All Figures

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4453fig3.eps} \end{figure}$ Figure 3: V magnitudes (Vw) of M92W versus V magnitudes (Vc) of M92C for stars that are common to both areas and brighter than V=14.5.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4453fig4.eps} \end{figure}$ Figure 4: Comparison between the (B-V) color-index by Sandage (1969) and the same color-index observed by Sandage & Walker (1966) for 17 stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4453fig5.eps} . \end{figure}$ Figure 5: The color-magnitude diagram for the stars observed in the field M92W: the empty circles indicate the stars brighter than V= 14.8; the empty squares the stars fainter than this value; filled circles and filled squares are photoelectric standards by Sandage & Walker (1966) and Sandage (1970), respectively. The measured [Fe/H] ratio for three stars is indicated (see text)
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,clip]{4453fig6.eps} \end{figure}$ Figure 6: The color-color diagrams (P-V) vs. (Y-V) and (X-V) vs. (Y-V) in both cluster and west fields. The continuous line represents the main sequence, and the dashed line the sequence of the normal G-K giants. The stars, observed in the fields M92C ( a) and c)) and M92W ( d)), are plotted by dots. The encircled dots are the stars brighter than about V=15th magnitude. In c) only the stars brighter than this limit are represented (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4453fig7.eps}\end{figure}$ Figure 7: The histograms of the six sets of [Fe/H] ratios measured in both fields cluster (in a), c), e)) and west (in b), d), f)), obtained from the three color excesses $\delta (X-Y), \delta (P-Y)$ and $\delta (P-X)$ . The Gaussian fittings for each distribution are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{4453fig1.eps} \end{figure}$ Figure 1: The finding chart of the M92C field. The central pixel ( $X_{\rm c}=1044$ ; $Y_{\rm c}=1022$ ) is at RA $\rm 17^{h}17^{m}00\hbox{$.\!\!^{\rm s}$ }7$ , Dec $+43^{\circ }08'00''$ (1950.0). The X,Y pixel coordinates, with their respective origins in the East and South, correspond to those in Table 1A (see Appendix).
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{4453fig2.eps} \end{figure}$ Figure 2: The finding chart of the M92W field. North is up, east to the left. The central pixel ( $X_{\rm c}: 1042$ ; $Y_{\rm c}: 1024$ ) is at RA $\rm 17^{h}16^{m}25\hbox{$.\!\!^{\rm s}$ }7$ , Dec $+43^{\circ }08'46''$ (1950.0). The X,Y pixel coordinates, with respective origins in the East and South, correspond to those in Table 2A (see Appendix).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4453fig3.eps} \end{figure}$	Figure 3: V magnitudes (Vw) of M92W versus V magnitudes (Vc) of M92C for stars that are common to both areas and brighter than V=14.5.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4453fig4.eps} \end{figure}$	Figure 4: Comparison between the (B-V) color-index by Sandage (1969) and the same color-index observed by Sandage & Walker (1966) for 17 stars.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4453fig5.eps} . \end{figure}$	Figure 5: The color-magnitude diagram for the stars observed in the field M92W: the empty circles indicate the stars brighter than V= 14.8; the empty squares the stars fainter than this value; filled circles and filled squares are photoelectric standards by Sandage & Walker (1966) and Sandage (1970), respectively. The measured [Fe/H] ratio for three stars is indicated (see text)
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4453fig7.eps}\end{figure}$	Figure 7: The histograms of the six sets of [Fe/H] ratios measured in both fields cluster (in a), c), e)) and west (in b), d), f)), obtained from the three color excesses $\delta (X-Y), \delta (P-Y)$ and $\delta (P-X)$ . The Gaussian fittings for each distribution are also shown.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{4453fig1.eps} \end{figure}$	Figure 1: The finding chart of the M92C field. The central pixel ( $X_{\rm c}=1044$ ; $Y_{\rm c}=1022$ ) is at RA $\rm 17^{h}17^{m}00\hbox{$.\!\!^{\rm s}$ }7$ , Dec $+43^{\circ }08'00''$ (1950.0). The X,Y pixel coordinates, with their respective origins in the East and South, correspond to those in Table 1A (see Appendix).
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$\begin{figure} \par\includegraphics[width=13cm,clip]{4453fig2.eps} \end{figure}$	Figure 2: The finding chart of the M92W field. North is up, east to the left. The central pixel ( $X_{\rm c}: 1042$ ; $Y_{\rm c}: 1024$ ) is at RA $\rm 17^{h}16^{m}25\hbox{$.\!\!^{\rm s}$ }7$ , Dec $+43^{\circ }08'46''$ (1950.0). The X,Y pixel coordinates, with respective origins in the East and South, correspond to those in Table 2A (see Appendix).
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