All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{0051fig1.ps}\end{figure}$ Figure 1: Observed colour-magnitude diagram of NGC 6397. The targets selected for the spectroscopic study are marked with black squares.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0051fig2.eps}\end{figure}$ Figure 2: The best-fit H $\alpha$ profiles for three stars. The thick line corresponds to a model with the stated effective temperature. The grey-shaded regions represent the regions used for fitting.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0051fig3.eps}\end{figure}$ Figure 3: Comparison between our H $\alpha$ -based effective temperatures and those obtained by applying the calibrated relations of Alonso et al. (1999,1996) to colour indices v-y and V-I. The y-axis shows $\Delta T_{\rm eff}=T_{\rm eff, H\alpha }-T_{\rm photometry}$ for the stated index and calibration.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0051fig4.eps}\end{figure}$ Figure 4: Comparison between our spectroscopic $T_{\rm eff}$ -scale, the photometric values obtained from v-y and V-I, and the results from six other studies.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0051fig5.eps}\end{figure}$ Figure 5: A selected part of two observed, normalised spectra (dotted lines) and the best fitting model spectra (solid lines), as determined by the analysis code. Note that the models in this figure only contain the spectral lines that are used in the abundance analysis. These lines are marked with labels. The top spectrum belongs to the bRGB star 23 267 and the bottom plot to the TO star 12318.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0051fig6.eps}\end{figure}$ Figure 6: A histogram of the slopes obtained for linear fits of iron abundance with excitation potential of Fe I lines.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{0051fig7.eps}\end{figure}$ Figure 7: Abundance trends (filled dots) with effective temperature for Mg, Ca, Ti, and Fe from analysis of 116 stars. The thick lines display general trends and the thin lines show estimated 1 $\sigma$ limits. Open squares represent the results from Paper I, in which Mg, Ca, and Fe are treated in NLTE and Ti in LTE.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0051fig8.eps}\end{figure}$ Figure 8: The figure shows a comparison between equivalent widths measured for the same lines in spectra of the same stars, obtained with GIRAFFE and UVES, respectively. The filled circles corresponds to stars located at the TO and the open circles to bRGB stars. The dashed line mark 1:1 agreement and the solid line is a linear fit to the measurements.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0051fig9.eps}\end{figure}$ Figure 9: Comparison between the abundance trends from Fig. 7 (here displayed with black dots) and the predictions from stellar structure models including atomic diffusion and turbulent mixing. The horizontal, black, solid lines represent the initial abundances of the models. The three arrows in the upper left corner of each plot indicate the abundance change at $T_{\rm eff}=6250$ K when raising the effective temperature by 100 K ( left), raising the surface gravity by 0.1 dex ( middle), and raising the microturbulence values by 0.1 km s^-1 ( right).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0051fig1.ps}\end{figure}$	Figure 1: Observed colour-magnitude diagram of NGC 6397. The targets selected for the spectroscopic study are marked with black squares.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0051fig2.eps}\end{figure}$	Figure 2: The best-fit H $\alpha$ profiles for three stars. The thick line corresponds to a model with the stated effective temperature. The grey-shaded regions represent the regions used for fitting.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0051fig3.eps}\end{figure}$	Figure 3: Comparison between our H $\alpha$ -based effective temperatures and those obtained by applying the calibrated relations of Alonso et al. (1999,1996) to colour indices v-y and V-I. The y-axis shows $\Delta T_{\rm eff}=T_{\rm eff, H\alpha }-T_{\rm photometry}$ for the stated index and calibration.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0051fig4.eps}\end{figure}$	Figure 4: Comparison between our spectroscopic $T_{\rm eff}$ -scale, the photometric values obtained from v-y and V-I, and the results from six other studies.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0051fig6.eps}\end{figure}$	Figure 6: A histogram of the slopes obtained for linear fits of iron abundance with excitation potential of Fe I lines.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{0051fig7.eps}\end{figure}$	Figure 7: Abundance trends (filled dots) with effective temperature for Mg, Ca, Ti, and Fe from analysis of 116 stars. The thick lines display general trends and the thin lines show estimated 1 $\sigma$ limits. Open squares represent the results from Paper I, in which Mg, Ca, and Fe are treated in NLTE and Ti in LTE.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0051fig8.eps}\end{figure}$	Figure 8: The figure shows a comparison between equivalent widths measured for the same lines in spectra of the same stars, obtained with GIRAFFE and UVES, respectively. The filled circles corresponds to stars located at the TO and the open circles to bRGB stars. The dashed line mark 1:1 agreement and the solid line is a linear fit to the measurements.
Open with DEXTER