All Figures

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0516fg02.eps}} \end{figure}$ Figure 1: Example of an interactively determined rotation curve (solid points) fit to six position-velocity diagrams (contours), which were taken along the position angels indicated in the top right of each panel. The galaxy shown here is UGC 4325. To determine the rotation curve the position angle, the inclination and the rotation velocity were changed until the projected points on the position-velocity diagrams were found to best match the data.
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In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0516fg05.eps}} \end{figure}$ Figure 2: Comparison between the data for the receding side of UGC 12732, shown in grayscale, and models of the observations (contours), based on an input rotation curve and the observed H I distribution at the full resolution. The input rotation curve is adjusted until the best match to the data is obtained (shown in the middle panel). The top panel shows the model based on the rotation curve derived by visual inspection, which underestimates the rotation velocities in the inner parts. The bottom panel shows a model based on a rotation curve that overestimates the rotation velocities between the center and 1 $\hbox {$^\prime $ }$ .
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{0516fg03.eps}} \end{figure}$ Figure 3: Comparison of the H $\alpha$ rotation curves (dots with error bars) with H I rotation curves (solid lines).
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{0516fg01.eps}} \end{figure}$ Figure 4: Compilation of the rotation curves of the galaxies in the high quality sample. The left panel shows the rotation curves with radii expressed in kpc, in the right panel the radii are expressed in units of disk scale lengths.
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In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0516fg10.eps}} \end{figure}$ Figure 5: Logarithmic slope of the rotation curve between 2 disk scale lengths and the last measured point $S_{\rm (2,L)}^{h}$ versus the numeric Hubble type. Only galaxies for which the last measured point lies beyond 3 disk scale lengths and with inclinations between $39^\circ$ and $80^\circ$ have been plotted. A random value between -0.5 and 0.5 has been added to the numeric Hubble type to spread the points in the plots. The filled circles represent the late-type galaxies with high quality rotation curves from the sample presented in this paper. The open triangles represent galaxies from the Ursa Major sample (Verheijen 1997; Verheijen & Sancisi 2001), filled triangles represent the galaxies from various sources presented in Broeils (1992a), open squares the galaxies from Spekkens & Giovanelli (2006). The stars represent galaxies with H $\alpha$ rotation curves from the samples of de Blok & Bosma (2002) and Swaters et al. (2003a). The long-dashed line represents the relation between Hubble and rotation curve shape as reported by Casertano & van Gorkom (1991), the short-dashed line the same relation as found by Broeils (1992a). The horizontal solid and dotted lines indicate the average value for $S_{\rm (2,L)}^{h}$ and the $1\sigma$ range for galaxies with Hubble type later than Sc (see text for details).
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{0516fg06.eps}} \end{figure}$ Figure 6: Rotation curves in bins of absolute magnitude with radii expressed in units of disk scale length. The full lines give the rotation curves of the galaxies in the high quality sample, the dotted lines those of the galaxies in the lower quality sample.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics{0516fg09.eps}} \end{figure}$ Figure 7: Logarithmic slope of the rotation curve between 2 disk scale lengths and the last measured point $S_{\rm (2,L)}^{h}$ versus the the absolute R-band magnitude M_R ( top), and numeric Hubble type versus M_R ( bottom). Only galaxies for which the last measured point lies beyond 3 disk scale lengths and with inclinations between $39^\circ$ and $80^\circ$ have been plotted. A random value between -0.5 and 0.5 has been added to the numeric Hubble type to spread the points in the plots. Symbol coding as in Fig. 5.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{0516fg08.eps}} \end{figure}$ Figure 8: Logarithmic slope of the rotation curve between 2 disk scale lengths and the last measured point $S_{\rm (2,L)}^{h}$ versus the maximum rotation velocity. Only galaxies for which the last measured point lies beyond 3 disk scale lengths and with inclinations between $39^\circ$ and $80^\circ$ have been plotted. Symbol coding as in Fig. 5. The dotted line represents the correlation between rotation curve shape and maximum rotation velocity found by Casertano & van Gorkom (1991).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{0516fg07.eps}} \end{figure}$ Figure 9: Logarithmic slope of the rotation curve between 2 disk scale lengths and the last measured point $S_{\rm (2,L)}^{h}$ versus the central extrapolated disk surface brightness $\mu _0^R$ . Only galaxies for which the last measured point lies beyond 3 disk scale lengths and with inclinations between $39^\circ$ and $80^\circ$ have been plotted. Symbol coding as in Fig. 5.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{0516fg04.eps}} \end{figure}$ Figure 10: Logarithmic slope of the rotation curve between 1 and 2 disk scale lengths $S_{\rm (1,2)}^{h}$ versus the difference between extrapolated disk surface brightness $\mu _0^R$ and the observed central surface brightness $\mu _c^R$ . Only galaxies with inclinations between $39^\circ$ and $80^\circ$ have been plotted. Symbol coding as in Fig. 5.
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In the text

$\begin{figure} \par\noindent \resizebox{8.2cm}{!}{\includegraphics{0516fg55.eps}... ...ps}}\kern0.5cm \resizebox{8.2cm}{!}{\includegraphics{0516fg28.eps}} \end{figure}$ Figure A.1:
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In the text

$\begin{figure}\vskip-0.15cm \noindent \resizebox{8.2cm}{!}{\includegraphics{0516... ...ps}}\kern0.5cm \resizebox{8.2cm}{!}{\includegraphics{0516fg40.eps}} \end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure}\par\vskip-0.15cm \noindent \resizebox{8.2cm}{!}{\includegraphics{... ...ps}}\kern0.5cm \resizebox{8.2cm}{!}{\includegraphics{0516fg52.eps}} \end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure}\par\vskip-0.15cm \noindent \resizebox{8.2cm}{!}{\includegraphics{... ...ps}}\kern0.5cm \resizebox{8.2cm}{!}{\includegraphics{0516fg65.eps}} \end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure}\par\vskip-0.15cm \noindent \resizebox{8.2cm}{!}{\includegraphics{... ...ps}}\kern0.5cm \resizebox{8.2cm}{!}{\includegraphics{0516fg77.eps}} \end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure}\par\vskip-0.15cm \noindent \resizebox{8.2cm}{!}{\includegraphics{... ....2cm}{!}{\includegraphics{0516fg17.eps}}\kern0.5cm \hspace*{8.8cm}\end{figure}$ Figure A.1: continued.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{0516fg03.eps}} \end{figure}$	Figure 3: Comparison of the H $\alpha$ rotation curves (dots with error bars) with H I rotation curves (solid lines).
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$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{0516fg01.eps}} \end{figure}$	Figure 4: Compilation of the rotation curves of the galaxies in the high quality sample. The left panel shows the rotation curves with radii expressed in kpc, in the right panel the radii are expressed in units of disk scale lengths.
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$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{0516fg06.eps}} \end{figure}$	Figure 6: Rotation curves in bins of absolute magnitude with radii expressed in units of disk scale length. The full lines give the rotation curves of the galaxies in the high quality sample, the dotted lines those of the galaxies in the lower quality sample.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{0516fg07.eps}} \end{figure}$	Figure 9: Logarithmic slope of the rotation curve between 2 disk scale lengths and the last measured point $S_{\rm (2,L)}^{h}$ versus the central extrapolated disk surface brightness $\mu _0^R$ . Only galaxies for which the last measured point lies beyond 3 disk scale lengths and with inclinations between $39^\circ$ and $80^\circ$ have been plotted. Symbol coding as in Fig. 5.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{0516fg04.eps}} \end{figure}$	Figure 10: Logarithmic slope of the rotation curve between 1 and 2 disk scale lengths $S_{\rm (1,2)}^{h}$ versus the difference between extrapolated disk surface brightness $\mu _0^R$ and the observed central surface brightness $\mu _c^R$ . Only galaxies with inclinations between $39^\circ$ and $80^\circ$ have been plotted. Symbol coding as in Fig. 5.
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$\begin{figure} \par\noindent \resizebox{8.2cm}{!}{\includegraphics{0516fg55.eps}... ...ps}}\kern0.5cm \resizebox{8.2cm}{!}{\includegraphics{0516fg28.eps}} \end{figure}$	Figure A.1:
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$\begin{figure}\vskip-0.15cm \noindent \resizebox{8.2cm}{!}{\includegraphics{0516... ...ps}}\kern0.5cm \resizebox{8.2cm}{!}{\includegraphics{0516fg40.eps}} \end{figure}$	Figure A.1: continued.
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