All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{9671f1.ps}\end{figure}$ Figure 1: Main-sequence eclipsing binaries with both components in the 1.1-1.5 $M_{\odot }$ range having masses and radii accurate to 2% or better. The nine systems shown are, in order of increasing mass of the primary component: EW Ori, UX Men, HS Hya, V505 Per, IT Cas, V1143 Cyg, CD Tau, DM Vir, and BW Aqr. WZ Oph, VZ Hya, and AD Boo, are shown with star symbols. The full drawn line is the Y² 0.3 Gyr isochrone for Z=0.0181(Demarque et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{9671f2.ps}\end{figure}$ Figure 2: FEROS spectra (black line) of AD Boo (phase 0.17), VZ Hya (phase 0.28), and WZ Oph (phase 0.33) in the region of the Fe I lines at 6056.0 and 6065.5 Å, shifted to laboratory wavelengths for the primary components. Synthetic spectra have been included: primary components (dashed blue); secondary components (dashed green); combined (continuous red line).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{9671f3.ps}\end{figure}$ Figure 3: Systematic errors in the raw TODCOR velocities of AD Boo determined from simulations with synthetic binary spectra (filled circles: primary; open circles: secondary). The differences are plotted both as function of orbital phase ( upper panel) and radial velocity ( lower panel), and have been applied to the measured velocities as corrections. Phase 0.0 corresponds to central primary eclipse.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f4.ps}\end{figure}$ Figure 4: Spectroscopic orbital solution for AD Boo (solid line: primary; dashed line: secondary) and radial velocities (filled circles: primary; open circles: secondary). The dotted line ( upper panel) represents the center-of-mass velocity of the system. Phase 0.0 corresponds to central primary eclipse.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f5.ps}\end{figure}$ Figure 5: (O-C) residuals of the AD Boo v-band observations from the theoretical light curve computed for the photometric elements given in Table 6. 1989 observations are shown with square symbols.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9671f6.ps}\end{figure}$ Figure 6: Best fitting parameter values for the 10 000 synthetic AD Boo y-band light curves created for the Monte Carlo analysis.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9671f7.ps}\end{figure}$ Figure 7: EBOP solutions for AD Boo for a range of fixed k values. Linear limb-darkening coefficients by van Hamme (1993) were adopted. The upper left panel shows normalized rms errors of the fit to the observations. Symbols are: cross y; diamond b; triangle v; square u.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f8.ps}\end{figure}$ Figure 8: Systematic errors in the raw TODCOR velocities of VZ Hya, determined from simulations with synthetic binary spectra (filled circles: primary; open circles: secondary). The differences are plotted both as function of orbital phase ( upper panel) and radial velocity ( lower panel), and have been applied to the measured velocities as corrections. Phase 0.0 corresponds to central primary eclipse.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f9.ps}\end{figure}$ Figure 9: Spectroscopic orbital solution for VZ Hya (solid line: primary; dashed line: secondary) and radial velocities (filled circles: primary; open circles: secondary). The dotted line ( upper panel) represents the center-of-mass velocity of the system. Phase 0.0 corresponds to central primary eclipse.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9671f10.ps}\end{figure}$ Figure 10: (O-C) residuals of the VZ Hya b-band observations from the theoretical light curve computed for the photometric elements given in Table 12.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9671f11.ps}\end{figure}$ Figure 11: Best fitting parameter values for the 10 000 synthetic VZ Hya y light curves created for the Monte Carlo analysis.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9671f12.ps}\end{figure}$ Figure 12: EBOP solutions for VZ Hya for a range of fixed k values. Linear limb-darkening coefficients by van Hamme (1993) were adopted. The upper left panel shows normalized rms errors of the fit to the observations. Symbols are: cross y; diamond b; triangle v; square u.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f13.ps}\end{figure}$ Figure 13: Systematic errors in the raw TODCOR velocities of WZ Oph, determined from simulations with synthetic binary spectra (filled circles: primary; open circles: secondary). The differences are plotted both as function of orbital phase ( upper panel) and radial velocity ( lower panel), and have been applied to the measured velocities as corrections. Phase 0.0 corresponds to central primary eclipse.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f14.ps}\end{figure}$ Figure 14: Spectroscopic orbital solution for WZ Oph (solid line: primary; dashed line: secondary) and radial velocities (filled circles: primary; open circles: secondary). The dotted line ( upper panel) represents the center-of-mass velocity of the system. Phase 0.0 corresponds to central primary eclipse.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9671f15.ps}\end{figure}$ Figure 15: (O-C) residuals of the WZ Oph y-band observations from the theoretical light curve computed for the photometric elements given in Table 17.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9671f16.ps}\end{figure}$ Figure 16: Best fitting parameter values for the 10 000 synthetic WZ Oph y light curves created for the Monte Carlo analysis.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9671f17.ps}\end{figure}$ Figure 17: EBOP solutions for WZ Oph for a range of fixed k values. Linear limb-darkening coefficients by van Hamme (1993) were adopted. The upper left panel shows normalized rms errors of the fit to the observations. Symbols are: cross y; diamond b; triangle v; square u.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f18.ps}\end{figure}$ Figure 18: Comparison between Y² (red) and Victoria-Regina VRSS (blue) models for $[{\rm Fe/H}]$ =-0.190 and $[{\rm\alpha /Fe}]$ = 0.0. Y²: (X, Y, Z) = (0.73400, 0.25400, 0.01200). VRSS: (X, Y, Z) = (0.72456, 0.26294, 0.01250). Tracks (solid lines) for 1.1, 1.2, 1,3. 1.4, and 1.5 $M_{\odot }$ and isochrones (dashed) between 0.5 and 2.5 Gyr (step 0.5 Gyr) are shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f19.ps}\end{figure}$ Figure 19: Comparison between Y² (red) and BaSTI core overshoot (blue) models for $[{\rm Fe/H}]$ =-0.253 and $[{\rm\alpha /Fe}]$ =0.0. Y²: (X, Y, Z) = (0.73865, 0.25090, 0.01045). BaSTI: (X, Y, Z) = (0.7310, 0.2590, 0.0100). Tracks (solid lines) for 1.1, 1.2, 1.3, 1.4, and 1.5 $M_{\odot }$ and isochrones (dashed) between 0.5 and 2.5 Gyr (step 0.5 Gyr) are shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f20.ps}\end{figure}$ Figure 20: AD Boo compared with Y² models for (X,Y,Z) = (0.7028,0.2748,0.0224), equivalent to the measured abundance $[{\rm Fe/H}]$ $=+0.10\pm 0.15$ for $[{\rm\alpha /Fe}]$ =0.0. Tracks for the component masses (solid lines) and isochrones from 0.5 to 3.0 Gyr (dashed; step 0.5 Gyr) are shown. The uncertainty in the location of the tracks coming from the mass errors are indicated (dotted lines). To illustrate the effect of the abundance uncertainty, tracks for $[{\rm Fe/H}]$ =+0.25 and $[{\rm\alpha /Fe}]$ =0.0 (dash-dot), corresponding to (X, Y, Z) = (0.6785, 0.2910, 0.0305), are included.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f21.ps}\end{figure}$ Figure 21: AD Boo compared with Y² models for (X,Y,Z) = (0.7028,0.2748,0.0224), equivalent to $[{\rm Fe/H}]$ =+0.10 for $[{\rm\alpha /Fe}]$ =0.0. Isochrones from 0.5 to 3.0 Gyr (step 0.5 Gyr) are shown. The 1.5 Gyr isochrone for $[{\rm Fe/H}]$ =+0.25 and $[{\rm\alpha /Fe}]$ =0.0 (dashed), corresponding to (X, Y, Z) = (0.6785, 0.2910, 0.0305), is included for comparison.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f22.ps}\end{figure}$ Figure 22: AD Boo compared with Y² models for (X, Y, Z) = (0.7028, 0.2748, 0.0224), equivalent to $[{\rm Fe/H}]$ =+0.10 for $[{\rm\alpha /Fe}]$ =0.0. Isochrones from 0.5 to 3.0 Gyr (step 0.5 Gyr) are shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f23.ps}\end{figure}$ Figure 23: VZ Hya compared with Y² models for (X, Y, Z) = (0.73478, 0.25348, 0.01174) equivalent to the measured abundance $[{\rm Fe/H}]$ $=-0.20\pm 0.12$ for $[{\rm\alpha /Fe}]$ =0.0. Tracks for the component masses (solid lines) and isochrones from 0.5 to 2.5 Gyr (dashed; step 0.5 Gyr) are shown. The uncertainty in the location of the tracks coming from the mass errors are indicated (dotted lines). To illustrate the effect of the abundance uncertainty, tracks for $[{\rm Fe/H}]$ =-0.08 and $[{\rm\alpha /Fe}]$ =0.0 (dash-dot), corresponding to (X, Y, Z) = (0.72425,0.26050,0.01525), are included.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f24.ps}\end{figure}$ Figure 24: VZ Hya compared with Y² models for (X, Y, Z) = (0.73478, 0.25348, 0.01174) equivalent to $[{\rm Fe/H}]$ =-0.20. Isochrones from 0.5 to 2.5 Gyr (step 0.5 Gyr) are shown. The 1.5 Gyr isochrone for $[{\rm Fe/H}]$ =-0.08 and $[{\rm\alpha /Fe}]$ =0.0 (dashed), corresponding to (X, Y, Z) = (0.72425,0.26050,0.01525), is included for comparison.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f25.ps}\end{figure}$ Figure 25: VZ Hya compared with Y² models for (X, Y, Z) = (0.73478, 0.25348, 0.01174) equivalent to $[{\rm Fe/H}]$ =-0.20. Isochrones from 0.5 to 2.5 Gyr (step 0.5 Gyr) are shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f26.ps}\end{figure}$ Figure 26: WZ Oph compared with Y² models for (X, Y, Z) = (0.73985, 0.25010, 0.01005), equivalent to the measured abundance $[{\rm Fe/H}]$ $-0.27\pm 0.07$ for $[{\rm\alpha /Fe}]$ =0.0. Tracks for the component masses (solid lines) and isochrones from 0.5 to 3.0 Gyr (dashed; step 0.5 Gyr) are shown. The uncertainty in the location of the primary track coming from the mass error is indicated (dotted line). For comparison, tracks for (X, Y, Z) = (0.7349, 0.2534, 0.0117) and $[{\rm\alpha /Fe}]$ =+0.1, also equivalent to $[{\rm Fe/H}]$ =-0.27, are included (dash-dot).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f27.ps}\end{figure}$ Figure 27: Assuming E(b-y) = 0.066: WZ Oph compared with Y² models for (X, Y, Z) = (0.72899, 0.25734, 0.013670), equivalent to $[{\rm Fe/H}]$ =-0.13 for $[{\rm\alpha /Fe}]$ =0.0. Tracks for the component masses (full drawn) and isochrones from 0.5 to 3.5 Gyr (dashed; step 0.5 Gyr) are shown. See text for details.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{9671f2.ps}\end{figure}$	Figure 2: FEROS spectra (black line) of AD Boo (phase 0.17), VZ Hya (phase 0.28), and WZ Oph (phase 0.33) in the region of the Fe I lines at 6056.0 and 6065.5 Å, shifted to laboratory wavelengths for the primary components. Synthetic spectra have been included: primary components (dashed blue); secondary components (dashed green); combined (continuous red line).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f4.ps}\end{figure}$	Figure 4: Spectroscopic orbital solution for AD Boo (solid line: primary; dashed line: secondary) and radial velocities (filled circles: primary; open circles: secondary). The dotted line ( upper panel) represents the center-of-mass velocity of the system. Phase 0.0 corresponds to central primary eclipse.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f5.ps}\end{figure}$	Figure 5: (O-C) residuals of the AD Boo v-band observations from the theoretical light curve computed for the photometric elements given in Table 6. 1989 observations are shown with square symbols.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9671f6.ps}\end{figure}$	Figure 6: Best fitting parameter values for the 10 000 synthetic AD Boo y-band light curves created for the Monte Carlo analysis.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9671f7.ps}\end{figure}$	Figure 7: EBOP solutions for AD Boo for a range of fixed k values. Linear limb-darkening coefficients by van Hamme (1993) were adopted. The upper left panel shows normalized rms errors of the fit to the observations. Symbols are: cross y; diamond b; triangle v; square u.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f9.ps}\end{figure}$	Figure 9: Spectroscopic orbital solution for VZ Hya (solid line: primary; dashed line: secondary) and radial velocities (filled circles: primary; open circles: secondary). The dotted line ( upper panel) represents the center-of-mass velocity of the system. Phase 0.0 corresponds to central primary eclipse.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9671f10.ps}\end{figure}$	Figure 10: (O-C) residuals of the VZ Hya b-band observations from the theoretical light curve computed for the photometric elements given in Table 12.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9671f11.ps}\end{figure}$	Figure 11: Best fitting parameter values for the 10 000 synthetic VZ Hya y light curves created for the Monte Carlo analysis.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{9671f12.ps}\end{figure}$	Figure 12: EBOP solutions for VZ Hya for a range of fixed k values. Linear limb-darkening coefficients by van Hamme (1993) were adopted. The upper left panel shows normalized rms errors of the fit to the observations. Symbols are: cross y; diamond b; triangle v; square u.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f14.ps}\end{figure}$	Figure 14: Spectroscopic orbital solution for WZ Oph (solid line: primary; dashed line: secondary) and radial velocities (filled circles: primary; open circles: secondary). The dotted line ( upper panel) represents the center-of-mass velocity of the system. Phase 0.0 corresponds to central primary eclipse.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9671f15.ps}\end{figure}$	Figure 15: (O-C) residuals of the WZ Oph y-band observations from the theoretical light curve computed for the photometric elements given in Table 17.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9671f16.ps}\end{figure}$	Figure 16: Best fitting parameter values for the 10 000 synthetic WZ Oph y light curves created for the Monte Carlo analysis.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{9671f17.ps}\end{figure}$	Figure 17: EBOP solutions for WZ Oph for a range of fixed k values. Linear limb-darkening coefficients by van Hamme (1993) were adopted. The upper left panel shows normalized rms errors of the fit to the observations. Symbols are: cross y; diamond b; triangle v; square u.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f18.ps}\end{figure}$	Figure 18: Comparison between Y² (red) and Victoria-Regina VRSS (blue) models for $[{\rm Fe/H}]$ =-0.190 and $[{\rm\alpha /Fe}]$ = 0.0. Y²: (X, Y, Z) = (0.73400, 0.25400, 0.01200). VRSS: (X, Y, Z) = (0.72456, 0.26294, 0.01250). Tracks (solid lines) for 1.1, 1.2, 1,3. 1.4, and 1.5 $M_{\odot }$ and isochrones (dashed) between 0.5 and 2.5 Gyr (step 0.5 Gyr) are shown.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f19.ps}\end{figure}$	Figure 19: Comparison between Y² (red) and BaSTI core overshoot (blue) models for $[{\rm Fe/H}]$ =-0.253 and $[{\rm\alpha /Fe}]$ =0.0. Y²: (X, Y, Z) = (0.73865, 0.25090, 0.01045). BaSTI: (X, Y, Z) = (0.7310, 0.2590, 0.0100). Tracks (solid lines) for 1.1, 1.2, 1.3, 1.4, and 1.5 $M_{\odot }$ and isochrones (dashed) between 0.5 and 2.5 Gyr (step 0.5 Gyr) are shown.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f21.ps}\end{figure}$	Figure 21: AD Boo compared with Y² models for (X,Y,Z) = (0.7028,0.2748,0.0224), equivalent to $[{\rm Fe/H}]$ =+0.10 for $[{\rm\alpha /Fe}]$ =0.0. Isochrones from 0.5 to 3.0 Gyr (step 0.5 Gyr) are shown. The 1.5 Gyr isochrone for $[{\rm Fe/H}]$ =+0.25 and $[{\rm\alpha /Fe}]$ =0.0 (dashed), corresponding to (X, Y, Z) = (0.6785, 0.2910, 0.0305), is included for comparison.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f22.ps}\end{figure}$	Figure 22: AD Boo compared with Y² models for (X, Y, Z) = (0.7028, 0.2748, 0.0224), equivalent to $[{\rm Fe/H}]$ =+0.10 for $[{\rm\alpha /Fe}]$ =0.0. Isochrones from 0.5 to 3.0 Gyr (step 0.5 Gyr) are shown.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f24.ps}\end{figure}$	Figure 24: VZ Hya compared with Y² models for (X, Y, Z) = (0.73478, 0.25348, 0.01174) equivalent to $[{\rm Fe/H}]$ =-0.20. Isochrones from 0.5 to 2.5 Gyr (step 0.5 Gyr) are shown. The 1.5 Gyr isochrone for $[{\rm Fe/H}]$ =-0.08 and $[{\rm\alpha /Fe}]$ =0.0 (dashed), corresponding to (X, Y, Z) = (0.72425,0.26050,0.01525), is included for comparison.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f25.ps}\end{figure}$	Figure 25: VZ Hya compared with Y² models for (X, Y, Z) = (0.73478, 0.25348, 0.01174) equivalent to $[{\rm Fe/H}]$ =-0.20. Isochrones from 0.5 to 2.5 Gyr (step 0.5 Gyr) are shown.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9671f27.ps}\end{figure}$	Figure 27: Assuming E(b-y) = 0.066: WZ Oph compared with Y² models for (X, Y, Z) = (0.72899, 0.25734, 0.013670), equivalent to $[{\rm Fe/H}]$ =-0.13 for $[{\rm\alpha /Fe}]$ =0.0. Tracks for the component masses (full drawn) and isochrones from 0.5 to 3.5 Gyr (dashed; step 0.5 Gyr) are shown. See text for details.
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