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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{0921FIG1.eps} } \end{figure}$ Figure 1: The contents of the BeppoSAX error box for the GRB 001109 field. This R band image was taken with the 2.56 NOT (+ALFOSC) on 14.0524-14.0734 UT August 2001. The source in between ticks is the galaxy coincident with the VLA J1830+5518 and consistent with the position of the X-ray afterglow. The numbered stars are the secondary standards indicated in Table 2. The large circle represents the refined WFC error box (Gandolfi et al. 2000b) and the small one the NFI error circle (Amati et al. 2000). The field of view covered by the figure is 5.1 $^\prime$ $\times$ 4.3 $^\prime$ . North is upwards and East is leftwards.
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In the text

$\begin{figure} \par {\includegraphics[width=7.9cm,clip]{0921FIG2.eps} } \end{figure}$ Figure 2: Optical spectrum of the galaxy coincident with the VLA J1830+5518, obtained with the 6.05 SAO (+SCORPIO). It shows rest frame emission lines for H $\alpha$ (6563 Å) and O[III](4959 Å, 5007 Å).
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{0921FIG3.eps} } \end{figure}$ Figure 3: Selected detections (X-ray) and upper limits ( ${\it UBVRIJHK}_{\rm S}$ ) associated with the GRB 001109. The most constraining upper limit corresponds to the 2.56 NOT I band measurement.
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In the text

$\begin{figure} \par {\includegraphics[width=6.6cm,clip]{0921FIG4.eps} } \end{figure}$ Figure 4: Contour plot displaying the galaxy coincident with the VLA J1830+5518. The figure shows the coadded I band image taken with the 2.56 NOT (+ALFOSC) (17.0720-17.1148/08/2001) of the source coincident with the VLA J1830+5518. A seeing of 0.8 $^{\prime \prime }$ allowed us to separate the two components, the objects A and B. The centre of the circle marks the position of the radio source (Taylor et al. 2000), RA (J2000) = 18 $\rm ^h$ 30 $\rm ^m$ 06.51 $\rm ^s$ , Dec (J2000) = 55°18 $^\prime$ 35.7 $^{\prime \prime }$ . The radius of the circle is 0.57 $^{\prime \prime }$ . The contours show the detection confidence level above the background in a logarithmic scale. North is upwards and East is leftwards.
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In the text

$\begin{figure} \par {\includegraphics[width=8.1cm,clip]{0921FIG5.eps} } \end{figure}$ Figure 5: SED of the galaxy coincident with the VLA J1830+5518. The solid line is the SED of a dusty galaxy at z= 0.381, with $A_{\rm V}= 1.4$ mag and an episode of star formation 0.25 Gyr ago. This episode of star formation dominates the optical continuum. The SED has been constructed with homogeneous data taken with the 2.56 NOT (+ALFOSC) for the optical and with the 4.20 WHT (+INGRID) for the NIR.
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In the text

$\begin{figure} \par {\includegraphics[width=7.9cm,clip]{0921FIG2.eps} } \end{figure}$	Figure 2: Optical spectrum of the galaxy coincident with the VLA J1830+5518, obtained with the 6.05 SAO (+SCORPIO). It shows rest frame emission lines for H $\alpha$ (6563 Å) and O[III](4959 Å, 5007 Å).
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$\begin{figure} \par {\includegraphics[width=8cm,clip]{0921FIG3.eps} } \end{figure}$	Figure 3: Selected detections (X-ray) and upper limits ( ${\it UBVRIJHK}_{\rm S}$ ) associated with the GRB 001109. The most constraining upper limit corresponds to the 2.56 NOT I band measurement.
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