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$\begin{figure} \par\includegraphics[width=18cm]{0204fig1.eps} \end{figure}$ Figure 1: ( Left panel) a) Visibility function versus redshift under WMAP5 cosmogony. ( Middle panel) b) Thomson optical depth versus redshift due to all electrons (solid line) and to those electrons contained in halos more massive than $5\times 10^{12}~ M_{\odot}$ (dashed line). ( Right panel) c) Showing square root of angular power spectra, note the $\mu$ K units. Thick solid line: total CMB temperature anisotropy amplitude. Filled circles: total kSZ induced temperature fluctuations generated during and after reionization. Thin solid line: total E polarization mode power spectrum. Thick dashed line: correlation term of the Thomson scattering induced fluctuations generated in galaxy clusters. Thin dashed line: Poisson term of the Thomson scattering induced fluctuations in galaxy clusters. Dot-dashed line: cross-correlation between the total E-mode polarization (thin solid line) and the correlated part of the kSZ generated in galaxy groups and clusters (thick dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=18cm]{0204fig2.eps} \end{figure}$ Figure 2: The total S/N ratio for the correlation of the E-mode polarization with the low redshift (z<3-4) kSZ generated by bulk flows in galaxy groups and clusters. Horizontal axes display the decimal logarithm of the individual group/cluster kSZ measurement S/N ratio ( $\xi$ ), whereas vertical axes display the decimal logarithm of the minimum mass of groups/clusters considered. Due to Poisson/shot noise, a low choice for $z_{\rm min}$ makes the high total S/N regions shrink, and this also happens if $z_{\rm min}$ is chosen too large and too much information is unused. The optimal minimum redshift is around $z_{\rm min} \simeq 0.05$ , and the maximum S/N ratio achievable for perfect E and kSZ surveys is $\sim$ 5.8. Note that we are assuming $f_{\rm sky} = 1$ .
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In the text