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Appendix A: Appendix

We report in this Appendix the analogous of Fig. 1 (the spectroscopic diagnostic diagrams), Fig. 2 (left panel) (H $\alpha$ flux vs. the continuum at the H $\alpha$ line), Fig. 3 (concentration index vs. 4000 Å break), Fig. 6 (D_n(4000) vs. $L_{\rm 1.4~GHz}$ /M_*), Fig. 9 (distributions of the SMBH masses for each spectroscopic class), and Fig. 7 (total radio power vs. [O III] luminosities) for the objects with redshift 0.1<z<0.3.

$\begin{figure} \par\includegraphics[angle=90,width=15cm,clip]{14446fa1.epsi} \end{figure}$	Figure A.1: Spectroscopic diagnostic diagrams for the objects with 0.1<z<0.3, with the same structure and symbols as Fig. 1.
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$\begin{figure} \par { \includegraphics[scale=0.4,angle=90]{14446fa2a.epsi}\inclu... ...46fa2c.epsi}\includegraphics[scale=0.4,angle=90]{14446fa2d.epsi} }\end{figure}$

Figure A.2:

Analogous of Fig. 2 ( left panel), Figs. 3, 6, and 9 for the higher redshift objects (0.1<z<0.3) i.e.: ( upper left panel) logarithm of the H $\alpha$ flux versus logarithm of the continuum at the H $\alpha$ line (in erg s^-1 and erg s^-1 Å^-1 units respectively); ( upper right panel) concentration index C_r vs. 4000 Å break; ( lower left panel) D_n(4000) vs. $L_{1.4~{\rm GHz}}/M_{*}$ ; ( lower right panel) distributions of the $M_{\rm BH}$ (in solar units) for the various spectroscopic classes. The filled portion of the histograms represent the contribution of galaxies with C_r<2.86.

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$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{14446fa3.epsi} \end{figure}$

Figure A.3:

Analogous of Fig. 7 for the higher redshift objects (0.1<z<0.3) i.e. logarithm of radio power $L_{1.4~ \rm {GHz}}$ vs. [O III] luminosities. For more clarity the large number of upper limits in $L_{\rm [O~III]}$ are not shown. The two dashed lines reproduce the line-radio correlation followed by the LEG and HEG of the 3CR sample (red plusses and blue asterisks respectively). The ellipse marks the boundaries of the location of Seyfert galaxies (e.g. Whittle 1985).

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