All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig1.ps} \end{figure}$ Figure 1: 15 min exposure $K_{\rm s}$ -band SofI image obtained on May 29, 2003. The initial and revised HETE-2 SXC confidence circles are indicated together with the positions of two X-ray sources detected by Chandra (see text). North is up and East to the left.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig2.ps} \end{figure}$ Figure 2: Combined late time VLT/ISAAC $J_{\rm s}$ -band image from September 2003 with a total exposure of 264 min. The position of GRB 030528 is marked by the circle, while the letters (from A-G) label the 2MASS stars used for the flux calibration (see also Table 3). The image size is $\sim$ $75\hbox {$^{\prime \prime }$ }\times 75$ $^{\prime \prime }$ and North is up and East to the left.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1545fig3.ps} \end{figure}$ Figure 3: Foreground extinction corrected magnitudes in I (marked by a cross), J/ $J_{\rm s}$ (triangle/filled triangle), H (star) and K/ $K_{\rm s}$ (square/filled square). For J and H only upper limits exist for $t\sim 1.7$ days. The $K_{\rm s}$ -band upper limit at t=5.8 days is from observations with the WIRC at the Palomar 200-inch Hale telescope (Bogosavljevic et al. 2003) and the I-band upper limit at t=7.6 days from the 1.3 m McGraw-Hill telescope at the MDM observatory (Mirabal & Halpern 2003). The dotted line corresponds to a decay with a power law slope of $\alpha =1.2$ with the host magnitude fixed to K=19.6.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig4.ps} \end{figure}$ Figure 4: 116 min exposure K-band image taken with the 3.8 m UKIRT equipped with the UFTI on June 12, 14.9 days after the prompt emission. North is up and East to the left. The potential host galaxy (RA(2000 $)=\rm 17^h04^m00.3^s$ , Dec(2000 $)=-22\degr37\hbox{$^\prime$ }10\hbox{$^{\prime\prime}$ }$ of GRB 030528 shows an elongation in East-West direction.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig5.ps} \end{figure}$ Figure 5: Results of the photometric redshift fit of C 1 with template spectra following Bender et al. (2001). Upper panel: the probability density of the redshift of the object for late type galaxies. The probability for the redshift drops above $z\sim$ 4 and has several maxima below. Lower panel: the photometric measurements (points) together with the best fitting late type galaxy at a redshift of z=0.2 (solid line). Empty circles correspond to the expected magnitudes in the observed photometric bands.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig6.ps} \end{figure}$ Figure 6: Same as Fig. 5 for early type galaxies.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1545fig7.ps} \end{figure}$ Figure 7: Published K-band magnitudes of all GRB afterglows observed by May 2004 (dots; references listed in Appendix B) in comparison to the faint K-band afterglow of GRB 030528 (filled squares). Data are not corrected for Galactic extinction. The straight lines indicate a decay with a slope $\alpha =1.2$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig8.ps} \end{figure}$ Figure A.1: V-band image of the field around C 10 taken with the D1m54 in June 2004. Coincident with the Chandra position (error circle as given in Butler et al. 2003a) we detect a point like source. North is up and East to the left.

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig9.ps} \end{figure}$ Figure A.2: Same as Fig. 5 for C 10. Upper panel: a global maximum of the probability density is evident at z<0.2. Lower panel: best fitting (late type) galaxy model (solid line) and best fitting (G0) stellar spectrum (dotted line).

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig1.ps} \end{figure}$	Figure 1: 15 min exposure $K_{\rm s}$ -band SofI image obtained on May 29, 2003. The initial and revised HETE-2 SXC confidence circles are indicated together with the positions of two X-ray sources detected by Chandra (see text). North is up and East to the left.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig2.ps} \end{figure}$	Figure 2: Combined late time VLT/ISAAC $J_{\rm s}$ -band image from September 2003 with a total exposure of 264 min. The position of GRB 030528 is marked by the circle, while the letters (from A-G) label the 2MASS stars used for the flux calibration (see also Table 3). The image size is $\sim$ $75\hbox {$^{\prime \prime }$ }\times 75$ $^{\prime \prime }$ and North is up and East to the left.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig4.ps} \end{figure}$	Figure 4: 116 min exposure K-band image taken with the 3.8 m UKIRT equipped with the UFTI on June 12, 14.9 days after the prompt emission. North is up and East to the left. The potential host galaxy (RA(2000 $)=\rm 17^h04^m00.3^s$ , Dec(2000 $)=-22\degr37\hbox{$^\prime$ }10\hbox{$^{\prime\prime}$ }$ of GRB 030528 shows an elongation in East-West direction.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1545fig6.ps} \end{figure}$	Figure 6: Same as Fig. 5 for early type galaxies.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1545fig7.ps} \end{figure}$	Figure 7: Published K-band magnitudes of all GRB afterglows observed by May 2004 (dots; references listed in Appendix B) in comparison to the faint K-band afterglow of GRB 030528 (filled squares). Data are not corrected for Galactic extinction. The straight lines indicate a decay with a slope $\alpha =1.2$ .
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