$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{aa3930f1.eps}}\end{figure}$ Figure 1: Coadded UVES spectra of the 10 Sgr giants analysed in this paper. The labels on the right denote the star number, those on the left the [FeI/H].
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{aa3930f3.eps}}\end{figure}$ Figure 3: The colour-magnitude diagram of field 1 of Marconi et al. (1998), the reddening adopted is E(V-I)=0.22, A_V=0.55 and the distance modulus (m-M)=16.95, from the same reference. The stars observed by UVES are shown with larger symbols, two Padova isochrones (Girardi et al. 2002), covering the range in Z found for the program stars are shown.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{aa3930f4.eps}}\end{figure}$ Figure 4: The [Fe/H], [ ${\alpha }$ /Fe] diagram for the programme stars (filled symbols. The 5 stars of M54 studied by Brown et al. (1999) are shown as open symbols. [ ${\alpha }$ /Fe] in this plot is defined as $1\over 3$ ([Mg/Fe]+[Si/Fe]+[Ca/Fe]).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{aa3930f5.eps}}\end{figure}$ Figure 5: The [Fe/H], [ ${\alpha }$ /Fe] diagram for the programme stars (filled symbols), the stars in the Local Group dwarf spheoridals, Draco, Ursa Minor, Sextans from Shetrone et al. (2001), Carina, Sculptor, Fornax and Leo from Shetrone et al. (2003) (open circles), Galactic stars from Gratton et al. (2003) (crosses) and for DLAs from Centuriòn et al. (2003) (asterisks). For the stars [ ${\alpha }$ /Fe], in this plot, is defined as $0.5\times \rm ([Mg/Fe]{+}[Ca/Fe])$ , for the DLAs [Si/Zn] is used as a proxy for [ ${\alpha }$ /Fe] and [Zn/H] as a proxy for [Fe/H].
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{aa3930f1.eps}}\end{figure}$	Figure 1: Coadded UVES spectra of the 10 Sgr giants analysed in this paper. The labels on the right denote the star number, those on the left the [FeI/H].
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{aa3930f2.eps}}\end{figure}$	Figure 2: The metallicity distribution of the 10 Sgr giants of the present paper and the two of Bonifacio et al. (2000).
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{aa3930f3.eps}}\end{figure}$	Figure 3: The colour-magnitude diagram of field 1 of Marconi et al. (1998), the reddening adopted is E(V-I)=0.22, A_V=0.55 and the distance modulus (m-M)=16.95, from the same reference. The stars observed by UVES are shown with larger symbols, two Padova isochrones (Girardi et al. 2002), covering the range in Z found for the program stars are shown.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{aa3930f4.eps}}\end{figure}$	Figure 4: The [Fe/H], [ ${\alpha }$ /Fe] diagram for the programme stars (filled symbols. The 5 stars of M54 studied by Brown et al. (1999) are shown as open symbols. [ ${\alpha }$ /Fe] in this plot is defined as $1\over 3$ ([Mg/Fe]+[Si/Fe]+[Ca/Fe]).
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