EDP Sciences
Free Access
Issue
A&A
Volume 505, Number 2, October II 2009
Page(s) L13 - L16
Section Letters
DOI https://doi.org/10.1051/0004-6361/200912713
Published online 15 September 2009

Online Material

 \begin{figure}
\par\includegraphics[width=8.50cm,clip]{12713f3.eps}
\end{figure} Figure 3:

Colour-magnitude diagram of the cluster NGC 6397. The stars studied in this work are depicted in small filled squares.

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Table 1:   Details of the 3D hydrodynamical model atmospheres.

 \begin{figure}
\par\includegraphics[width=8.5cm,angle=0]{12713f4.eps}
\end{figure} Figure 4:

Observed GIRAFFE/FLAMES spectra of a dwarf star MSS005634 ( bottom, S/N = 102) and a subgiant star SGB002930 ( top, S/N= 111)of the globular cluster NGC 6397.

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 \begin{figure}
\par\includegraphics[width=8.5cm,angle=0]{12713f5.eps}
\end{figure} Figure 5:

Comparison between the equivalent widths derived in this work and those provided by Lind et al. (2009). Filled circles and open circles correspond to dwarf and subgiant stars, respectively.

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 \begin{figure}
\par\includegraphics[width=8.5cm,angle=0]{12713f6.eps}
\end{figure} Figure 6:

Comparison between 3D and 1D effective temperatures of the observed stars. Filled circles and open circles correspond to dwarf and subgiant stars, respectively. The dashed line shows the one-to-one relationship.

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 \begin{figure}
\par\includegraphics[width=8.5cm,angle=0]{12713f7.eps}
\end{figure} Figure 7:

Comparison between 3D effective temperatures of the observed stars and the 1D effective temperatures derived from colors by Lind et al. (2009). Filled circles and open circles correspond to dwarf and subgiant stars, respectively. The dashed line shows the one-to-one relationship. Since our stars have been selected in a B-V range of 0.06 mag, their temperature range should be of, at least 250 K. It could be larger due to stars being moved into our selection box by photometric and reddening uncertainties. There is no plausible reason why this range should be as small as that implied by the Lind et al. (2009) effective temperatures $\sim $80 K.

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 \begin{figure}
\par\includegraphics[width=8.5cm,angle=0]{12713f8.eps}
\end{figure} Figure 8:

Comparison between 3D effective temperatures and B-V colours of the observed stars. Filled circles and open circles correspond to dwarf and subgiant stars, respectively. The lack of correlation between B-V and effective temperature is consistent with photometric errors and reddening variations.

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 \begin{figure}
\par\includegraphics[width=8.5cm,angle=0.]{12713f9a.eps}\includegraphics[width=8.5cm,angle=0.]{12713f9b.eps}
\end{figure} Figure 9:

Observed GIRAFFE/FLAMES H$\alpha $ profile fitted with a synthetic 3D profile for a dwarf star MSS005634 ( left panel, S/N = 102, $T_{\rm eff,3D}=6327$ K) and for a subgiant star SGB002930 ( right panel, S/N = 111, $T_{\rm eff,3D}=6126$ K).

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 \begin{figure}
\par\includegraphics[width=8.5cm,angle=0.]{12713f10a.eps}\include...
...2713f10c.eps}\includegraphics[width=8.5cm,angle=0.]{12713f10d.eps}
\end{figure} Figure 10:

Observed spectra of two dwarf stars, MSS005634 ( top-left panel, S/N= 102, EW(Li) = 32.21 mÅ) and MSS006561 ( top-right panel, S/N=71, EW(Li) = 27.97 mÅ) and two subgiant stars, SGB002930 ( bottom-left panel, S/N=111, EW(Li) = 36.83 mÅ) and SGB004904 ( bottom-left panel, S/N =68, EW(Li) = 48.52 mÅ), showing the fit of the Li line with a synthetic profile.

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Table 2:   Photometric data of the dwarf and subgiant stars of the globular cluster NGC 6397. We also provide the signal-to-noise of the spectra, the 3D and 1D H$\alpha $-based effective temperatures, 3D Li abundances, and the equivalent widths and errors.


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