Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{0084fig1.ps} \end{figure}$ Figure 1: Samples of the spectra. The spectra have been shifted to the 0 radial velocity and an offset in flux has been added for best clarity of the sample. Some Lick-index passband are indicated at the bottom of the panel.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0084fig2.ps} \end{figure}$ Figure 2: Velocity distributions of the globular clusters. The bin size is 20 km s^-1. The number on each pannel corresponds to the globular cluster ID.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{0084fig3.ps} \end{figure}$ Figure 3: Main panel: position of the bona fide globular clusters with overplotted isovelocity contours from Chemin et al. (2006). Arrow indicates the north and East is on the left. The sub panels on the bottom as well as on the right show the globular cluster velocity projections of the main panel as function of RA and Dec respectively. Blue lines indicate isovelocity lines for 480 km s^-1 and 452 km s^-1. The straight line crossing the main panel has the purpose of illustrating the velocity changes when it is projected as function of RA and Dec on the sub panels. Numbers next to the isovelocity contours indicate the velocity in km s^-1.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.6cm,clip]{0084fig4.ps} \includ... ...s} \includegraphics[width=5.6cm,clip]{0084fig8.ps}\hspace*{2.8cm}} \end{figure}$ Figure 4: Age diagnostic plots. The over-plotted grid corresponds to SSP model from Thomas et al. (2004) for [ $\alpha /$ Fe] = 0.0. Doted lines correspond to metallicities [Z/H] = -2.25, -1.35, -0.33, 0.0, 0.35 and, 0.67 dex. Solid lines correspond to ages of 1, 2, 3, 5, 10 and 15 Gyr.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.8cm,clip]{0084fig9.ps} \includ... ...ip]{0084fi10.ps} \includegraphics[width=5.8cm,clip]{0084fi11.ps} } \end{figure}$ Figure 5: Left panel: iron $\langle$ Fe $\rangle$ as function of Mg2. Central panel: Fe₅₂₇₈ index versus Mgb. Right panel: Fe₅₃₃₅ index versus Mgb.
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In the text

$\begin{figure} \par\includegraphics[width=15cm]{0084fi12.ps}\end{figure}$ Figure 6: Comparison of Worthey Lick/IDS indices with the one measured by us. Lines represent the one-to-one comparison.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0084fig1.ps} \end{figure}$	Figure 1: Samples of the spectra. The spectra have been shifted to the 0 radial velocity and an offset in flux has been added for best clarity of the sample. Some Lick-index passband are indicated at the bottom of the panel.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0084fig2.ps} \end{figure}$	Figure 2: Velocity distributions of the globular clusters. The bin size is 20 km s^-1. The number on each pannel corresponds to the globular cluster ID.
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$\begin{figure} \par\mbox{\includegraphics[width=5.6cm,clip]{0084fig4.ps} \includ... ...s} \includegraphics[width=5.6cm,clip]{0084fig8.ps}\hspace*{2.8cm}} \end{figure}$	Figure 4: Age diagnostic plots. The over-plotted grid corresponds to SSP model from Thomas et al. (2004) for [ $\alpha /$ Fe] = 0.0. Doted lines correspond to metallicities [Z/H] = -2.25, -1.35, -0.33, 0.0, 0.35 and, 0.67 dex. Solid lines correspond to ages of 1, 2, 3, 5, 10 and 15 Gyr.
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$\begin{figure} \par\mbox{\includegraphics[width=5.8cm,clip]{0084fig9.ps} \includ... ...ip]{0084fi10.ps} \includegraphics[width=5.8cm,clip]{0084fi11.ps} } \end{figure}$	Figure 5: Left panel: iron $\langle$ Fe $\rangle$ as function of Mg2. Central panel: Fe₅₂₇₈ index versus Mgb. Right panel: Fe₅₃₃₅ index versus Mgb.
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$\begin{figure} \par\includegraphics[width=15cm]{0084fi12.ps}\end{figure}$	Figure 6: Comparison of Worthey Lick/IDS indices with the one measured by us. Lines represent the one-to-one comparison.
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