All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{3744f1.ps} \end{figure}$ Figure 1: The radio luminosity at 1.4 GHz ( $L_{{{\rm 1.4~GHz}}}$ ) vs. the total FIR luminosity (of the warm + cold dust emission components) ( $L_{{\rm FIR}}$ ) for the full sample of 72 objects under investigation. The plot shows a tight correlation between $L_{{{\rm 1.4~GHz}}}$ and $L_{{\rm FIR}}$ , over three orders of magnitude in both luminosities. From the fit (solid line) we conclude that this correlation is only slightly non-linear (see the slope of the fit and its uncertainty, here indicated). The dashed line represents the fit to the $L_{{{\rm 1.4~GHz}}}$ vs. L_40-120 correlation, which is the equivalent of what would have been derived from IRAS.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3744f2.ps} \end{figure}$ Figure 2: The radio luminosity at 1.4 GHz vs. the FIR luminosity of the warm component ( $L_{{\rm FIR}}^{{\rm warm}}$ ) for the full sample of 72 objects under investigation. The plot shows a tight correlation between these two emissions, over three orders of magnitude in both luminosities. The fit to the correlation (plotted with the solid line) indicates a linear relation. The value of the slope and its uncertainty are indicated on the figure. The dashed line represents again the fit to the $L_{{{\rm 1.4~GHz}}}$ vs. L_40-120 correlation, i.e., the equivalent of the IRAS FIR/radio correlation.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3744f3.ps} \end{figure}$ Figure 3: The radio luminosity at 1.4 GHz vs. the FIR luminosity of the cold component ( $L_{{\rm FIR}}^{{\rm cold}}$ ) for the full sample of 72 objects under investigation. The plot shows a tight correlation between these two emissions, over three orders of magnitude in both luminosities. The fit to the correlation (plotted with solid line) indicates a slightly non-linear correlation. The value of the slope and its uncertainty are indicated on the figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3744fA1.ps} \end{figure}$ Figure A.1: Comparison of the radio fluxes at 1.4 GHz determined in this study from direct aperture photometry of the NVSS images and the NVSS catalogue fluxes for the radio counterparts of the 72 sample objects under investigation. The latter fluxes are obtained from Gaussian model components fitted to the survey images. Here the solid and long-dashed lines represent the 1:1 and 1.25:1 ratios, respectively, while the box delimited by a short-dashed line corresponds to the region zoomed in the enclosed box. On average, our fluxes are 25 per cent larger than the NVSS catalogue ones (see text).

In the text