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

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

The Cosmological Matter Power Spectrum Inflation: ? Perturbations enter horizon: Matter Domination Radiation Domination [ δΦ mat const] [ δΦ rad decays] horizon size P(k) → k →

How does probe neutrinos? (Assuming thermal equilibrium)

How does probe neutrinos? (Assuming thermal equilibrium) P(k) → k →

How does probe neutrinos? (Assuming thermal equilibrium) Radiation Matter Domination Domination P(k) → k →

How does probe neutrinos? (Assuming thermal equilibrium) Radiation Matter Domination Domination P(k) → Is this a coincidence? k →

How does probe neutrinos? (Assuming thermal equilibrium) � Radiation Matter Domination ρ ν = m i n ν i Domination � m ν i P(k) → Ω ν ≈ 93 h 2 eV E 2 = p 2 + m 2 Is this a coincidence? k →

Distinguishing Features in the Power Spectrum Σ m ν i = 0 . 14 eV P(k) → Σ m ν i = 1 . 4 eV Lesgourgues & Pastor (2006) k → 1. Shape Information: Galaxy Surveys (Future: CMB lensing, Weak Lensing) 2. Relative Amplitude Information: ∆ P ( k ) = − 8 Ω ν CMB plus Lyman-alpha Forest, Galaxy Bias P ( k ) Ω m

Distinguishing Features in the Power Spectrum Σ m ν i = 0 . 14 eV P(k) → Galaxy Surveys Σ m ν i = 1 . 4 eV Lesgourgues & Pastor (2006) k → 1. Shape Information: Galaxy Surveys (Future: CMB lensing, Weak Lensing) 2. Relative Amplitude Information: ∆ P ( k ) = − 8 Ω ν CMB plus Lyman-alpha Forest, Galaxy Bias P ( k ) Ω m

Distinguishing Features in the Power Spectrum Σ m ν i = 0 . 14 eV P(k) → Galaxy Surveys Σ m ν i = 1 . 4 eV Relative Amplitude:CMB+Lya Lesgourgues & Pastor (2006) k → 1. Shape Information: Galaxy Surveys (Future: CMB lensing, Weak Lensing) 2. Relative Amplitude Information: ∆ P ( k ) = − 8 Ω ν CMB plus Lyman-alpha Forest, Galaxy Bias P ( k ) Ω m

The Primordial Spectrum: Precision Determination at Large Scales P(k) → k → P ( k ) = Ak n Planck 1-Year + WMAP Pol.: (Planck Collab. 2013) A = 2 . 196 +0 . 051 (3%) − 0 . 060 n = 0 . 9603 ± 0 . 0073 (0 . 8%)

Measuring P ( k ): from largest to smallest scales CMB SDSS Ly- α

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

Ω m & Other Parameter Degeneracy Ω m

Cosmological Matter Power Spectrum & CMB Constraints on N eff For LSS: Perturbations enter horizon at M/R equality Matter Domination Radiation Domination [ δΦ mat const] [ δΦ rad decays] horizon size P(k) → k → For BAO: Extra radiation changes expansion rate from perturbation evolution through baryon decoupling

& N eff [Dodelson (SLAC Cosmic Frontiers)]

Summary of Cosmological N eff Measures • SDSS BOSS Galaxy Clustering + BAO + WMAP 7 + SNe + H 0 (Zhao et. al 2012) N e ff = 4 . 308 ± 0 . 794 WMAP7 68% CL • SPT + WMAP 7 + H 0 (Hou et al. 2012) ... N e ff = 3 . 71 ± 0 . 35 • ACT + WMAP 7 + BAO + H 0 (Sievers et. al 2013) N e ff = 2 . 78 ± 0 . 55 • WMAP 9 + eCMB + BAO + H 0 (Hinshaw et al. 2012 v2 ) WMAP9 N e ff = 3 . 84 ± 0 . 40 Planck • Planck + high-l CMB + WMAP P + BAO (Planck Collab. 2013) N e ff = 3 . 30 ± 0 . 27

Estimating Upcoming Cosmological Neutrino Mass Constraints ∆ P ( k ) ≈ 1% ≈ − 8 Ω ν Hu, Eisenstein & Tegmark 1998 P ( k ) Ω m

Estimating Upcoming Cosmological Neutrino Mass Constraints ∆ P ( k ) ≈ 1% ≈ − 8 Ω ν Hu, Eisenstein & Tegmark 1998 P ( k ) Ω m � m ν i Ω ν ≈ 93 h 2 eV

Estimating Upcoming Cosmological Neutrino Mass Constraints ∆ P ( k ) ≈ 1% ≈ − 8 Ω ν Hu, Eisenstein & Tegmark 1998 P ( k ) Ω m � m ν i Ω ν ≈ 93 h 2 eV ⇒ m ν . (1% / 8) × Ω m (93 h 2 eV) =

Estimating Upcoming Cosmological Neutrino Mass Constraints ∆ P ( k ) ≈ 1% ≈ − 8 Ω ν Hu, Eisenstein & Tegmark 1998 P ( k ) Ω m � m ν i Ω ν ≈ 93 h 2 eV ⇒ m ν . (1% / 8) × Ω m (93 h 2 eV) = ⇒ m ν . 20 meV =

Estimating Upcoming Cosmological Neutrino Mass Constraints ∆ P ( k ) ≈ 1% ≈ − 8 Ω ν Hu, Eisenstein & Tegmark 1998 P ( k ) Ω m � m ν i Ω ν ≈ 93 h 2 eV ⇒ m ν . (1% / 8) × Ω m (93 h 2 eV) = ⇒ m ν . 20 meV = 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

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 Hu & Okamoto 2001 potential C L φφ

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

Σ m ν : The March of Time

Σ m ν : The March of Time 2 (95% CL) m ν [eV] 1 X

Σ m ν : The March of Time 2 (95% CL) m ν [eV] 1 X 2003

Σ m ν : The March of Time 2 (95% CL) 2dFGRS m ν [eV] 1 X 2003

Σ m ν : The March of Time 2 (95% CL) 2dFGRS m ν [eV] 1 X 2003 2006

(95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time

(95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS

(95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010

(95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone

(95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone 2012

(95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012

(95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012 WMAP 9 + BAO

(95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012 WMAP 9 + BAO 2013

(95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012 WMAP 9 + BAO ACT + WMAP 7 + BAO 2013

(95% CL) X m ν [eV] 1 2 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012 WMAP 9 + BAO ACT + WMAP 7 + BAO 2013 Planck + BAO

(95% CL) X m ν [eV] 1 2 Oscillations 2003 2dFGRS SDSS P g + WMAP 1 2006 Σ m ν : The March of Time WMAP 3 + LSS 2010 WMAP 7 + SDSS LRG BAO WMAP 7 alone SDSS BOSS + WMAP 7 2012 WMAP 9 + BAO ACT + WMAP 7 + BAO 2013 Planck + BAO

Cosmological & Laboratory Complementarity

CMB & LSS Complementarity: Parameter Degeneracy

Stage IV CMB + DESI: Σ m ν vs. N eff

Forecast Sensitivities σ ( N eff ) σ ( Σ m ν ) CF5 Neutrino Paper

Neutrino Mass from Cosmology: What would break if cosmology and neutrino experiment disagree? P(k) → 1. Primordial power spectrum P ( k ) is a simple power law k → 2. No other prevalent “non-vanilla” cosmological parameters and physics: w , N eff , modified gravity...

Summary

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

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