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$\begin{figure} \par\includegraphics[width=14cm,clip]{2586fg1a.ps} \end{figure}$ Figure 1: Radio continuum and CO comparison in BIMA SONG galaxies. ( Upper left) RC contours overlaid on CO emission for 55 $^{\prime \prime }$ images. ( Lower left) RC contours overlaid on CO emission for 6 $^{\prime \prime }$ images. Contours start at 5 $\sigma$ and scale by a factor of $\sqrt {2}$ ; the bright contours are chosen to match the dynamic range of the CO emission. ( Upper right) $I_{\rm 1.4}$ as a function of $I_{\rm CO}$ for the 55 $^{\prime \prime }$ and 6 $^{\prime \prime }$ data sets. The insets show the box grids used; the grid size corresponds to the resolution, so that each point is essentially independent. The dotted (dashed) lines represent the mean (dispersion) of the RC/CO ratio for all nine sources. The solid blue line is a weighted fit to the points shown which takes into account the errors in both coordinates. ( Lower right) Radial profiles of $I_{\rm CO}$ and $I_{\rm 1.4}$ ( top) and $Q_{\rm CO/RC}$ $\equiv$ $I_{\rm CO}$ / $I_{\rm 1.4}$ ( bottom) for the 55 $^{\prime \prime }$ and 6 $^{\prime \prime }$ images. The mean and dispersion of $q_{\rm CO/RC}$ $\equiv \log (Q_{\rm CO/RC})$ is also given. See Sect. 3 for further details on the presentation; notes on individual galaxies are given in Appendix A. a) IC 342.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{2586fig2.ps} \end{figure}$ Figure 2: Global CO-RC, FIR-CO, and RC-FIR fluxes for 24 BIMA SONG galaxies, shown with least squares fits (from which NGC 1068 is omitted). The data are listed in Table 4. Crosses are galaxies included in the high-resolution analysis of this paper. The dashed-line represents a least squares fit restricted to the data of the 9 galaxies analyzed in this work and yields a CO-RC correlation of $\log (S_{\rm RC}) \propto 1.06 \pm 0.17 \log(S_{\rm CO})$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2586fig3.ps} \end{figure}$ Figure 3: CO-RC correlation in sample galaxies. Each point represents the average value in an annulus. The solid blue line is a weighted fit to the points shown which takes into account the errors in both coordinates and has a slope of 1.08.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2586fig4.ps} \end{figure}$ Figure 4: Histogram of all measured $q_{\rm CO/RC}$ pixels. The mean and dispersion are also given.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{2586fig5.ps} \end{figure}$ Figure 5: Spatially resolved CO-RC correlation within NGC 5194 spiral arms. The RC and CO intensities are measured at independent positions in boxes of about $200\times 200$ pc in size. Spiral arms show a RC-CO correlation with a slope of 1.04 and with a scatter which is less than a factor of 2. The RC/CO ratio in the arms is $q_{\rm CO/RC}$ $=1.2\pm 0.20$ , while in the interarm regions $q_{\rm CO/RC}$ $=1.0 \pm 0.25$ .
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In the text

$\begin{figure} \par\includegraphics[width=13.5cm,clip]{2586fig6.ps} \end{figure}$ Figure 6: Images of $q_{\rm CO/RC}$ as defined in Sect. 3. The scale is given as a color wedge at the top of the figure.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2586fig7.ps} \end{figure}$ Figure 7: Histogram of the CO to RC scale lengths ratio. The average ratio considering all galaxies results $0.98\pm 0.41$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2586fig8.ps} \end{figure}$ Figure 8: $\bar{P}$ for the Milky Way.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2586fig9.ps} \end{figure}$ Figure 9: Spectral index between 327 MHz and 1.4 GHz as a function of $t_{\rm c}/t_{\rm syn}$ for a leaky-box model with an injection spectral index $\alpha _{0}=0.8$ , see text.
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In the text

$\begin{figure} \par\includegraphics[width=13.5cm,clip]{2586fg10.ps} \end{figure}$ Figure 10: Spectral index images ( left panels) and radial averaged profiles ( right panel) for IC 342 and NGC 5194. The spectral index is measured between 327 MHz and 1.4 GHz. Only pixels with an intensity level above $3\sigma$ at both frequencies have been considered.
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In the text

$\begin{figure}\par\includegraphics[width=14cm,clip]{2586fg1b.ps}\end{figure}$	Figure 1: continued. b) NGC 4258.
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$\begin{figure}\par\includegraphics[width=14cm,clip]{2586fg1c.ps}\end{figure}$	Figure 1: continued. c) NGC 4414.
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$\begin{figure}\par\includegraphics[width=14cm,clip]{2586fg1d.ps}\end{figure}$	Figure 1: continued. d) NGC 4736.
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$\begin{figure}\par\includegraphics[width=14cm,clip]{2586fg1e.ps}\end{figure}$	Figure 1: continued. e) NGC 5005.
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$\begin{figure}\par\includegraphics[width=14cm,clip]{2586fg1f.ps}\end{figure}$	Figure 1: continued. f) NGC 5033.
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$\begin{figure}\par\includegraphics[width=14cm,clip]{2586fg1g.ps}\end{figure}$	Figure 1: continued. g) NGC 5055.
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$\begin{figure}\par\includegraphics[width=14cm,clip]{2586fg1h.ps}\end{figure}$	Figure 1: continued. h) NGC 5194.
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$\begin{figure}\par\includegraphics[width=14cm,clip]{2586fg1i.ps}\end{figure}$	Figure 1: continued. i) NGC 6946.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2586fig3.ps} \end{figure}$	Figure 3: CO-RC correlation in sample galaxies. Each point represents the average value in an annulus. The solid blue line is a weighted fit to the points shown which takes into account the errors in both coordinates and has a slope of 1.08.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2586fig4.ps} \end{figure}$	Figure 4: Histogram of all measured $q_{\rm CO/RC}$ pixels. The mean and dispersion are also given.
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$\begin{figure} \par\includegraphics[width=13.5cm,clip]{2586fig6.ps} \end{figure}$	Figure 6: Images of $q_{\rm CO/RC}$ as defined in Sect. 3. The scale is given as a color wedge at the top of the figure.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2586fig7.ps} \end{figure}$	Figure 7: Histogram of the CO to RC scale lengths ratio. The average ratio considering all galaxies results $0.98\pm 0.41$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2586fig8.ps} \end{figure}$	Figure 8: $\bar{P}$ for the Milky Way.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2586fig9.ps} \end{figure}$	Figure 9: Spectral index between 327 MHz and 1.4 GHz as a function of $t_{\rm c}/t_{\rm syn}$ for a leaky-box model with an injection spectral index $\alpha _{0}=0.8$ , see text.
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$\begin{figure} \par\includegraphics[width=13.5cm,clip]{2586fg10.ps} \end{figure}$	Figure 10: Spectral index images ( left panels) and radial averaged profiles ( right panel) for IC 342 and NGC 5194. The spectral index is measured between 327 MHz and 1.4 GHz. Only pixels with an intensity level above $3\sigma$ at both frequencies have been considered.
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