Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0332_f1.eps}\end{figure}$ Figure 1: Toomre diagram for the full stellar sample (102 stars). Thick and thin disk stars are marked by filled and open symbols, respectively. Stars that have been observed with SOFIN or UVES are marked by triangles and those from Bensby et al. (2003) are marked by circles. "Transition objects'' are marked by "open stars''.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0332_f2a.eps} \includegrap... ...]{0332_f2c.eps} \includegraphics[width=8.55cm,clip]{0332_f2d.eps} % \end{figure}$ Figure 2: $\rm [Fe {\sc i}/Fe {\sc ii}]$ versus $\rm [Fe/H]$ , $\log T_{\rm eff}$ , $\log g$ , and $\xi _{\rm t}$ . Thin and thick disk stars are marked by open and filled circles, respectively, and transition objects by "stars''.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332_f3.eps}\end{figure}$ Figure 3: Comparison between equivalent widths measured in the FEROS solar spectrum and the SOFIN and UVES solar spectra. The average differences are $\rm \langle {\it EW}_{FEROS}-{\it EW}_{SOFIN}\rangle = 1.02\pm 2.1$ mÅ (251 lines in common) and $\rm \langle {\it EW}_{FEROS}-{\it EW}_{UVES}\rangle = 0.58\pm 1.9$ mÅ. (165 lines in common)
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0332_f4a.eps}\hspace*{5mm} \includegraphics[width=8.2cm,clip]{0332_f4b.eps}\end{figure}$ Figure 4: Synthetic and observed solar (FEROS) spectra for: a) the Eu II at 4129 Å, and b) the Eu II line at 6645 Å. Five synthetic spectra with different Eu abundances, in steps of 0.03 dex have been plotted for each line. The hyperfine components for the two Eu isotopes are indicated as well as other important lines in the regions. The bottom panels shows the differences between the observed and synthetic spectra.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0332_f5.eps}\end{figure}$ Figure 5: Comparison of our abundances with Reddy et al. (2003) for four stars in common. The differences for each individual star are marked by symbols as indicated in the figure. The differences are defined as $\rm [X/Fe]_{This~~Work} - [X/Fe]_{Reddy}$ except for Fe which is $\rm [Fe/H]_{This~~Work} - [Fe/H]_{Reddy}$ . Note that for four elements, Ca, Ti, Cr, Ni, the differences between two stars are identical and hence we only see three symbols.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0332_f6.eps}\end{figure}$ Figure 6: Comparison of abundances for eight stars that we have in common with the studies by Mashonkina & Gehren (2000, 2001) and Mashonkina et al. (2003). The differences are defined as our abundances minus theirs. Note that the Mashonkina studies have no Eu abundances for two of the stars: HIP 93185 and HIP 107975.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332_f7.eps}\end{figure}$ Figure 7: [Fe/H] versus age for the 36 stars from this study and the 66 stars from Bensby et al. (2003). Thin disk and thick disk stars are marked by open and filled circles, respectively. Transition objects are marked by asterisks.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.3cm,clip]{0332_f8a.eps}\hspace... ...hspace{8mm} \includegraphics[width=8.3cm,clip]{0332_f8j.eps} } \par\end{figure}$ Figure 8: Elemental abundances relative to Fe. Dotted lines indicate solar values. Thin disk and thick disk stars are marked by empty and filled circles, respectively. Stars from Bensby et al. (2003, 2004a) are marked by circles and stars from the new northern sample by triangles. Transition objects are marked by asterisks.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332_f9.eps}\end{figure}$ Figure 9: [O/Fe] versus $Z_{\rm max}$ for the 36 stars from this study and the 66 stars from Bensby et al. (2003). Thin disk and thick disk stars are marked by empty and filled circles, respectively. Transition objects are marked by asterisks.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0332_f10.eps}\end{figure}$ Figure 10: Abundance trends in the thick disk for oxygen. The thick disk sample has been divided into two sub-groups: stars that have $Z_{\rm max}>500$ pc (open squares); and stars that have $Z_{\rm max} \leq 500$ pc (open stars).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.3cm,clip]{0332f11a.eps}\hspace... ...ps}\hspace{8mm} \includegraphics[width=8.3cm,clip]{0332f11f.eps} } \end{figure}$ Figure 11: Elemental abundances relative to Fe. Dotted lines indicate solar values. Thin disk and thick disk stars are marked by empty and filled circles, respectively. Transition objects are marked by asterisks.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0332f12.eps}\end{figure}$ Figure 12: An illustration of the relative contributions from the r- and s-process to the elements Eu and Ba. The dotted line shows the pure r-process contribution to Eu and Ba while the full line shows the solar system mix of r- and s-process contributions (Arlandini et al. 1999). Thin and thick disk stars are marked by open and filled circles, respectively. Transition objects are marked by asterisks ( $\ast$ ), and "open stars'' data from Burris et al. (2000).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332f13.eps}\end{figure}$ Figure 13: [Eu/Ba] versus [Fe/H]. The dashed lines show the pure r-process ratio which is [Eu/Ba] = 0.7 and has been calculated from the yields given in Arlandini et al. (1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332f14.eps}\end{figure}$ Figure 14: [Y/Ba] versus [O/H] for the a) thick disk stars and in b) for the thin disk stars (with the four "transition'' objects included as well).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332fA1.eps}\end{figure}$ Figure A.1: CMD for the full stellar sample (12 634 stars).

In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{0332fA2.eps}\end{figure}$ Figure A.2: CMDs for different interval of ${\it TD}/D$ when changing the local density of thick disk stars (2%, 6%, 10%, and 14%). The number of stars in each CMD is given in Table A.2.

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0332_f1.eps}\end{figure}$	Figure 1: Toomre diagram for the full stellar sample (102 stars). Thick and thin disk stars are marked by filled and open symbols, respectively. Stars that have been observed with SOFIN or UVES are marked by triangles and those from Bensby et al. (2003) are marked by circles. "Transition objects'' are marked by "open stars''.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0332_f2a.eps} \includegrap... ...]{0332_f2c.eps} \includegraphics[width=8.55cm,clip]{0332_f2d.eps} % \end{figure}$	Figure 2: $\rm [Fe {\sc i}/Fe {\sc ii}]$ versus $\rm [Fe/H]$ , $\log T_{\rm eff}$ , $\log g$ , and $\xi _{\rm t}$ . Thin and thick disk stars are marked by open and filled circles, respectively, and transition objects by "stars''.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332_f3.eps}\end{figure}$	Figure 3: Comparison between equivalent widths measured in the FEROS solar spectrum and the SOFIN and UVES solar spectra. The average differences are $\rm \langle {\it EW}_{FEROS}-{\it EW}_{SOFIN}\rangle = 1.02\pm 2.1$ mÅ (251 lines in common) and $\rm \langle {\it EW}_{FEROS}-{\it EW}_{UVES}\rangle = 0.58\pm 1.9$ mÅ. (165 lines in common)
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0332_f6.eps}\end{figure}$	Figure 6: Comparison of abundances for eight stars that we have in common with the studies by Mashonkina & Gehren (2000, 2001) and Mashonkina et al. (2003). The differences are defined as our abundances minus theirs. Note that the Mashonkina studies have no Eu abundances for two of the stars: HIP 93185 and HIP 107975.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332_f7.eps}\end{figure}$	Figure 7: [Fe/H] versus age for the 36 stars from this study and the 66 stars from Bensby et al. (2003). Thin disk and thick disk stars are marked by open and filled circles, respectively. Transition objects are marked by asterisks.
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$\begin{figure} \par\mbox{\includegraphics[width=8.3cm,clip]{0332_f8a.eps}\hspace... ...hspace{8mm} \includegraphics[width=8.3cm,clip]{0332_f8j.eps} } \par\end{figure}$	Figure 8: Elemental abundances relative to Fe. Dotted lines indicate solar values. Thin disk and thick disk stars are marked by empty and filled circles, respectively. Stars from Bensby et al. (2003, 2004a) are marked by circles and stars from the new northern sample by triangles. Transition objects are marked by asterisks.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332_f9.eps}\end{figure}$	Figure 9: [O/Fe] versus $Z_{\rm max}$ for the 36 stars from this study and the 66 stars from Bensby et al. (2003). Thin disk and thick disk stars are marked by empty and filled circles, respectively. Transition objects are marked by asterisks.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0332_f10.eps}\end{figure}$	Figure 10: Abundance trends in the thick disk for oxygen. The thick disk sample has been divided into two sub-groups: stars that have $Z_{\rm max}>500$ pc (open squares); and stars that have $Z_{\rm max} \leq 500$ pc (open stars).
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$\begin{figure} \par\mbox{\includegraphics[width=8.3cm,clip]{0332f11a.eps}\hspace... ...ps}\hspace{8mm} \includegraphics[width=8.3cm,clip]{0332f11f.eps} } \end{figure}$	Figure 11: Elemental abundances relative to Fe. Dotted lines indicate solar values. Thin disk and thick disk stars are marked by empty and filled circles, respectively. Transition objects are marked by asterisks.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332f13.eps}\end{figure}$	Figure 13: [Eu/Ba] versus [Fe/H]. The dashed lines show the pure r-process ratio which is [Eu/Ba] = 0.7 and has been calculated from the yields given in Arlandini et al. (1999).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0332f14.eps}\end{figure}$	Figure 14: [Y/Ba] versus [O/H] for the a) thick disk stars and in b) for the thin disk stars (with the four "transition'' objects included as well).
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