• Review Home
• Introduction
• Observables
  • Cosmological Paradigm
  • Temperature Field
  • Polarization Field
• Acoustic Peaks
  • Introduction
  • Basics
  • Initial Conditions
  • Gravitational Forcing
  • Baryon Loading
  • Radiation Driving
  • Damping
  • Polarization
  • Integral Approach
  • Parameter Sensitivity
• Matter Power Spectrum
  • Introduction
  • Physical Description
  • Cosmological Implications
• Gravitational Secondaries
  • Introduction
  • ISW Effect
  • RS/Moving Halo
  • Gravitational Waves
  • Gravitational Lensing
• Scattering Secondaries
  • Introduction
  • Peak Suppression
  • Large Angle Polarization
  • Doppler Effect
  • Modulated Doppler Effect
  • SZ Effect
• Non-Gaussianity
• Data Analysis
  • Introduction
  • Mapmaking
  • Bandpower Estimation
  • Parameter Estimation
• Discussion
  • Discussion
  • Bibliography

Scattering Secondaries

From the observations both of the lack of of a Gunn-Peterson trough [Gunn & Peterson, 1965] in quasar spectra and its preliminary detection [Becker et al, 2001], we know that hydrogen was reionized at . This is thought to occur through the ionizing radiation of the first generation of massive stars (see e.g. [Loeb & Barkana, 2001] for a review). The consequent recoupling of CMB photons to the baryons causes a few percent of them to be rescattered. Linearly, rescattering induces three changes to the photon distribution: suppression of primordial anisotropy, generation of large angle polarization, and a large angle Doppler effect. The latter two are suppressed on small scales by the cancellation highlighted in §4.2.1. Non-linear effects can counter this suppression; these are the subject of active research and are outlined in §4.3.4.

Plate 5b: Secondary anisotropies: (b) Scattering secondaries: rescattering suppression, Doppler, modulated Doppler (density and ionization), and SZ effects.

Subsections

• Peak Suppression
• Large-Angle Polarization
• Doppler Effect
• Modulated Doppler Effects
• Sunyaev-Zel'dovich Effect