All Figures

$\begin{figure} \par\includegraphics[width=17.19cm,clip]{h3785f1.eps}\end{figure}$ Figure 1: R band CCD image of NGC 3226 (top left), NGC 3656 (top right), Arp 299 (center left), NGC 520 (center right), NGC 772 (bottom left) & Arp 141 (bottom right). Light blue, yellow and red open circles represent detected EO, SO and ambiguous objects respectively. South is at the top and East towards the left.
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In the text

$\begin{figure} \par\mbox{\epsfig{file=h3785f2a.eps,width=7.6cm}\hspace*{3mm}\psf... ...s,width=7.6cm}\hspace*{3mm}\psfig{file=h3785f2f.eps,width=7.6cm} }\end{figure}$ Figure 2: Density distribution of objects versus distance for each field. The solid line represents EOs, the dashed line SOs and the dot-dashed line ambiguous objects. From left to right: (top) NGC 520 & NGC 772; (center) Arp 141 & NGC 3226/7; (bottom) NGC 3656 & Arp 299. The plots include all galaxies detected within the completeness limit (see Table 2).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h3785f3.eps}\end{figure}$ Figure 3: (V - R) color index of the detected objects as a function of spatial distance in pixels (1 pixel = 0.55 arcsec) to the parent galaxies' center. The symbols and error bars show the averaged colors over different radial distances. Arp 299 is not included since no colors are available.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h3785f4.eps}\end{figure}$ Figure 4: (V - R) color index as a function of Vmagnitude. Crosses with error bars indicate the averaged V-R values per half V magnitude, with the corresponding standard deviation. Over-plotted are the mean values (filled circles) and $1\sigma$ standard deviation of the colors (dashed lines) for the photometric sample of background galaxies reported by Arnouts et al. (1997).
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In the text

$\begin{figure} \par\includegraphics[width=17.19cm,clip]{h3785f1.eps}\end{figure}$	Figure 1: R band CCD image of NGC 3226 (top left), NGC 3656 (top right), Arp 299 (center left), NGC 520 (center right), NGC 772 (bottom left) & Arp 141 (bottom right). Light blue, yellow and red open circles represent detected EO, SO and ambiguous objects respectively. South is at the top and East towards the left.
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$\begin{figure} \par\mbox{\epsfig{file=h3785f2a.eps,width=7.6cm}\hspace{3mm}\psf... ...s,width=7.6cm}\hspace{3mm}\psfig{file=h3785f2f.eps,width=7.6cm} }\end{figure}$	Figure 2: Density distribution of objects versus distance for each field. The solid line represents EOs, the dashed line SOs and the dot-dashed line ambiguous objects. From left to right: (top) NGC 520 & NGC 772; (center) Arp 141 & NGC 3226/7; (bottom) NGC 3656 & Arp 299. The plots include all galaxies detected within the completeness limit (see Table 2).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h3785f3.eps}\end{figure}$	Figure 3: (V - R) color index of the detected objects as a function of spatial distance in pixels (1 pixel = 0.55 arcsec) to the parent galaxies' center. The symbols and error bars show the averaged colors over different radial distances. Arp 299 is not included since no colors are available.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h3785f4.eps}\end{figure}$	Figure 4: (V - R) color index as a function of Vmagnitude. Crosses with error bars indicate the averaged V-R values per half V magnitude, with the corresponding standard deviation. Over-plotted are the mean values (filled circles) and $1\sigma$ standard deviation of the colors (dashed lines) for the photometric sample of background galaxies reported by Arnouts et al. (1997).
Open with DEXTER