All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{h4465f1.ps} \end{figure}$ Figure 1: The MOSAIC field is overlaid on a DSS image of the central part of the Antlia cluster. North is up, East to the left.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{h4465f2.ps} \end{figure}$ Figure 2: The color magnitude diagram of all point sources in the MOSAIC field. Globular cluster candidates are known to occupy the color range of approximately 0.9<C-T1<2.3. Objects with a color redder than C-T1>3 are in their majority Galactic foreground stars. Objects fainter than approximately T1=23.5 and bluer than C-T1=1 predominately are background galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{h4465f3.ps} \end{figure}$ Figure 3: In the upper panel the completeness function for globular cluster candidates ( 0.9<(C-T1)<2.3) is shown. In the lower panel the DAOPhot errors (dots) are compared to the mean standard deviation between the input and output magnitude of the artificial stars (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{h4465f4.ps} \end{figure}$ Figure 4: The spatial distribution of all point sources fainter than T1=21.5 within the color range 0.9<(C-T1)<2.3 are plotted with the same orientation as Fig. 1. We indicate the areas which were used to derive the color distributions of point sources plotted in Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=14.2cm,clip]{h4465f5.ps} \end{figure}$ Figure 5: The color distribution functions for the GC candidates (background corrected) within a radial distance of 4.5 $^\prime$ around NGC 3258 and NGC 3268 are shown as the solid lines. We used an Epanechnikov kernel for the adaptive smoothing. The applied background for the correction is displayed as the dashed line. The dotted line shows the histogram of the data and the errors.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{h4465f6.ps} \end{figure}$ Figure 6: This graph shows the radial distribution for the GC candidates ( 0.9<(C-T1)<2.3, 21.5<T1<23) for NGC 3258 and NGC 3268. Within $0\hbox {$.\mkern -4mu^\prime $ }7$ the measurements are affected by radial incompleteness effects. The dashed lines show the fit to the data described in the text. The galaxy T1 luminosity profile multiplied by -0.4 and arbitrarily shifted is shown as the solid line with $1 \sigma$ uncertainties (dotted lines). The galaxy measurements are described in Sect. 4.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{h4465f7.ps} \end{figure}$ Figure 7: The azimuthal distribution of the globular clusters within a radial distance of $1\hbox {$.\mkern -4mu^\prime $ }6<r<4\hbox {$.\mkern -4mu^\prime $ }5$ around NGC 3258 and NGC 3268. The dotted line shows the binned azimuthal distribution and the solid line the smoothed one that was also used for a $\sin^2$ -fit shown as the dashed line. This graph shows that both GCSs have an elliptical shape. The vertical dashed lines show the position angle of the galaxy light (see Sect. 4).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{h4465f8.ps} \end{figure}$ Figure 8: The completeness corrected luminosity function of GC candidates ( 1<(C-T1)<2) with a radial distance between $0.46\hbox {$^\prime $ }<{r}<4.5\hbox {$^\prime $ }$ is plotted as histogram and adaptively filtered distribution with a solid line for NGC 3258 in the upper panel and for NGC 3268 in the lower panel. The short dashed line shows the luminosity function before the completeness correction. The lower long dashed lines in the panels indicate the background luminosity function and the upper long dashed line the fitted Gaussian described in the text.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{h4465f9.ps} \end{figure}$ Figure 9: The luminosity profiles of NGC 3268 and NGC 3258 (solid curves) and $1 \sigma$ uncertainties (dotted line) are compared to the luminosity profile of NGC 1399 (long dashed line). For this comparison the diameter of NGC 1399 has been shrunk by a factor of three to account for the distance difference (a distance modulus of (m-M)=31.4 is assumed for NGC 1399). The short dashed lines are the V profiles for NGC 3268 and NGC 3258 published by Reid et al. (1994).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{h4465f10.ps} \end{figure}$ Figure 10: The integrated luminosity dependence on radius is shown for NGC 3268 and NGC 3258 in the R band (we tranformed our T1 measurements using the tiny shift mentioned in Sect. 2). For NGC 3268 the measurements of Godwin et al. (1977) are plotted as open symbols. For NGC 3268 and NGC 3258 aperture photometry is provided by Poulain et al. (1994) (filled symbols).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{h4465f11.ps} \end{figure}$ Figure 11: The color profiles of the two ellipticals are shown together with the $1 \sigma$ uncertainties.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4465f12.ps} \end{figure}$ Figure A.1: C image of NGC 3269 that shows the compact absorption feature in the spiral arm to the lower left. North is to the right, East to the top. The size of the image is $4.9\hbox {$^\prime $ }\times 3.7\hbox {$^\prime $ }$ .

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{h4465f1.ps} \end{figure}$	Figure 1: The MOSAIC field is overlaid on a DSS image of the central part of the Antlia cluster. North is up, East to the left.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{h4465f2.ps} \end{figure}$	Figure 2: The color magnitude diagram of all point sources in the MOSAIC field. Globular cluster candidates are known to occupy the color range of approximately 0.9<C-T1<2.3. Objects with a color redder than C-T1>3 are in their majority Galactic foreground stars. Objects fainter than approximately T1=23.5 and bluer than C-T1=1 predominately are background galaxies.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{h4465f3.ps} \end{figure}$	Figure 3: In the upper panel the completeness function for globular cluster candidates ( 0.9<(C-T1)<2.3) is shown. In the lower panel the DAOPhot errors (dots) are compared to the mean standard deviation between the input and output magnitude of the artificial stars (solid line).
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{h4465f4.ps} \end{figure}$	Figure 4: The spatial distribution of all point sources fainter than T1=21.5 within the color range 0.9<(C-T1)<2.3 are plotted with the same orientation as Fig. 1. We indicate the areas which were used to derive the color distributions of point sources plotted in Fig. 5.
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$\begin{figure} \par\includegraphics[width=14.2cm,clip]{h4465f5.ps} \end{figure}$	Figure 5: The color distribution functions for the GC candidates (background corrected) within a radial distance of 4.5 $^\prime$ around NGC 3258 and NGC 3268 are shown as the solid lines. We used an Epanechnikov kernel for the adaptive smoothing. The applied background for the correction is displayed as the dashed line. The dotted line shows the histogram of the data and the errors.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{h4465f10.ps} \end{figure}$	Figure 10: The integrated luminosity dependence on radius is shown for NGC 3268 and NGC 3258 in the R band (we tranformed our T1 measurements using the tiny shift mentioned in Sect. 2). For NGC 3268 the measurements of Godwin et al. (1977) are plotted as open symbols. For NGC 3268 and NGC 3258 aperture photometry is provided by Poulain et al. (1994) (filled symbols).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{h4465f11.ps} \end{figure}$	Figure 11: The color profiles of the two ellipticals are shown together with the $1 \sigma$ uncertainties.
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