All Figures

$\begin{figure} \par\includegraphics[angle=-90, width=13cm,clip]{1512fig01.ps} \end{figure}$ Figure 1: Spectral region near the Ba II line at 6141.73 Å for our averaged spectra (UVES, VLT-UT2) in 47 Tuc and NGC 6397. Vertical offsets have been added in order to avoid any overlap and to compare the line intensities between these two clusters, and in each cluster between stars near the TO point and stars at the base of the RGB. Line identification is shown for the Ba II line.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.8cm]{1512fig02.ps}$\ $\space \... ...2fig06.ps}$\ $\space \includegraphics[width=5.8cm]{1512fig07.ps} } \end{figure}$ Figure 2: Superimposition of spectra in 47 Tuc and NGC 6397. Panel a): Y II ( $\lambda$ 3950.36) line in the subgiants of 47 Tuc. Panels b) and c): Sr II ( $\lambda$ 4215.52) line in NGC 6397 (subgiants and TO stars). Panels d) and e): Ba II ( $\lambda$ 6141.73) line in the subgiants of 47 Tuc and NGC 6397. Panel f): Eu II ( $\lambda$ 4219.70) line in the subgiants of 47 Tuc.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm]{1512fig08.ps}\\ \vspace{0.14cm}... ....ps}\\ \vspace{0.14cm} \includegraphics[width=8.4cm]{1512fig11.ps} \end{figure}$ Figure 3: [X/Fe] mean ratios for the n-capture elements in Galactic globular clusters compared to field stars. Filled squares ( $\blacksquare$ ): subgiants in 47 Tuc, NGC 6752 and NGC 6397. Filled triangles ( $\blacktriangle$ ): TO stars in the three clusters (a line joins the two mean points for each globular cluster). Open stars ( $\star$ ): our sample of field halo stars. Small crosses ( +, $\times$ , $\ast$ ): other field stars taken from the literature (Fulbright 2000; Mashonkina et al. 2003; Mashonkina & Gehren 2001; Burris et al. 2000). Filled circles ( $\bullet$ ): other Galactic globular clusters (with increasing metallicity: M 15, M 92, NGC 6287, NGC 6293, NGC 6541, M 13, M 79, M 3, NGC 288, NGC 362, M 5, M 4 and M 71); abundances are from François (1991), Armosky et al. (1994), Shetrone (1996), Sneden et al. (1997), Ivans et al. (1999,2001), Shetrone & Keane (2000), Lee & Carney (2002), Ramírez & Cohen (2003) and Sneden et al. (2004).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{1512fig12.ps}\\ \vspace{0.1cm} \includegraphics[width=8.5cm]{1512fig13.ps} \end{figure}$ Figure 4: Comparison of the [Ba/Eu] (Panel a)) and [Sr/Ba] (Panel b)) ratios for Galactic globular clusters and field halo stars (same symbols than in Fig. 3).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90, width=13cm,clip]{1512fig01.ps} \end{figure}$	Figure 1: Spectral region near the Ba II line at 6141.73 Å for our averaged spectra (UVES, VLT-UT2) in 47 Tuc and NGC 6397. Vertical offsets have been added in order to avoid any overlap and to compare the line intensities between these two clusters, and in each cluster between stars near the TO point and stars at the base of the RGB. Line identification is shown for the Ba II line.
Open with DEXTER

$\begin{figure} \par\mbox{\includegraphics[width=5.8cm]{1512fig02.ps}$\ $\space \... ...2fig06.ps}$\ $\space \includegraphics[width=5.8cm]{1512fig07.ps} } \end{figure}$	Figure 2: Superimposition of spectra in 47 Tuc and NGC 6397. Panel a): Y II ( $\lambda$ 3950.36) line in the subgiants of 47 Tuc. Panels b) and c): Sr II ( $\lambda$ 4215.52) line in NGC 6397 (subgiants and TO stars). Panels d) and e): Ba II ( $\lambda$ 6141.73) line in the subgiants of 47 Tuc and NGC 6397. Panel f): Eu II ( $\lambda$ 4219.70) line in the subgiants of 47 Tuc.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm]{1512fig12.ps}\\ \vspace{0.1cm} \includegraphics[width=8.5cm]{1512fig13.ps} \end{figure}$	Figure 4: Comparison of the [Ba/Eu] (Panel a)) and [Sr/Ba] (Panel b)) ratios for Galactic globular clusters and field halo stars (same symbols than in Fig. 3).
Open with DEXTER