Secondary CMB Anisotropy

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Polarized Landscape 100 10 reionization ΘE ∆ (µK) 1 EE BB 0.1 0.01 Hu & Dodelson (2002) gravitational waves 10 100 1000 l (multipole) gravitational lensing
Power Spectrum Measurements • Lensed field is non-Gaussian in that a single degree scale lens controls the polarization at arcminutes • Increased variance and covariance implies that 10x as much sky needed compared with Gaussian fields fractional power deviation 0.02 0.01 0 -0.01 -0.02 realizations Gaussian variance 100 Smith, Hu & Kaplinghat (2004) l 1000
Page 1 and 2: Secondary CMB Anisotropy II: B-Mode
Page 3 and 4: Polarized Landscape 100 10 reioniza
Page 5 and 6: Electric & Magnetic Polarization (a
Page 7 and 8: Quadrupoles from Gravitational Wave
Page 9 and 10: Energy Scale of Inflation • Ampli
Page 11 and 12: Slow Roll Consistency Relation •
Page 13 and 14: Modulated Polarization • Ionizati
Page 15 and 16: B-mode Contamination from Reionizat
Page 17 and 18: Example of CMB Lensing • Toy exam
Page 19 and 20: Lensing by a Gaussian Random Field
Page 21 and 22: Gravitational Lensing • Lensing i
Page 23 and 24: Flat-sky Treatment • Mode couplin
Page 25 and 26: • If ˜C ΘΘ l Smoothing Power S
Page 27 and 28: Generation of Power • On scales b
Page 29 and 30: Lensing Smoothing • Lensing smoot
Page 31 and 32: Polarization Lensing • Since E an
Page 33: Polarization Power Spectra • Carr
Page 37 and 38: Redshift Sensitivity • Lensing ob
Page 39 and 40: Lensing Observables • Lensing obs
Page 41 and 42: Lensing Reconstruction
Page 43 and 44: Quadratic Reconstruction • Matche
Page 45 and 46: High Signal-to-Noise B-modes • Co
Page 47 and 48: Matter Power Spectrum • Measuring
Page 49 and 50: Tomography & Growth Rate • Cross
Page 51 and 52: Cross Correlation with Temperature
Page 53 and 54: Reconstruction in the Halo Regime
Page 55 and 56: Reconstruction in the Halo Regime
Page 57 and 58: Cluster Lensing • In combination

Secondary CMB Anisotropy

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