Cosmic Microwave Background Anisotropies from the Rees-Sciama Effect in $Ω_{0} \le 1$ Universes

Details Cosmic Microwave Background Anisotropies from the Rees-Sciama Effect in $Ω_{0} \le 1$ Universes Cosmic Microwave Background Anisotropies from the Rees-Sciama Effect in $Ω_{0} \le 1$ Universes

1995-10-04

arxiv.org/abs/astro-ph/9510019v1

Astrophys.J.463:15,1996

Astronomy and Astrophysics

Astrophysics

20 pages + 7 figures + 4 plates, self-expanding uuencoded compressed tar archive of postscript files

Scientific paper

10.1086/177220

We investigate the imprint of nonlinear matter condensations on the Cosmic Microwave Background (CMB) in $\Omega_{0}<1$ cold dark matter (CDM) model universes. We consider simulation domains ranging from $120h^{-1}$ Mpc to $360h^{-1}$ Mpc in size. We concentrate on the secondary temperature anisotropies induced by time varying gravitational potentials occurring after decoupling. Specifically, we investigate the importance of the Rees-Sciama effect due to: (1) intrinsic changes in the gravitational potential of forming, nonlinear structures, (2) proper motion of nonlinear structures, and (3) late time decay of gravitational potential perturbations in open universes. CMB temperature anisotropies are obtained by numerically evolving matter inhomogeneities and CMB photons from an early, linear epoch ($z=100$) to the present, nonlinear epoch $(z=0)$. We test the dependence and relative importance of these secondary temperature anisotropies as a function of the scale of the underlying matter (voids, superclusters) and as a function of $\Omega_{0}$. The results of the $\Omega_{0}<1$ models are compared to a similarly executed $\Omega_{0}=1.0$ simulation. We find that in low density models all three sources of anisotropy could be relevant and reach levels of $\Delta T/T \sim 10^{-6}$. In particular, we find that for $\Omega_{0}<1$ at large scales, secondary temperature anisotropies are dominated by the decaying potential.

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