.4σ to 2.5σ 😐CMB fit is not degraded 😃Direct connection with Seesaw 😃
Strong Neutrino Scattering + Dark Radiation Kreisch, Cyr-Racine, Doré 1902.00543
⌫
⌫
⌫
⌫
H0 tension solved if TEEE data is ignored 😃
Almost excluded by Lab data (Blinov++1905.02727)☹If pol data is included no solution for H0 😐
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
19
Dark Radiation
(68 % CL, Planck+BAO+H0)
�Ne↵ = 0.23± 0.15 H0 tension from 4.4σ to 3σCMB fit is degraded
Clear Interpretation 😃😐☹
Early Dark Energy sourced by neutrinos Sakstein & Trodden 1911.11760
Light Neutrinophilic Scalar + Dark Radiation Escudero & Witte 1909.04044
⌫̄
⌫
�H0 tension from 4.4σ to 2.5σ 😐CMB fit is not degraded 😃Direct connection with Seesaw 😃
Strong Neutrino Scattering + Dark Radiation Kreisch, Cyr-Racine, Doré 1902.00543
⌫
⌫
⌫
⌫
H0 tension solved if TEEE data is ignored 😃
Almost excluded by Lab data (Blinov++1905.02727)☹If pol data is included no solution for H0 😐
![Page 64: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/64.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrinos and the Hubble Tension
19
Dark Radiation
(68 % CL, Planck+BAO+H0)
�Ne↵ = 0.23± 0.15 H0 tension from 4.4σ to 3σCMB fit is degraded
Clear Interpretation 😃😐☹
Early Dark Energy sourced by neutrinos Sakstein & Trodden 1911.11760
Use which is excluded at 3σ by KATRIN! m⌫ = 2 eVGood attempt to solve the coincidence problem 😃
☹
Light Neutrinophilic Scalar + Dark Radiation Escudero & Witte 1909.04044
⌫̄
⌫
�H0 tension from 4.4σ to 2.5σ 😐CMB fit is not degraded 😃Direct connection with Seesaw 😃
Strong Neutrino Scattering + Dark Radiation Kreisch, Cyr-Racine, Doré 1902.00543
⌫
⌫
⌫
⌫
H0 tension solved if TEEE data is ignored 😃
Almost excluded by Lab data (Blinov++1905.02727)☹If pol data is included no solution for H0 😐
![Page 65: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/65.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Conclusions
20
Neutrino Masses:New lab bound from KATRIN: (95 % CL)
Bounds from Planck+BAO:X
m⌫ < 0.12 eV (95 % CL)
Xm⌫ < 3.9 eV
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Conclusions
20
Neutrino Masses:New lab bound from KATRIN: (95 % CL)
Bounds from Planck+BAO:X
m⌫ < 0.12 eV (95 % CL)
Xm⌫ < 3.9 eV
Neff:Planck Constraints:BBN Constraints:
Ne↵ = 2.99± 0.17
Ne↵ = 2.88± 0.28
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Conclusions
20
Neutrino Masses:New lab bound from KATRIN: (95 % CL)
Bounds from Planck+BAO:X
m⌫ < 0.12 eV (95 % CL)
Xm⌫ < 3.9 eV
Neff:Planck Constraints:BBN Constraints:
Ne↵ = 2.99± 0.17
Ne↵ = 2.88± 0.28
The Hubble Tension:Many neutrino related approaches
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Outlook
21
Neutrino Masses:KATRIN reach: (90% CL)
Next Galaxy Surveys+CMB should detect neutrino masses
Xm⌫ < 0.6 eV
e.g.: 1308.4164 Font-Ribera et. al., 1408.7052 Kitching et. al.
DESI/EUCLID+Planck: �⇣X
m⌫
⌘' 0.02 eV (1�)
![Page 69: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/69.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Outlook
21
Neutrino Masses:KATRIN reach: (90% CL)
Next Galaxy Surveys+CMB should detect neutrino masses
Xm⌫ < 0.6 eV
e.g.: 1308.4164 Font-Ribera et. al., 1408.7052 Kitching et. al.
DESI/EUCLID+Planck: �⇣X
m⌫
⌘' 0.02 eV (1�)
Neff:Stage-IV experiments will reach 1% precision, e.g. CMB-S4Strong constraints on new physics
![Page 70: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/70.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Outlook
21
Neutrino Masses:KATRIN reach: (90% CL)
Next Galaxy Surveys+CMB should detect neutrino masses
Xm⌫ < 0.6 eV
e.g.: 1308.4164 Font-Ribera et. al., 1408.7052 Kitching et. al.
DESI/EUCLID+Planck: �⇣X
m⌫
⌘' 0.02 eV (1�)
Neff:Stage-IV experiments will reach 1% precision, e.g. CMB-S4Strong constraints on new physics
The Hubble Tension:Further data on the way: Gaia, Strong Lensing, GW, DESI ...More models will appear and neutrinos will play a leading role
![Page 71: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/71.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Time for Questions and Comments
22
Upcoming years are going to be exciting!
Thank you for your attention!
⌫
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Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Back Up
23
![Page 73: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/73.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
KATRIN
24
a)
18535 18555 18575 18595 18615
100
101
Count
rate
(cp
s)
KATRIN data with 1 errorbars 50 Fit result
b)
18535 18555 18575 18595 18615-2
0
2
Res
idual
s (
)
Stat. Stat. and syst.
c)
18535 18555 18575 18595 18615
Retarding energy (eV)
0
20
40
Tim
e (h
)
m⌫̄e = 0
m⌫̄e = 1 eV
Ch. Weinheimer hep-ex/0210050
1909.06048
![Page 74: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/74.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Mass Models
25
Asai et. al. 1811.07571
U(1)Lµ�L⌧
Particle Physicists take very seriously neutrino mass constraints:
![Page 75: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/75.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
ΛCDM in 2020
26
Weak lensing
BAOs
SNIa
Lyman-α forest
BBN CMBΛCDM model tested on very different time/length scales
![Page 76: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/76.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
CMB constraints on Neff
27
Planck Results
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
Ne↵ = 2.92± 0.18 (68 % CL, TTTEEE+lowE)
(68 % CL, TTTEEE+lowE+len+BAO)Ne↵ = 2.99± 0.17Ne↵ = 3.27± 0.15 (68 % CL, TTTEEE+lowE+len+BAO+H0)
ΔNeff ~ 0.2-0.5 can ameliorate the Hubble tension
But values ΔNeff ~ 0.2-0.5 are not favoured by Planck Observations within ΛCDM
Beyond ΛCDM : ΔNeff ~ 0.5 can occur: e.g. Escudero & Witte 1909.04044
![Page 77: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/77.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Interactions
28
Neutrino Perturbations have a strong effect on the CMB spectra.
Gµ⌫ = 8⇡GTµ⌫ �Gµ⌫ = 8⇡G �Tµ⌫
Bashinsky & Seljak astro-ph/0310198
CMB: Follin, Knox, Millea & Pan, PRL 1503.07863BAO: Baumann et. al., Nature Phys. 1803.10741
Free Streaming effect detection:
This can be used to test relevant particle physics models:Annihilations Decays Scatterings Light Species
![Page 78: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/78.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
29
Parametrization mattersVagnozzi et. al. 1701.08172 Mahony et. al. 1907.04331
Choudhury & Hannestad 1907.12598 Gariazzo et. al. 1801.04946 Loureiro et. al. 1811.02578
⌫1⌫2
⌫3
Degenerate
⌫1 ⌫2 ⌫3
Normal
⌫1⌫2
⌫3Inverted
![Page 79: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/79.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
29
Parametrization mattersVagnozzi et. al. 1701.08172
Xm⌫ < 0.12 eVPlanck+BAO Degenerate
Planck+BAO Normal Hierarchy (vary mlight)X
m⌫ < 0.15 eV
bounds from Choudhury & Hannestad 1907.12598
Planck+BAO Inverted Hierarchy (vary mlight)X
m⌫ < 0.17 eV
Mahony et. al. 1907.04331Choudhury & Hannestad 1907.12598
Gariazzo et. al. 1801.04946 Loureiro et. al. 1811.02578
⌫1⌫2
⌫3
Degenerate
⌫1 ⌫2 ⌫3
Normal
⌫1⌫2
⌫3Inverted
![Page 80: Neutrino Cosmology in 2020: Where do we Stand? · 2020. 1. 28. · Choudhury & Hannestad 19' CDM+mν+ωa+ω X m ⌫ < 0.25eV Dark Energy dynamics Varying Curvature X m ⌫ < 0.15eV](https://reader035.vdocuments.mx/reader035/viewer/2022071510/612dbfad1ecc5158694261ed/html5/thumbnails/80.jpg)
Neutrino Cosmology in 2020 LCDM 23-01-20Miguel Escudero (KCL)
Neutrino Masses from Cosmology
29
Parametrization mattersVagnozzi et. al. 1701.08172
Xm⌫ < 0.12 eVPlanck+BAO Degenerate
Planck+BAO Normal Hierarchy (vary mlight)X
m⌫ < 0.15 eV
bounds from Choudhury & Hannestad 1907.12598
Planck+BAO Inverted Hierarchy (vary mlight)X
m⌫ < 0.17 eV
Mahony et. al. 1907.04331Choudhury & Hannestad 1907.12598
Gariazzo et. al. 1801.04946 Loureiro et. al. 1811.02578
Constraints are prior dependent (see next talk by Constance)
⌫1⌫2
⌫3
Degenerate
⌫1 ⌫2 ⌫3
Normal
⌫1⌫2
⌫3Inverted