All Figures

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3706f1.ps} \end{figure}$ Figure 1: Evolution of the dark energy density ( top panel) and equation of state ( bottom panel) with redshift for the models considered in this paper: w = -1 (solid line), w = -1.2 (long dashed line), w = -0.8 (triple dot-dashed line), 2EXP₁ $(\alpha ,\beta )=(6.2,0.1)$ (dashed line), and 2EXP₂ $(\alpha ,\beta )=(20.1,0.5)$ (dot-dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3706f2.ps} \end{figure}$ Figure 2: Redshift evolution of the modified Press-Schechter mass function at $M=10^{14} ~h^{-1}~M_\odot$ for homogeneous ( top panel) and inhomogeneous ( bottom panel) dark energy models. In the main panels models were normalized to reproduce the present-day abundance of dark mater halos of the $\Lambda$ -model with $\sigma _8=0.9$ . In the embedded panels models were normalized to the same $\sigma _8=0.9$ . Lines are the same as for Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3706f3.ps} \end{figure}$ Figure 3: Evolution of the volume element with redshift in both homogeneous ( top panel) and inhomogeneous ( bottom panel) dark energy scenarios. Lines are the same as for Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3706f4.ps} \end{figure}$ Figure 4: Evolution of number counts ( top panels) with redshift and differences from the w=-1 (cosmological constant $\Lambda$ ) model ( bottom panels) for objects with mass within the range $10^{13}<M/(h^{-1}M_\odot )<10^{14}$ . Panels on the left show results for homogeneous dark energy whereas panels on the right show the same models in the inhomogeneous dark energy scenario. Lines are the same as for Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3706f5.ps} \end{figure}$ Figure 5: Same as Fig. 4 for objects with mass within the range $10^{14}<M/(h^{-1}M_\odot )<10^{15}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3706f6.ps} \end{figure}$ Figure 6: Same as Fig. 4 for objects with mass within the range $10^{15}<M/(h^{-1}M_\odot )<10^{16}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3706f7.ps} \end{figure}$ Figure 7: Difference of $\xi =\delta _{\rm c}/g \sigma _8$ between inhomogeneous ( $\xi ^{\rm inhom}$ ) and homogeneous ( $\xi ^{\rm hom}$ ) dark energy models.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3706f8.ps} \end{figure}$ Figure 8: Integrated number counts up to redshift z( top panels) and count differences to the w=-1 ( $\Lambda$ ) model ( bottom panels) for objects with mass $M>10^{13}~ h^{-1}~M_\odot$ . Panels on the left show results for homogeneous dark energy whereas panels on the right show the same models in the inhomogeneous dark energy case. Lines are the same as for Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3706f9.ps} \end{figure}$ Figure 9: Same as Fig. 8 for objects with mass $M>10^{14}~ h^{-1}~M_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3706f10.ps} \end{figure}$ Figure 10: Redshift dependence of number counts ( top panels) and count differences relative to the $\Lambda$ -model ( bottom panels) for objects with mass within the $10^{14}<M/(h^{-1}M_\odot )<10^{15}$ , assuming dark energy is inhomogeneous. Panels on the left show results assuming models are normalized to the same halo abundance at z=0, whereas panel on the right assume that models have all $\sigma _8=0.9$ (which implies different halo abundances at z=0, see text). Lines are the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3706f11.ps} \end{figure}$ Figure 11: Integrated number counts up to redshift z ( top panels) and integrated count differences relative to the $\Lambda$ -model ( bottom panels) for objects with mass above $10^{14}~h^{-1}~M_\odot$ , assuming dark energy is inhomogeneous. Panels on the left show results assuming models are normalized to the same halo abundance at z=0, whereas panels on the right assume that models have all $\sigma _8=0.9$ . Lines are the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3706f1.ps} \end{figure}$	Figure 1: Evolution of the dark energy density ( top panel) and equation of state ( bottom panel) with redshift for the models considered in this paper: w = -1 (solid line), w = -1.2 (long dashed line), w = -0.8 (triple dot-dashed line), 2EXP₁ $(\alpha ,\beta )=(6.2,0.1)$ (dashed line), and 2EXP₂ $(\alpha ,\beta )=(20.1,0.5)$ (dot-dashed line).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3706f3.ps} \end{figure}$	Figure 3: Evolution of the volume element with redshift in both homogeneous ( top panel) and inhomogeneous ( bottom panel) dark energy scenarios. Lines are the same as for Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3706f5.ps} \end{figure}$	Figure 5: Same as Fig. 4 for objects with mass within the range $10^{14}<M/(h^{-1}M_\odot )<10^{15}$ .
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3706f6.ps} \end{figure}$	Figure 6: Same as Fig. 4 for objects with mass within the range $10^{15}<M/(h^{-1}M_\odot )<10^{16}$ .
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3706f7.ps} \end{figure}$	Figure 7: Difference of $\xi =\delta _{\rm c}/g \sigma _8$ between inhomogeneous ( $\xi ^{\rm inhom}$ ) and homogeneous ( $\xi ^{\rm hom}$ ) dark energy models.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3706f8.ps} \end{figure}$	Figure 8: Integrated number counts up to redshift z( top panels) and count differences to the w=-1 ( $\Lambda$ ) model ( bottom panels) for objects with mass $M>10^{13}~ h^{-1}~M_\odot$ . Panels on the left show results for homogeneous dark energy whereas panels on the right show the same models in the inhomogeneous dark energy case. Lines are the same as for Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3706f9.ps} \end{figure}$	Figure 9: Same as Fig. 8 for objects with mass $M>10^{14}~ h^{-1}~M_\odot$ .
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