All Figures

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{5512fig1.eps} \end{figure}$ Figure 1: Continuum subtracted spectra taken 1 $\rm ^h$ 49 $\rm ^m$ before impact (red) and 17 $\rm ^h$ 59 $\rm ^m$ after impact (black). The spectra are integrated from $0{-} \rm 6.5 \times 10^4$ km along the projected Sun direction to enhance the signal-to-noise ratio. Remnants of night sky lines are marked with NS.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5512fig2.eps} \end{figure}$ Figure 2: Continuum flux along the Sun-comet line, measured at 5540 Å to 5575 Å. The different colors give the profiles at different nights. Isolated peaks in the profiles are caused by stars within the slit. Positive distance is counted towards the projected solar direction, negative in the antisolar direction.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5512fig3.eps} \end{figure}$ Figure 3: Continuum flux perpendicular to the Sun-comet line, measured at 5540 Å to 5575 Å. The different colors give the profiles at different nights. Isolated peaks in the profiles are caused by stars within the slit. Positive distance is counted towards the 270 $^\circ$ direction, negative in the 90 $^\circ$ direction.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{5512fig4.eps} \end{figure}$ Figure 4: CN emission flux along the Sun-comet line for different nights. Positive distance values are counted in the projected solar direction, negative values in the antisolar direction.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{5512fig5.eps} \end{figure}$ Figure 5: CN emission flux perpendicular to the Sun-comet line for different nights. Positive distance values are counted in the 270 $^\circ$ direction, negative values in the 90 $^\circ$ direction.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5512fig6.eps} \end{figure}$ Figure 6: CN line flux in the inner coma ( $\pm$ 5.8 $^{\prime \prime }$ around the nucleus excluding the inner 1.8 $^{\prime \prime }$ ) over time. The values displayed are taken at the 0 $^\circ$ -180 $^\circ$ slit orientation. The points or groups of points belong to the nights from July 02/03 to July 11/12, 2005.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5512fig7.eps} \end{figure}$ Figure 7: CN line flux over rotational phase. The values displayed are taken at the 0 $^\circ -$ 180 $^\circ$ slit orientation. Phase 0 corresponds to the impact time (July 04, 05:52 UT). The night of July 05/06 was non-photometric and the real errors may be even larger. The data from the night of July 04/05 include a significant contribution from the impact cloud and therefore are enhanced compared to data from the undisturbed coma at similar rotational phase.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{5512fig1.eps} \end{figure}$	Figure 1: Continuum subtracted spectra taken 1 $\rm ^h$ 49 $\rm ^m$ before impact (red) and 17 $\rm ^h$ 59 $\rm ^m$ after impact (black). The spectra are integrated from $0{-} \rm 6.5 \times 10^4$ km along the projected Sun direction to enhance the signal-to-noise ratio. Remnants of night sky lines are marked with NS.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{5512fig2.eps} \end{figure}$	Figure 2: Continuum flux along the Sun-comet line, measured at 5540 Å to 5575 Å. The different colors give the profiles at different nights. Isolated peaks in the profiles are caused by stars within the slit. Positive distance is counted towards the projected solar direction, negative in the antisolar direction.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{5512fig3.eps} \end{figure}$	Figure 3: Continuum flux perpendicular to the Sun-comet line, measured at 5540 Å to 5575 Å. The different colors give the profiles at different nights. Isolated peaks in the profiles are caused by stars within the slit. Positive distance is counted towards the 270 $^\circ$ direction, negative in the 90 $^\circ$ direction.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{5512fig4.eps} \end{figure}$	Figure 4: CN emission flux along the Sun-comet line for different nights. Positive distance values are counted in the projected solar direction, negative values in the antisolar direction.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{5512fig5.eps} \end{figure}$	Figure 5: CN emission flux perpendicular to the Sun-comet line for different nights. Positive distance values are counted in the 270 $^\circ$ direction, negative values in the 90 $^\circ$ direction.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{5512fig6.eps} \end{figure}$	Figure 6: CN line flux in the inner coma ( $\pm$ 5.8 $^{\prime \prime }$ around the nucleus excluding the inner 1.8 $^{\prime \prime }$ ) over time. The values displayed are taken at the 0 $^\circ$ -180 $^\circ$ slit orientation. The points or groups of points belong to the nights from July 02/03 to July 11/12, 2005.
Open with DEXTER