CMB: Sound Waves in the Early Universe

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Dependence on w Tangential Radial Assum<strong>in</strong>g constant Ω m Measure k A to 1% plus known s yields w to ~5%
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: Correlation Function Measure redshi
Page 39 and 40: Large-scale Correlations of SDSS L
Page 41: Constraints € Galaxy pair with se
Page 45 and 46: BAO from SDSS + 2dFGRS BAO detected
Page 47: Galaxy Clustering varies with Gala
Page 50 and 51: δn gal Correct For Luminosity Bias
Page 52 and 53: Halos vs. Dark Matter Real Space Re
Page 54 and 55: III. Baryon Acoustic Oscillations B
Page 56 and 57: Photometric Redshifts • Measure r

CMB: Sound Waves in the Early Universe

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