Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=14.8cm,clip]{7140fig2.eps}\end{figure}$ Figure 2: ATCA H I image of SCG 2159-3210, superimposed on a red DSS-2 optical plate. The contour levels are at 0.12, 0.17, 0.24, 0.34, 0.48 0.68, and 0.96 Jy km s^-1 beam^-1. The field of view is $12\hbox {$.\mkern -4mu^\prime $ }2\times 12\hbox {$.\mkern -4mu^\prime $ }6$ and the angular resolution ( FWHM = $80\hbox {$^{\prime \prime }$ }\times 45\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. N is up and E to the left.
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In the text

$\begin{figure} \includegraphics[width=14cm,clip]{7140fi1a.eps} \end{figure}$ Figure 1: Optical images ( left panel) and GALFIT residual images ( right panel) for SCG2353-6101, from galaxy a to c from top to bottom. Residual brightness for galaxy A is of the order of 5 $\%$ of the peak brightness, while for the other galaxies is less than 1 $\%$ . In all images N is up and E is left.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{7140fi1b.eps} \end{figure}$ Figure 1: continued. Optical images ( left panel) and GALFIT residual images ( right panel) for SCG0018-4854, from galaxy a to c from top to bottom. Residual brightness for all galaxies is of the order of 10 $\%$ of the peak brightness. In all images N is up and E is left.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{7140fi1c.eps} \end{figure}$ Figure 1: continued. Optical images ( left panel) and GALFIT residual images ( right panel) for SCG0018-4854, from galaxy d to e from top to bottom. Residual brightness for all galaxies is of the order of 7 $\%$ of the peak brightness. In all images N is up and E is left.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{7140fi1d.eps} \end{figure}$ Figure 1: continued. Optical images ( left panel) and GALFIT residual images ( right panel) for SCG0122-3819, from galaxy a to c from top to bottom. Residual brightness for all galaxies is of the order of 5 $\%$ of the peak brightness, with the exception of galaxy B, where the residuals are of the order of 15 $\%$ . In all images N is up and E is left.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{7140fi1e.eps} \end{figure}$ Figure 1: continued. Optical images ( left panel) and GALFIT residual images ( right panel) for SCG0122-3819 d; residuals are of the order of 8 $\%$ of the peak brightness. N is up and E is left.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{7140fi1f.eps} \end{figure}$ Figure 1: continued. Optical images ( left panel) and GALFIT residual images ( right panel) for SCG0141-3429, from galaxy a to c from top to bottom. Residual brightness for all galaxies is of the order of 12 $\%$ of the peak brightness. In all images N is up and E is left.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{7140fi1g.eps} \end{figure}$ Figure 1: continued. Optical images ( left panel) and GALFIT residual images ( right panel) for SCG0141-3429, from galaxy d to e from top to bottom. Residual brightness for all galaxies is of the order of 10 $\%$ of the peak brightness. In all images N is up and E is left.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{7140fi1h.eps} \end{figure}$ Figure 1: continued. Optical images ( left panel) and GALFIT residual images ( right panel) for SCG0227-4312, from galaxy a to c from top to bottom. Residual brightness for all galaxies is of the order of 3 $\%$ of the peak brightness, with the exception of galaxy C, where the residuals are of the order of 8 $\%$ . In all images N is up and E is left.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{7140fi1i.eps} \end{figure}$ Figure 1: continued. Optical images ( left panel) and GALFIT residual images ( right panel) for SCG0227-4312, from galaxy d to f from top to bottom. Residual brightness for all galaxies is of the order of 3 $\%$ of the peak brightness. In all images N is up and E is left.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{7140fig3.eps}\end{figure}$ Figure 3: ATCA H I image of SCG 2353-6101, superimposed on a red DSS-2 optical plate. The contour levels are at 0.24, 0.34, 0.48, 0.68, 0.96 and 1.36 Jy km s^-1 beam^-1. The field of view is $13\hbox {$.\mkern -4mu^\prime $ }0\times 12\hbox {$.\mkern -4mu^\prime $ }6$ and the angular resolution ( FWHM = $50\hbox {$^{\prime \prime }$ }\times 42\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. N is up and E to the left.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{7140fig4.eps}\end{figure}$ Figure 4: ATCA H I image of SCG 2353-6101 superimposed on the H I velocity field, the white crosses indicate the center of galaxy a and b. The contours are the same as in Fig. 3, the field of view is $5\hbox {$.\mkern -4mu^\prime $ }9\times 6\hbox {$^\prime $ }1$ and the angular resolution ( FWHM = 50 $\hbox {$^{\prime \prime }$ }\times$ 42 $\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. The velocity scale is shown on the right and the orientation is N up and E to the left.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{7140fig5.eps}\end{figure}$ Figure 5: ATCA H I image of SCG 0018-4854, superimposed on a red DSS-2 optical plate. The contour levels are at 0.12, 0.17, 0.24, 0.34, 0.48, 0.68 and 0.96 Jy km s^-1 beam^-1. The field of view is $24\hbox {$.\mkern -4mu^\prime $ }2\times 25\hbox {$.\mkern -4mu^\prime $ }2$ and the angular resolution ( FWHM = $38\hbox {$^{\prime \prime }$ }\times 22\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. N is up and E to the left.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{7140fig6.eps}\end{figure}$ Figure 6: ATCA H I image of SCG 0018-4854, superimposed on the H I velocity field. The contours are the same as in Fig. 5, the field of view is $10\hbox {$.\mkern -4mu^\prime $ }2\times 10\hbox {$^\prime $ }5$ and the angular resolution ( FWHM = $38\hbox {$^{\prime \prime }$ }\times 22\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. Crosses indicate the center of each member galaxy, the velocity scale is shown on the right, and the orientation is N up and E to the left.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{7140fig7.eps}\end{figure}$ Figure 7: ATCA H I image of SCG 0122-3819, superimposed on a red DSS-2 optical plate. The contour levels are at 0.2 0.28 0.4 0.56 0.8 1.12 1.6 2.24 Jy km s^-1 beam^-1. The field of view is $20\hbox {$.\mkern -4mu^\prime $ }2\times 20\hbox {$.\mkern -4mu^\prime $ }9$ and the angular resolution ( FWHM = $38\hbox {$^{\prime \prime }$ }\times 22\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. N is up and E to the left.
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In the text

$\begin{figure} \par\mbox{\subfigure[]{\includegraphics[width=8.4cm,clip]{7140fi8... ...m} \subfigure[]{\includegraphics[width=8.4cm,clip]{7140fi8b.eps} }} \end{figure}$ Figure 8: ATCA H I image of SCG 0122-3819C ( left panel) and E ( right panel) superimposed on the H I velocity field. The contours are at the same levels as in Fig. 7; the field of view is $9\hbox {$.\mkern -4mu^\prime $ }6 \times 10\hbox {$.\mkern -4mu^\prime $ }0$ and the angular resolution ( FWHM = 60 $\hbox {$^{\prime \prime }$ }\times$ 40 $\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. The velocity scale is shown on the right, and the orientation of the image is N up and E to the left.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{7140fig9.eps}\end{figure}$ Figure 9: ATCA H I image of SCG 0141-3429, superimposed on a red DSS-2 optical plate. The contour levels are at 0.17 0.24 0.34 0.48 0.68 0.96 1.36 1.92 2.6 Jy km s^-1 beam^-1. The field of view is $13\hbox {$.\mkern -4mu^\prime $ }4\times 12\hbox {$.\mkern -4mu^\prime $ }7$ and the angular resolution ( FWHM = $80\hbox {$^{\prime \prime }$ }\times 44\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. N is up and E to the left.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{7140fi10.eps}\end{figure}$ Figure 10: ATCA H I contours of SCG 0141-3429 superimposed on the H I velocity field; the crosses indicate the centers of the member galaxies. The contours are the same as in Fig. 9, the field of view is $12\hbox {$.\mkern -4mu^\prime $ }6\times 10\hbox {$^\prime $ }1$ and the angular resolution ( FWHM = $38\hbox {$^{\prime \prime }$ }\times 22\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. The velocity scale is shown on the right and the orientation is N up and E to the left.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{7140fi11.eps}\end{figure}$ Figure 11: ATCA H I image of SCG 0227-4312, superimposed on a red DSS-2 optical plate. The contour levels are at 0.2 0.28 0.4 0.56 0.8 1.12 1.6 2.24 Jy km s^-1 beam^-1. The field of view is $26\hbox {$.\mkern -4mu^\prime $ }6\times 25\hbox {$.\mkern -4mu^\prime $ }4$ and the angular resolution ( FWHM = $38\hbox {$^{\prime \prime }$ }\times 22\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. N is up and E to the left.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{7140fi12.eps}\end{figure}$ Figure 12: ATCA H I image of SCG 0227-4212, superimposed on the H I velocity field. The contours are the same as in Fig. 11, the field of view is $23\hbox {$.\mkern -4mu^\prime $ }5\times 16\hbox {$^\prime $ }2$ and the angular resolution ( FWHM = 104 $\hbox {$^{\prime \prime }$ }\times$ 57 $\hbox {$^{\prime \prime }$ }$ ) is indicated in the lower left. The velocity scale is shown on the right and the orientation is N up and E to the left.
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In the text

$\begin{figure} \includegraphics[width=14cm,clip]{7140fi1a.eps} \end{figure}$	Figure 1: Optical images ( left panel) and GALFIT residual images ( right panel) for SCG2353-6101, from galaxy a to c from top to bottom. Residual brightness for galaxy A is of the order of 5 $\%$ of the peak brightness, while for the other galaxies is less than 1 $\%$ . In all images N is up and E is left.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{7140fi1b.eps} \end{figure}$	Figure 1: continued. Optical images ( left panel) and GALFIT residual images ( right panel) for SCG0018-4854, from galaxy a to c from top to bottom. Residual brightness for all galaxies is of the order of 10 $\%$ of the peak brightness. In all images N is up and E is left.
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