Figure 10

Figure 10: Secondary anisotropies from the proper motion of galaxy clusters across the sky and Rees–Sciama effects are presented in the upper-left image over $8∘ × 8∘$ in a critically closed Cold Dark Matter model. The corresponding column density of matter over the same region ( $z = 0.43$ , $Δz = 0.025$ ) is displayed in the upper-right, clearly showing the dipolar nature of the proper motion effect. Anisotropies arising from decaying potentials in an open $Ω = 0.3$ model over a scale of $8∘ × 8∘$ are shown in the bottom left image, along with the gravitational potential over the same region ( $z = 0.33$ , $Δz = 0.03$ ) in the bottom right, demonstrating a clear anti-correlation. Maximum temperature fluctuations in each simulation are $ΔT ∕T = (5 × 10− 7, 1.0 × 10− 6)$ respectvely. Secondary anisotropies are dominated by decaying potentials at large scales, but all three sources (decaying potential, proper motion, and R-S) produce signatures of order 10^–6.