Neutrino Physics from the CMB & Large Scale Structure - Report - - PowerPoint PPT Presentation

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Neutrino Physics from the CMB & Large Scale Structure - Report - - PowerPoint PPT Presentation

Sep 24, 2022 137 likes •732 views

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,

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SLIDE 1

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 2013 August 1, 2013

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SLIDE 2

k → P(k) →

?

Perturbations enter horizon:

horizon size

Matter Domination

[δΦmat const]

Radiation Domination

[δΦrad decays]

The Cosmological Matter Power Spectrum Inflation:

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SLIDE 3

How does probe neutrinos?

(Assuming thermal equilibrium)

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SLIDE 4

How does probe neutrinos?

k → P(k) → (Assuming thermal equilibrium)

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SLIDE 5

How does probe neutrinos?

k → P(k) →

Matter Domination Radiation Domination

(Assuming thermal equilibrium)

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SLIDE 6

How does probe neutrinos?

k → P(k) →

Matter Domination Radiation Domination

(Assuming thermal equilibrium)

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SLIDE 7

How does probe neutrinos?

k → P(k) →

Matter Domination Radiation Domination Is this a coincidence?

(Assuming thermal equilibrium)

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SLIDE 8

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

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SLIDE 9

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 Ων Ωm

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SLIDE 10

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 Ων Ωm

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SLIDE 11

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 Ων Ωm

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SLIDE 12

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+0.051

−0.060

(3%) n = 0.9603 ± 0.0073 (0.8%)

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SLIDE 13

CMB

Measuring P(k): from largest to smallest scales

SDSS Ly-α

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SLIDE 14

Upcoming High-Precision Era: Relative Change to P(k)

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SLIDE 15

Ωm & Other Parameter Degeneracy

Ωm

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SLIDE 16

k → P(k) →

For LSS: Perturbations enter horizon at M/R equality

horizon 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

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SLIDE 17

[Dodelson (SLAC Cosmic Frontiers)] & Neff

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SLIDE 18
  • 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

...

WMAP7

WMAP9 68% CL Neff = 4.308 ± 0.794 Neff = 3.71 ± 0.35 Neff = 3.84 ± 0.40 Neff = 2.78 ± 0.55 Neff = 3.30 ± 0.27

Planck

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SLIDE 19

Estimating Upcoming Cosmological Neutrino Mass Constraints

Hu, Eisenstein & Tegmark 1998

∆P(k) P(k) ≈ 1% ≈ −8 Ων Ωm

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SLIDE 20

Estimating Upcoming Cosmological Neutrino Mass Constraints

Ων ≈ mνi 93 h2 eV

Hu, Eisenstein & Tegmark 1998

∆P(k) P(k) ≈ 1% ≈ −8 Ων Ωm

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SLIDE 21

Estimating Upcoming Cosmological Neutrino Mass Constraints

Ων ≈ mνi 93 h2 eV

Hu, Eisenstein & Tegmark 1998

∆P(k) P(k) ≈ 1% ≈ −8 Ων Ωm

= ⇒ mν . (1%/8) × Ωm(93h2 eV)

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SLIDE 22

Estimating Upcoming Cosmological Neutrino Mass Constraints

Ων ≈ mνi 93 h2 eV

Hu, Eisenstein & Tegmark 1998

∆P(k) P(k) ≈ 1% ≈ −8 Ων Ωm

= ⇒ mν . (1%/8) × Ωm(93h2 eV) = ⇒ mν . 20 meV

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SLIDE 23

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 Ων Ωm

= ⇒ mν . (1%/8) × Ωm(93h2 eV) = ⇒ mν . 20 meV

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SLIDE 24

Lensing of the CMB

Hu & Okamoto 2001

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SLIDE 25

Lensing of the CMB

Hu & Okamoto 2001

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SLIDE 26

Lensing of the CMB

  • Higher-order statistics in

CMB T maps can reconstruct the lensing

  • potential. (detected by

SPT, ACT, Planck)

Hu & Okamoto 2001

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SLIDE 27

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

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SLIDE 28

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 CLφφ

Hu & Okamoto 2001

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SLIDE 29

Lensing Potential Power: Relative Change over an Integrated P(k)

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SLIDE 30

Σmν: The March of Time

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SLIDE 31

Σmν: The March of Time

1

X mν [eV]

2 (95% CL)

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SLIDE 32

Σmν: The March of Time

1

X mν [eV]

2 (95% CL)

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SLIDE 33

Σmν: The March of Time

2003 1

X mν [eV]

2 (95% CL)

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SLIDE 34

Σmν: The March of Time

2dFGRS

2003 1

X mν [eV]

2 (95% CL)

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SLIDE 35

Σmν: The March of Time

2dFGRS

2003 2006 1

X mν [eV]

2 (95% CL)

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SLIDE 36

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003 2006 1

X mν [eV]

2 (95% CL)

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SLIDE 37

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003

WMAP 3 + LSS

2006 1

X mν [eV]

2 (95% CL)

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SLIDE 38

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003 2010

WMAP 3 + LSS

2006 1

X mν [eV]

2 (95% CL)

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SLIDE 39

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003

WMAP 7 alone WMAP 7 + SDSS LRG BAO

2010

WMAP 3 + LSS

2006 1

X mν [eV]

2 (95% CL)

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SLIDE 40

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003

WMAP 7 alone WMAP 7 + SDSS LRG BAO

2010

WMAP 3 + LSS

2006 1

X mν [eV]

2 (95% CL) 2012

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SLIDE 41

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003

WMAP 7 alone WMAP 7 + SDSS LRG BAO

2010

WMAP 3 + LSS

2006

SDSS BOSS + WMAP 7

1

X mν [eV]

2 (95% CL) 2012

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SLIDE 42

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003

WMAP 7 alone WMAP 7 + SDSS LRG BAO

2010

WMAP 3 + LSS

2006

SDSS BOSS + WMAP 7 WMAP 9 + BAO

1

X mν [eV]

2 (95% CL) 2012

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SLIDE 43

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003

WMAP 7 alone WMAP 7 + SDSS LRG BAO

2010

WMAP 3 + LSS

2006

SDSS BOSS + WMAP 7 WMAP 9 + BAO

1

X mν [eV]

2 (95% CL) 2012 2013

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SLIDE 44

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003

WMAP 7 alone WMAP 7 + SDSS LRG BAO

2010

WMAP 3 + LSS

2006

SDSS BOSS + WMAP 7 ACT + WMAP 7 + BAO WMAP 9 + BAO

1

X mν [eV]

2 (95% CL) 2012 2013

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SLIDE 45

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003

WMAP 7 alone WMAP 7 + SDSS LRG BAO

2010

WMAP 3 + LSS

2006

SDSS BOSS + WMAP 7 ACT + WMAP 7 + BAO WMAP 9 + BAO

1

X mν [eV]

2 (95% CL) 2012 2013

Planck + BAO

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SLIDE 46

Σmν: The March of Time

2dFGRS SDSS Pg + WMAP 1

2003

WMAP 7 alone WMAP 7 + SDSS LRG BAO

2010

WMAP 3 + LSS

2006

SDSS BOSS + WMAP 7 ACT + WMAP 7 + BAO WMAP 9 + BAO

1

X mν [eV]

2 (95% CL) 2012 2013

Planck + BAO

Oscillations

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SLIDE 47

Cosmological & Laboratory Complementarity

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SLIDE 48

CMB & LSS Complementarity: Parameter Degeneracy

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SLIDE 49

Stage IV CMB + DESI: Σmν vs. Neff

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SLIDE 50

CF5 Neutrino Paper σ(Σmν) σ(Neff) Forecast Sensitivities

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SLIDE 51

CF5 Neutrino Paper σ(Σmν) σ(Neff) Forecast Sensitivities

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SLIDE 52

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 →

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SLIDE 53

Summary

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SLIDE 54

Summary

  • Cosmology has the strongest inferred experimental sensitivity on the

total neutrino mass, and are forecast to maintain that position.

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SLIDE 55

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

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SLIDE 56

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.

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SLIDE 57

Backups

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SLIDE 58
  • 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 ...

WMAP1 WMAP7

Σmνi < 0.58 eV Σmνi < 1.3 eV

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SLIDE 59
  • 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 ...

WMAP7 WMAP9

Σmνi ≤ 0.34 eV Σmνi ≤ 0.44 eV Σmνi ≤ 0.39 eV 0.10 eV ≤ Σmνi ≤ 0.54 eV