All Figures

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{0617f1.eps}\end{figure}$ Figure 1: Velocity diagrams $v\times u$ and $v\times w$ for the active stars ( left panels) and inactive stars ( right panels). Compare the increase in the velocity dispersion of the inactive stars with that of the active stars. Note that, in spite of their low velocity dispersion, amongst active stars there are objects with velocity components typical of an old population (Rocha-Pinto et al. 2002).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0617f2.eps}\end{figure}$ Figure 2: Spatial velocities as a function of age. The disk heating can be clearly seen in this picture. Some stars, marked in the plot by solid circles and empty triangles, were discarded from the sample, before the final calculations of the age-velocity dispersion relation (see text).
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0617f3.eps}\end{figure}$ Figure 3: Characterization of the kinematical sample with a velocity ellipsoid. The panels a)- d) stand for the relations between the age and the velocity dispersions in the components u, v, w, and for the total space velocity ( $\sigma ^2_{\rm tot}=\sigma ^2_u+ \sigma ^2_v+\sigma ^2_w$ ), respectively. The velocity dispersions were calculated with respect to the principal axis of the velocity ellipsoid for each age group. Panels e) and f) show the evolution of the axial ratios $\sigma _v/\sigma _u$ and $\sigma _w/\sigma _u$ of the ellipsoid. Panel g) shows the asymmetrical drift as a function of age. In these plots the symbols indicate: error bars, our data, calculated by binning the stars in intervals of equal star number (N = 40 stars), without applying the |W| weights; semifilled triangles, Cayrel de Strobel (1974); letters W, Wielen (1974); letters K, Knude et al. (1987); letters S, Strömgren (1987); empty circles, Meusinger et al. (1991).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0617f4.eps} \end{figure}$ Figure 4: Increase of the u peculiar velocity with age, for uncorrected (panel a)) and corrected (panel b)) chromospheric ages. The effect of neglecting the [Fe/H] dependence of the chromospheric age calibration is seen in panel a), where the mixing of old hotter stars with intermediate-age stars boosts the velocity dispersion around 4-6 Gyr, yielding a steeper AVR, which otherwise would present a slower increase (panel b)).
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{0617f5.eps}\end{figure}$ Figure 5: Projection of the velocity ellipsoid of the stars younger than 1 Gyr onto the uv-plane. The tilted ellipsis with respect to the coordinate axes illustrates the vertex deviation of the data points.
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In the text

$\begin{figure} \par\includegraphics[width=5.3cm,clip]{0617f6.eps}\end{figure}$ Figure 6: Comparison between two proposed birthplace indicators. The solid line shows the prediction by Wielen et al. (1996).
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In the text

$\begin{figure} \par\includegraphics[width=17.7cm,clip]{0617f7.eps}\end{figure}$ Figure 7: Correlation between two proposed birthplace indicators. Panel a), R_m versus age for our sample; panel b), R_i versus age for our sample; panel c), R_m versus age for the sample of Edv93; panel d), R_i versus age for the sample of Edv93. The dashed line indicates the present galactocentric radius of the Sun.
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{0617f8.eps}\end{figure}$ Figure 8: Comparison of constraints for two samples, one internal to the solar radius, and the other external to it. Panel a), age-metallicity relation; panel b), metallicity distribution; panel c), age distribution.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0617f9.eps}\end{figure}$ Figure 9: Metallicity-R_m diagram. Upper panel: our data; lower panel, Edv93's data. The symbols indicate: filled squares, stars having ages lower than 1 Gyr; open circles, stars aging 1-3 Gyr; dotted triangles, stars having ages from 3 to 6 Gyr; upside down triangles, stars with ages greater than 6 Gyr.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0617f10.eps}\end{figure}$ Figure 10: Temporal evolution of the vertical velocity dispersion of the cloudy gas phase in the solar vicinity (at 8.5 kpc galactocentric distance) as the result of the chemodynamical Milky Way model by Samland et al. (1997), adapted from Samland (1995).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0617f2.eps}\end{figure}$	Figure 2: Spatial velocities as a function of age. The disk heating can be clearly seen in this picture. Some stars, marked in the plot by solid circles and empty triangles, were discarded from the sample, before the final calculations of the age-velocity dispersion relation (see text).
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$\begin{figure} \par\includegraphics[width=7.25cm,clip]{0617f5.eps}\end{figure}$	Figure 5: Projection of the velocity ellipsoid of the stars younger than 1 Gyr onto the uv-plane. The tilted ellipsis with respect to the coordinate axes illustrates the vertex deviation of the data points.
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$\begin{figure} \par\includegraphics[width=5.3cm,clip]{0617f6.eps}\end{figure}$	Figure 6: Comparison between two proposed birthplace indicators. The solid line shows the prediction by Wielen et al. (1996).
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$\begin{figure} \par\includegraphics[width=17.7cm,clip]{0617f7.eps}\end{figure}$	Figure 7: Correlation between two proposed birthplace indicators. Panel a), R_m versus age for our sample; panel b), R_i versus age for our sample; panel c), R_m versus age for the sample of Edv93; panel d), R_i versus age for the sample of Edv93. The dashed line indicates the present galactocentric radius of the Sun.
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$\begin{figure} \par\includegraphics[width=16.7cm,clip]{0617f8.eps}\end{figure}$	Figure 8: Comparison of constraints for two samples, one internal to the solar radius, and the other external to it. Panel a), age-metallicity relation; panel b), metallicity distribution; panel c), age distribution.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0617f9.eps}\end{figure}$	Figure 9: Metallicity-R_m diagram. Upper panel: our data; lower panel, Edv93's data. The symbols indicate: filled squares, stars having ages lower than 1 Gyr; open circles, stars aging 1-3 Gyr; dotted triangles, stars having ages from 3 to 6 Gyr; upside down triangles, stars with ages greater than 6 Gyr.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0617f10.eps}\end{figure}$	Figure 10: Temporal evolution of the vertical velocity dispersion of the cloudy gas phase in the solar vicinity (at 8.5 kpc galactocentric distance) as the result of the chemodynamical Milky Way model by Samland et al. (1997), adapted from Samland (1995).
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