All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=11cm,clip]{1847f1.ps} \end{figure}$ Figure 1: Location of the six study areas in galactic coordinates. The dots show the positions of the RASS X-ray sources with stellar counterparts in the respective area. The solid and dashed curves denote the position and width, respectively, of the Gould Belt according to Guillout et al. (1998). In addition positions of several associations are shown.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1847f2.ps} \end{figure}$ Figure 2: Comparison of the spectral types derived from the classification spectra used in Paper III (Sp(old)) and from the new high resolution spectra (Sp(rev.)). The abscissa is the difference (in spectral classes) between the revised and the original spectral types.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1847f3.ps} \end{figure}$ Figure 3: Distribution of rotational velocities of the G and K stars.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.9cm,clip]{1847f4.ps} \end{figure}$ Figure 4: Comparison of the equivalent widths of Li I determined from the low- and the high-resolution spectra. The dashed line denotes a ratio of 1 of the two measurements.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1847f5.ps} \end{figure}$ Figure 5: Two-colour diagram for the infrared magnitudes from 2MASS. Circles denote M stars, crosses stars with spectral types F to K. The solid, dotted, and dashed lines denote the loci of main sequence stars, giants, and supergiants, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{1847f6.ps} \end{figure}$ Figure 6: Comparison of the distances $d({\rm LC})$ derived from spectroscopic or photometric parallaxes and from trigonometric parallaxes, $d({\rm trig})$ . The dashed line denotes equal distance values. M stars with distance estimates from the 2MASS IR photometry are plotted as circles.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{1847f7.ps} \end{figure}$ Figure 7: Histogram of the distance distribution. The solid lines represent the distribution of trigonometric, spectroscopic, and photometric parallaxes. The dashed lines include distance estimates derived from assuming absolute visual magnitude of main-sequence stars for the remaining stars without other distance estimate.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1847f8.ps} \end{figure}$ Figure 8: H-R-diagram for single stars with either a trigonometric parallax from Hipparcos or other sources (+ sign) or with a spectroscopic parallax (triangles).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1847f9.ps} \end{figure}$ Figure 9: X-ray luminosity for single stars vs. distance. + signs mark stars in study areas I, II, III, IV, and VI, $\times$ signs represent stars in area V. The solid and dotted lines mark the flux limits for the two groups of study areas.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.9cm,clip]{1847f10.ps} \end{figure}$ Figure 10: X-ray luminosity for single stars as a function of effective temperature, $T_{\rm eff}$ . Different symbols identify stars with trigonometric (+ sign), spectroscopic (triangles), or IR photometric parallaxes (circles). The variability range of solar X-ray emission in the ROSAT-PSPC pass band is marked by the vertical bar.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1847f11.ps} \end{figure}$ Figure 11: X-ray luminosity for all single stars with trigonometric (+ sign), spectroscopic (triangles), or IR photometric parallaxes (circles) as a function of absolute visual magnitude, M_V. The variability range of solar X-ray emission is marked by the vertical bar.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1847f12.ps} \end{figure}$ Figure 12: Ratio of X-ray and bolometric luminosity for all single stars with trigonometric (+ sign), spectroscopic (triangles), or IR photometric parallaxes (circles) as a function of bolometric magnitude, $M_{\rm bol}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1847f13.ps} \end{figure}$ Figure 13: X-ray surface flux density for all single stars with trigonometric (+ sign), spectroscopic (triangles), or IR photometric parallaxes (circles) as a function of absolute visual magnitude, M_V. The vertical bar marks the typical flux level of solar coronal holes in the ROSAT-PSPC pass band.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1847f14.ps} \end{figure}$ Figure 14: X-ray surface flux density for all single stars as a function of effective temperature, $T_{\rm eff}$ . The meaning of the symbols is the same as in Fig. 10. The vertical bar marks the typical flux level of solar coronal holes in the ROSAT-PSPC pass band.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{1847f15.ps} \end{figure}$ Figure 15: $\log L_{\rm X}/L_{\rm bol}$ as a function of $v~\sin i$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{1847f16.ps} \end{figure}$ Figure 16: Equivalent widths of Li I $\lambda 6708$ as a function of $T_{\rm eff}$ for all stars in the six study areas. Crosses and triangles are high and low resolution measurements, respectively. The solid lines represent the upper and lower envelope of the lithium equivalent widths in the Pleiades adopted from Soderblom et al. (1993b). The dashed line shows the upper envelope for the Hyades cluster taken from Thorburn et al. (1993).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{1847f17.ps} \end{figure}$ Figure 17: Lithium abundances versus effective temperature for the complete sample. Upper limits are plotted as downward arrows. Circles denote high-resolution measurements with the symbol size depending on $v~\sin i$ . Low and medium resolution data are plotted as triangles. The solid lines are the upper and lower limit of $\log N$ (Li I ) in the Pleiades; the long dashed and short dashed lines show the upper $\log N$ (Li I ) limits for the UMaG and the Hyades, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1847f18.ps} \end{figure}$ Figure 18: Spectra of the lithium-rich sample listed in Table 5. The wavelengths of Li I $\lambda 6708$ Å and Ca I $\lambda 6718$ Å are indicated by the dashed lines.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1847f19.ps} \end{figure}$ Figure 19: Low-resolution spectrum of the M4 star B026. The dashed lines indicate Li I $\lambda 6708$ Å and Ca I $\lambda 6718$ Å.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{1847f20.ps} \end{figure}$ Figure 20: Comparison of observed co-added number densities of G and K stars, $N(>\!S)$ , for three RASS count rates S with models of Guillout et al. (1996) for $\vert b\vert = 30\hbox {$^\circ $ }$ . Open symbols denote the sum of all age groups. Lower and upper filled symbols represent the sum of age groups "PMS'' and "Pl_ZAMS'', and of "PMS'', "Pl_ZAMS'', and UMa, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1847f21.eps} \end{figure}$ Figure 21: Proper motions for the six study areas. The different symbols denote the different age groups: filled circles = PMS, filled triangles = Pl_ZAMS, open circles = UMa, open triangles = Hya+, ${\ast }$ = giants, + = M stars without Li detection.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1847f22.eps} \end{figure}$ Figure 22: Space velocities U, V, and W in the LSR frame. Stars of age groups "PMS'' and "Pl_ZAMS'' are plotted as filled circles. Open circles denote stars of the UMa and "Hya+'' age group. Giants are plotted as asterisks.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1847f23.eps} \end{figure}$ Figure 23: Upper panel: U-V velocity diagram for the youngest age groups "PMS'' (circles) and "Pl_ZAMS'' (triangles). The solid line encircles the region defined by Eggen (1984, 1989) to contain the young disk population. Also shown as large crossed circles are the U and V velocities of the Hyades supercluster, the Local Association (designated "local''), the Castor MG, and the UMa MG. Lower panel: W-V diagram for the same sample of stars. All velocities are in the LSR reference frame.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{1847fA1.eps} \end{figure}$ Figure A.1: Equivalent widths of Li I $\lambda 6708$ as a function of $T_{\rm eff}$ plotted for each study area individually. The solid and dashed lines have the same meaning as in Fig. 16.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=11cm,clip]{1847f1.ps} \end{figure}$	Figure 1: Location of the six study areas in galactic coordinates. The dots show the positions of the RASS X-ray sources with stellar counterparts in the respective area. The solid and dashed curves denote the position and width, respectively, of the Gould Belt according to Guillout et al. (1998). In addition positions of several associations are shown.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1847f2.ps} \end{figure}$	Figure 2: Comparison of the spectral types derived from the classification spectra used in Paper III (Sp(old)) and from the new high resolution spectra (Sp(rev.)). The abscissa is the difference (in spectral classes) between the revised and the original spectral types.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1847f3.ps} \end{figure}$	Figure 3: Distribution of rotational velocities of the G and K stars.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.9cm,clip]{1847f4.ps} \end{figure}$	Figure 4: Comparison of the equivalent widths of Li I determined from the low- and the high-resolution spectra. The dashed line denotes a ratio of 1 of the two measurements.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1847f5.ps} \end{figure}$	Figure 5: Two-colour diagram for the infrared magnitudes from 2MASS. Circles denote M stars, crosses stars with spectral types F to K. The solid, dotted, and dashed lines denote the loci of main sequence stars, giants, and supergiants, respectively.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{1847f6.ps} \end{figure}$	Figure 6: Comparison of the distances $d({\rm LC})$ derived from spectroscopic or photometric parallaxes and from trigonometric parallaxes, $d({\rm trig})$ . The dashed line denotes equal distance values. M stars with distance estimates from the 2MASS IR photometry are plotted as circles.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{1847f7.ps} \end{figure}$	Figure 7: Histogram of the distance distribution. The solid lines represent the distribution of trigonometric, spectroscopic, and photometric parallaxes. The dashed lines include distance estimates derived from assuming absolute visual magnitude of main-sequence stars for the remaining stars without other distance estimate.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1847f8.ps} \end{figure}$	Figure 8: H-R-diagram for single stars with either a trigonometric parallax from Hipparcos or other sources (+ sign) or with a spectroscopic parallax (triangles).
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1847f9.ps} \end{figure}$	Figure 9: X-ray luminosity for single stars vs. distance. + signs mark stars in study areas I, II, III, IV, and VI, $\times$ signs represent stars in area V. The solid and dotted lines mark the flux limits for the two groups of study areas.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.9cm,clip]{1847f10.ps} \end{figure}$	Figure 10: X-ray luminosity for single stars as a function of effective temperature, $T_{\rm eff}$ . Different symbols identify stars with trigonometric (+ sign), spectroscopic (triangles), or IR photometric parallaxes (circles). The variability range of solar X-ray emission in the ROSAT-PSPC pass band is marked by the vertical bar.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1847f11.ps} \end{figure}$	Figure 11: X-ray luminosity for all single stars with trigonometric (+ sign), spectroscopic (triangles), or IR photometric parallaxes (circles) as a function of absolute visual magnitude, M_V. The variability range of solar X-ray emission is marked by the vertical bar.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1847f12.ps} \end{figure}$	Figure 12: Ratio of X-ray and bolometric luminosity for all single stars with trigonometric (+ sign), spectroscopic (triangles), or IR photometric parallaxes (circles) as a function of bolometric magnitude, $M_{\rm bol}$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1847f13.ps} \end{figure}$	Figure 13: X-ray surface flux density for all single stars with trigonometric (+ sign), spectroscopic (triangles), or IR photometric parallaxes (circles) as a function of absolute visual magnitude, M_V. The vertical bar marks the typical flux level of solar coronal holes in the ROSAT-PSPC pass band.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1847f14.ps} \end{figure}$	Figure 14: X-ray surface flux density for all single stars as a function of effective temperature, $T_{\rm eff}$ . The meaning of the symbols is the same as in Fig. 10. The vertical bar marks the typical flux level of solar coronal holes in the ROSAT-PSPC pass band.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{1847f15.ps} \end{figure}$	Figure 15: $\log L_{\rm X}/L_{\rm bol}$ as a function of $v~\sin i$ .
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1847f18.ps} \end{figure}$	Figure 18: Spectra of the lithium-rich sample listed in Table 5. The wavelengths of Li I $\lambda 6708$ Å and Ca I $\lambda 6718$ Å are indicated by the dashed lines.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1847f19.ps} \end{figure}$	Figure 19: Low-resolution spectrum of the M4 star B026. The dashed lines indicate Li I $\lambda 6708$ Å and Ca I $\lambda 6718$ Å.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{1847f20.ps} \end{figure}$	Figure 20: Comparison of observed co-added number densities of G and K stars, $N(>\!S)$ , for three RASS count rates S with models of Guillout et al. (1996) for $\vert b\vert = 30\hbox {$^\circ $ }$ . Open symbols denote the sum of all age groups. Lower and upper filled symbols represent the sum of age groups "PMS'' and "Pl_ZAMS'', and of "PMS'', "Pl_ZAMS'', and UMa, respectively.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1847f21.eps} \end{figure}$	Figure 21: Proper motions for the six study areas. The different symbols denote the different age groups: filled circles = PMS, filled triangles = Pl_ZAMS, open circles = UMa, open triangles = Hya+, ${\ast }$ = giants, + = M stars without Li detection.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1847f22.eps} \end{figure}$	Figure 22: Space velocities U, V, and W in the LSR frame. Stars of age groups "PMS'' and "Pl_ZAMS'' are plotted as filled circles. Open circles denote stars of the UMa and "Hya+'' age group. Giants are plotted as asterisks.
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