Table 1: The sources and their core luminosities in the radio, $L_{\nu {\rm r}}$ ( $\times 10^{23}$ W Hz-1), and IR/optical/UV bands, $L_{\nu {\rm IR}}$, $L_{\nu {\rm o}}$ and $L_{\nu {\rm UV}}$( $\times 10^{19}$ W Hz-1).

Source		 Alt. name z Envir. $L^{a}_{\nu {\rm r}}$ $L_{\nu {\rm IR}}$ $L^{e}_{\nu {\rm o}}$ $L_{\nu {\rm UV}}$

3C  29		   0.0438 A 119 3.5   4.1 *
3C  31 NGC 383 0.0169 Arp 331 0.51   1.6  
3C 66B   0.0215   1.6   8.8 3.5h, 2.5i, 1.35m
3C  78 NGC 1218 0.0288   15   96, 85f 27.5m
3C 83.1 NGC 1265 0.0251 Perseus 0.26   0.42  
3C  189 NGC 2484 0.0413   6.5   25g  
3C 272.1 M 84 0.0037 Virgo 0.047 1.0b, 0.95c, 1.1d 0.37g, 0.13f  
3C 277.3   0.0857 Coma A 1.8   3.7, 5.4f  
3C 288   0.246   39   15.1  
3C 296 NGC 5532 0.0237   0.84   0.65  
3C 310   0.0535   4.5   3.6  
3C 317   0.0342 A 2052 8.9 27b 5.1g, 3.8f 0.22m
3C 338 NGC 6166 0.0303 A 2199 1.9 2.6b 3.0 0.14m
3C 346   0.162   120   241 29l
3C 348   0.154 Her A 4.9   8.1  
3C 442 NGC 7237 0.0262 Arp 169 0.027   0.23, 0.13f  
3C 449   0.0171   0.21   2.5 *
a 5 GHz; b 16 000 Å; c 11 000 Å; d 20 500 Å; e 7020 Å; f 5500 Å; g 8140 Å; h 4440 Å; i 3400 Å; l 1400 Å; m 2500 Å; * we did not use the HST data in the UV band for 3C 29 and 3C 449 since the nuclear emission of these sources is clearly affected by obscuration from extended (kpc-scale) dusty structures (Chiaberge et al. 2002).

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