All Figures

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{6087fig1.ps}\end{figure}$ Figure 1: Evolutionary track EW for HII regions determined by the Starburst99 model. Open squares correspond to the measured EW(H $\alpha$ ) for the observed HII regions. The upper right shows an uncertainty bar of log(EW(H $\alpha ))=0.1$ Å.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{6087fig2.ps}\end{figure}$ Figure 2: Colour-colour diagram of the HII regions. The continuous line corresponds to the evolutionary track (B-V) vs. (V-I), determined by the Starburst99 model. Open stars on the continuous line mark the ages 10⁴, 10⁶, $2.5 \times 10^6$ , $5\times 10^6$ , $7.5\times 10^6$ , 10⁷, $5\times 10^7$ , 10⁸ years for the clusters. The arrow (located below to the right) represents the value and the direction of the A_V=1 mag reddening. The filled triangles correspond to the colours of the observed HII regions.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{6087fig3.ps}\end{figure}$ Figure 3: Distribution of H $\alpha$ luminosity-free reddening of the star-forming regions of our sample (white area) and the sample of Temporin et al. (2003) (shadowed area). The dotted lines indicate the limits in H $\alpha$ luminosity of HII regions observed in normal galaxies with morphological type Sa/Sb and Sc.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{6087fig4.ps}\end{figure}$ Figure 4: Distribution of mass for the HII region of the sample obtained by the H $\alpha$ luminosity ( upper panel) and obtained by the blue absolute magnitude ( lower panel). We exclude the nucleus and suspected nucleus of the sample. The histogram was constructed taking bins of $M=0.2~M_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6087fig5.ps}\end{figure}$ Figure 5: Percentage difference between ${\it SFR}$ (H $\alpha$ ) and ${\it SFR}$ (QH₀) relative to ${\it SFR}$ (H $\alpha$ ) for the regions with H $\alpha$ calibration ordered according to increasing right ascension.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6087fig6.ps}\end{figure}$ Figure 6: Distribution of luminosity of the star-forming regions of the sample. The dashed vertical line indicates the magnitude limit of the TDG observed at or near the tip of long tidal tails.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6087fig7.ps}\end{figure}$ Figure 7: Percentage difference between Age(EW(H $\alpha$ )) and Age(colour-colour) relative to Age(EW(H $\alpha$ )) for the regions internal reddening estimated ordered according to increasing right ascension.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA1a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA1b.ps}\end{figure}$ Figure A.1: AM1256-433. Top panel a): H $\alpha$ image and contours map. Bottom panel b): $\cal L$ (H $\alpha$ ) evolutionary track for HII regions of the pair with masses between $1\times 10^5 < M/M_\odot < 1\times 10^9$ determined by Starburst99 model. The continuous lines from bottom to top correspond to the evolutionary track of the H $\alpha$ luminosity for HII regions with 10⁵, 10⁶, 10⁷, 10⁸, and 10⁹ solar masses. The dashed lines from the bottom correspond to HII regions with $3\times 10^5$ , $3\times 10^6$ , $3\times 10^7$ , and $3\times 10^8$ solar masses, and the short dashed lines correspond to HII region with $5\times 10^5$ , $5\times 10^6$ , $5\times 10^7$ , and $5\times 10^8$ solar masses. The filled triangles correspond to H $\alpha$ luminosity (corrected by internal reddening) vs. age of the HII regions and the open stars correspond to the nucleus of the host galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA2a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA2b.ps}\end{figure}$ Figure A.2: AM1401-324. Same as Fig. A.1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA3a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA3b.ps}\end{figure}$ Figure A.3: AM2030-303. Same as Fig. A.1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA4a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA4b.ps}\end{figure}$ Figure A.4: AM2058-381. Same as Fig. A.1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA5a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA5b.ps}\end{figure}$ Figure A.5: AM2105-332. Same as Fig. A.1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA6a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA6b.ps}\end{figure}$ Figure A.6: AM2229-735. Same as Fig. A.1
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In the text

$\begin{figure} \includegraphics[width=8cm,height=8cm]{6087fA7a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA7b.ps}\end{figure}$ Figure A.7: AM2306-721. Same as Fig. A.1.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{6087fig1.ps}\end{figure}$	Figure 1: Evolutionary track EW for HII regions determined by the Starburst99 model. Open squares correspond to the measured EW(H $\alpha$ ) for the observed HII regions. The upper right shows an uncertainty bar of log(EW(H $\alpha ))=0.1$ Å.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{6087fig3.ps}\end{figure}$	Figure 3: Distribution of H $\alpha$ luminosity-free reddening of the star-forming regions of our sample (white area) and the sample of Temporin et al. (2003) (shadowed area). The dotted lines indicate the limits in H $\alpha$ luminosity of HII regions observed in normal galaxies with morphological type Sa/Sb and Sc.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{6087fig4.ps}\end{figure}$	Figure 4: Distribution of mass for the HII region of the sample obtained by the H $\alpha$ luminosity ( upper panel) and obtained by the blue absolute magnitude ( lower panel). We exclude the nucleus and suspected nucleus of the sample. The histogram was constructed taking bins of $M=0.2~M_\odot$ .
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6087fig5.ps}\end{figure}$	Figure 5: Percentage difference between ${\it SFR}$ (H $\alpha$ ) and ${\it SFR}$ (QH₀) relative to ${\it SFR}$ (H $\alpha$ ) for the regions with H $\alpha$ calibration ordered according to increasing right ascension.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6087fig6.ps}\end{figure}$	Figure 6: Distribution of luminosity of the star-forming regions of the sample. The dashed vertical line indicates the magnitude limit of the TDG observed at or near the tip of long tidal tails.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6087fig7.ps}\end{figure}$	Figure 7: Percentage difference between Age(EW(H $\alpha$ )) and Age(colour-colour) relative to Age(EW(H $\alpha$ )) for the regions internal reddening estimated ordered according to increasing right ascension.
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$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA2a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA2b.ps}\end{figure}$	Figure A.2: AM1401-324. Same as Fig. A.1.
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$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA3a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA3b.ps}\end{figure}$	Figure A.3: AM2030-303. Same as Fig. A.1.
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$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA4a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA4b.ps}\end{figure}$	Figure A.4: AM2058-381. Same as Fig. A.1.
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$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA5a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA5b.ps}\end{figure}$	Figure A.5: AM2105-332. Same as Fig. A.1.
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$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{6087fA6a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA6b.ps}\end{figure}$	Figure A.6: AM2229-735. Same as Fig. A.1
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$\begin{figure} \includegraphics[width=8cm,height=8cm]{6087fA7a.ps}\par\includegraphics[width=8cm,height=8cm]{6087fA7b.ps}\end{figure}$	Figure A.7: AM2306-721. Same as Fig. A.1.
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