All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{9405f1a.ps}\vspace*{3mm} \includegraphics[width=6.5cm,clip]{9405f1b.ps}\end{figure}$ Figure 1: The optical V, B-V CMD of M71. Top: dots: Cudworth (1985, 2006) photometry; filled circles: sample stars; open squares: stars identified in Geffert & Maintz (2000). Bottom: stars with membership probability P $\geq$ 80% (symbols are the same as above). A Yonsei-Yale isochrone by Kim et al. (2002) with parameters as indicated is overplotted.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{9405f2.ps}\end{figure}$ Figure 2: Spectrum of the star 484 (1-55, V = 14.26) observed in the Mask # 2. Gaps are due to the 3 CCD configuration of the detector. Central wavelengths of studied indices are indicated.
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In the text

$\begin{figure} \par\hspace*{1mm}\includegraphics[width=6.7cm,clip]{9405f3a.ps}\vspace*{3mm} \includegraphics[width=6.6cm,clip]{9405f3b.ps}\end{figure}$ Figure 3: a) CN₁ plotted against V, and b) CN₁ vs. $(B-V)_{\rm0}$ for the M71 sample stars, where the locus CN-strong ( filled circles) and CN-weak ( open circles) are seen. Error bars quoted correspond to the rms on all measurements available.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{9405f4.ps}\end{figure}$ Figure 4: V, B-V CMD with the CN-strong stars ( open stars), CN-weak ( filled circles), and the subgiants ( filled squares) for which the CN measurements are not qualified as strong or weak.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{9405f5.ps}\end{figure}$ Figure 5: CN₁ vs. effective temperature. Error bar on CN₁ is as explained in Fig. 3, while on $T_{\rm eff}$ it resembles the value determined with the photometric calibration employed.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9405f6.ps}\end{figure}$ Figure 6: CN₁ vs. log g. Error bar is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9405f7.ps}\end{figure}$ Figure 7: G-band as function of V magnitude, where CN-strong ( filled circles) and CN-weak ( open circles) stars are plotted separately.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{9405f8.ps}\end{figure}$ Figure 8: Stars 390 and 399 in the molecular CN and CH band region. The full and dashed lines represent the CN-strong and CN-weak stars, respectively. These stars display approximately the same temperatures.
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In the text

$\begin{figure} \par\hspace*{1mm}\includegraphics[width=6.8cm,clip]{9405f9a.ps}\vspace*{3mm} \includegraphics[width=6.65cm,clip]{9405f9b.ps}\end{figure}$ Figure 9: Upper panel: Mg₂ plotted against CN₁; lower panel: Mg₂ as a function of the effective temperature. Error bars are as previously discussed.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{9405f10.ps}\end{figure}$ Figure 10: Ca4227 feature against the effective temperature.
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In the text

$\begin{figure} \par\hspace*{-1mm}\includegraphics[width=6.6cm,clip]{9405f11a.ps}\vspace*{3mm} \includegraphics[width=6.7cm,clip]{9405f11b.ps}\end{figure}$ Figure 11: Upper panel: Ca4227 vs. $\langle$ Fe $\rangle$ , and lower panel: Ca4227 vs. Mg₂. $\langle$ Fe $\rangle$ = (Fe4383 + Fe5270 + Fe5335 + Fe5406)/4.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9405f12a.ps}\vspace*{3mm} \includegraphics[width=6.5cm,clip]{9405f12b.ps}\end{figure}$ Figure 12: a) H ${_{\beta }}$ plotted against V, and b) H ${_{\beta }}$ against $T_{\rm eff}$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9405f13a.ps}\vspace*{3mm} \includegraphics[width=6.7cm,clip]{9405f13b.ps}\end{figure}$ Figure 13: NaD and Al3953 as a function of the CN index.
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In the text

$\begin{figure} \par\hspace*{1mm}\includegraphics[width=6.6cm,clip]{9405f14a.ps}\vspace*{3mm} \includegraphics[width=6.6cm,clip]{9405f14b.ps}\end{figure}$ Figure 14: Top: Al3953 vs. NaD. Bottom: Mg₂ vs. Al3953.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{9405f15a.ps}\vspace*{3mm} \includegraphics[width=6.6cm,clip]{9405f15b.ps}\end{figure}$ Figure 15: Synthetic (solid line) and observed spectra (dotted line) in the region of CN and CH bands. Upper panel: star 390 (CN-strong): $T_{\rm eff}$ , log g, $v_{\rm t}$ ) = (4434 K, 1.54, 1.5 km s^-1) computed for [C/Fe] = 0.0, [N/Fe] = +1.0; lower panel: star 399 (CN-weak): (4419 K, 1.8, 1.5 km s^-1) computed for [C/Fe] = 0.0, [N/Fe] = +0.50.
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In the text