All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0322fig1.ps} \end{figure}$ Figure 1: The expected error-bars (red) on the Compton parameter for the Planck experiment, without contamination. The open triangles (blue) show the effect due to non-removed radio contamination. The open squares (purple) are for correlated IR galaxies, and the filled circles (green) are when none of the dust emission fluctuations have been removed.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0322fig2.ps} \end{figure}$ Figure 2: Derived electron temperature in keV. Open triangles (blue) are for radio contamination, open squares (purple) are for Poisson+correlated IR galaxies, and filled circles (green) are for dust fluctuations. Statistical error-bars (of the order few to ten keV) are not shown in order to avoid confusion.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0322fig3.ps} \end{figure}$ Figure 3: Upper limit to the expected effect of contamination in the derived peculiar velocity in km s^-1. Open triangles (blue) are for radio contamination, open squares (purple) for Poisson+correlated IR galaxies, and filled circles (green) for dust fluctuation. Statistical error-bars (on the order of a few 100 to a few 1000 km s^-1) are not shown, in order to avoid confusion.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0322fig4.ps} \end{figure}$ Figure 4: Compton parameter for an ideal experiment with 4 observing frequencies at 100, 150, 217, and 270 GHz, and with $0.1~\mu$ K sensitivity. Open triangles (blue) for radio contamination; open squares (purple) are for Poisson+correlated IR galaxies. The very small statistical error-bars without contamination are shown in red. Systematic shift from dust fluctuations is very small and is not shown as it would obscure the statistical error-bars.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0322fig5.ps} \end{figure}$ Figure 5: Derived electron temperature in keV for an ideal experiment. The very small statistical error-bars are shown in red. Open triangles (blue) are radio contamination, open squares (purple) are Poisson+correlated IR galaxies, and filled circles (green) are for dust fluctuations.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0322fig6.ps} \end{figure}$ Figure 6: Compton parameter for ACT-like survey. The statistical error-bars without contamination are shown in red. Open triangles (blue) are radio contamination, open squares (purple) Poisson+correlated IR galaxies, and filled circles (green) dust fluctuations.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0322fig7.ps} \end{figure}$ Figure 7: Derived electron temperature in keV. Open triangles (blue) are radio contamination, open squares (purple) are Poisson+correlated IR galaxies, and filled circles (green) are dust fluctuations. Statistical error-bars (the smallest about 5 keV, but more typical error-bars are around 10-20 keV) are not shown in order to avoid confusion.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0322fig8.ps} \end{figure}$ Figure 8: Upper limit to the expected effect of contamination in the derived peculiar velocity in km s^-1. Open triangles (blue) are radio contamination, open squares (purple) Poisson+correlated IR galaxies, and filled circles (green) dust fluctuations. Statistical error-bars (the smallest are about 500 km s^-1, but more typical error-bars are 2000-6000 km s^-1) are not shown, in order to avoid confusion.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0322fig1.ps} \end{figure}$	Figure 1: The expected error-bars (red) on the Compton parameter for the Planck experiment, without contamination. The open triangles (blue) show the effect due to non-removed radio contamination. The open squares (purple) are for correlated IR galaxies, and the filled circles (green) are when none of the dust emission fluctuations have been removed.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0322fig2.ps} \end{figure}$	Figure 2: Derived electron temperature in keV. Open triangles (blue) are for radio contamination, open squares (purple) are for Poisson+correlated IR galaxies, and filled circles (green) are for dust fluctuations. Statistical error-bars (of the order few to ten keV) are not shown in order to avoid confusion.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0322fig3.ps} \end{figure}$	Figure 3: Upper limit to the expected effect of contamination in the derived peculiar velocity in km s^-1. Open triangles (blue) are for radio contamination, open squares (purple) for Poisson+correlated IR galaxies, and filled circles (green) for dust fluctuation. Statistical error-bars (on the order of a few 100 to a few 1000 km s^-1) are not shown, in order to avoid confusion.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0322fig5.ps} \end{figure}$	Figure 5: Derived electron temperature in keV for an ideal experiment. The very small statistical error-bars are shown in red. Open triangles (blue) are radio contamination, open squares (purple) are Poisson+correlated IR galaxies, and filled circles (green) are for dust fluctuations.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0322fig6.ps} \end{figure}$	Figure 6: Compton parameter for ACT-like survey. The statistical error-bars without contamination are shown in red. Open triangles (blue) are radio contamination, open squares (purple) Poisson+correlated IR galaxies, and filled circles (green) dust fluctuations.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0322fig7.ps} \end{figure}$	Figure 7: Derived electron temperature in keV. Open triangles (blue) are radio contamination, open squares (purple) are Poisson+correlated IR galaxies, and filled circles (green) are dust fluctuations. Statistical error-bars (the smallest about 5 keV, but more typical error-bars are around 10-20 keV) are not shown in order to avoid confusion.
Open with DEXTER