All Figures

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig1.eps} \end{figure}$ Figure 1: The spectrum of Ruprecht 7-7 ( upper panel) and Berkeley 73-12 ( lower panel) in the wave-length interval 6000-6025 Å. Several spectral lines are identified.
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In the text

$\begin{figure} \includegraphics[width=11.5cm,clip]{8113fig2.eps} \end{figure}$ Figure 2: Revision of clusters' fundamental parameters. In each panel we show the isochrone solutions and indicate radial velocity members (filled squares) and non-members (empty squares) for a) Berkeley 75, b) Berkeley 25, c) Ruprecht 7, d) Ruprecht 4, and e) Berkeley 73, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig3.eps} \end{figure}$ Figure 3: The trend of $\alpha$ element abundances with metallicity. Open triangles indicate the five program clusters, while filled squares are additional anti-center clusters culled from the literature.The dashed line is a fit through the data.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig4.eps} \end{figure}$ Figure 4: Age metallicity distribution, with symbols as in Fig. 3. The dashed lines indicate the metallicity range of old open clusters in the Galactic disk, from Friel et al. (2002).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig5.eps} \end{figure}$ Figure 5: The radial abundance gradient from old open clusters in the distant anticenter direction. Symbols are as in Fig. 3. The solid line is the Friel et al. (2002) mean abundance gradient, while the dashed line is the gradient when outer disk clusters are added.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig6.eps} \end{figure}$ Figure 6: The radial abundance gradient of Mg, Si, Ca and Ti from old open clusters in the distant Galactic anti-center. The symbols are the same as those used in Fig. 3. On the right the gradient slopes in the range 12 to 22 kpc are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig7.eps} \end{figure}$ Figure 7: Distribution of star clusters according to their height above the Galactic plane and distance from the Galactic center. The various lines indicate the warping/flaring of the disk for $b=0\hbox {$^\circ $ }$ (solid line) and $\pm$ 1, 2 and 3 scale heights (dashed lines). Symbols are as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig8.eps} \end{figure}$ Figure 8: Rotational velocity of old open clusters in the third Galactic quadrant beyond 12 kpc from the Galactic center. The dashed line is the stellar disk rotation curve from Olling & Merrifield (2000), while the thick solid line is the typical location of old open clusters in the solar vicinity. Symbols are as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{8113fig9.eps} \end{figure}$ Figure 9: Location and kinematics of old open clusters in the Galactic anti-center. Superimposed are Peñarubia et al. (2005) models of the Monoceros Ring. The filled circle indicates Saurer 1, whilst the filled square Berkeley 29 and the filled triangle Tombaugh 2, previously indicated as MRi members.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig1.eps} \end{figure}$	Figure 1: The spectrum of Ruprecht 7-7 ( upper panel) and Berkeley 73-12 ( lower panel) in the wave-length interval 6000-6025 Å. Several spectral lines are identified.
Open with DEXTER

$\begin{figure} \includegraphics[width=11.5cm,clip]{8113fig2.eps} \end{figure}$	Figure 2: Revision of clusters' fundamental parameters. In each panel we show the isochrone solutions and indicate radial velocity members (filled squares) and non-members (empty squares) for a) Berkeley 75, b) Berkeley 25, c) Ruprecht 7, d) Ruprecht 4, and e) Berkeley 73, respectively.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig3.eps} \end{figure}$	Figure 3: The trend of $\alpha$ element abundances with metallicity. Open triangles indicate the five program clusters, while filled squares are additional anti-center clusters culled from the literature.The dashed line is a fit through the data.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig4.eps} \end{figure}$	Figure 4: Age metallicity distribution, with symbols as in Fig. 3. The dashed lines indicate the metallicity range of old open clusters in the Galactic disk, from Friel et al. (2002).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig5.eps} \end{figure}$	Figure 5: The radial abundance gradient from old open clusters in the distant anticenter direction. Symbols are as in Fig. 3. The solid line is the Friel et al. (2002) mean abundance gradient, while the dashed line is the gradient when outer disk clusters are added.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig6.eps} \end{figure}$	Figure 6: The radial abundance gradient of Mg, Si, Ca and Ti from old open clusters in the distant Galactic anti-center. The symbols are the same as those used in Fig. 3. On the right the gradient slopes in the range 12 to 22 kpc are indicated.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig7.eps} \end{figure}$	Figure 7: Distribution of star clusters according to their height above the Galactic plane and distance from the Galactic center. The various lines indicate the warping/flaring of the disk for $b=0\hbox {$^\circ $ }$ (solid line) and $\pm$ 1, 2 and 3 scale heights (dashed lines). Symbols are as in Fig. 3.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm]{8113fig8.eps} \end{figure}$	Figure 8: Rotational velocity of old open clusters in the third Galactic quadrant beyond 12 kpc from the Galactic center. The dashed line is the stellar disk rotation curve from Olling & Merrifield (2000), while the thick solid line is the typical location of old open clusters in the solar vicinity. Symbols are as in Fig. 3.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{8113fig9.eps} \end{figure}$	Figure 9: Location and kinematics of old open clusters in the Galactic anti-center. Superimposed are Peñarubia et al. (2005) models of the Monoceros Ring. The filled circle indicates Saurer 1, whilst the filled square Berkeley 29 and the filled triangle Tombaugh 2, previously indicated as MRi members.
Open with DEXTER