Table 2: Sample of B3-VLA quasars studied: results of the analysis.
Object z $S_{\rm 408}$ $\alpha_{\rm 408}^{\rm 1460}$ Obs. K mag $\chi^2/\nu$ $P_{\rm ext}$ % $_{\rm ext}$ Ext. $\alpha$ $P_{\rm e}$ $P_{\rm d}$ $P_{\rm e}/P_{\rm d}$ $K_{\rm HG}$ $K_{\rm nuc}$ $r_{\rm e}$

(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) (15) (16) (17)

0006+397 1.830 1.15 0.66 O₁ 16.72 $\pm$ 0.12 1.98 95.8 19.5 Yes 0.55 48 13 3.7 18.5 $\pm$ 0.2 17.0 $\pm$ 0.2 2.39 $\pm$ 0.09

0019+431 1.050 2.22 1.34 O₁ 15.47 $\pm$ 0.12 0.38 90.4 5.5 No - - - - - - -

0022+390 1.932 1.10 0.10 O₁ 16.65 $\pm$ 0.13 8.70 99.8 41.4 Yes 0.38 84 9 9.1 17.6 $\pm$ 0.2 17.2 $\pm$ 0.1 2.00 $\pm$ 0.02

0032+423 1.588 0.92 0.94 W 16.24 $\pm$ 0.08 <0.03 90.0 <1.0 No - - - - - - -

0110+401 1.479 1.08 0.65 O₁ 17.13 $\pm$ 0.09 4.48 98.6 51.8 Yes 0.40 84 11 7.7 17.9 $\pm$ 0.2 17.9 $\pm$ 0.2 3.60 $\pm$ 0.02

0137+401 1.620 0.82 0.85 O₁ 16.94 $\pm$ 0.05 0.91 91.8 16.5 No - - - - - - -

0143+446 0.813 1.71 0.99 O₁ 13.99 $\pm$ 0.16 6.89 99.5 11.5 ? 0.40 84 11 7.7 16.3 $\pm$ 0.1 14.1 $\pm$ 0.2 7.09 $\pm$ 0.02

0144+430 1.790 0.92 1.01 W 16.17 $\pm$ 0.03 <0.03 90.0 15.3 No - - - - - - -

0144+432 1.260 0.82 0.70 O₁ 17.12 $\pm$ 0.18 8.73 99.8 80.2 Yes 0.40 84 11 7.7 17.4 $\pm$ 0.1 18.9 $\pm$ 0.4 4.45 $\pm$ 0.02

0157+442 0.721 3.26 0.91 O₁ 16.32 $\pm$ 0.17 18.74 99.9 83.4 Yes 0.39 84 11 7.7 16.5 $\pm$ 0.1 18.3 $\pm$ 0.4 4.09 $\pm$ 0.02

0158+394 0.780 0.12 0.18 O₂ 16.34 $\pm$ 0.07 5.45 99.1 6.8 No - - - - - - -

0217+417 1.430 0.85 0.94 O₁ 17.18 $\pm$ 0.15 2.16 96.2 <1.0 No - - - - - - -

0219+443 0.852 0.89 1.17 W 14.88 $\pm$ 0.02 2.55 96.7 42.3 Yes 0.51 61 13 4.8 15.8 $\pm$ 0.1 15.4 $\pm$ 0.1 1.73 $\pm$ 0.15

0226+467 1.216 2.45 0.93 O₁ 16.27 $\pm$ 0.08 8.23 99.8 44.7 Yes 0.37 84 9 9.1 17.2 $\pm$ 0.2 16.9 $\pm$ 0.1 5.25 $\pm$ 0.02

0232+411b 0.500 2.75 0.99 W 14.27 $\pm$ 0.02 7.63 99.6 34.2 Yes 0.36 84 9 9.1 15.4 $\pm$ 0.1 14.7 $\pm$ 0.1 1.44 $\pm$ 0.01

0249+383 1.120 0.95 0.34 W 16.17 $\pm$ 0.06 4.38 98.5 46.0 Yes 0.60 40 17 2.3 16.8 $\pm$ 0.1 17.0 $\pm$ 0.1 2.01 $\pm$ 0.13

0255+460 1.210 1.74 0.77 O₁ 17.89 $\pm$ 0.20 0.30 90.2 <1.0 No - - - - - - -

0704+384 0.579 2.87 1.06 O₁ 15.02 $\pm$ 0.16 17.62 99.9 33.5 Yes 0.37 84 9 9.1 16.2 $\pm$ 0.1 15.5 $\pm$ 0.2 5.91 $\pm$ 0.02

0729+391 0.663 0.26 0.43 O₁ 15.60 $\pm$ 0.14 20.38 99.9 91.7 Yes 0.57 48 15 3.2 15.7 $\pm$ 0.1 18.3 $\pm$ 0.2 3.77 $\pm$ 0.02

0740+380C 1.063 5.55 1.29 O₂ 15.62 $\pm$ 0.05 23.02 99.9 35.5 Yes 0.60 40 17 2.3 16.8 $\pm$ 0.3 16.1 $\pm$ 0.2 4.08 $\pm$ 0.08

0926+388 1.630 0.50 1.09 O₂ 17.09 $\pm$ 0.08 9.95 99.9 23.6 Yes 0.56 48 15 3.2 18.7 $\pm$ 0.4 17.4 $\pm$ 0.1 4.05 $\pm$ 0.14

1123+395 1.470 0.36 0.82 O₂ 15.72 $\pm$ 0.05 5.45 99.1 2.2 No - - - - - - -

1148+387 1.303 1.83 0.94 O₂ 14.93 $\pm$ 0.05 3.85 97.9 <1.0 No - - - - - - -

1206+439B 1.400 5.69 0.85 O₂ 15.10 $\pm$ 0.05 4.85 98.8 <1.0 No - - - - - - -

1315+396 1.560 1.16 0.49 O₂ 15.93 $\pm$ 0.06 4.85 98.8 28.3 Yes 0.49 61 13 4.8 17.3 $\pm$ 0.3 16.3 $\pm$ 0.1 3.20 $\pm$ 0.11

1435+383 1.600 0.54 0.85 O₂ 16.32 $\pm$ 0.06 4.25 98.3 <1.0 No - - - - - - -

2311+469 0.745 4.34 0.69 O₁ 14.79 $\pm$ 0.06 1.01 92.2 3.5 No - - - - - - -

2332+388 3.200 0.42 0.94 O₁ 17.66 $\pm$ 0.14 0.68 91.0 12.5 No - - - - - - -

2344+429 1.556 0.92 0.58 O₁ 16.30 $\pm$ 0.07 1.10 92.7 <1.0 No - - - - - - -

2349+410 2.046 1.38 0.98 O₁ 16.78 $\pm$ 0.18 3.18 97.5 13.8 Yes 0.48 61 13 4.8 19.1 $\pm$ 0.4 17.1 $\pm$ 0.2 3.35 $\pm$ 0.02

2351+456 2.000 2.21 0.27 O₁ 16.03 $\pm$ 0.16 6.39 99.4 17.9 Yes 0.39 84 11 7.7 18.0 $\pm$ 0.2 16.4 $\pm$ 0.2 2.54 $\pm$ 0.08

(1) Object name in the B3-VLA sample. (2) Object redshift (Vigotti et al. 1997). (3) Radio flux in Jy at 408 MHz. (4) Radio spectral index, $\alpha_{\rm 408}^{\rm 1460}$ , defined as $S_{1460}=S_{408}\nu^{-\alpha_{\rm 408}^{\rm 1460}}$ . (5) Observing run: W, September 1996, WHT La Palma. O₁, October 1997, 3.5m Calar Alto. O₂, February 1999, 3.5 m Calar Alto. (6) K-band aperture photometry. (7) $\chi^2/\nu$ of the surface brightness fitting to the PSF model. (8) percentage probability of being extended, derived from the previous $\chi^2/\nu$ . (9) Contribution of the possible extension to the total flux. (10) Classification output (Yes = Extended, No = Not Extended). (11) Free parameter of the generalized model ( $\alpha=1$ for disk galaxies, $\alpha=0.25$ for elliptical galaxies). (12) percentage probability of being an elliptical galaxy. (13) percentage probability of being a disk galaxy. (14) Ratio of both probabilities. (15) Host K-band magnitude. (16) Nucleus K-band magnitude. (17) Effective radius of the Host in arcsec.

**Table 2:** Sample of B3-VLA quasars studied: results of the analysis.
Object	z	$S_{\rm 408}$	$\alpha_{\rm 408}^{\rm 1460}$	Obs.	K mag	$\chi^2/\nu$	$P_{\rm ext}$	% $_{\rm ext}$	Ext.	$\alpha$	$P_{\rm e}$	$P_{\rm d}$	$P_{\rm e}/P_{\rm d}$	$K_{\rm HG}$	$K_{\rm nuc}$	$r_{\rm e}$
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)	(14)	(15)	(16)	(17)
0006+397	1.830	1.15	0.66	O₁	16.72 $\pm$ 0.12	1.98	95.8	19.5	Yes	0.55	48	13	3.7	18.5 $\pm$ 0.2	17.0 $\pm$ 0.2	2.39 $\pm$ 0.09
0019+431	1.050	2.22	1.34	O₁	15.47 $\pm$ 0.12	0.38	90.4	5.5	No	-	-	-	-	-	-	-
0022+390	1.932	1.10	0.10	O₁	16.65 $\pm$ 0.13	8.70	99.8	41.4	Yes	0.38	84	9	9.1	17.6 $\pm$ 0.2	17.2 $\pm$ 0.1	2.00 $\pm$ 0.02
0032+423	1.588	0.92	0.94	W	16.24 $\pm$ 0.08	<0.03	90.0	<1.0	No	-	-	-	-	-	-	-
0110+401	1.479	1.08	0.65	O₁	17.13 $\pm$ 0.09	4.48	98.6	51.8	Yes	0.40	84	11	7.7	17.9 $\pm$ 0.2	17.9 $\pm$ 0.2	3.60 $\pm$ 0.02
0137+401	1.620	0.82	0.85	O₁	16.94 $\pm$ 0.05	0.91	91.8	16.5	No	-	-	-	-	-	-	-
0143+446	0.813	1.71	0.99	O₁	13.99 $\pm$ 0.16	6.89	99.5	11.5	?	0.40	84	11	7.7	16.3 $\pm$ 0.1	14.1 $\pm$ 0.2	7.09 $\pm$ 0.02
0144+430	1.790	0.92	1.01	W	16.17 $\pm$ 0.03	<0.03	90.0	15.3	No	-	-	-	-	-	-	-
0144+432	1.260	0.82	0.70	O₁	17.12 $\pm$ 0.18	8.73	99.8	80.2	Yes	0.40	84	11	7.7	17.4 $\pm$ 0.1	18.9 $\pm$ 0.4	4.45 $\pm$ 0.02
0157+442	0.721	3.26	0.91	O₁	16.32 $\pm$ 0.17	18.74	99.9	83.4	Yes	0.39	84	11	7.7	16.5 $\pm$ 0.1	18.3 $\pm$ 0.4	4.09 $\pm$ 0.02
0158+394	0.780	0.12	0.18	O₂	16.34 $\pm$ 0.07	5.45	99.1	6.8	No	-	-	-	-	-	-	-
0217+417	1.430	0.85	0.94	O₁	17.18 $\pm$ 0.15	2.16	96.2	<1.0	No	-	-	-	-	-	-	-
0219+443	0.852	0.89	1.17	W	14.88 $\pm$ 0.02	2.55	96.7	42.3	Yes	0.51	61	13	4.8	15.8 $\pm$ 0.1	15.4 $\pm$ 0.1	1.73 $\pm$ 0.15
0226+467	1.216	2.45	0.93	O₁	16.27 $\pm$ 0.08	8.23	99.8	44.7	Yes	0.37	84	9	9.1	17.2 $\pm$ 0.2	16.9 $\pm$ 0.1	5.25 $\pm$ 0.02
0232+411b	0.500	2.75	0.99	W	14.27 $\pm$ 0.02	7.63	99.6	34.2	Yes	0.36	84	9	9.1	15.4 $\pm$ 0.1	14.7 $\pm$ 0.1	1.44 $\pm$ 0.01
0249+383	1.120	0.95	0.34	W	16.17 $\pm$ 0.06	4.38	98.5	46.0	Yes	0.60	40	17	2.3	16.8 $\pm$ 0.1	17.0 $\pm$ 0.1	2.01 $\pm$ 0.13
0255+460	1.210	1.74	0.77	O₁	17.89 $\pm$ 0.20	0.30	90.2	<1.0	No	-	-	-	-	-	-	-
0704+384	0.579	2.87	1.06	O₁	15.02 $\pm$ 0.16	17.62	99.9	33.5	Yes	0.37	84	9	9.1	16.2 $\pm$ 0.1	15.5 $\pm$ 0.2	5.91 $\pm$ 0.02
0729+391	0.663	0.26	0.43	O₁	15.60 $\pm$ 0.14	20.38	99.9	91.7	Yes	0.57	48	15	3.2	15.7 $\pm$ 0.1	18.3 $\pm$ 0.2	3.77 $\pm$ 0.02
0740+380C	1.063	5.55	1.29	O₂	15.62 $\pm$ 0.05	23.02	99.9	35.5	Yes	0.60	40	17	2.3	16.8 $\pm$ 0.3	16.1 $\pm$ 0.2	4.08 $\pm$ 0.08
0926+388	1.630	0.50	1.09	O₂	17.09 $\pm$ 0.08	9.95	99.9	23.6	Yes	0.56	48	15	3.2	18.7 $\pm$ 0.4	17.4 $\pm$ 0.1	4.05 $\pm$ 0.14
1123+395	1.470	0.36	0.82	O₂	15.72 $\pm$ 0.05	5.45	99.1	2.2	No	-	-	-	-	-	-	-
1148+387	1.303	1.83	0.94	O₂	14.93 $\pm$ 0.05	3.85	97.9	<1.0	No	-	-	-	-	-	-	-
1206+439B	1.400	5.69	0.85	O₂	15.10 $\pm$ 0.05	4.85	98.8	<1.0	No	-	-	-	-	-	-	-
1315+396	1.560	1.16	0.49	O₂	15.93 $\pm$ 0.06	4.85	98.8	28.3	Yes	0.49	61	13	4.8	17.3 $\pm$ 0.3	16.3 $\pm$ 0.1	3.20 $\pm$ 0.11
1435+383	1.600	0.54	0.85	O₂	16.32 $\pm$ 0.06	4.25	98.3	<1.0	No	-	-	-	-	-	-	-
2311+469	0.745	4.34	0.69	O₁	14.79 $\pm$ 0.06	1.01	92.2	3.5	No	-	-	-	-	-	-	-
2332+388	3.200	0.42	0.94	O₁	17.66 $\pm$ 0.14	0.68	91.0	12.5	No	-	-	-	-	-	-	-
2344+429	1.556	0.92	0.58	O₁	16.30 $\pm$ 0.07	1.10	92.7	<1.0	No	-	-	-	-	-	-	-
2349+410	2.046	1.38	0.98	O₁	16.78 $\pm$ 0.18	3.18	97.5	13.8	Yes	0.48	61	13	4.8	19.1 $\pm$ 0.4	17.1 $\pm$ 0.2	3.35 $\pm$ 0.02
2351+456	2.000	2.21	0.27	O₁	16.03 $\pm$ 0.16	6.39	99.4	17.9	Yes	0.39	84	11	7.7	18.0 $\pm$ 0.2	16.4 $\pm$ 0.2	2.54 $\pm$ 0.08

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