Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0273F1.ps} \end{figure}$ Figure 1: Normalized UVES spectra of Q0100+13 showing the DLA Ly $\alpha$ and Ly $\beta$ profiles with the Voigt profile fits. The vertical bar corresponds to the wavelength centroid of the component used for the best fit, z = 2.309027. The measured H I column density is $\log N(H {\sc i})~= 21.37\pm 0.08$ .
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In the text

$\begin{figure} \par\includegraphics[width=14.6cm,clip]{0273F2.ps} \end{figure}$ Figure 2: Velocity plots of the metal line transitions (normalized intensities shown by dots with $1 \sigma$ error bars) for the DLA toward Q0100+13. The zero velocity is fixed at z = 2.309027. For this and all the following figures with velocity plots, the vertical bars mark the positions of the fitted velocity components and the symbols $\oplus$ correspond to the telluric lines. The letter K refers to the Keck spectra.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0273F3.ps} \end{figure}$ Figure 3: Same as Fig. 1 but for Q1331+17. The vertical bars correspond to the wavelength centroids of the components used for the best fit, z = 1.776724 and z = 1.786345, referring to the DLA system and an additional absorber, respectively. The measured H I column densities are $\log N$ (H I $) = 21.14\pm 0.08$ and $19.80\pm 0.10$ , respectively.
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In the text

$\begin{figure} \par\includegraphics[width=16.1cm,clip]{0273F4.ps} \end{figure}$ Figure 4: Same as Fig. 2 for the DLA toward Q1331+17. The zero velocity is fixed at z = 1.776370.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0273F5.ps} \end{figure}$ Figure 5: Same as Fig. 1 but for Q2231-00. The vertical bar corresponds to the wavelength centroid of the component used for the best fit left as a free parameter, z = 2.065774. The measured H I column density is $\log N$ (H I) $= 20.53\pm 0.08$ .
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In the text

$\begin{figure} \par\includegraphics[width=16.6cm,clip]{0273F6.ps} \end{figure}$ Figure 6: Same as Fig. 2 for the DLA toward Q2231-00. The zero velocity is fixed at z = 2.066161.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0273F7.ps} \end{figure}$ Figure 7: Same as Fig. 1 but for Q2343+12. The Voigt fit was performed with the H I column density measured by D'Odorico et al. (2002, Sect. 3.2) from the Ly $\alpha$ line ( $\log N$ (H I) $= 20.35\pm 0.05$ ). The vertical bar corresponds to the wavelength centroid of the component used for the best fit by these authors, z = 2.43125.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{0273F8.ps} \end{figure}$ Figure 8: Same as Fig. 2 for the DLA toward Q2343+12. The zero velocity is fixed at z = 2.429942.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{0273F9.ps} \end{figure}$ Figure 9: The nucleosynthetic abundance pattern of the DLA at $z_{\rm abs} = 2.309$ toward Q0100+13. The dust-corrected elemental abundances are represented on a logarithmic scale, where hydrogen is defined to have $\epsilon ({\rm H}) = 12$ and in a general way, for any element X, $\epsilon({\rm X}) = \log ({\rm X/H}) + 12$ . They are compared with the solar abundance pattern from Grevesse & Sauval (1998) shown by the solid line and scaled to match the observed sulfur metallicity, [S/H] = -1.44, of the DLA system. The dust corrections were obtained via the Vladilo (2002a,b) method. The filled circles correspond to the dust-corrected abundances obtained with the E00 dust correction model and the open squares to the dust-corrected abundances obtained with the E11 dust correction model.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{0273F10.ps} \end{figure}$ Figure 10: The nucleosynthetic abundance pattern of the DLA at $z_{\rm abs} = 1.776$ toward Q1331+17. The solar values were scaled to match the observed sulfur metallicity, [S/H] = -1.26. Same as Fig. 9.
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In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{0273F11.ps}\end{figure}$ Figure 11: The nucleosynthetic abundance pattern of the DLA at $z_{\rm abs} = 2.066$ toward Q2231-00. The solar values were scaled to match the dust-corrected silicon metallicity, [Si/H] $_{\rm cor} = -0.78$ . Same as Fig. 9.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0273F12.eps} \end{figure}$ Figure 12: Observed and predicted [Ni/Fe] versus [Fe/H] distributions in the solar neighborhood for two different nucleosynthetic prescriptions for the production of Ni. The dashed line corresponds to the model with $\beta = 0.0065$ and the solid line to the model with $\beta = 0.0049$ , where $\beta$ is a multiplicative factor between the Fe and Ni yields (see text). The solid squares are the data from Ryan et al. (1996), the open circles the ones from Chen et al. (2000), the open triangles the ones from Jehin et al. (1999), the filled triangles the ones from Stephens (1999), the filled circles the ones from McWillian et al. (1995), and the open squares the ones from Gratton & Sneden (1991).
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In the text

$\begin{figure} \par\includegraphics[width=15.2cm,clip]{0273F13.eps}\end{figure}$ Figure 13: Observed and predicted abundance ratios versus metallicity for the DLA at $z_{\rm abs} = 2.309$ toward Q0100+13. The thick dashed-dotted curves correspond to the "spiral'' model at R = 8 kpc. The thin solid curves correspond to the "dwarf irregular'' model with a single burst of SF occurring at $t_{\rm b} = 2$ Gyr and with a star formation efficiency $\nu = 0.9$ Gyr^-1 and a duration $\Delta t = 0.07$ Gyr. In this and all the following figures, the open squares represent the measured abundance ratio measurements, and the filled triangles and the filled squares represent the abundance ratios corrected for dust depletion according to the Vladilo (2002a) method using the models E00 and E11, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=15.2cm,clip]{0273F14.eps} \end{figure}$ Figure 14: Observed and predicted abundance ratios versus redshift for the DLA at $z_{\rm abs} = 2.309$ toward Q0100+13. The thick dashed-dotted curves correspond to the "spiral'' model at R = 8 kpc and a redshift of formation $z_{\rm f} = 2.5$ . For the definition of symbols, see Fig. 13.
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In the text

$\begin{figure} \par\includegraphics[width=15.2cm,clip]{0273F15.eps} \end{figure}$ Figure 15: Observed and predicted abundance ratios versus metallicity for the DLA at $z_{\rm abs} = 1.776$ toward Q1331+17. The thick dashed-dotted curves correspond to the "spiral'' model at R = 16 kpc and the thin solid curves correspond to the "dwarf irregular'' model with a continuous SF at an efficiency $\nu = 0.03$ Gyr^-1. For the definition of symbols, see Fig. 13.
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In the text

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{0273F16.eps} \end{figure}$ Figure 16: Observed and predicted abundance ratios versus redshift for the DLA at $z_{\rm abs} = 1.776$ toward Q1331+17. The thick dashed-dotted curves correspond to the "spiral'' model at R = 16 kpc and a redshift of formation $z_{\rm f} = 2.8$ . The thin solid curves correspond to the "dwarf irregular'' model with a continuous SF at an efficiency $\nu = 0.03$ Gyr^-1 and a redshift of formation $z_{\rm f} = 10$ . For the definition of symbols, see Fig. 13.
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In the text

$\begin{figure} \par\includegraphics[width=15.2cm,clip]{0273F17.eps} \end{figure}$ Figure 17: Observed and predicted abundance ratios versus metallicity for the DLA at $z_{\rm abs} = 2.066$ toward Q2231-00. The thick dashed-dotted curves correspond to the "spiral'' model at R = 2 kpc. The thin solid curves correspond to the "dwarf irregular'' model with a single burst of SF occurring at $t_{\rm b} = 0.5$ Gyr and with a star formation efficiency $\nu = 4.2$ Gyr^-1 and a duration $\Delta t = 0.1$ Gyr. For the definition of symbols, see Fig. 13.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0273F1.ps} \end{figure}$	Figure 1: Normalized UVES spectra of Q0100+13 showing the DLA Ly $\alpha$ and Ly $\beta$ profiles with the Voigt profile fits. The vertical bar corresponds to the wavelength centroid of the component used for the best fit, z = 2.309027. The measured H I column density is $\log N(H {\sc i})~= 21.37\pm 0.08$ .
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0273F3.ps} \end{figure}$	Figure 3: Same as Fig. 1 but for Q1331+17. The vertical bars correspond to the wavelength centroids of the components used for the best fit, z = 1.776724 and z = 1.786345, referring to the DLA system and an additional absorber, respectively. The measured H I column densities are $\log N$ (H I $) = 21.14\pm 0.08$ and $19.80\pm 0.10$ , respectively.
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$\begin{figure} \par\includegraphics[width=16.1cm,clip]{0273F4.ps} \end{figure}$	Figure 4: Same as Fig. 2 for the DLA toward Q1331+17. The zero velocity is fixed at z = 1.776370.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0273F5.ps} \end{figure}$	Figure 5: Same as Fig. 1 but for Q2231-00. The vertical bar corresponds to the wavelength centroid of the component used for the best fit left as a free parameter, z = 2.065774. The measured H I column density is $\log N$ (H I) $= 20.53\pm 0.08$ .
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$\begin{figure} \par\includegraphics[width=16.6cm,clip]{0273F6.ps} \end{figure}$	Figure 6: Same as Fig. 2 for the DLA toward Q2231-00. The zero velocity is fixed at z = 2.066161.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0273F7.ps} \end{figure}$	Figure 7: Same as Fig. 1 but for Q2343+12. The Voigt fit was performed with the H I column density measured by D'Odorico et al. (2002, Sect. 3.2) from the Ly $\alpha$ line ( $\log N$ (H I) $= 20.35\pm 0.05$ ). The vertical bar corresponds to the wavelength centroid of the component used for the best fit by these authors, z = 2.43125.
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$\begin{figure} \par\includegraphics[width=16.4cm,clip]{0273F8.ps} \end{figure}$	Figure 8: Same as Fig. 2 for the DLA toward Q2343+12. The zero velocity is fixed at z = 2.429942.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{0273F10.ps} \end{figure}$	Figure 10: The nucleosynthetic abundance pattern of the DLA at $z_{\rm abs} = 1.776$ toward Q1331+17. The solar values were scaled to match the observed sulfur metallicity, [S/H] = -1.26. Same as Fig. 9.
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$\begin{figure} \par\includegraphics[width=13cm,clip]{0273F11.ps}\end{figure}$	Figure 11: The nucleosynthetic abundance pattern of the DLA at $z_{\rm abs} = 2.066$ toward Q2231-00. The solar values were scaled to match the dust-corrected silicon metallicity, [Si/H] $_{\rm cor} = -0.78$ . Same as Fig. 9.
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$\begin{figure} \par\includegraphics[width=15.2cm,clip]{0273F14.eps} \end{figure}$	Figure 14: Observed and predicted abundance ratios versus redshift for the DLA at $z_{\rm abs} = 2.309$ toward Q0100+13. The thick dashed-dotted curves correspond to the "spiral'' model at R = 8 kpc and a redshift of formation $z_{\rm f} = 2.5$ . For the definition of symbols, see Fig. 13.
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$\begin{figure} \par\includegraphics[width=15.2cm,clip]{0273F15.eps} \end{figure}$	Figure 15: Observed and predicted abundance ratios versus metallicity for the DLA at $z_{\rm abs} = 1.776$ toward Q1331+17. The thick dashed-dotted curves correspond to the "spiral'' model at R = 16 kpc and the thin solid curves correspond to the "dwarf irregular'' model with a continuous SF at an efficiency $\nu = 0.03$ Gyr^-1. For the definition of symbols, see Fig. 13.
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