All Figures

$\begin{figure} \par\includegraphics[height=14cm,angle=-90,clip]{6577fig1.ps} \end{figure}$ Figure 1: Examples of Laplace-filtered images of 9P/Tempel 1, taken with FORS2 at the ESO VLT through I filter around 0UT on 4 and 5 July 2005. The coma structures, caused by normal activity and annotated A, B, C, D, E, F, G, H, I in the two subpanels, are also detectable when the ejecta cloud expanded throughout the coma. The rotation axis proposed by Thomas et al. (2006) and Lara et al. (2006) projects roughly in North-South direction about half way between structures D and E. The field of view is 40 000 $\times$ 40 000 km at the distance of the comet. North is up, East to the left; Sun direction PA $_{\rm sun} = 290$ deg. The brightness peak in the coma (nucleus position) is in the center of the field of view. Noise fluctuations appear as random small-scale pixel areas in the processed images.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6577fig2.ps} \end{figure}$ Figure 2: CN filter image of 9P/Tempel 1, taken with EMMI at the ESO NTT on 3 July 2005. Laplace filtering (see Sect. 2) is applied for structure enhancement. Structures A, DEF and G are identified, but not structure B. Field of view = 64 000 $\times$ 64 000 km at the distance of the comet. North is up, East to the left; Sun direction PA $_{\rm sun} = 290$ deg.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6577fig3.ps} \end{figure}$ Figure 3: Image of 9P/Tempel 1, taken with FORS2 at the ESO VLT through I filter around 23 UT on 7 July 2005, here processed by the radial renormalization method described in Sect. 2. Jet G is easily seen as is the southern fan which contains structures D, E, F. The field of view is 64 000 $\times$ 64 000 km at the distance of the comet. North is up, East to the left; Sun direction PA $_{\rm sun} = 290$ deg. The dark segments in the image corners are due to masking and do not show science data.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6577fig4.ps} \end{figure}$ Figure 4: Laplace-filtered image of 9P/Tempel 1, taken with FORS2 at the ESO VLT through I filter around 23UT on 7 July 2005. Here a wider numerical filter is used to visualize the extension of the coma structures caused by normal activity of the comet. They extend between 17 000 km (sunward direction at PA = 290 deg) to 58 000 km (tailward direction at PA = 110 deg). The field of view is 100 000 $\times$ 100 000 km at the distance of the comet. North is up, East to the left; Sun direction PA $_{\rm sun}$ = 290 deg. The brightness peak in the coma (nucleus position) is in the center of the field of view. The horizontal bars and noise structure South of the nucleus position is produced by the inter-chip gap of the FORS2 detector assembly.
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In the text

$\begin{figure} \par\includegraphics[height=13cm,angle=-90,clip]{6577fig5.ps} \end{figure}$ Figure 5: I filter images of the dust ejecta cloud produced by DI. The sub-panels show the isophote pattern of the expanding cloud on 5, 6, 7, and 8 July 2005 around 0UT. Enhancement method 3 described in Sect. 2 is applied to remove the coma background from normal activity of the comet. The field of view is 87 000 $\times$ 87 000 km at the distance of the comet. North is up, East to the left; sun direction PA $_{\rm sun} = 290$ deg. The brightness peak in the coma (nucleus position) is in the center of the field of view. The horizontal bars and noise structure South of the nucleus position is due to the inter-chip gap of the FORS2 detector assembly.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6577fig6.ps} \end{figure}$ Figure 6: R filter images of the DI dust ejecta cloud on 7 July 2005. The image shows a moderate dust activity in the southwestern coma quadrant. Image processing and image orientation as for Fig. 5, the field of view is 14 000 $\times$ 14 000 km at the distance of the comet.
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In the text

$\begin{figure} \par\includegraphics[width=4.4cm,clip]{6577fi7a.ps}\includegraphics[width=4.4cm,clip]{6577fi7b.ps} \end{figure}$ Figure 7: R filter intensity ( left) and R-V color ( right) of the DI dust ejecta cloud on 5 July 2005. The surface brightness is higher in the sunward sector compared to the tailward side (brighter region in left panel). The sunward cloud sector is also redder than the tailward one (brighter region in right panel). Image processing and image orientation as for Fig. 5, the field of view is 43 000 $\times$ 43 000 km at the distance of the comet.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6577fig2.ps} \end{figure}$	Figure 2: CN filter image of 9P/Tempel 1, taken with EMMI at the ESO NTT on 3 July 2005. Laplace filtering (see Sect. 2) is applied for structure enhancement. Structures A, DEF and G are identified, but not structure B. Field of view = 64 000 $\times$ 64 000 km at the distance of the comet. North is up, East to the left; Sun direction PA $_{\rm sun} = 290$ deg.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{6577fig6.ps} \end{figure}$	Figure 6: R filter images of the DI dust ejecta cloud on 7 July 2005. The image shows a moderate dust activity in the southwestern coma quadrant. Image processing and image orientation as for Fig. 5, the field of view is 14 000 $\times$ 14 000 km at the distance of the comet.
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