All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2438fg01.eps} \end{figure}$ Figure 1: Structure of the adopted GDCE model (not to scale). A_iis the abundance of element i. The indices 1 and 2 represent the prompt and delayed contributions, respectively. The indices s, c, $c^{\prime }$ , and r are relative to the simple model (s), Clayton model with delayed production contribution from stars born during the simple model phase (c) and after the start of infall ( $c^{\prime }$ ), and ISM dilution due to effect of refuse (r).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2438fg02.eps} \end{figure}$ Figure 2: Metallicity distribution of G dwarfs in the solar neighbourhood, where $\Delta {N}/{N}$ is the normalised number of stars. The thick curve is the observational distribution of Rocha-Pinto & Maciel (1996). The thin curves were calculated using our GDCE model for the four different Galactic disk ages shown in the legend.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2438fg03.eps} \end{figure}$ Figure 3: ${T}{_{\rm G}}$ vs. $\chi$ diagram for our GDCE model. The dotted curve is a linear fit. The solid lines display the value adopted from the literature for the $\chi$ parameter ( 1.371^+0.444_-0.305) and its respective disk age ( $8.7^{+5.3}_{-3.6}~{\rm Gyr}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2438fg04.eps} \end{figure}$ Figure 4: [Th/Eu] vs. [Fe/H] diagram for all sample stars. Curves were calculated using our GDCE model for the four different Galactic disk ages shown in the legend.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2438fg05.eps} \end{figure}$ Figure 5: Determination of Galactic disk age that best fits our stellar [Th/Eu] abundance ratio data. Points are the total deviations between each curve and the stellar data presented in Fig. 4, calculated according to Eq. (8). The curve is a 2nd order polynomial fit. The vertical line marks the polynomial minimum, corresponding to best Galactic disk age $T_{{\rm G}}=8.2~{\rm Gyr}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2438fg06.eps} \end{figure}$ Figure 6: Galactic disk age distribution obtained through a Monte Carlo simulation of the [Th/Eu] and [Fe/H] abundance ratio uncertainties. Simulation results have been counted in 0.5 Gyr bins, and N is the total count per bin. The vertical line marks the age at which the distribution was cut (125 Gyr), corresponding to a count fall below 100 (i.e., 10% uncertainty).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2438fg07.eps} \end{figure}$ Figure 7: Integrands of Eqs. (9) and (10), used to calculate the variance and the mean absolute deviation (MAbD) of the age distribution,respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2438fg02.eps} \end{figure}$	Figure 2: Metallicity distribution of G dwarfs in the solar neighbourhood, where $\Delta {N}/{N}$ is the normalised number of stars. The thick curve is the observational distribution of Rocha-Pinto & Maciel (1996). The thin curves were calculated using our GDCE model for the four different Galactic disk ages shown in the legend.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2438fg03.eps} \end{figure}$	Figure 3: ${T}{_{\rm G}}$ vs. $\chi$ diagram for our GDCE model. The dotted curve is a linear fit. The solid lines display the value adopted from the literature for the $\chi$ parameter ( 1.371^+0.444_-0.305) and its respective disk age ( $8.7^{+5.3}_{-3.6}~{\rm Gyr}$ ).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2438fg04.eps} \end{figure}$	Figure 4: [Th/Eu] vs. [Fe/H] diagram for all sample stars. Curves were calculated using our GDCE model for the four different Galactic disk ages shown in the legend.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2438fg05.eps} \end{figure}$	Figure 5: Determination of Galactic disk age that best fits our stellar [Th/Eu] abundance ratio data. Points are the total deviations between each curve and the stellar data presented in Fig. 4, calculated according to Eq. (8). The curve is a 2nd order polynomial fit. The vertical line marks the polynomial minimum, corresponding to best Galactic disk age $T_{{\rm G}}=8.2~{\rm Gyr}$ .
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2438fg06.eps} \end{figure}$	Figure 6: Galactic disk age distribution obtained through a Monte Carlo simulation of the [Th/Eu] and [Fe/H] abundance ratio uncertainties. Simulation results have been counted in 0.5 Gyr bins, and N is the total count per bin. The vertical line marks the age at which the distribution was cut (125 Gyr), corresponding to a count fall below 100 (i.e., 10% uncertainty).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2438fg07.eps} \end{figure}$	Figure 7: Integrands of Eqs. (9) and (10), used to calculate the variance and the mean absolute deviation (MAbD) of the age distribution,respectively.
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