Astronomy & Astrophysics

All Figures

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=-90,clip]{vrsky.p... ... \resizebox{8.4cm}{!}{\includegraphics[angle=-90,clip]{novrsky.ps}} \end{figure}$ Figure 1: Distribution on the sky of the 16 682 programme stars. Top: the 14 139 stars with radial velocity data (note the overdensity of stars in the Hyades cluster and south of $\delta = -26\hbox {$^\circ $ }$ ). Bottom: the 2543 stars with no radial velocity.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{byhist.ps}} \end{figure}$ Figure 2: Distribution of the whole sample in b-y colour.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{vr1.ps}}\par\vspace*{2mm} \resizebox{8.5cm}{!}{\includegraphics[clip]{vr2.ps}} \end{figure}$ Figure 3: Distribution of the mean errors of the mean radial velocities in the catalogue ( top), and the time span covered for each star ( bottom).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{vsini.ps}} \end{figure}$ Figure 4: Distribution of rotational velocities in the sample.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{par1.ps}}... ...2mm} \resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{par2.ps}} \end{figure}$ Figure 5: Distribution of Hipparcos parallaxes ( top) and their relative errors ( bottom) for the whole sample.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{ebyhist.ps}} \end{figure}$ Figure 6: Distribution of reddening values in the sample.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{tehist.ps}} \end{figure}$ Figure 7: Distribution of the sample in $T_{\rm eff}$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{fehcomp.ps}} \end{figure}$ Figure 8: Comparison between our final photometric metallicities ([Me/H]) and the spectroscopic ([Fe/H]) values used to establish the calibrations. Open circles denote the cool (GK) stars, dots the hot (F) stars (see text).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{mehhist.ps}} \end{figure}$ Figure 9: Distribution of metallicities for the whole sample (full histogram). For comparison, the dotted curve shows a Gaussian distribution with mean of -0.14 and dispersion of 0.19 dex, covering the same area as the histogram.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{dcompf.ps}}\par\vspace*{2mm} \resizebox{8.5cm}{!}{\includegraphics[clip]{dcompg.ps}} \end{figure}$ Figure 10: Photometric vs. Hipparcos distances for the single main sequence stars with parallax errors below 3%. Top: F dwarfs; bottom: G dwarfs.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{mv.ps}}\p... ...{2mm} \resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{dmv.ps}} \end{figure}$ Figure 11: M_V ( top) and $\delta M_{V}$ ( bottom) vs. $\log T_{\rm eff}$ for our sample, which by design consists of F and G dwarf stars.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{isocomp.ps}} \end{figure}$ Figure 12: Comparison between the observed stars (known binaries excluded) and Padova isochrones for 0, 2, 4, 6, 8, 10, and 15 Gyr at $\rm [Fe/H] = 0.00\pm 0.02$ , $-0.50\pm 0.05$ , $-0.90\pm 0.20$ , and $-1.50\pm 0.25$ , after allowing for the $\alpha$ -enhancement and temperature corrections discussed in the text.
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In the text

$\begin{figure} \par\resizebox{5.7cm}{!}{\includegraphics[angle=0,clip]{gfunkOK.ps}} \end{figure}$ Figure 13: Top: three slices of the three-dimensional HR "cube'' showing the observed point (central panel) and three cuts through the 1- $\sigma$ error ellipsoid. The probability distribution function (G-function, bottom) is computed from all points on the isochrones, not just those on or inside the error ellipsoid.
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In the text

$\begin{figure} \par\vspace{-2mm} \resizebox{7.8cm}{!}{\includegraphics[angle=0,clip]{gfunkBAD.ps}} \end{figure}$ Figure 14: Right: examples of stars located in regions of the HR diagram where reliable ages cannot be determined, and ( left) the corresponding G-functions. The stars plotted as plus, asterisk, triangle, and diamond symbols in the HR diagram correspond to the solid, dotted, dashed, and dot-dashed curves, respectively. Isochrones are for 0, 2, 4, 6, 8, and 10 Gyr.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{relagedist.ps}} \end{figure}$ Figure 15: The distribution of upper (dotted line) and lower (solid line) 1- $\sigma$ relative errors for the ages in the catalogue.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{relagerror.ps}} \end{figure}$ Figure 16: Relative age error (mean of lower and upper bounds) vs. age for the 11 445 stars with "well-defined'' ages.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{agedistma... ...\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{agedistvol.ps}} \end{figure}$ Figure 17: Top: age distributions for single stars in the full sample. The curves show (top to bottom): (i) all ages (solid); (ii) "well-defined'' ages (dots); (iii) ages with errors <50% (short-dashed); and (iv) ages with errors <25% (long-dashed). Bottom: "Well-defined'' ages in thefull, magnitude-limited sample (solid) and in the volume-limited subsample for d < 40 pc (dots). Note that increasing the demand onaccuracy progressively removes most of the oldest stars.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{edv93age.ps}} \end{figure}$ Figure 18: Ages from Edvardsson et al. (1993) vs. our results for the 160 stars in common with "well-defined'' ages.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{massdist.ps}} \end{figure}$ Figure 19: The distribution of derived masses for single stars in the full (solid line) and volume-limited sample for d < 40 pc (dotted line).
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[angle=0,clip]{uv.eps}}\pa... ...eps}}\par\resizebox{8cm}{!}{\includegraphics[angle=0,clip]{vw.eps}} \end{figure}$ Figure 20: U-V, U-W, and V-W diagrams for all stars in the sample.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{orb.ps}} \end{figure}$ Figure 21: Key parameters of the Galactic orbits for the whole sample.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{magv.ps}} \end{figure}$ Figure 22: Distribution of observed V magnitudes for the full sample (full line), and for the stars with measured radial velocities (dotted line). The dashed curve shows the expected relation for a uniform, volume complete sample.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[angle=0,clip]{magvby.ps}} \end{figure}$ Figure 23: Distribution of V magnitudes by interval of b-y colour. Markings as in Fig. 22.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{distby.ps}} \end{figure}$ Figure 24: Distance distributions by interval in b-y colour (full line). The dashed curves show the expected relation for a uniform, volume complete sample. In the last panel, the lower histogram shows the distribution of stars south of $\delta = -26\hbox {$^\circ $ }$ .
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{agemass.ps}} \end{figure}$ Figure 25: Age vs. mass for stars with well-defined ages. The apparent correlation of age and mass is an artifact caused by the over-representation of evolved stars and the fact that reliable ages cannot be determined for unevolved stars.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{mehdist.ps}} \end{figure}$ Figure 26: Distribution of metallicities for the volume complete sample of single stars (full histogram). For comparison the dotted curve shows the reconstructed distribution for G dwarfs from Jørgensen (2000), which is corrected for scale height effects and measurement errors.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{amrall.ps}} \end{figure}$ Figure 27: Age-metallicity diagram for 7566 single stars with "well-defined'' ages in the magnitude-limited sample. Note that individual age errors may still exceed 50% (cf. Fig. 16).
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[angle=0,clip]{amrvol1.p... ...m} \resizebox{8.3cm}{!}{\includegraphics[angle=0,clip]{amrvol2.ps}} \end{figure}$ Figure 28: Age-metallicity diagrams for single stars in the volume-limited subsample within 40 pc; large dots show mean ages and metallicities in 10 bins with equal numbers of stars. Top: the 462 stars with "well-defined'' ages (no limit on actual errors). Bottom: the 142 stars with ages better than 25%; average error bars (14%) in three age bins are shown.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{radmet.ps}} \end{figure}$ Figure 29: Radial metallicity gradient for single stars in three age ranges. $R_{\rm m}$ is the mean radius of the stellar orbits.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{avr.ps}}\... ...mm} \resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{avrlim.ps}} \end{figure}$ Figure 30: U, V and W velocities as functions of age for all single stars with complete data. Top panels: all 7237 stars with "well-defined'' ages and all velocity data; bottom panels: the 2852 stars with ages better than 25%.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[angle=0,clip]{avrbin.ps}} \end{figure}$ Figure 31: Velocity dispersions for single stars with relative age errors <25% as functions of age (Fig. 30, bottom). From top to bottom, the total, U, V, and W velocity dispersion are plotted in 10 bins with equal numbers of stars. The lines show fitted power laws; see text for full details. The youngest and oldest age bins have been excluded from the fits to avoid biases due to unrelaxed young structures and thick disk stars, respectively.
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In the text

$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics[angle=0]{fehu.ps}}\par\re... ...fehv.ps}}\par\resizebox{7cm}{!}{\includegraphics[angle=0]{fehw.ps}} \end{figure}$ Figure 32: U, V, and W as functions of metallicity for all single stars in the sample.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=-90,clip]{vrsky.p... ... \resizebox{8.4cm}{!}{\includegraphics[angle=-90,clip]{novrsky.ps}} \end{figure}$	Figure 1: Distribution on the sky of the 16 682 programme stars. Top: the 14 139 stars with radial velocity data (note the overdensity of stars in the Hyades cluster and south of $\delta = -26\hbox {$^\circ $ }$ ). Bottom: the 2543 stars with no radial velocity.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{byhist.ps}} \end{figure}$	Figure 2: Distribution of the whole sample in b-y colour.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{vr1.ps}}\par\vspace*{2mm} \resizebox{8.5cm}{!}{\includegraphics[clip]{vr2.ps}} \end{figure}$	Figure 3: Distribution of the mean errors of the mean radial velocities in the catalogue ( top), and the time span covered for each star ( bottom).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{vsini.ps}} \end{figure}$	Figure 4: Distribution of rotational velocities in the sample.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{par1.ps}}... ...2mm} \resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{par2.ps}} \end{figure}$	Figure 5: Distribution of Hipparcos parallaxes ( top) and their relative errors ( bottom) for the whole sample.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{ebyhist.ps}} \end{figure}$	Figure 6: Distribution of reddening values in the sample.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{tehist.ps}} \end{figure}$	Figure 7: Distribution of the sample in $T_{\rm eff}$ .
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{fehcomp.ps}} \end{figure}$	Figure 8: Comparison between our final photometric metallicities ([Me/H]) and the spectroscopic ([Fe/H]) values used to establish the calibrations. Open circles denote the cool (GK) stars, dots the hot (F) stars (see text).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{mehhist.ps}} \end{figure}$	Figure 9: Distribution of metallicities for the whole sample (full histogram). For comparison, the dotted curve shows a Gaussian distribution with mean of -0.14 and dispersion of 0.19 dex, covering the same area as the histogram.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{dcompf.ps}}\par\vspace*{2mm} \resizebox{8.5cm}{!}{\includegraphics[clip]{dcompg.ps}} \end{figure}$	Figure 10: Photometric vs. Hipparcos distances for the single main sequence stars with parallax errors below 3%. Top: F dwarfs; bottom: G dwarfs.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{mv.ps}}\p... ...{2mm} \resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{dmv.ps}} \end{figure}$	Figure 11: M_V ( top) and $\delta M_{V}$ ( bottom) vs. $\log T_{\rm eff}$ for our sample, which by design consists of F and G dwarf stars.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[angle=0,clip]{isocomp.ps}} \end{figure}$	Figure 12: Comparison between the observed stars (known binaries excluded) and Padova isochrones for 0, 2, 4, 6, 8, 10, and 15 Gyr at $\rm [Fe/H] = 0.00\pm 0.02$ , $-0.50\pm 0.05$ , $-0.90\pm 0.20$ , and $-1.50\pm 0.25$ , after allowing for the $\alpha$ -enhancement and temperature corrections discussed in the text.
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$\begin{figure} \par\resizebox{5.7cm}{!}{\includegraphics[angle=0,clip]{gfunkOK.ps}} \end{figure}$	Figure 13: Top: three slices of the three-dimensional HR "cube'' showing the observed point (central panel) and three cuts through the 1- $\sigma$ error ellipsoid. The probability distribution function (G-function, bottom) is computed from all points on the isochrones, not just those on or inside the error ellipsoid.
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$\begin{figure} \par\vspace{-2mm} \resizebox{7.8cm}{!}{\includegraphics[angle=0,clip]{gfunkBAD.ps}} \end{figure}$	Figure 14: Right: examples of stars located in regions of the HR diagram where reliable ages cannot be determined, and ( left) the corresponding G-functions. The stars plotted as plus, asterisk, triangle, and diamond symbols in the HR diagram correspond to the solid, dotted, dashed, and dot-dashed curves, respectively. Isochrones are for 0, 2, 4, 6, 8, and 10 Gyr.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{relagedist.ps}} \end{figure}$	Figure 15: The distribution of upper (dotted line) and lower (solid line) 1- $\sigma$ relative errors for the ages in the catalogue.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{relagerror.ps}} \end{figure}$	Figure 16: Relative age error (mean of lower and upper bounds) vs. age for the 11 445 stars with "well-defined'' ages.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{edv93age.ps}} \end{figure}$	Figure 18: Ages from Edvardsson et al. (1993) vs. our results for the 160 stars in common with "well-defined'' ages.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{massdist.ps}} \end{figure}$	Figure 19: The distribution of derived masses for single stars in the full (solid line) and volume-limited sample for d < 40 pc (dotted line).
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$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[angle=0,clip]{uv.eps}}\pa... ...eps}}\par\resizebox{8cm}{!}{\includegraphics[angle=0,clip]{vw.eps}} \end{figure}$	Figure 20: U-V, U-W, and V-W diagrams for all stars in the sample.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{orb.ps}} \end{figure}$	Figure 21: Key parameters of the Galactic orbits for the whole sample.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{magv.ps}} \end{figure}$	Figure 22: Distribution of observed V magnitudes for the full sample (full line), and for the stars with measured radial velocities (dotted line). The dashed curve shows the expected relation for a uniform, volume complete sample.
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$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[angle=0,clip]{magvby.ps}} \end{figure}$	Figure 23: Distribution of V magnitudes by interval of b-y colour. Markings as in Fig. 22.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{distby.ps}} \end{figure}$	Figure 24: Distance distributions by interval in b-y colour (full line). The dashed curves show the expected relation for a uniform, volume complete sample. In the last panel, the lower histogram shows the distribution of stars south of $\delta = -26\hbox {$^\circ $ }$ .
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{agemass.ps}} \end{figure}$	Figure 25: Age vs. mass for stars with well-defined ages. The apparent correlation of age and mass is an artifact caused by the over-representation of evolved stars and the fact that reliable ages cannot be determined for unevolved stars.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{mehdist.ps}} \end{figure}$	Figure 26: Distribution of metallicities for the volume complete sample of single stars (full histogram). For comparison the dotted curve shows the reconstructed distribution for G dwarfs from Jørgensen (2000), which is corrected for scale height effects and measurement errors.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{amrall.ps}} \end{figure}$	Figure 27: Age-metallicity diagram for 7566 single stars with "well-defined'' ages in the magnitude-limited sample. Note that individual age errors may still exceed 50% (cf. Fig. 16).
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$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[angle=0,clip]{amrvol1.p... ...m} \resizebox{8.3cm}{!}{\includegraphics[angle=0,clip]{amrvol2.ps}} \end{figure}$	Figure 28: Age-metallicity diagrams for single stars in the volume-limited subsample within 40 pc; large dots show mean ages and metallicities in 10 bins with equal numbers of stars. Top: the 462 stars with "well-defined'' ages (no limit on actual errors). Bottom: the 142 stars with ages better than 25%; average error bars (14%) in three age bins are shown.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[angle=0,clip]{radmet.ps}} \end{figure}$	Figure 29: Radial metallicity gradient for single stars in three age ranges. $R_{\rm m}$ is the mean radius of the stellar orbits.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{avr.ps}}\... ...mm} \resizebox{8.5cm}{!}{\includegraphics[angle=0,clip]{avrlim.ps}} \end{figure}$	Figure 30: U, V and W velocities as functions of age for all single stars with complete data. Top panels: all 7237 stars with "well-defined'' ages and all velocity data; bottom panels: the 2852 stars with ages better than 25%.
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$\begin{figure} \par\resizebox{7cm}{!}{\includegraphics[angle=0]{fehu.ps}}\par\re... ...fehv.ps}}\par\resizebox{7cm}{!}{\includegraphics[angle=0]{fehw.ps}} \end{figure}$	Figure 32: U, V, and W as functions of metallicity for all single stars in the sample.
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