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$\begin{figure} \par\includegraphics[width=6.8cm]{8634fig1.eps}\end{figure}$ Figure 1: Three bands HST/ACS imaging of J033226.23-274222.8 ( $\sim$ 0.03 arcsec/pix). The B band is coded in blue, the V band in green, and the z band in red. The FoV is $16\times 16$ arcsec²; North is up, East is left. The contrast has been optimized by hand. White circles indicate the position of low surface brightness debris. The position of the infalling satellite is indicated by a red circle. Upper-right inset: B-z color map of J033226.23-274222.8 from HST/ACS imaging. The FoV is a $\sim$ $4.3\times 2.5$ arcsec² zoom on J033226.23-274222.8.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm]{8634fig2.eps}\end{figure}$ Figure 2: Top panel: closer view of J033226.23-274222.8, which has been rotated to be aligned with the GIRAFFE IFU compared to Fig. 1 (contrast has been optimized by hand). The two elliptical apertures used to estimate the stellar mass ratio between the two galaxies are shown in red for the main progenitor, and in blue for the infalling satellite (see Sect. 4.1). Middle and bottom panels: three bands ACS imaging of J033226.23-274222.8, superimposed with the GIRAFFE velocity field (middle), or $\sigma$ -map (bottom). The IFU bundle is overlaid in white dashed lines (0.52 arcsec/pix). Note that a S/N=3 threshold is used to limit measurement uncertainties, which explains why kinematical data do not extend over the whole IFU FoV. Contours range approximatly from -155 to 130 km s^-1 with a 15 km s^-1 spacing for the VF, and from 14 to 73 km s^-1 with a 4 km s^-1 spacing for the velocity dispersion map.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8634fig3.eps}\end{figure}$ Figure 3: GIRAFFE spectra in the IFU pixels surrounding the peak of the $\sigma$ map (here in the upper-middle panel). Observed sky-subtracted spectra are plotted in black, while the [OII] emission line fits are in red. The corresponding $\sigma$ and its associated uncertainty are indicated in each pixel, together with the level of significance of the difference with the $\sigma$ peak. The probability that the difference is significant is indicated into parenthesis (see text). Spectra have been smoothed for ease of visualization. A typical 1- $\sigma$ error bar due to photon noise is represented in each upper-right corner.
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In the text