Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{3007fig1.ps}\par\vspace*{1mm... ...p]{3007fig2.ps}\par\includegraphics[width=7.8cm,clip]{3007fig3.ps} \end{figure}$ Figure 1: Upper panel: section of the LR afterglow spectrum showing the DLA line at the GRB redshift, $z_{\rm abs}=4.048$ . Overlaid is the best fitting DLA profile, corresponding to $\log N$ (H I) = 20.85 $\pm$ 0.10. Middle panel: fits to the O I, O I*, O I**, Si II, Si II*, and S II lines in the MR spectrum. The zero-point for the velocity scale is $z_{\rm abs}=4.048$ . Lower panel: the likely H₂ lines at the GRB redshift in the MR spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3007fig4.ps} \end{figure}$ Figure 2: Metallicity as a function of redshift for different classes of objects. The black circles are the measurements for GRBs from Table 2 (GRB 060206 is also marked with $\times$ ). The open triangles show the metallicity of three low-z GRB host galaxies (Sollerman et al. 2005). The squares and the dashed line represent the column density weighted metallicity evolution derived by Zwaan et al. (2005, their Fig. 22). The small dots with no error-bars are measurements for 121 DLAs from Prochaska et al. (2003). The hatched region indicates the metallicity above which GRBs cannot form in the collapsar models.
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In the text