All Figures

	Figure 1: Comparison of equivalent widths obtained using Gaussian and Voigt profiles for the star Eridani (HD 23249). Voigt-profile fitting gives larger values because of the inclusion of the damping wings in the measurements for   mÅ.
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In the text

	Figure 2: Comparison between a portion (around Ca I 6162 Å) of the  Eridani (HD 23249) spectrum (filled dots) and the synthetic profile (solid line).
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In the text

	Figure 3: Abundance patterns for the program stars, determined from Method 1 (filled circles) and Method 2 (open circles).
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In the text

Figure 4: Comparison between the abundance ratio of the -synthesized elements as a function of [Fe/H] obtained from Method 1 (filled circles) for the stars in our sample and those obtained by Morel et al. (2003, 2004) with a similar approach, for a different sample of stars: active binaries (open circles) and inactive (presumably single) control stars (crosses) of similar spectral types (late G- to early-K subgiants).

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In the text

	Figure 5: [Fe/H] as a function of peculiar space velocities for Method 1 for the stars in our sample.
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In the text

Figure 6: Diagrams used to estimate ages for our program stars (Method 1). The theoretical isochrones are taken from Yi et al. (2003). The metallicities of the isochrones refer to a solar iron abundance: (Fe) = 7.50 (Yi et al. 2001, 2003; Kim et al. 2002). The isochrones are shown for [/Fe] = 0.0 and [Fe/H] = 0.05 (left-hand panel), [/Fe] = 0.0 and [Fe/H] = +0.38 (middle panel), and [/Fe] = 0.0 and [Fe/H] = -0.27 (right-hand panel). The ages of the isochrones (in Gyr) are indicated in every panel.

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In the text

	Figure 7: Comparison of the gravities derived by Method 1 with the values given by the theoretical isochrones. The error bars for the theoretical gravities were derived from the uncertainties in the position of the stars in the HR diagrams.
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In the text