All Figures

	Figure 1: Upper panel: vs. (MW: Mount Wilson) for the "standard'' stars in Table 1 corresponding to the September 2003 and March 2004 observing runs. Lower panel: Log R' values for both observing sites (i.e., CASLEO and Mount Wilson). The open circles indicate 2003 data and the crosses 2004 observations.
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In the text

	Figure 2: CE (measured by Log R') versus the semi-major axis a, for the EH sample. 51 Peg-like objects (i.e., those with a <0.1 AU) and the rest of the sample are represented by filled and empty circles, respectively.
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In the text

Figure 3: Comparison between the CE index, Log R', and the age for the H sample stars derived by Wright et al. (2004) and those reported in this contribution. To make these comparisons we have used stars in common and eliminated Wright et al. (2004)'s data from the averages reported in Table 2. The ages have been obtained from the D93 calibration. The large circles indicate stars with the largest discrepancies: (A) HD 19994, (B) HD 89744 and (C) HD 130322, see Table 5.

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In the text

	Figure 4: Transverse velocity dispersion S vs. dereddened B-V. Solar neighborhood stars and EH stars are represented by squares and filled circles, respectively. Error bars are derived as , where n is the number of objects per bin. The age scale on the right side was obtained from Binney et al. (2000).
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In the text

	Figure 5: Upper panels: chromospheric age distributions derived from the D93 and RPM98 calibrations. The lower panel correspond to the isochrone distribution. Vertical continuous lines show the medians of each histogram. In the isochrone age distribution we superpose with continuous and dotted lines upper and lower limits estimations from Nördstrom et al. (2004).
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In the text

	Figure 6: Chromospheric ages against isochrone and lithium ages, and [Fe/H] upper limits, respectively.
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In the text

Figure 7: Isochrone and chromospheric age distributions for the Solar Neighborhood stars. Isochrone ages for samples A and B were taken from Nördstrom et al. (2004). Chromospheric ages for sample C from Henry et al. (1996) and Strassmeier et al. (2000). Spectral types G and F in samples B and C are indicated by dashed and empty histograms, respectively. The vertical continuous lines show the median positions of each histogram. The thicker lines correspond to the F type and the lighter to the G type.

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In the text

	Figure 8: Chromospheric ages vs isochrone ages for F and G-type solar neighborhood stars. Filled and empty circles correspond to F and G spectral types, respectively. Isochrone ages are taken from Nördstrom et al. (2004) and chromospheric determinations from Henry et al. (1996) and Strassmeier et al. (2000).
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In the text

	Figure 9: Chromospheric and isochrone age distributions of EH stars. Spectral types G and F are indicated by dashed and empty histograms, respectively. The vertical continuous lines show the median positions of each histogram. The thicker lines correspond to the F type and the lighter to the G type.
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In the text

	Figure 10: Isochrone age distributions for EH stars (shade histograms) and sample B (empty histograms). The right panel corresponds to stars of spectral type F in both samples and the left panel to G-type objects. The vertical continuous lines show the median positions of each histogram. The thicker lines correspond to the F type and the lighter to the G type.
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In the text

	Figure 11: Upper panels: / vs. chromospheric and isochrone ages. Lower panel: [Fe/H] vs. chromospheric and isochrone ages.
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In the text