NEUTRINOS AND FUTURE CONCORDANCE COSMOLOGIES Neutrino 2008 / - - PowerPoint PPT Presentation

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NEUTRINOS AND FUTURE CONCORDANCE COSMOLOGIES Neutrino 2008 / - - PowerPoint PPT Presentation

Jun 18, 2023 236 likes •576 views

NEUTRINOS AND FUTURE CONCORDANCE COSMOLOGIES Neutrino 2008 / Richard Easther (Yale) INTRODUCTION... Integrated History of the Universe... Probes: CMB Large scale structure 21 cm Summary... C OSMOLOGY : O VERVIEW Image: NASA C OSMOLOGY

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SLIDE 1 NEUTRINOS AND FUTURE CONCORDANCE COSMOLOGIES Neutrino 2008 / Richard Easther (Yale)
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SLIDE 2 INTRODUCTION... Integrated History of the Universe... Probes: CMB Large scale structure 21 cm Summary...
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SLIDE 3 Image: NASA COSMOLOGY: OVERVIEW
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SLIDE 4 Image: NASA COSMOLOGY: OVERVIEW Overall expansion...
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SLIDE 5 Image: NASA COSMOLOGY: OVERVIEW

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Stars, galaxies...
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SLIDE 6 Image: NASA COSMOLOGY: OVERVIEW Dark Ages...
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SLIDE 7 Image: NASA COSMOLOGY: OVERVIEW Microwave Background
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SLIDE 8 Image: NASA COSMOLOGY: OVERVIEW Inflation “Big Bang” +BBN
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SLIDE 9 CONCORDANCE COSMOLOGY b Baryon fraction (Mass known, #??) Baryogenesis (? - GUT, Electroweak?) CDM Dark matter (Mass ??, #??) TeV Scale physics?? Supersymmetry? LHC?
  • Cosmological constant
Quantum Gravity Tooth fairy?
  • Reionization
First stars (gastrophysics, nuclear physics) h Hubble’s “constant” When we are looking As,ns Primordial Perturbations Inflation GUT/string physics?
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SLIDE 10 THE FUTURE... Parameter set will expand Neutrino sector! Scale dependence of n? Dark energy parameters? Tensor modes? Helium fraction? Curvature? Secondary anisotropies? Parameter set will shrink Neutrino masses from experiments? Recombination observed directly in 21cm? Specific models of inflation?
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SLIDE 11 NUMBERS... Photons: T = 2.726 K = 2.35 10-4 eV (measured) Massless : T ~ 1.9K = 1.7 10-4 eV (inferred) Photons at z = 1,089: T = 2.97 103 K = 0.255 eV Massless : T ~ 2.07 103 K = .17 eV Minimum m ~ 0.05 eV (normal hierarchy) Change in equation of state as universe expands!
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SLIDE 12 CMB: WMAP
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SLIDE 13 BEST FIT Early universe is a simple system General relativity and small inhomogeneities e-, p, He nuclei, dark matter, , , also , Ho and k Boltzmann equations Beautiful and largely classical classical physics Compute Cl & polarization (E and B mode)
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SLIDE 14 THE SPECTRAL INDEX
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SLIDE 15 THE BARYON FRACTION
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SLIDE 16 HUBBLE PARAMETER
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SLIDE 17 WHAT DO WE LEARN? Count the significant figures... Cosmology graduated from back of the envelope! WMAP 5 +
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SLIDE 18 TOTAL NEUTRINO MASS
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SLIDE 19 ERROR FORECASTS (Rough & Overly Optimistic) Planck’ “Ideal” Perfect m H0
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SLIDE 20 CURRENT CONSTRAINTS WMAP5 + All Care needed Priors Systematics between datasets m < ~1eV Komatsu et al.
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SLIDE 21 LARGE SCALE STRUCTURE
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SLIDE 22 LARGE SCALE STRUCTURE & LENSING Galaxies clustered in space Bubbles and voids Orthogonal information to microwave background Large scale structure Get power spectrum P(k) Break degeneracies Nonlinear at short scales (function of redshift)
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SLIDE 23 MATTER POWER...
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SLIDE 24 Before first stars, universe is mostly neutral H Neutral hydrogen emits a 21cm line Redshifted; H at redshift 10: 2.1 meters. HIGH-REDSHIFT 21CM
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SLIDE 25 HIGH-REDSHIFT 21CM Observe sky at ~100 MHz Remove foregrounds (!) Map neutral hydrogen density as a function of z Needs radio-quiet location Get “slices” by tuning receiver
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SLIDE 26 (Steve Furlanetto)
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SLIDE 27 HIGH-REDSHIFT 21CM Instruments Mileura (Australia) LOFAR (Belguim) SKA (To be decided) Lunar Array (Far side of the moon / vaporware!)
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SLIDE 28 PROSPECT FOR NEUTRINOS First observations: “Low” redshift Focus on reionization / first stars Longer term: High redshift Weaker signal Probe short wavelengths (uncollapsed) Perturbations small; challenging experiments Foregrounds??? Terrestrial noise???
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SLIDE 29 A BOLD PREDICTION? Total mass: 0.3eV Nonlinear scales at z=0.3,4 and 8 Pritchard and Pierpaoli
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SLIDE 30 A BOLD PREDICTION? Total mass 0.12eV Both hierarchies Solid z=8 Theoretically distinguishable Pritchard and Pierpaoli
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SLIDE 31 COMMENTS AND CONCLUSIONS... Neutrinos provide definite target Very good reason to believe they are there (WMAP) We know their total mass is non-zero Probe thermal history of very early universe Small effect: precision cosmology Terrestrial measurements of neutrino mass constrain other cosmological parameters
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SLIDE 32 COMMENTS AND CONCLUSIONS... Current bound ~10 times larger than minimum m Next few years: Planck, ACT, EBEX, DEC Better SN1a bounds & BAO, first 21cm data Somewhat longer term: JDEM, LSST, CMBPol (?) Very long term: High precision high-z 21cm GUESS: A factor of 10 on m in 10 years??