All Figures

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{4343fig5.eps} \end{figure}$ Figure 5: Spectroscopic versus Fourier [Fe/H] computed for 46 stars of the database set #1. Two lines show the $\pm$ 0.3 dex boundaries for [Fe/H] $_{\rm Spec.}=[$ Fe/H] $_{\rm Four.}$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{4343fig6.eps} \end{figure}$ Figure 6: Spectroscopic versus Fourier [Fe/H] computed for 72 stars of the database set #2. Two lines show the $\pm$ 0.4 dex boundaries for [Fe/H] $_{\rm Spec.}=\rm [Fe/H]_{Four.}$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{4343fig7.eps}\end{figure}$ Figure 7: The relation of ${\varphi _{31}}$ between the W and the V bands. The line is a linear fit for the relation. The asterisk is TZ Aur with a deviation of more than $3\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4343fig8.eps} \end{figure}$ Figure 8: Top: plot of [Fe/H] predicted by JK96 against those of ours for the common star. The solid line indicates $\rm [Fe/H]_{our}=[Fe/H]_{JK96}$ . Bottom: plot of $\rm\Delta [Fe/H]$ versus $\rm [Fe/H]_{JK96}$ ( $\rm\Delta [Fe/H]=[Fe/H]_{our}-[Fe/H]_{JK96}$ ). Two dashed lines present $\rm\Delta [Fe/H]=\pm 0.3$ around the $\rm\Delta [Fe/H]=0$ (solid line). Circles and triangles indicate the common stars in the datasets of JK96 and set #2 of K05, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{4343fig9.eps} %\end{figure}$ Figure 9: Light curves of five RRab stars from data set #1 observed by the 0.8-m telescope in the Xinglong Station with an unfiltered CCD.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{4343fi10.eps} \end{figure}$ Figure 10: Histogram of the [Fe/H] of set #3.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{4343fi11.eps} \end{figure}$ Figure 11: Plot of the predicted [Fe/H] vs. distance (Z) from the galactic plane. The solid squares are the mean [Fe/H] of set #3 in the bin of 2 kpc, and the open squares indicate data from Suntzeff et al. (1991). Triangles are the data from Table 10 in L94. Their [Fe/H] are all converted to the same scale as L94. The error bars indicate the standard error of the mean in each abundance bin.
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In the text

$\begin{figure} \par\includegraphics[width=14.8cm,height=17cm,clip]{4343fig1.eps} \end{figure}$ Figure 1: Folded light curves from the ROTSE-I database. All variables also appear in the compilation of JK96. The orders of the Fourier fits were determined from the SNR of the light curves, as described in the text. Headers: Name, average brightness in W band, and total amplitude [mag] of the fitted light curve (continuous line). The light curves are plotted in the 1.4 phase interval.
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In the text

$\begin{figure} \par\includegraphics[width=14.8cm,height=15.3cm,clip]{4343fig2.eps} \end{figure}$ Figure 2: Folded light curves from the ROTSE-I database. None of the variables is contained in the compilation of JK96, but all have low-dispersion spectroscopic metallicities from L94. The notation is the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{4343fig3.eps} \end{figure}$ Figure 3: Folded light curves from the ROTSE-I database. Data selection and notation are the same as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,height=11.8cm,clip]{4343fig4.eps}\end{figure}$ Figure 4: Light curves of 31 RRab variables from W05. Headers: ID of the star (as given in Wu05), average brightness in the band of the W05 system (see footnote 7), and total amplitude [mag] of the fitted light curve (continuous line). The light curves are plotted in the 1.4 phase interval.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{4343fig5.eps} \end{figure}$	Figure 5: Spectroscopic versus Fourier [Fe/H] computed for 46 stars of the database set #1. Two lines show the $\pm$ 0.3 dex boundaries for [Fe/H] $_{\rm Spec.}=[$ Fe/H] $_{\rm Four.}$ .
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$\begin{figure} \par\includegraphics[width=6.3cm,clip]{4343fig6.eps} \end{figure}$	Figure 6: Spectroscopic versus Fourier [Fe/H] computed for 72 stars of the database set #2. Two lines show the $\pm$ 0.4 dex boundaries for [Fe/H] $_{\rm Spec.}=\rm [Fe/H]_{Four.}$ .
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$\begin{figure} \par\includegraphics[width=6.3cm,clip]{4343fig7.eps}\end{figure}$	Figure 7: The relation of ${\varphi _{31}}$ between the W and the V bands. The line is a linear fit for the relation. The asterisk is TZ Aur with a deviation of more than $3\sigma$ .
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{4343fig9.eps} %\end{figure}$	Figure 9: Light curves of five RRab stars from data set #1 observed by the 0.8-m telescope in the Xinglong Station with an unfiltered CCD.
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$\begin{figure} \par\includegraphics[width=6.3cm,clip]{4343fi10.eps} \end{figure}$	Figure 10: Histogram of the [Fe/H] of set #3.
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$\begin{figure} \par\includegraphics[width=6.3cm,clip]{4343fi11.eps} \end{figure}$	Figure 11: Plot of the predicted [Fe/H] vs. distance (Z) from the galactic plane. The solid squares are the mean [Fe/H] of set #3 in the bin of 2 kpc, and the open squares indicate data from Suntzeff et al. (1991). Triangles are the data from Table 10 in L94. Their [Fe/H] are all converted to the same scale as L94. The error bars indicate the standard error of the mean in each abundance bin.
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$\begin{figure} \par\includegraphics[width=14.8cm,height=17cm,clip]{4343fig1.eps} \end{figure}$	Figure 1: Folded light curves from the ROTSE-I database. All variables also appear in the compilation of JK96. The orders of the Fourier fits were determined from the SNR of the light curves, as described in the text. Headers: Name, average brightness in W band, and total amplitude [mag] of the fitted light curve (continuous line). The light curves are plotted in the 1.4 phase interval.
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$\begin{figure} \par\includegraphics[width=14.8cm,height=15.3cm,clip]{4343fig2.eps} \end{figure}$	Figure 2: Folded light curves from the ROTSE-I database. None of the variables is contained in the compilation of JK96, but all have low-dispersion spectroscopic metallicities from L94. The notation is the same as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{4343fig3.eps} \end{figure}$	Figure 3: Folded light curves from the ROTSE-I database. Data selection and notation are the same as in Fig. 2.
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$\begin{figure} \par\includegraphics[width=15cm,height=11.8cm,clip]{4343fig4.eps}\end{figure}$	Figure 4: Light curves of 31 RRab variables from W05. Headers: ID of the star (as given in Wu05), average brightness in the band of the W05 system (see footnote 7), and total amplitude [mag] of the fitted light curve (continuous line). The light curves are plotted in the 1.4 phase interval.
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