Neutrino Physics from the CMB & Large Scale Structure
- Report -Topical Conveners:
K.N. Abazajian, J.E. Carlstrom, A.T. Lee
Contributors:K.N. Abazajian, B.A. Benson, J. Bock, J. Borrill, J.E. Carlstrom, C.L. Chang, S. Church,
A. Cooray, T.M. Crawford, K.S. Dawson, S. Das, S. Dodelson, J. Errard, S. Hanany, W.L. Holzapfel, K. Honscheid, M. Kamionkowski, R. Keisler, L. Knox, J. Kovac, C.-L. Kuo, C. Lawrence, A.T. Lee, E. Linder, P. Lubin, A. Miller, M.D. Niemack, C. Pryke, C.
Reichardt, U. Seljak, E. Silverstein, A. Slosar, R. Stompor,A. Vieregg, E.J. Wollack, W.L.K. Wu, K.W. Yoon, and O. Zahn
Paper: http://is.gd/AnSecR [arXiv on Friday (?)]
Cosmic Frontier Snowmass Community Summer Study 2013August 1, 2013
k →
P(k)
→
?
Perturbations enter horizon:
hori
zon
size
Matter Domination[δΦmat const]
Radiation Domination[δΦrad decays]
The Cosmological Matter Power Spectrum
Inflation:
How does probe neutrinos?
(Assuming thermal equilibrium)
How does probe neutrinos?
k →
P(k)
→
(Assuming thermal equilibrium)
How does probe neutrinos?
k →
P(k)
→
Matter Domination Radiation Domination
(Assuming thermal equilibrium)
How does probe neutrinos?
k →
P(k)
→
Matter Domination Radiation Domination
(Assuming thermal equilibrium)
How does probe neutrinos?
k →
P(k)
→
Matter Domination Radiation Domination
Is this a coincidence?
(Assuming thermal equilibrium)
How does probe neutrinos?
k →
P(k)
→
Matter Domination Radiation Domination
Is this a coincidence?
(Assuming thermal equilibrium)
ρν =
∑minνi
E2= p2
+ m2
Ων ≈
∑mνi
93 h2 eV
Distinguishing Features in the Power Spectrum
k →
P(k)
→
Σmνi= 0.14 eV
Σmνi= 1.4 eV
1. Shape Information: Galaxy Surveys (Future: CMB lensing, Weak Lensing)
2. Relative Amplitude Information: CMB plus Lyman-alpha Forest, Galaxy Bias
Lesgourgues & Pastor (2006)
P (k)
P (k)= 8
m
Distinguishing Features in the Power Spectrum
k →
P(k)
→
Σmνi= 0.14 eV
Σmνi= 1.4 eV
1. Shape Information: Galaxy Surveys (Future: CMB lensing, Weak Lensing)
2. Relative Amplitude Information: CMB plus Lyman-alpha Forest, Galaxy Bias
Galaxy Surveys
Lesgourgues & Pastor (2006)
P (k)
P (k)= 8
m
Distinguishing Features in the Power Spectrum
k →
P(k)
→
Σmνi= 0.14 eV
Σmνi= 1.4 eV
1. Shape Information: Galaxy Surveys (Future: CMB lensing, Weak Lensing)
2. Relative Amplitude Information: CMB plus Lyman-alpha Forest, Galaxy Bias
Galaxy Surveys
Lesgourgues & Pastor (2006)Relative Amplitude:CMB+Lya
P (k)
P (k)= 8
m
The Primordial Spectrum: Precision Determination
at Large Scales
Planck 1-Year + WMAP Pol.: (Planck Collab. 2013)
P(k)
→
k → P (k) = Akn
A = 2.196+0.0510.060 (3%)
n = 0.9603± 0.0073 (0.8%)
CMB
Measuring P(k): from largest to smallest scales
SDSS Ly-α
Upcoming High-Precision Era: Relative Change to P(k)
Ωm & Other Parameter Degeneracy
Ωm
k →
P(k)
→
For LSS: Perturbations enter horizon at M/R equality
hori
zon
size
Matter Domination[δΦmat const]
Radiation Domination[δΦrad decays]
Cosmological Matter Power Spectrum &CMB Constraints on Neff
For BAO: Extra radiation changes expansion rate from perturbation evolution through baryon decoupling
[Dodelson (SLAC Cosmic Frontiers)]
& Neff
• SDSS BOSS Galaxy Clustering + BAO + WMAP 7 + SNe + H0 (Zhao et. al 2012)
• SPT + WMAP 7 + H0 (Hou et al. 2012)
• ACT + WMAP 7 + BAO + H0(Sievers et. al 2013)
• WMAP 9 + eCMB + BAO + H0 (Hinshaw et al. 2012 v2)
• Planck + high-l CMB + WMAP P + BAO (Planck Collab. 2013)
Summary of Cosmological Neff Measures
...
WMAP
7WM
AP9
68% CLNe↵ = 4.308± 0.794
Ne↵ = 3.71± 0.35
Ne↵ = 3.84± 0.40
Ne↵ = 2.78± 0.55
Ne↵ = 3.30± 0.27
Plan
ck
Estimating Upcoming Cosmological Neutrino Mass Constraints
Hu, Eisenstein & Tegmark 1998
P (k)
P (k) 1% 8
m
Estimating Upcoming Cosmological Neutrino Mass Constraints
Ων ≈
∑mνi
93 h2 eV
Hu, Eisenstein & Tegmark 1998
P (k)
P (k) 1% 8
m
Estimating Upcoming Cosmological Neutrino Mass Constraints
Ων ≈
∑mνi
93 h2 eV
Hu, Eisenstein & Tegmark 1998
P (k)
P (k) 1% 8
m
=) m . (1%/8) m(93h2 eV)
Estimating Upcoming Cosmological Neutrino Mass Constraints
Ων ≈
∑mνi
93 h2 eV
Hu, Eisenstein & Tegmark 1998
P (k)
P (k) 1% 8
m
=) m . (1%/8) m(93h2 eV)
=) m . 20 meV
Estimating Upcoming Cosmological Neutrino Mass Constraints
Kaplinghat et al PRL 2003 (CMB WL)Wang et al PRL 2005 (WL Clusters)De Bernardis et al. 2009 (Opt. WL)Joudaki & Kaplinghat 2011 (LSST)Basse et al. 2013 (Euclid)CF5 Neutrino Report 2013
Ων ≈
∑mνi
93 h2 eV
Hu, Eisenstein & Tegmark 1998
P (k)
P (k) 1% 8
m
=) m . (1%/8) m(93h2 eV)
=) m . 20 meV
Lensing of the CMB
Hu & Okamoto 2001
Lensing of the CMB
Hu & Okamoto 2001
Lensing of the CMB•Higher-order statistics in
CMB T maps can reconstruct the lensing potential. (detected by SPT, ACT, Planck)
Hu & Okamoto 2001
Lensing of the CMB•Higher-order statistics in
CMB T maps can reconstruct the lensing potential. (detected by SPT, ACT, Planck)
•Lensing also mixes polarization E modes to B modes, providing more information. (detected by SPT)
Hu & Okamoto 2001
Lensing of the CMB•Higher-order statistics in
CMB T maps can reconstruct the lensing potential. (detected by SPT, ACT, Planck)
•Lensing also mixes polarization E modes to B modes, providing more information. (detected by SPT)
•Detailed, high signal-to-noise measurements of arcminute polarization can therefore be used to reconstruct the lensing potential CL
φφHu & Okamoto 2001
Lensing Potential Power: Relative Change over an Integrated P(k)
Σmν: The March of Time
Σmν: The March of Time
1
Xm
[eV]
2(9
5% C
L)
Σmν: The March of Time
1
Xm
[eV]
2(9
5% C
L)
Σmν: The March of Time
2003
1
Xm
[eV]
2(9
5% C
L)
Σmν: The March of Time
2dFG
RS
2003
1
Xm
[eV]
2(9
5% C
L)
Σmν: The March of Time
2dFG
RS
2003 2006
1
Xm
[eV]
2(9
5% C
L)
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003 2006
1
Xm
[eV]
2(9
5% C
L)
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003
WM
AP
3 +
LSS
2006
1
Xm
[eV]
2(9
5% C
L)
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003 2010
WM
AP
3 +
LSS
2006
1
Xm
[eV]
2(9
5% C
L)
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003
WM
AP
7 al
one
WM
AP
7 +
SDSS
LR
G B
AO
2010
WM
AP
3 +
LSS
2006
1
Xm
[eV]
2(9
5% C
L)
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003
WM
AP
7 al
one
WM
AP
7 +
SDSS
LR
G B
AO
2010
WM
AP
3 +
LSS
2006
1
Xm
[eV]
2(9
5% C
L)
2012
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003
WM
AP
7 al
one
WM
AP
7 +
SDSS
LR
G B
AO
2010
WM
AP
3 +
LSS
2006
SDSS
BO
SS +
WM
AP
7
1
Xm
[eV]
2(9
5% C
L)
2012
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003
WM
AP
7 al
one
WM
AP
7 +
SDSS
LR
G B
AO
2010
WM
AP
3 +
LSS
2006
SDSS
BO
SS +
WM
AP
7
WM
AP
9 +
BAO
1
Xm
[eV]
2(9
5% C
L)
2012
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003
WM
AP
7 al
one
WM
AP
7 +
SDSS
LR
G B
AO
2010
WM
AP
3 +
LSS
2006
SDSS
BO
SS +
WM
AP
7
WM
AP
9 +
BAO
1
Xm
[eV]
2(9
5% C
L)
2012 2013
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003
WM
AP
7 al
one
WM
AP
7 +
SDSS
LR
G B
AO
2010
WM
AP
3 +
LSS
2006
SDSS
BO
SS +
WM
AP
7
AC
T +
WM
AP
7 +
BAO
WM
AP
9 +
BAO
1
Xm
[eV]
2(9
5% C
L)
2012 2013
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003
WM
AP
7 al
one
WM
AP
7 +
SDSS
LR
G B
AO
2010
WM
AP
3 +
LSS
2006
SDSS
BO
SS +
WM
AP
7
AC
T +
WM
AP
7 +
BAO
WM
AP
9 +
BAO
1
Xm
[eV]
2(9
5% C
L)
2012 2013
Plan
ck +
BA
O
Σmν: The March of Time
2dFG
RS
SDSS
Pg +
WM
AP
1
2003
WM
AP
7 al
one
WM
AP
7 +
SDSS
LR
G B
AO
2010
WM
AP
3 +
LSS
2006
SDSS
BO
SS +
WM
AP
7
AC
T +
WM
AP
7 +
BAO
WM
AP
9 +
BAO
1
Xm
[eV]
2(9
5% C
L)
2012 2013
Plan
ck +
BA
O
Oscillations
Cosmological & Laboratory Complementarity
CMB & LSS Complementarity: Parameter Degeneracy
Stage IV CMB + DESI: Σmν vs. Neff
CF5 Neutrino Paper
σ(Σmν) σ(Neff)Forecast Sensitivities
CF5 Neutrino Paper
σ(Σmν) σ(Neff)Forecast Sensitivities
Neutrino Mass from Cosmology: What would break if cosmology and neutrino experiment disagree?
1. Primordial power spectrum P(k) is a simple power law
2. No other prevalent “non-vanilla” cosmological parameters and physics: w, Neff, modified gravity...
P(k)
→
k →
Summary
Summary
• Cosmology has the strongest inferred experimental sensitivity on the total neutrino mass, and are forecast to maintain that position.
Summary
• Cosmology has the strongest inferred experimental sensitivity on the total neutrino mass, and are forecast to maintain that position.
• CF5 Neutrino group has analyzed all current forecast constraints from cosmology, and forecast that for a Stage IV CMB experiment and DESI galaxy survey 1-σ sensitivities are:
σ(Σmν) = 16 meV &σ(Neff) = 0.020
providing > 3σ sensitivity to the oscillation-required Σmν =58 meV and >2σ sensitivity to Neff
Summary
• Cosmology has the strongest inferred experimental sensitivity on the total neutrino mass, and are forecast to maintain that position.
• CF5 Neutrino group has analyzed all current forecast constraints from cosmology, and forecast that for a Stage IV CMB experiment and DESI galaxy survey 1-σ sensitivities are:
σ(Σmν) = 16 meV &σ(Neff) = 0.020
providing > 3σ sensitivity to the oscillation-required Σmν =58 meV and >2σ sensitivity to Neff
• What if we do not detect the minimal model? If the minimal neutrino sector, with Σmν = 58 meV and Neff = 3.046, is not robustly detected, it would imply something is “broken” in another aspect or aspects of cosmology, including possibly: non-constant dark energy, a non-power-law primordial perturbation spectrum, extra particle or radiation species, non-zero curvature, as well as other possibilities, e.g., a nonthermal cosmological neutrino background.
Backups
• 2dFGRS Shape (conservative but very important limits on ) [Elgaroy et al 2002]:
• SDSS 3D Pg(k) shape + WMAP I[Tegmark et al, 2003]:
• CMB + SDSS 2-point correlation function (nonlinear modeling):[Abazajian et al 2005]:
• WMAP 7 alone [Komatsu et al 2010]:
• SDSS Ly-alpha forest + WMAP 3-year[Seljak et al., 2006]:
• WMAP 7 + SDSS LRG BAO + H0 [Komatsu et al, 2010]:
Summary of Cosmological Neutrino Mass Constraints: 2010
Ωm
Σmνi≤ 1.8 eV
Σmνi≤ 1.8 eV
Σmνi≤ 0.69 eV
Σmνi≤ 0.17 eV
95% CL
...
WMAP
1WM
AP7
Σmνi< 0.58 eV
Σmνi< 1.3 eV
• SDSS BOSS Galaxy Clustering + BAO + WMAP 7 + SNe + H0 (Zhao et. al 2012)
• SPT + WMAP 7 + H0 + SPTCL (Hou et al. 2012) ⇒ See, however, Rozo et al 2012
• ACT + WMAP 7 + BAO + H0(Sievers et. al 2013)
• WMAP 9 + eCMB + BAO + H0 (Hinshaw et al. 2012)
Summary of Cosmological Neutrino Mass Constraints: today
95% CL
...
WMAP
7WM
AP9
mi 0.34 eV
mi 0.44 eV
mi 0.39 eV
0.10 eV mi 0.54 eV