All Figures

$\begin{figure} \par\resizebox{8.5cm}{8.5cm}{\includegraphics{8533fig1.eps}} \end{figure}$ Figure 1: Comparison of the NVSS catalog flux (abscissa) at 1.4 GHz and the reprocessed fluxes for the CIG sources (ordinates).
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In the text

$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig2.eps}} \end{figure}$ Figure 2: Detection rate at 1.4 GHz with NVSS as a function of Hubble type.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{8.5cm}{\includegraphics{8533fig3.eps}} \end{figure}$ Figure 3: Distribution of radio luminosity at 1.4 GHz as a function of Hubble type. Only detections are shown. The open triangles give the mean value of $\log\ (L_{1.4~{\rm{GHz}}}$ ) for each Hubble type, calculated with ASURV and taking the upper limits into account. The open squares are the median values for the detections only.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig4.eps}}\vspa... ...*{3mm} \resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig6.eps}}\par \end{figure}$ Figure 4: Distribution of the 325 MHz ( top), 1.4 GHz ( bottom) and 4.8 GHz ( middle) radio power for the CIG sample. The dotted line indicates the completeness for a velocity of 9300 km s^-1 (80% of the sample). The x-axis indicates the logarithm of the power in W Hz^-1.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{7.3cm}{\includegraphics{8533fig7.eps}} \end{figure}$ Figure 5: Frequency distribution of the 1.4 GHz radio power for the CIG sample (solid line) compared with the frequency distribution of the UGC-SF sample (dashed line) of Condon et al. (2002).
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In the text

$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig8.eps}} \end{figure}$ Figure 6: Optical luminosity distribution in B for the CIG (solid line) and the UGC-SF (dashed line) sample.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{8.5cm}{\includegraphics{8533fig9.eps}} \end{figure}$ Figure 7: Radio flux density at 1.4 GHz (mJy) vs. apparent B magnitude. The lines represent constant radio-to-optical ratio R. The dashed line shows the value of R corresponding to the NVSS sensitivity level (2 mJy). In order not to overload the figure, we show only detections. The radio continuum upper limits were however taken into account in the calculation of the mean values. The plus signs denote galaxies within the complete AMIGA subsample and the crosses indicate galaxies outside this subsample.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig10.eps}} \end{figure}$ Figure 8: Distribution of the radio-to-optical ratio R (logarithmic scale) for the CIG sample (solid line). The elliptical and spiral galaxy distribution are represented respectively by black and grey shaded areas.The dashed line shows the R distribution for the UGC-SF sample (Condon et al. 2002).
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In the text

$\begin{figure} \par\resizebox{8.5cm}{8.5cm}{\includegraphics{8533fig11.eps}}\resizebox{8.5cm}{8.5cm}{\includegraphics{8533fig12.eps}} \end{figure}$ Figure 9: Left: radio power at 1.4 GHz vs. absolute optical magnitude for the Sb-Sc galaxies together with the fitted line obtained using ASURV. The full line gives the bisector fit. We also plot the fit assumming M_B as the independent variable (dotted line) for direct comparison with the fit (dashed line) for the KISS starburst galaxies in Van Duyne et al. (2004). Detections are indicated by crosses while upper limits in radio emission by arrows. Right: radio power at 1.4 GHz vs. absolute optical magnitude for the detected E-S0 (filled squares), Sa-Sab (filled triangles) and Scd-Irr (filled circles) galaxies. The upper limits are indicated with arrows of the same color. The lines correspond to the same fits as in the left panel.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig13.eps}} \end{figure}$ Figure 10: Histogram of the flux ratio between the FIRST and NVSS detections for the CIGs.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig14.eps}} \end{figure}$ Figure 11: Cumulative distribution of the FIRST/NVSS flux ratio for the CIG (solid line) and the center/total flux ratio (dotted line) from Menon (1995).
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In the text

$\begin{figure} \par\resizebox{8.5cm}{8.5cm}{\includegraphics{8533fig15.ps}} \end{figure}$ Figure 12: RLF at 1.4 GHz for the CIG sample (triangles) with 1- $\sigma$ error bars. The RLF is shown in Mpc^-3 mag^-1. The line represents the Schechter fit to the CIG sample, taking into account only data points with $\log~(P) \ge 20.75$ .
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In the text

$\begin{figure} \par\resizebox{8.5cm}{8.5cm}{\includegraphics{8533fig1.eps}} \end{figure}$	Figure 1: Comparison of the NVSS catalog flux (abscissa) at 1.4 GHz and the reprocessed fluxes for the CIG sources (ordinates).
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$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig2.eps}} \end{figure}$	Figure 2: Detection rate at 1.4 GHz with NVSS as a function of Hubble type.
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$\begin{figure} \par\resizebox{8.5cm}{8.5cm}{\includegraphics{8533fig3.eps}} \end{figure}$	Figure 3: Distribution of radio luminosity at 1.4 GHz as a function of Hubble type. Only detections are shown. The open triangles give the mean value of $\log\ (L_{1.4~{\rm{GHz}}}$ ) for each Hubble type, calculated with ASURV and taking the upper limits into account. The open squares are the median values for the detections only.
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$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig4.eps}}\vspa... ...*{3mm} \resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig6.eps}}\par \end{figure}$	Figure 4: Distribution of the 325 MHz ( top), 1.4 GHz ( bottom) and 4.8 GHz ( middle) radio power for the CIG sample. The dotted line indicates the completeness for a velocity of 9300 km s^-1 (80% of the sample). The x-axis indicates the logarithm of the power in W Hz^-1.
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$\begin{figure} \par\resizebox{8.3cm}{7.3cm}{\includegraphics{8533fig7.eps}} \end{figure}$	Figure 5: Frequency distribution of the 1.4 GHz radio power for the CIG sample (solid line) compared with the frequency distribution of the UGC-SF sample (dashed line) of Condon et al. (2002).
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$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig8.eps}} \end{figure}$	Figure 6: Optical luminosity distribution in B for the CIG (solid line) and the UGC-SF (dashed line) sample.
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$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig10.eps}} \end{figure}$	Figure 8: Distribution of the radio-to-optical ratio R (logarithmic scale) for the CIG sample (solid line). The elliptical and spiral galaxy distribution are represented respectively by black and grey shaded areas.The dashed line shows the R distribution for the UGC-SF sample (Condon et al. 2002).
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$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig13.eps}} \end{figure}$	Figure 10: Histogram of the flux ratio between the FIRST and NVSS detections for the CIGs.
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$\begin{figure} \par\resizebox{8.5cm}{7.5cm}{\includegraphics{8533fig14.eps}} \end{figure}$	Figure 11: Cumulative distribution of the FIRST/NVSS flux ratio for the CIG (solid line) and the center/total flux ratio (dotted line) from Menon (1995).
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$\begin{figure} \par\resizebox{8.5cm}{8.5cm}{\includegraphics{8533fig15.ps}} \end{figure}$	Figure 12: RLF at 1.4 GHz for the CIG sample (triangles) with 1- $\sigma$ error bars. The RLF is shown in Mpc^-3 mag^-1. The line represents the Schechter fit to the CIG sample, taking into account only data points with $\log~(P) \ge 20.75$ .
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