All Figures

$\begin{figure} \par\includegraphics[width=8cm, height=6cm]{9499fig1.ps} \end{figure}$ Figure 1: The angular power spectrum of the correlation between LSS and CMB signals is shown for different cosmologies (see Table 1 for details). The $\Lambda$ CDM model is shown in black, model A2 in dark blue, model B in green, model C with a transition at $a_{\rm t}=0.5$ ( $a_{\rm t}=0.2$ ) in red solid (dotted) line.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{9499fig2.ps} \end{figure}$ Figure 2: Top: dark-energy equation of state, following parametrisation A1 (black), A2 (blue), B (green) and C (red) with the cosmological parameters given in Table 1. The dotted line corresponds to a parametrisation C with $a_{\rm t}=0.2$ ; bottom: corresponding $\dot{F}(z)$ (cf. Eq. (5)).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4cm]{9499fig3.ps} \includegraphics[width=4cm]{9499fig4.ps} } \end{figure}$ Figure 3: Total signal-to-noise for a ISW detection in the $\Lambda$ CDM model (parametrisation A1) as a function of the galaxy survey parameters $f^{\rm c}_{\rm sky}$ , $\bar{N}$ in units of arcmin^-2 and $z_{\rm med}$ . The different colours show different levels of detection in number of sigmas.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4cm]{9499fig5.ps} \includegraphics[width=4cm]{9499fig6.ps} } \end{figure}$ Figure 4: Total signal-to-noise for a ISW detection in the constant equation of state model with w=-0.9 (parametrisation A2) as function of the galaxy survey parameters $f^{\rm c}_{\rm sky}$ , $\bar{N}$ in units of arcmin^-2 and $z_{\rm med}$ .
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4cm]{9499fig7.ps} \includegraphics[width=4cm]{9499fig8.ps} } \end{figure}$ Figure 5: Total signal-to-noise for a ISW detection in the linearly varying equation of state model (parametrisation B) as function of the galaxy survey parameters $f^{\rm c}_{\rm sky}$ , $\bar{N}$ in units of arcmin^-2 and $z_{\rm med}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{9499fig9.ps} \end{figure}$ Figure 6: Two-dimensional marginalised confidence intervals on the plane $(\Omega _{\rm M},w)$ obtained with a Fisher matrix analysis centred on model A2 with w=-0.9. Left: ISW constraints; center: CMB (temperature) constraints; right: combined constraints (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{9499fg10.ps} \includegraphics[width=8cm]{9499fg11.ps} \end{figure}$ Figure 7: Two-dimensional marginalised confidence intervals obtained with a Fisher matrix analysis centered on model A2 with w=-0.9 for different combinations of parameters: $(\Omega _{\rm M},w)$ and $(\sigma _8,w)$ . Left: ISW constraints; right: ISW constraints obtained with a strong prior on $\sigma _8$ (see text for details). Note that the scales for $\Omega _{\rm M}$ are different from Fig. 6.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{9499fg12.ps} \end{figure}$ Figure 8: Two-dimensional marginalized confidence intervals obtained with a Fisher matrix analysis for $(w_0,w_{\rm a})$ centered on model B with w(a)=-0.9+0.1(1-a). Left: CMB (temperature) constraints; right: CMB+ISW combined constraints (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{9499fg13.ps} \end{figure}$ Figure 9: Two-dimensional marginalized confidence intervals obtained with a Fisher matrix analysis centered for $(\Omega _{\rm M},a_{\rm t})$ on model C with w(0)=-1, $w(\infty )=-0.2$ and $a_{\rm t}=0.5$ ; left: CMB (temperature) constraints; right: combined constraints (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8cm, height=6cm]{9499fig1.ps} \end{figure}$	Figure 1: The angular power spectrum of the correlation between LSS and CMB signals is shown for different cosmologies (see Table 1 for details). The $\Lambda$ CDM model is shown in black, model A2 in dark blue, model B in green, model C with a transition at $a_{\rm t}=0.5$ ( $a_{\rm t}=0.2$ ) in red solid (dotted) line.
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$\begin{figure} \par\includegraphics[width=8cm]{9499fig2.ps} \end{figure}$	Figure 2: Top: dark-energy equation of state, following parametrisation A1 (black), A2 (blue), B (green) and C (red) with the cosmological parameters given in Table 1. The dotted line corresponds to a parametrisation C with $a_{\rm t}=0.2$ ; bottom: corresponding $\dot{F}(z)$ (cf. Eq. (5)).
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$\begin{figure} \par\mbox{\includegraphics[width=4cm]{9499fig3.ps} \includegraphics[width=4cm]{9499fig4.ps} } \end{figure}$	Figure 3: Total signal-to-noise for a ISW detection in the $\Lambda$ CDM model (parametrisation A1) as a function of the galaxy survey parameters $f^{\rm c}_{\rm sky}$ , $\bar{N}$ in units of arcmin^-2 and $z_{\rm med}$ . The different colours show different levels of detection in number of sigmas.
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$\begin{figure} \par\mbox{\includegraphics[width=4cm]{9499fig5.ps} \includegraphics[width=4cm]{9499fig6.ps} } \end{figure}$	Figure 4: Total signal-to-noise for a ISW detection in the constant equation of state model with w=-0.9 (parametrisation A2) as function of the galaxy survey parameters $f^{\rm c}_{\rm sky}$ , $\bar{N}$ in units of arcmin^-2 and $z_{\rm med}$ .
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$\begin{figure} \par\mbox{\includegraphics[width=4cm]{9499fig7.ps} \includegraphics[width=4cm]{9499fig8.ps} } \end{figure}$	Figure 5: Total signal-to-noise for a ISW detection in the linearly varying equation of state model (parametrisation B) as function of the galaxy survey parameters $f^{\rm c}_{\rm sky}$ , $\bar{N}$ in units of arcmin^-2 and $z_{\rm med}$ .
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$\begin{figure} \par\includegraphics[width=8cm]{9499fig9.ps} \end{figure}$	Figure 6: Two-dimensional marginalised confidence intervals on the plane $(\Omega _{\rm M},w)$ obtained with a Fisher matrix analysis centred on model A2 with w=-0.9. Left: ISW constraints; center: CMB (temperature) constraints; right: combined constraints (see text for details).
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$\begin{figure} \par\includegraphics[width=8cm]{9499fg12.ps} \end{figure}$	Figure 8: Two-dimensional marginalized confidence intervals obtained with a Fisher matrix analysis for $(w_0,w_{\rm a})$ centered on model B with w(a)=-0.9+0.1(1-a). Left: CMB (temperature) constraints; right: CMB+ISW combined constraints (see text for details).
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$\begin{figure} \par\includegraphics[width=8cm]{9499fg13.ps} \end{figure}$	Figure 9: Two-dimensional marginalized confidence intervals obtained with a Fisher matrix analysis centered for $(\Omega _{\rm M},a_{\rm t})$ on model C with w(0)=-1, $w(\infty )=-0.2$ and $a_{\rm t}=0.5$ ; left: CMB (temperature) constraints; right: combined constraints (see text for details).
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