All Figures

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{Figure1.eps} \end{figure}$ Figure 1: (J-K,K) CMDs of three halo clusters (M 3, NGC 5897, M 13) and five bulge clusters (NGC 6541, NGC 6642, NGC 6681, NGC 6717, NGC 6723). Open squares indicate the measurements of Cohen et al. (1978) for bright giants in the outer regions of M 3 and M 13.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{Figure2.eps} \end{figure}$ Figure 2: (J-H,H) CMDs of three halo clusters (M 3, NGC 5897, M 13) and five bulge clusters (NGC 6541, NGC 6642, NGC 6681, NGC 6717, NGC 6723). Open squares indicate the measurements of Cohen et al. (1978) for bright giants in the outer regions of M 3 and M 13.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure3.eps} \end{figure}$ Figure 3: Generated synthetic HBs with [M/H ] = -1.42, -1.30, -0.88, and -0.73. The solid lines indicate ZAHB and dots are the generated HBs in each panel. The arrow indicates the theoretical ZAHB level at log $T_{\rm eff}=3.85$ .
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{Figure4.eps} \end{figure}$ Figure 4: Fiducial normal points of target clusters in (J-K)_o-M_K and (J-H)_o-M_H planes. For clarity, the colors are given zero-point offsets; from left to right, these are const. =0.0, 0.4, 0.8, 1.2, 1.6, 2.0, 2.4 and 2.8 mag. Open circles indicate fiducial normal points of M 3 determined from the 2MASS data.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure5.eps} \end{figure}$ Figure 5: RGB (J-K)_o color indices at fixed magnitudes of M_K as a function of the metallicity [Fe/H] $_{\rm CG97}$ and the global metallicity [M/H]. Filled triangles and circles represent three halo clusters and five metal-poor bulge clusters observed here, respectively. Vertical bars represent the halo clusters and the metal-rich bulge clusters of Valenti et al. (2005, 2004a). Solid lines are the calibration relations of Valenti et al. (2004a).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure6.eps} \end{figure}$ Figure 6: RGB (J-H)_o color indices at fixed magnitudes of M_H as a function of the metallicity [Fe/H] $_{\rm CG97}$ and the global metallicity [M/H]. Symbols are the same as Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{Figure7.eps} \end{figure}$ Figure 7: RGB magnitude indices M_K and M_H at fixed color (J-K)_o=(J-H)_o=0.7 as a function of the metallicity [Fe/H] $_{\rm CG97}$ and the global metallicity [M/H]. Symbols are the same as Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure8.eps} \end{figure}$ Figure 8: The RGB slope as a function of metallicity. Symbols are the same as Fig. 5. The dotted lines are the relations found by Ivanov & Borissova (2002).
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In the text

$\begin{figure} \par\includegraphics[width=13.8cm,clip]{Figure9.eps} \end{figure}$ Figure 9: The cumulative ( upper) and differential ( lower) LFs for RGB stars in the observed halo clusters. The arrows indicate the RGB bump position. The dashed lines in the cumulative LF are the linear fit to the regions above and below the RGB bump.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{Figure10.eps} \end{figure}$ Figure 10: As in Fig. 9 for the observed metal-poor bulge clusters.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure11.eps} \end{figure}$ Figure 11: The behavior of the M_K and $M_{\rm bol}$ magnitudes of the RGB bumps for the observed clusters as a function of metallicity [Fe/H] and global metallicity [M/H]. The dotted and dashed lines are the theoretical prediction of the Yonsei-Yale isochrone (Yi et al. 2003; Kim et al. 2002) at t=12 and 10 Gyr, respectively. The other symbols are the same as Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure12.eps} \end{figure}$ Figure 12: As in Fig. 11 for the RGB tip. The open circles indicate the TRGB measurements of the post-core-collapse cluster NGC 6717.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{Figure1.eps} \end{figure}$	Figure 1: (J-K,K) CMDs of three halo clusters (M 3, NGC 5897, M 13) and five bulge clusters (NGC 6541, NGC 6642, NGC 6681, NGC 6717, NGC 6723). Open squares indicate the measurements of Cohen et al. (1978) for bright giants in the outer regions of M 3 and M 13.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{Figure2.eps} \end{figure}$	Figure 2: (J-H,H) CMDs of three halo clusters (M 3, NGC 5897, M 13) and five bulge clusters (NGC 6541, NGC 6642, NGC 6681, NGC 6717, NGC 6723). Open squares indicate the measurements of Cohen et al. (1978) for bright giants in the outer regions of M 3 and M 13.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure3.eps} \end{figure}$	Figure 3: Generated synthetic HBs with [M/H ] = -1.42, -1.30, -0.88, and -0.73. The solid lines indicate ZAHB and dots are the generated HBs in each panel. The arrow indicates the theoretical ZAHB level at log $T_{\rm eff}=3.85$ .
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{Figure4.eps} \end{figure}$	Figure 4: Fiducial normal points of target clusters in (J-K)_o-M_K and (J-H)_o-M_H planes. For clarity, the colors are given zero-point offsets; from left to right, these are const. =0.0, 0.4, 0.8, 1.2, 1.6, 2.0, 2.4 and 2.8 mag. Open circles indicate fiducial normal points of M 3 determined from the 2MASS data.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure6.eps} \end{figure}$	Figure 6: RGB (J-H)_o color indices at fixed magnitudes of M_H as a function of the metallicity [Fe/H] $_{\rm CG97}$ and the global metallicity [M/H]. Symbols are the same as Fig. 5.
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$\begin{figure} \par\includegraphics[width=8.5cm]{Figure7.eps} \end{figure}$	Figure 7: RGB magnitude indices M_K and M_H at fixed color (J-K)_o=(J-H)_o=0.7 as a function of the metallicity [Fe/H] $_{\rm CG97}$ and the global metallicity [M/H]. Symbols are the same as Fig. 5.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure8.eps} \end{figure}$	Figure 8: The RGB slope as a function of metallicity. Symbols are the same as Fig. 5. The dotted lines are the relations found by Ivanov & Borissova (2002).
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$\begin{figure} \par\includegraphics[width=13.8cm,clip]{Figure9.eps} \end{figure}$	Figure 9: The cumulative ( upper) and differential ( lower) LFs for RGB stars in the observed halo clusters. The arrows indicate the RGB bump position. The dashed lines in the cumulative LF are the linear fit to the regions above and below the RGB bump.
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$\begin{figure} \par\includegraphics[width=15.7cm,clip]{Figure10.eps} \end{figure}$	Figure 10: As in Fig. 9 for the observed metal-poor bulge clusters.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure11.eps} \end{figure}$	Figure 11: The behavior of the M_K and $M_{\rm bol}$ magnitudes of the RGB bumps for the observed clusters as a function of metallicity [Fe/H] and global metallicity [M/H]. The dotted and dashed lines are the theoretical prediction of the Yonsei-Yale isochrone (Yi et al. 2003; Kim et al. 2002) at t=12 and 10 Gyr, respectively. The other symbols are the same as Fig. 5.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{Figure12.eps} \end{figure}$	Figure 12: As in Fig. 11 for the RGB tip. The open circles indicate the TRGB measurements of the post-core-collapse cluster NGC 6717.
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