Calculation of the Ostriker-Vishniac Effect in Cold Dark Matter Models

Details Calculation of the Ostriker-Vishniac Effect in Cold Dark Matter Models Calculation of the Ostriker-Vishniac Effect in Cold Dark Matter Models

1998-01-05

arxiv.org/abs/astro-ph/9801022v3

Phys.Rev. D58 (1998) 043001

Astronomy and Astrophysics

Astrophysics

19 pages, 2 figures, Revtex. Phys. Rev. D, accepted. Final version to be published, with minor changes to open universe scalin

Scientific paper

10.1103/PhysRevD.58.043001

We present a new derivation of the cosmic microwave background anisotropy spectrum from the Ostriker-Vishniac effect for an open, flat, or closed Universe, and calculate the anisotropy expected in cold dark-matter (CDM) models. We provide simple semi-analytic fitting formulas for the Vishniac power spectrum that can be used to evaluate the expected anisotropy in CDM models for any arbitrary ionization history. In a flat Universe, CDM models normalized to cluster abundances produce rms temperature anisotropies of 0.8--2.4 $\mu$K on arcminute angular scales for a constant ionization fraction of unity, whereas an ionization fraction of 0.2 yields rms anisotropies of 0.3--0.8 $\mu$K. In an open and/or high-baryon-density Universe, the level of anisotropy is somewhat higher. The signal in some of these models may be detectable with planned interferometry experiments. The damping of the acoustic peaks in the primary-anisotropy spectrum at degree angular scales depends primarily on the optical depth and only secondarily on the epoch of reionization. On the other hand, the amplitude of Ostriker-Vishniac anisotropies depends sensitively on the epoch of reionization. Therefore, when combined with the estimate of the reionization optical depth provided by maps of degree-scale anisotropies, the Ostriker-Vishniac effect can provide a unique probe of the epoch of reionization.

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