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<!-- DOI: 10.1051/0004-6361/200912713 -->

<h2 class="sec">Online Material</h2>

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<table>
<tr><td><!-- init Label --><A NAME="figcmd">&#160;</A><!-- end Label--><A NAME="726"></A><A NAME="figure562"
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\par\includegraphics[width=8.50cm,clip]{12713f3.eps}
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<td class="img-txt"><span class="bold">Figure 3:</span><p>
Colour-magnitude diagram of the cluster NGC
6397. The stars studied in this work are depicted in small filled
squares.</p></td>
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<A NAME="tabmod"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/38/aa12713-09/table1.html"><span class="bold">Table 1:</span></a>&#160;&#160;
Details of the 3D hydrodynamical model atmospheres.</p><div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="figspec">&#160;</A><!-- end Label--><A NAME="767"></A><A NAME="figure582"
 HREF="img32.png"><IMG
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 ALT="\begin{figure}
\par\includegraphics[width=8.5cm,angle=0]{12713f4.eps}
\end{figure}"></A><!-- HTML Figure number: 4 --></td>
<td class="img-txt"><span class="bold">Figure 4:</span><p>
Observed GIRAFFE/FLAMES spectra of a dwarf star
MSS005634 (<I> bottom</I>, <I>S</I>/<I>N</I>&nbsp;= 102) and a subgiant star SGB002930 
(<I> top</I>, <I>S</I>/<I>N</I>= 111)of the globular cluster NGC&nbsp;6397.</p></td>
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<tr><td><!-- init Label --><A NAME="figew1d">&#160;</A><!-- end Label--><A NAME="768"></A><A NAME="figure589"
 HREF="img33.png"><IMG
 WIDTH="95" HEIGHT="71" SRC="Timg33.png"
 ALT="\begin{figure}
\par\includegraphics[width=8.5cm,angle=0]{12713f5.eps}
\end{figure}"></A><!-- HTML Figure number: 5 --></td>
<td class="img-txt"><span class="bold">Figure 5:</span><p>
Comparison between the equivalent widths
derived in this work and those provided by Lind et&nbsp;al. (2009). 
Filled circles and open circles correspond to dwarf and subgiant
stars, respectively.</p></td>
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<tr><td><!-- init Label --><A NAME="figteff1d">&#160;</A><!-- end Label--><A NAME="769"></A><A NAME="figure594"
 HREF="img34.png"><IMG
 WIDTH="95" HEIGHT="67" SRC="Timg34.png"
 ALT="\begin{figure}
\par\includegraphics[width=8.5cm,angle=0]{12713f6.eps}
\end{figure}"></A><!-- HTML Figure number: 6 --></td>
<td class="img-txt"><span class="bold">Figure 6:</span><p>
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.</p></td>
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<tr><td><!-- init Label --><A NAME="figteffteffl">&#160;</A><!-- end Label--><A NAME="770"></A><A NAME="figure600"
 HREF="img35.png"><IMG
 WIDTH="95" HEIGHT="67" SRC="Timg35.png"
 ALT="\begin{figure}
\par\includegraphics[width=8.5cm,angle=0]{12713f7.eps}
\end{figure}"></A><!-- HTML Figure number: 7 --></td>
<td class="img-txt"><span class="bold">Figure 7:</span><p>
Comparison between 3D effective
temperatures of the observed stars and the 1D&nbsp;effective temperatures
derived from colors by Lind et&nbsp;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 <I>B</I>-<I>V</I>&nbsp;range of 0.06&nbsp;mag, their temperature
range should be of, at least 250&nbsp;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&nbsp;al. (2009) effective
temperatures <IMG
 WIDTH="12" HEIGHT="14" ALIGN="BOTTOM" BORDER="0"
 SRC="img2.png"
 ALT="$\sim $">80&nbsp;K.</p></td>
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<div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="figteffbv">&#160;</A><!-- end Label--><A NAME="771"></A><A NAME="figure605"
 HREF="img36.png"><IMG
 WIDTH="95" HEIGHT="67" SRC="Timg36.png"
 ALT="\begin{figure}
\par\includegraphics[width=8.5cm,angle=0]{12713f8.eps}
\end{figure}"></A><!-- HTML Figure number: 8 --></td>
<td class="img-txt"><span class="bold">Figure 8:</span><p>
Comparison between 3D effective
temperatures and <I>B</I>-<I>V</I>&nbsp;colours of the observed stars. 
Filled circles and open circles correspond to 
dwarf and subgiant stars, respectively. The lack of correlation
between <I>B</I>-<I>V</I> and effective temperature is consistent with 
photometric errors and reddening variations.</p></td>
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<div class="inset-old">
<table>
<tr><td><!-- init Label --><A NAME="fighalpha">&#160;</A><!-- end Label--><A NAME="772"></A><A NAME="figure611"
 HREF="img37.png"><IMG
 WIDTH="192" HEIGHT="67" SRC="Timg37.png"
 ALT="\begin{figure}
\par\includegraphics[width=8.5cm,angle=0.]{12713f9a.eps}\includegraphics[width=8.5cm,angle=0.]{12713f9b.eps}
\end{figure}"></A><!-- HTML Figure number: 9 --></td>
<td class="img-txt"><span class="bold">Figure 9:</span><p>
Observed GIRAFFE/FLAMES H<IMG
 WIDTH="12" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img3.png"
 ALT="$\alpha $">
profile
fitted with a synthetic 3D&nbsp;profile for a dwarf star MSS005634 
(<I> left panel</I>, <I>S</I>/<I>N</I> = 102, 
<!-- MATH: $T_{\rm eff,3D}=6327$ -->
<IMG
 WIDTH="81" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img4.png"
 ALT="$T_{\rm eff,3D}=6327$">&nbsp;K) and for a subgiant star
SGB002930 (<I> right panel</I>, <I>S</I>/<I>N</I> = 111, 
<!-- MATH: $T_{\rm eff,3D}=6126$ -->
<IMG
 WIDTH="82" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img5.png"
 ALT="$T_{\rm eff,3D}=6126$">&nbsp;K).</p></td>
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<tr><td><!-- init Label --><A NAME="figewobs">&#160;</A><!-- end Label--><A NAME="773"></A><A NAME="figure621"
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 ALT="\begin{figure}
\par\includegraphics[width=8.5cm,angle=0.]{12713f10a.eps}\include...
...2713f10c.eps}\includegraphics[width=8.5cm,angle=0.]{12713f10d.eps}
\end{figure}"></A><!-- HTML Figure number: 10 --></td>
<td class="img-txt"><span class="bold">Figure 10:</span><p>
Observed spectra of two dwarf stars, MSS005634
(<I> top-left panel</I>, <I>S</I>/<I>N</I>= 102, <I> EW</I>(Li)&nbsp;=&nbsp;32.21&nbsp;m&#197;) and MSS006561 
(<I> top-right panel</I>, <I>S</I>/<I>N</I>=71, <I> EW</I>(Li)&nbsp;=&nbsp;27.97&nbsp;m&#197;) and two subgiant
stars, SGB002930 (<I> bottom-left panel</I>, <I>S</I>/<I>N</I>=111,
<I> EW</I>(Li)&nbsp;=&nbsp;36.83&nbsp;m&#197;) and SGB004904 (<I> bottom-left panel</I>, <I>S</I>/<I>N</I> =68,
<I> EW</I>(Li)&nbsp;=&nbsp;48.52&nbsp;m&#197;), showing the fit of the Li line with a
synthetic profile.</p></td>
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<p>
<A NAME="BIGtable"></A><p class="inset-old"><a href="/articles/aa/full_html/2009/38/aa12713-09/table2.html"><span class="bold">Table 2:</span></a>&#160;&#160;
Photometric data of the dwarf and subgiant stars of the
globular cluster NGC&nbsp;6397. We also provide the signal-to-noise of the
spectra, the 3D and 1D H<IMG
 WIDTH="12" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img3.png"
 ALT="$\alpha $">-based effective temperatures, 3D Li
abundances, and the equivalent widths and errors.
</p>
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