CMB: Sound Waves in the Early Universe

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Cosmological constraints: BAO Consider two simple models: 1. ΛCDM 2. Flat, constant w Constraint from D V (0.35)/D V (0.2) Constraint fitting s/D V with model for s Constraint including distance to CMB d A (z LS )/D V Percival et al. 2007 46
Galaxy Clustering varies with Galaxy Type How are each of them related to the underlying Dark Matter distribution? BIAS Caveat for inference of Cosmological Parameters from LSS
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 23: Cold Dark Matter Models Power Spect
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 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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