All Figures

$\begin{figure} \par\includegraphics[width=5.2cm,clip]{3583fig1.eps} \end{figure}$ Figure 1: The results from artificial star experiments. Solid, dotted and dashed lines represent J, H and K bands, respectively. Completeness is defined as the number of recovered artificial stars divided by the total number of stars added. $\Delta M$ (mag) is the mean difference between the actual input magnitudes and the measured magnitudes by DAOPHOT II/ALLSTAR, while $\sigma$ (mag) is the standard deviation of the $\Delta M$ .
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In the text

$\begin{figure} \par\includegraphics[width=10.2cm,clip]{3583fig2.eps} \end{figure}$ Figure 2: (K, J-K) and (K, H-K) CMDs of the total observed area ( upper) and the outer region ( lower) of NGC 147. The loci with thin lines trace the photometric evolution of AGB tip in the range of log $(t_{\rm yr}) = 7.8\sim 10.2$ with Z = 0.004, 0.008 and 0.019, respectively (Girardi et al. 2002). The color and magnitude range of the RGB tip at the distance of NGC 147 is also presented with a thick line. Open circles indicate 34 C stars cross-identified in both near-infrared photometry (this paper) and TiO and CN photometry (Nowotny et al. 2003).
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{3583fig3.eps} % \end{figure}$ Figure 3: (H-K)-(J-H) and (H-K)-(J-K) color-color diagrams for AGB stars brighter than K=18. Dotted boxes contain C stars with (J-K) > 1.34 and (H-K) > 0.44. The loci are the color sequences of the tip of AGB stars as in Fig. 2. Open circles are 34 C stars cross-identified in both near-infrared photometry (this paper) and TiO and CN bands photometry (Nowotny et al. 2003).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3583fig4.eps} \end{figure}$ Figure 4: Color-color diagrams of JHK and VRI bands for 34 cross-identified C stars with (V-i)₀ indices from Nowotny et al. (2003) and 14 cross-identified C stars with (R-I) indices from Battinelli & Demers (2004c). Vertical dotted lines are the near-infrared color ranges of C stars, i.e. (J-K)>1.34 and (H-K)>0.44, while horizontal dotted lines are the color ranges of C stars in VRI bands, i.e. (V-i)₀>1.16 and (R-I)>1.06, given by Nowotny et al. (2003) and Battinelli & Demers (2004c).
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In the text

$\begin{figure} \par\includegraphics[width=10cm,clip]{3583fig5.eps} \end{figure}$ Figure 5: Histogram distributions of the (J-K) and (H-K) colors of stars with K between 15.5 and 18.0 mag. Arrows mark the theoretically predicted colors of the AGB tip for Z = 0.019 isochrones of log $(t_{\rm yr}) = 8.1, 8.4$ and 9.5 (Girardi et al. 2002) at the distance of NGC 147. The shaded sections represent the distribution of the 91 C stars identified.
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In the text

$\begin{figure} \par\includegraphics[width=10.5cm,clip]{3583fig6.eps} % \end{figure}$ Figure 6: Left: the completeness corrected LFs in M_K for M giant stars and C stars. The inner small panel in the lower panel shows the logarithmic LF of M giant stars in NGC 147. Right: the completeness corrected bolometric LFs for M giant stars and C stars.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3583fig7.eps} \end{figure}$ Figure 7: Relationship between the K magnitude of the AGB tip and age at the distance of NGC 147, as predicted by isochrones (Girardi et al. 2002) for Z = 0.004 (solid line), 0.008 (dotted line) and 0.019 (dashed line). The shadow bar represents the range of AGB tip brightness for stars having log ( $t_{\rm yr})=10.0$ . The estimated mean magnitude of the AGB tip in NGC 147 is also represented by a dot with a measurement error.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{3583fig3.eps} % \end{figure}$	Figure 3: (H-K)-(J-H) and (H-K)-(J-K) color-color diagrams for AGB stars brighter than K=18. Dotted boxes contain C stars with (J-K) > 1.34 and (H-K) > 0.44. The loci are the color sequences of the tip of AGB stars as in Fig. 2. Open circles are 34 C stars cross-identified in both near-infrared photometry (this paper) and TiO and CN bands photometry (Nowotny et al. 2003).
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$\begin{figure} \par\includegraphics[width=10cm,clip]{3583fig5.eps} \end{figure}$	Figure 5: Histogram distributions of the (J-K) and (H-K) colors of stars with K between 15.5 and 18.0 mag. Arrows mark the theoretically predicted colors of the AGB tip for Z = 0.019 isochrones of log $(t_{\rm yr}) = 8.1, 8.4$ and 9.5 (Girardi et al. 2002) at the distance of NGC 147. The shaded sections represent the distribution of the 91 C stars identified.
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$\begin{figure} \par\includegraphics[width=10.5cm,clip]{3583fig6.eps} % \end{figure}$	Figure 6: Left: the completeness corrected LFs in M_K for M giant stars and C stars. The inner small panel in the lower panel shows the logarithmic LF of M giant stars in NGC 147. Right: the completeness corrected bolometric LFs for M giant stars and C stars.
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