Primordial helium recombination. I. Feedback, line transfer, and continuum opacity
Abstract
Precision measurements of the cosmic microwave background temperature anisotropy on scales ℓ>500 will be available in the near future. Successful interpretation of these data is dependent on a detailed understanding of the damping tail and cosmological recombination of both hydrogen and helium. This paper and two companion papers are devoted to a precise calculation of helium recombination. We discuss several aspects of the standard recombination picture, and then include feedback, radiative transfer in He i lines with partial redistribution, and continuum opacity from H i photoionization. In agreement with past calculations, we find that He ii recombination proceeds in Saha equilibrium, whereas He i recombination is delayed relative to Saha due to the low rates connecting excited states of He i to the ground state. However, we find that at z<2200 the continuum absorption by the rapidly increasing H i population becomes effective at destroying photons in the He i 21Po-11S line, causing He i recombination to finish around z≈1800, much earlier than previously estimated.
- Publication:
-
Physical Review D
- Pub Date:
- April 2008
- DOI:
- arXiv:
- arXiv:astro-ph/0702143
- Bibcode:
- 2008PhRvD..77h3006S
- Keywords:
-
- 98.70.Vc;
- 95.30.Jx;
- Background radiations;
- Radiative transfer;
- scattering;
- Astrophysics
- E-Print:
- 30 pages, 13 figures, to be submitted to PRD