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$\begin{figure} \par\includegraphics[width=12cm,height=7.4cm,clip]{6552fig1.ps} \end{figure}$ Figure 1: Evolution of the carbon isotopic ratio with respect to the stellar $K_{\rm s}$ -magnitude above the bump in the RGB luminosity function of each globular cluster. The adopted $K_{\rm s}$ -bump magnitudes are reported in Table 1. The maximum error on ( $K_{\rm s}-K_{\rm s}^{\rm Bump}$ ) is shown in the upper right corner and, for a given cluster, the uncertainty on the relative stellar luminosities with respect to their bump is $\pm$ 0.04 mag (see text for more details). The reported metallicity (in dex) of each GC is from Kraft & Ivans (2003). For two stars (one in M 4 and one in NGC 6397), we have only been able to derive lower limits for their carbon isotopic ratios. These limits are represented by a symbol located at the lower end of their error bar.
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In the text