Linear effects of perturbed recombination

Abstract

Perturbations in the ionization fraction after recombination affect the Compton cooling of density perturbations. Once the gas temperature starts to decouple from the CMB temperature, ionization fraction perturbations can have a significant influence on the subsequent gas temperature perturbation evolution. This directly affects the 21cm spin temperature of the gas, and also modifies the small-scale baryon perturbation evolution via the difference in baryon pressure. The effect on the gas temperature perturbations can be significant on all scales, and galactic-scale baryon perturbations are modified at the percent level at redshifts z >~ 100 where numerical simulations are typically started.

5 pages; for more details of effect on 21cm see astro-ph/0702600; code available at http://camb.info/sources/

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• An extensive investigation of the Generalised Dark Matter model
• Modeling Dark Photon Oscillations in Our Inhomogeneous Universe
• Background reionization history from omniscopes
• The Dark Ages' 21-cm Trispectrum
• Non-comoving Cosmology
• Exploring compensated isocurvature perturbations with CMB spectral distortion anisotropies
• Cosmic Microwave Background Anisotropy numerical solution (CMBAns) I: An introduction to $C_l$ calculation
• AEther as an Inevitable Consequence of Quantum Gravity
• Stability of small-scale baryon perturbations during cosmological recombination
• Impact of inhomogeneous CMB heating of gas on the HI 21-cm signal during dark ages
• Magnetic fields from small-scale primordial perturbations