$\begin{figure} \par\includegraphics[height=3.8cm,width=7.7cm,clip]{0433fig1.ps}\end{figure}$ Figure 1: Trajectories for the extended PS process (Markovian process, jagged curves, T=0) and for the non-Markovian process (smooth curves, T=0.23).
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In the text

$\begin{figure} \par\includegraphics[height=5.55cm,width=5.65cm,clip]{0433fi2a.ps... ...0.5mm} \includegraphics[height=5.5cm,width=5.15cm,clip]{0433fi2c.ps}\end{figure}$ Figure 2: Filter profiles W_T(k) as a function of comoving wavenumber k in units of $[h~{\rm Mpc}^{-1}]$ for three values of the T parameter ( left: T=0.00, middle: T=0.23, right: T=0.50). Each panel shows two groups of filters. Left group: filter radius $R=8~h^{-1}~{\rm Mpc}$ , right group: $R=3~h^{-1}~{\rm Mpc}$ . Each group consists of three filter curves. From up to down: n=0 (continuous), -1 (dotted) ,-2 (dashed). The normalization of the power spectrum P₀ is adjusted to give $\sigma _8=0.9$ (at T=0).
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In the text

$\begin{figure} \par\includegraphics[height=5.3cm,width=5.9cm,clip]{0433fi3a.ps}\... ...{4mm} \includegraphics[height=5.25cm,width=4.85cm,clip]{0433fi3c.ps}\end{figure}$ Figure 3: Mass functions f(M) for Gaussian fluctuation fields with a power spectrum with n=0,-1,-2. Mass M in solar units: T=0, $\beta =0$ (dashed lines), and T=0.23, $\beta =0$ (continuous lines). The computations assume the normalized cosmic mass density $\Omega _m=0.27$ , the standard normalization $\sigma _8=0.9$ and the normalized Hubble constant h=0.7.
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In the text

$\begin{figure} \par\includegraphics[height=6cm,width=6.5cm,clip]{0433fig4.ps}\end{figure}$ Figure 4: Mass functions f(M) for Gaussian fluctuation fields with a power spectrum with n=-2.0. Mass M in solar units. T=0, $\beta =0$ (dashed line), and T=0.23, $\beta =0.12$ (continuous line). Further normalizations as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[height=6cm,width=6.65cm,clip]{0433fig5.ps}\end{figure}$ Figure 5: Best fit mass function f(M) with T=0.23, $\beta =0.12$ (continuous line) and the transformed mass function of Jenkins et al. (2001) with 20% Gaussian random errors (dots with error bars). Normalizations as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[height=4.8cm,width=5cm,clip]{0433fi6a.ps}\hs... ...ace*{2mm} \includegraphics[height=4.8cm,width=5cm,clip]{0433fi6c.ps}\end{figure}$ Figure 6: $\chi ^2$ distribution ( $1{-}3\sigma$ contours for three parameters) for the spectral index n=-2 obtained from the comparison of mass functions f(M) with different T and $\beta$ parameter values and the transformed Jenkins et al. (2001) mass function. Normalizations as in Fig. 3. The $\chi ^2$ test assumes errors of 30% ( left), 20% ( middle), 10% ( right) of the Jenkins et al. mass function.
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In the text

$\begin{figure} \par\includegraphics[height=5.65cm,width=5.7cm]{0433fig7.ps}\end{figure}$ Figure 7: $\chi ^2$ distribution ( $1{-}3\sigma$ contours for three parameters) in the $\beta =0.12$ plane, assuming 10% errors of the Jenkins et al. (2001) mass function.
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In the text

$\begin{figure} \par\includegraphics[height=3.8cm,width=7.7cm,clip]{0433fig1.ps}\end{figure}$	Figure 1: Trajectories for the extended PS process (Markovian process, jagged curves, T=0) and for the non-Markovian process (smooth curves, T=0.23).
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$\begin{figure} \par\includegraphics[height=5.3cm,width=5.9cm,clip]{0433fi3a.ps}\... ...{4mm} \includegraphics[height=5.25cm,width=4.85cm,clip]{0433fi3c.ps}\end{figure}$	Figure 3: Mass functions f(M) for Gaussian fluctuation fields with a power spectrum with n=0,-1,-2. Mass M in solar units: T=0, $\beta =0$ (dashed lines), and T=0.23, $\beta =0$ (continuous lines). The computations assume the normalized cosmic mass density $\Omega _m=0.27$ , the standard normalization $\sigma _8=0.9$ and the normalized Hubble constant h=0.7.
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$\begin{figure} \par\includegraphics[height=6cm,width=6.5cm,clip]{0433fig4.ps}\end{figure}$	Figure 4: Mass functions f(M) for Gaussian fluctuation fields with a power spectrum with n=-2.0. Mass M in solar units. T=0, $\beta =0$ (dashed line), and T=0.23, $\beta =0.12$ (continuous line). Further normalizations as in Fig. 3.
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$\begin{figure} \par\includegraphics[height=6cm,width=6.65cm,clip]{0433fig5.ps}\end{figure}$	Figure 5: Best fit mass function f(M) with T=0.23, $\beta =0.12$ (continuous line) and the transformed mass function of Jenkins et al. (2001) with 20% Gaussian random errors (dots with error bars). Normalizations as in Fig. 3.
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$\begin{figure} \par\includegraphics[height=5.65cm,width=5.7cm]{0433fig7.ps}\end{figure}$	Figure 7: $\chi ^2$ distribution ( $1{-}3\sigma$ contours for three parameters) in the $\beta =0.12$ plane, assuming 10% errors of the Jenkins et al. (2001) mass function.
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