Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=16cm,clip]{4670.f1.ps} \end{figure}$ Figure 1: BVRIJHK light curves of GRB 030323. The magnitudes have been corrected for the Galactic extinction of E_B-V=0.049 (Schlegel et al. 1998); note that in Table 2 they have not been corrected. The dashed lines are simple power law fits to the observations before day 2, and extrapolated to later epochs.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4670.f2.ps} \end{figure}$ Figure 2: Milky Way (MW), Large- and Small Magellanic Cloud (LMC and SMC) extinction-curve fits to the spectral energy distribution (SED) of the afterglow at day 2.44 after the burst, assuming that the intrinsic SED is a power law with slope $\beta = -0.28$ (see text). These fits result in the conservative upper limits to the host-galaxy extinction: $A_{\rm V}{\rm (MW)}<0.50$ mag, $A_{\rm V}{\rm (LMC)}<0.25$ mag and $A_{\rm V}{\rm (SMC)}<0.16$ mag.
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In the text

$\begin{figure} \par\includegraphics[width=21.5cm,height=17cm,clip]{4670.f3.ps} \end{figure}$ Figure 3: Combined 1400V+1200R spectrum of GRB 030323, including the Poisson error spectrum. The inset on the left shows the normalized spectrum with the hydrogen column fit to the damped Ly $\alpha$ line, including the 1 $\sigma$ errors. This column density is currently the highest for any DLA system measured using Ly $\alpha$ in absorption (see Fig. 4). Redward of Ly $\alpha$ we detect numerous metal-absorption lines (see Table 3), whose average redshift (in this high-resolution spectrum) is $z=3.3716 \pm 0.0005$ . In the inset on the right, we zoom in on the C IV doublet, which is split into separate components. In the Ly $\alpha$ trough, Ly $\alpha$ is detected in emission. Lines that could not be identified, atmospheric absorption lines (indicated with an $\oplus$ ), and lines belonging to the tentative absorber at z=1.41, are indicated with a dashed line instead of a solid one.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4670.f4.ps} \end{figure}$ Figure 4: Histogram of the column densities of DLA systems measured through the damping wings of Ly $\alpha$ discovered in the spectrum of a background QSO (compilation taken from Curran et al. 2002). The shaded histogram shows measurements in GRBs for which the redshift was large enough to detect Ly $\alpha$ . Out of 7 GRBs, 5 show neutral hydrogen column densities above the DLA definition of $2\times 10^{20}$ atoms cm^-2 ( $\log~ N(\mbox{H {\sc i}})=20.3$ ). The host of GRB 030323 contains a column density larger than in any observed (GRB- or QSO-) DLA system.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4670.f5.ps} \end{figure}$ Figure 5: Simultaneous one-component fit to low-ionization metal lines with little saturation.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4670.f6.ps} \end{figure}$ Figure 6: Comparison of the metallicities of a sample of QSO-DLAs, taken from Prochaska et al. (2003a) (open circles), with the two GRBs for which a metallicity has been determined (solid triangles): GRB 000926 and GRB 030323 (this paper). The GRB hosts are located at the metal-rich end of the QSO-DLA distribution.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4670.f7a.ps}\includegraphics[width=8.8cm,clip]{4670.f7b.ps} \end{figure}$ Figure 7: HST/ACS F606W imaging of the field of GRB 030323. On the left panel the $1\hbox {$^\prime $ }\times 1\hbox {$^\prime $ }$ field surrounding the burst is shown, whose location is indicated by the cross hair. On the right panel the central $5\hbox {$^{\prime \prime }$ }\times 5\hbox {$^{\prime \prime }$ }$ region is shown, where in this case the image has been median filtered using a box with 3 pixels on a side. The position of the early afterglow and its uncertainty (0 $.\!\!^{\prime\prime}$ 06 in radius) is depicted by the black circle. At a distance of 0 $.\!\!^{\prime\prime}$ 14 (1 kpc), an extended object is detected. This is the probable host galaxy of GRB 030323 for which we measure ${\it AB}(F606W)=28.0 \pm 0.3$ mag.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{4670.f1.ps} \end{figure}$	Figure 1: BVRIJHK light curves of GRB 030323. The magnitudes have been corrected for the Galactic extinction of E_B-V=0.049 (Schlegel et al. 1998); note that in Table 2 they have not been corrected. The dashed lines are simple power law fits to the observations before day 2, and extrapolated to later epochs.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4670.f5.ps} \end{figure}$	Figure 5: Simultaneous one-component fit to low-ionization metal lines with little saturation.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{4670.f6.ps} \end{figure}$	Figure 6: Comparison of the metallicities of a sample of QSO-DLAs, taken from Prochaska et al. (2003a) (open circles), with the two GRBs for which a metallicity has been determined (solid triangles): GRB 000926 and GRB 030323 (this paper). The GRB hosts are located at the metal-rich end of the QSO-DLA distribution.
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