All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f1.ps} \end{figure}$ Figure 1: The six template spectra (see Table 2) are shown in 100 $\AA$ wide regions around the H $\beta$ line ( $\sim$ $4860~\AA$ , left panels) and the Na I doublet ( $\sim$ $5890~\AA$ , right panels). The spectra are ordered by increasing metallicity as indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f2.ps} \end{figure}$ Figure 2: The five object spectra (see Table 1) are shown in 100 $\AA$ wide regions around the H $\beta$ line ( $\sim$ $4885~\AA$ , left panels) and the Na I doublet ( $\sim$ $5920~\AA$ , right panels). The 1-sigma error are plotted as well (grey lines).
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{6429f3.ps} \end{figure}$ Figure 3: The "blue'' part ( upper panel) and the "red'' part ( lower panel) of the spectrum of UCD4 are shown. Dark regions mark the eight direct fitting regions for velocity dispersion measurements (see Table 3). The grey wavy lines are the 1-sigma error spectra.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f4.ps} \end{figure}$ Figure 4: The direct fitting regions for the spectrum of UCD4 are shown (grey lines) together with the best fitting template (black lines). The name of the template, the velocity dispersion of the Gaussian kernel and the number of the direct fitting region are indicated in each panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f5.ps} \end{figure}$ Figure 5: The Na doublet region for the five studied objects is shown (UCD2, UCD3, UCD4, UCD5 and FCC303 from top to bottom). The bold lines are averages of the three best-fitting templates for this region (region 6, see Table 3). The corresponding velocity dispersions are given on the left. Thin lines represent the averages of the three best-fitting templates in the regions 4, 5 and 7. Their velocity dispersions are given on the right.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f6.ps} \end{figure}$ Figure 6: The model output of four different light profile representations of UCD4 is shown; the line types are: black solid - Nuker law, black dot-dashed - Sersic law, grey long dashed - King profile, grey short dashed - generalized King profile. The upper panel shows the 3-dimensional density distribution, the middle panel the cumulative mass distribution, and the lower panel the projected velocity dispersion profile of the z-component of the 3-dimensional velocity. The vertical short dashed lines indicate the radii of 0.5 ( left) and 1 pixel. The dotted line is half the slit width, and the bold dashed line shows the projected half-light radius of UCD4.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f7.ps} \end{figure}$ Figure 7: The model output of two different light profile representations of UCD3 is shown; the line types are: solid - 2-component King+Sersic profile, dashed - Nuker law. The upper panel shows the 3-dimensional density distribution, the middle panel the cumulative mass distribution, and the lower panel the projected velocity dispersion profile of the z-component of the 3-dimensional velocity. The vertical short dashed lines indicate the radii of 0.5 ( left) and 1 pixel. The dotted line is half the slit width, and the bold dashed line shows the projected half-light radius of UCD3.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f8.ps} \end{figure}$ Figure 8: The x-y-plane of the modelled generalized King representation of UCD2 is shown. Grey dots are all 100 000 test particles. Black dots are those "stars'' whose centres fall into the analysed slit area. The grey circle indicates the projected half-light radius of UCD2. The Gaussian in the lower right corner corresponds to the convolution kernel used to estimate the fraction of light that falls into the slit region for each "star''.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f9.ps} \end{figure}$ Figure 9: Velocity histograms of the z-component velocities for the Nuker ( top panel) and generalized King ( lower panel) models of UCD4. The bin width is 1 km s^-1. Black solid lines indicate the velocity distributions of all test particles, the light grey lines those of the "stars'' with centres in the slit area, and the grey lines the luminosity weighted number counts of those "stars'' whose "light'' falls into the slit area. The corresponding velocity dispersions are given in the plots.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f10.ps} \end{figure}$ Figure 10: Luminosity vs. mass plot for five Fornax UCDs (the data for UCD1 were taken from Drinkwater et al. (2003). The symbols indicate the following models: grey open circles - King, filled circles - generalized King, grey triangles - Sersic; grey squares - Nuker, open hexagons - King+Sersic, and crosses - virial mass estimator. Lines of constant mass-to-light ratio are shown as indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f11.ps} \end{figure}$ Figure 11: The dynamical M/L_V ratios of Fornax UCDs (filled circles) and the nucleus of FCC303 (filled triangle) are compared to expected M/L_V values from stellar population models. Also shown are data for Virgo UCDs (open squares from Evstigneeva et al. (2006). In the left panels M/L_V is plotted versus metallicity [Z/H], in the right panels versus the colour (V-I)₀. The references to the models and the adopted IMF are indicated in the panels. The three lines in each plot represent ages of 15, 13 and 5 Gyr from top to botton, respectively. For the Fornax UCDs an $\alpha$ abundance of [ $\alpha$ /Fe]=0.3 was adopted to derive their [Z/H] values. Note, however, that their $\alpha$ abundance might be different (solar) if they possess a significant contribution of intermediate age stellar populations.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f1.ps} \end{figure}$	Figure 1: The six template spectra (see Table 2) are shown in 100 $\AA$ wide regions around the H $\beta$ line ( $\sim$ $4860~\AA$ , left panels) and the Na I doublet ( $\sim$ $5890~\AA$ , right panels). The spectra are ordered by increasing metallicity as indicated.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f2.ps} \end{figure}$	Figure 2: The five object spectra (see Table 1) are shown in 100 $\AA$ wide regions around the H $\beta$ line ( $\sim$ $4885~\AA$ , left panels) and the Na I doublet ( $\sim$ $5920~\AA$ , right panels). The 1-sigma error are plotted as well (grey lines).
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{6429f3.ps} \end{figure}$	Figure 3: The "blue'' part ( upper panel) and the "red'' part ( lower panel) of the spectrum of UCD4 are shown. Dark regions mark the eight direct fitting regions for velocity dispersion measurements (see Table 3). The grey wavy lines are the 1-sigma error spectra.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6429f4.ps} \end{figure}$	Figure 4: The direct fitting regions for the spectrum of UCD4 are shown (grey lines) together with the best fitting template (black lines). The name of the template, the velocity dispersion of the Gaussian kernel and the number of the direct fitting region are indicated in each panel.
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