CMB: Sound Waves in the Early Universe

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The Structure Formation Cookbook 1. Initial Conditions: A Theory for the Origin of Density Perturbations in the Early Universe P m (k)~k n , n~1 Primordial Inflation: initial spectrum of density perturbations 2. Cooking with Gravity: Growing Perturbations to Form Structure Set the Oven to Cold (or Hot or Warm) Dark Matter Season with a few Baryons and add Dark Energy P m (k)~T(k)k n 3. Let Cool for 13 Billion years Turn Gas into Stars P g (k)~b 2 (k)T(k)k n 4. Tweak (1) and (2) until it tastes like the observed Universe.
Cold Dark Matter Models Power Spectrum of the Mass Density ( ) = d 3 δ k ∫ δ( k 1 )δ( k 2 ) = ( 2π) 3 P k 1 ( ) x ⋅ e i k ⋅x δρ x ρ ( k 2 ) ( )δ 3 k 1 +
Page 1: CMB: Sound Waves in the Early Unive
Page 4 and 5: WMAP
Page 6 and 7: Standard ruler
Page 8 and 9: Geometry of three-dimensional space
Page 10 and 11: Angular positions of acoustic peaks
Page 12 and 13: CMB Results
Page 14 and 15: Assuming k=0 as changing Ω DE
Page 16: CMB shift parameter CMB anisotropy
Page 20: Standard ruler
Page 26 and 27: Sound Waves again Each initial
Page 28 and 29: Origin of Baryon Acoustic Oscillati
Page 30: sound horizon scale 30
Page 33 and 34: Simulation plus Poisson errors: mul
Page 35 and 36: Correlation Function Measure redshi
Page 38 and 39: SDSS Galaxy Distribution Luminous R
Page 40 and 41: Model Comparison Fixed Ω b h 2 =0.
Page 44 and 45: SALT MLCS SDSS only: Nearby+SDSS: M
Page 46 and 47: Cosmological constraints: BAO Consi
Page 49 and 50: Galaxy Clustering as a function of
Page 51 and 52: Systematic Issues for BAO Effects o
Page 53 and 54: III. Baryon Acoustic Oscillations G
Page 55 and 56: DES Science Program Four Probes of
Page 57: Galaxy Photo-z Simulations DES +VHS

CMB: Sound Waves in the Early Universe

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