3 Observations and final sample selection

All the 122 pre-selected sources were observed with the VLA between 1995 and 1998 (see Table 1 for details). At least one snapshot at 1.4 and 4.9 GHz was obtained for each source. When possible, we obtained for the same source snapshots in B- and C-configurations at both frequencies to increase the image quality by combining the two different configuration data. The radio sources 3C286 and/or 3C48 served as primary flux density calibrators. The interferometric phases were calibrated using nearby radio sources selected from the VLA calibrator manual (Perley & Taylor 2000). The processes of self-calibration and imaging of the data were carried out with the NRAO AIPS package, following standard procedures. Due to the large size of the sources, all the maps made at 4.9 GHz and, when necessary, also at 1.4 GHz, were corrected for primary beam attenuation.

The aims of the observations were to confirm large angular size radio galaxies, reject those objects which were in fact the result of the superposition of two or three adjacent sources (see Fig. 1) and isolate the core emission to obtain accurate positions for subsequent optical identification and redshift determination.

Figure 1: Illustration of the necessity of high resolution observations of NVSS sources in order to discard some objects resulting from superposition of several unrelated sources. Top: an image of a presumed large size double radio galaxy selected from the NVSS. Bottom: the corresponding image obtained from VLA B-configuration observations at 1.4 GHz

82 of the 122 pre-selected radio sources were identified beyond doubt with single radio galaxies. 13 of those 82 sources turned out to have a size slightly smaller than 4 $\hbox {$^\prime $ }$ after accurate measurements from higher resolution observations. Another source has a total flux density at 1.4 GHz below 100 mJy after the subtraction of the flux density from a closeby unrelated source. However, we have kept them all in the final sample since this fact will not influence our considerations. Although the integration time (10 min on average) was not too long on each single source, thanks to the use of combined arrays and to the good uv-coverage of the VLA observing with the snapshot technique, we obtained the high quality images shown in Fig. 10. We present only total intensity data.

In Table 2 we report the most relevant physical parameters of the 84 radio galaxies in the final sample (82 selected objects plus the two forementioned giants 4C+73.08 and 4C+74.26). Coordinates are derived from Gaussian fits of the core component at our highest angular resolution observations (commonly 4.9 GHz, B-configuration). Total flux densities at 1.4 GHz ( $S_{\rm t}^{1.4}$) are from the NVSS, except when a higher resolution image is necessary to isolate and subtract discrete unrelated sources. Angular sizes are measured along the spine of the sources using our VLA maps at 1.4 GHz, or the NVSS maps when there is extended emission resolved out in our observations. The core flux density at 1.4 GHz ( $S_{\rm c}^{1.4}$) and 4.9 GHz ( $S_{\rm c}^{4.9}$) has been estimated fitting a Gaussian component to the core using AIPS task JMFIT. The peak flux density of the Gaussian was taken as the core flux density. The core peak flux densities of those sources whose cores have very different peak and integrated fluxes (peak to integrated ratio <0.8) have been marked with an "e'' in Table 2. Known redshifts were compiled from the NASA Extragalactic Database (NED) and from Schoenmakers (1999). 44 new redshifts were derived from our optical observations (Paper II). At present, the distance information is available for 71 of the sources (6 of which have uncertain redshift determination). When a redshift measure is available, we give also physical results as the projected linear size, the total radio power at 1.4 GHz ( $P_{\rm t}^{1.4}$) and the core radio power at 1.4 GHz ( $P_{\rm c}^{1.4}$) and 4.9 GHz ( $P_{\rm c}^{4.9}$).

   

Table 1: VLA observations

Array	$\nu$	$\Delta\nu$	Date	Codea
	(MHz)	(MHz)
B	1465	50	19 Nov. 95	a
C	1465	50	19 Feb. 96	b
C	4885	100	19 Feb. 96	c
B	1418	50	18-21 Feb. 97	d
B	4885	100	18-21 Feb. 97	e
B	1452	50	25 May 97	f
B	4885	100	25 May 97	g
C	1465	50	27 Jul. 97	h
C	4885	100	27 Jul. 97	i
B	1465	50	7 Oct. 98	j
B	4885	100	7 Oct. 98	k
C	1465	50	28 Dec. 98	l
C	4885	100	28 Dec. 98	m

^a Letter code used in Table 3 to show the observations made on each source.

   

Table 2: Radio sample of large angular size radio galaxies from the NVSS survey

Name	RA (J2000.0)	Dec. (J2000.0)	$S_{\rm t}^{1.4}$	Size	$S_{\rm c}^{1.4}$		$S_{\rm c}^{4.9}$		.	z	Size	$P_{\rm t}^{1.4}$	$P_{\rm c}^{1.4}$	$P_{\rm c}^{4.9}$	Type$^{\ast}$
	( $^{\rm h}~~^{\rm m}~~^{\rm s}$)	($^{\circ}$   $\hbox {$^\prime $ }$   $\hbox{$^{\prime\prime}$ }$)	(mJy)	( $\hbox {$^\prime $ }$)	(mJy)		(mJy)		.		(Kpc)	W/Hz	W/Hz	W/Hz
J0109+731	01 09 44.265	73 11 57.17	3030	4.0	22	.	0	10	.	0	0.181a	943	26.67	24.53	24.18	II
J0153+712	01 53 25.786	71 15 06.53	1200	7.0	512	.	3	292	.	2	0.022a	259	24.40	24.03	23.79	I
J0317+769	03 17 54.061	76 58 37.82	196	3.4	25	.	3e	11	.	9	0.094	476	24.89	24.00	23.67	I
J0318+684	03 18 19.026	68 29 32.08	823	15.1	22	.	0	44	.	0	0.090b	2040	25.48	23.90	24.20	II
J0342+636	03 42 10.148	63 39 33.73	284	4.1	10	.	4	11	.	3	0.128	741	25.33	23.89	23.93	II
J0430+773	04 30 49.490	77 22 58.44	150	4.9	3	.	3	5	.	6	0.215	1306	25.52	23.86	24.09	II
J0455+603	04 55 47.039	60 23 36.17	109	4.0	21	.	5	7	.	3	--	--	--	--	--	I
J0502+670	05 02 54.732	67 02 30.15	104	4.8	6	.	9	2	.	3	0.085	617	24.53	23.35	22.87	I
J0508+609	05 08 27.258	60 56 27.48	221	10.4	71	.	0	74	.	8	0.071	1142	24.69	24.20	24.22	I
J0519+702	05 19 17.132	70 13 48.68	254	4.8	18	.	9e	11	.	3	0.144	952	25.38	24.26	24.03	I
J0525+718	05 25 27.094	71 52 39.25	69	4.6	4	.	7e	1	.	5	0.150	942	24.85	23.68	23.19	I
J0531+677	05 31 25.925	67 43 50.23	210	9.6	106	.	6e	10	.	6e	0.017	276	23.42	23.13	22.12	I
J0546+633	05 46 24.622	63 21 32.50	392	11.0	29	.	0	13	.	5	0.049a	865	24.62	23.49	23.15	I
J0559+607	05 59 38.690	60 44 00.96	115	7.1	2	.	5	2	.	2	0.042	484	23.95	22.29	22.23	I
J0607+612	06 07 34.919	61 14 43.52	358	5.3	4	.	5	4	.	1	0.227	1465	25.94	24.04	24.00	?
J0624+630	06 24 29.063	63 04 02.50	181	5.4	3	.	5	4	.	4	0.085	694	24.77	23.05	23.15	I
J0633+721	06 33 40.842	72 09 24.92	308	5.0	14	.	0	12	.	0	0.090b	675	25.05	23.71	23.64	?
J0654+733	06 54 26.525	73 19 50.36	868	12.2	3	.	2	4	.	1	0.115b	2015	25.71	23.28	23.39	II
J0750+656	07 50 34.425	65 41 25.50	120	3.7	26	.	8	29	.	4	0.747	1798	26.57	25.92	25.96	II
J0757+826	07 57 35.172	82 39 40.86	153	4.0	33	.	7	17	.	1e	0.087?	524	24.71	24.06	23.76	I
J0803+669	08 03 45.829	66 56 11.39	182	4.7	5	.	2	3	.	8	0.247?	1374	25.73	24.18	24.04	II
J0807+740	08 07 10.070	74 00 41.58	152	9.1	14	.	0	12	.	4	0.120b	1566	25.00	23.96	23.91	?
J0819+756	08 19 50.504	75 38 39.53	616	7.8	30	.	7	56	.	6	0.232b	2190	26.20	24.90	25.16	II
J0825+693	08 25 59.770	69 20 38.59	141	7.2	7	.	1	7	.	1	0.538a	3162	26.33	25.03	25.03	II
J0828+632	08 28 56.363	63 13 45.05	182	4.0	6	.	3	3	.	7	--	--	--	--	--	?
J0856+663	08 56 16.260	66 21 26.50	236	3.8	5	.	3	10	.	3	0.489	1607	26.47	24.82	25.11	II
J0926+653	09 26 00.822	65 19 22.88	101	5.3	1	.	0e	2	.	2e	0.140	1028	24.96	22.95	23.30	I
J0926+610	09 26 53.408	61 00 24.87	300	3.7	6	.	8	7	.	2	0.243	1070	25.93	24.28	24.31	II
J0939+740	09 39 46.833	74 05 30.78	100	8.0	3	.	9	4	.	5	0.122b	1387	24.83	23.42	23.48	I
J0949+732c	09 49 46.157	73 14 23.82	2537	15.0	15	.	6	20	.	0	0.058a	1375	25.58	23.37	23.47	II
J1015+683	10 15 21.620	68 23 58.24	390	4.0	--		5	6	.	0.199	1010	25.86	--	24.02	?
J1036+677	10 36 41.237	67 47 53.44	231	4.0	2	.	6	3	.	8	--	--	--	--	--	II
J1124+749	11 24 47.045	74 55 45.31	125	5.6	38	.	4	23	.	8	0.052	465	24.17	23.66	23.45	I
J1137+613	11 37 21.289	61 20 01.88	1160	3.4	13	.	1e	12	.	5	0.111	549	25.81	23.87	23.85	II
J1211+743	12 11 58.710	74 19 04.12	628	7.5	9	.	7	11	.	3	0.107	1171	25.51	23.70	23.77	?
J1216+674	12 16 37.239	67 24 41.97	187	5.8	2	.	0	3	.	2	0.362	2126	26.09	24.12	24.32	II
J1220+636	12 20 36.477	63 41 43.82	261	5.2	4	.	2	6	.	4	--	--	--	--	--	II
J1247+673	12 47 33.319	67 23 16.34	388	12.4	262	.	4	179	.	0	0.107a	1938	25.30	25.13	24.97	II
J1251+756	12 51 05.977	75 37 38.94	100	4.0	2	.	9	4	.	4	0.197	1002	25.26	23.72	23.90	II
J1251+787	12 51 23.839	78 42 36.29	166	19.5	13	.	2	15	.	5	--	--	--	--	--	I
J1313+696	13 13 58.878	69 37 18.74	1384	6.9	10	.	2e	3	.	8	0.106a	1062	25.85	23.71	23.29	II
J1410+633	14 10 30.609	63 19 00.55	249	3.4	3	.	1e	1	.	1e	0.158	724	25.46	23.55	23.10	II

$^{\ast}$ I and II stand for FR I and FR II type radio galaxies, respectively.
^a Redshift taken from the NASA Extragalactic Database.
^b Redshift from Schoenmakers (1999).
^c Coordinates taken from Saripalli et al. (1997).
Label "e'' by the core flux density means extended core (see text).
New giant radio galaxies are written in boldface.

 

Table 2: continued

Name	RA (J2000.0)	Dec. (J2000.0)	$S_{\rm t}^{1.4}$	Size	$S_{\rm c}^{1.4}$		$S_{\rm c}^{4.9}$		.	z	Size	$P_{\rm t}^{1.4}$	$P_{\rm c}^{1.4}$	$P_{\rm c}^{4.9}$	Type$^{\ast}$
	( $^{\rm h}~~^{\rm m}~~^{\rm s}$)	($^{\circ}$   $\hbox {$^\prime $ }$   $\hbox{$^{\prime\prime}$ }$)	(mJy)	( $\hbox {$^\prime $ }$)	(mJy)		(mJy)		.		(Kpc)	W/Hz	W/Hz	W/Hz
J1504+689	15 04 12.781	68 56 12.75	451	3.4	88	.	4	72	.	1	0.318a	1160	26.35	25.64	25.55	II-QSS
J1523+636	15 23 45.900	63 39 23.78	676	3.5	18	.	3e	14	.	5	0.204a	899	26.12	24.55	24.45	II
J1530+824	15 30 56.110	82 27 21.02	180	6.6	40	.	6	27	.	2e	0.021a	236	23.55	22.90	22.73	I
J1536+843	15 36 57.335	84 23 10.42	375	8.0	4	.	9	3	.	3	0.201b	2033	25.85	23.97	23.80	II
J1557+706	15 57 30.190	70 41 20.79	1800	11.3	25	.	2	31	.	3	0.026a	490	24.72	22.87	22.96	I
J1632+825	16 32 31.630	82 32 16.28	2200	66.0	428	.	2	286	.	0	0.023a	2544	24.70	23.99	23.82	I
J1650+815	16 50 58.686	81 34 28.11	313	5.6	44	.	4	32	.	8	0.038a	348	24.30	23.45	23.32	I
J1732+714	17 32 33.001	71 24 10.50	616	4.0	35	.	1e	9	.	5e	0.059a	372	24.98	23.73	23.16	I
J1733+707	17 33 12.525	70 46 30.36	240	4.5	10	.	6e	8	.	1	0.041a	299	24.24	22.89	22.77	I
J1743+712	17 43 17.681	71 12 53.98	142	4.0	9	.	2	13	.	1	--	--	--	--	--	II
J1745+712	17 45 43.573	71 15 48.55	883	4.4	25	.	9e	10	.	9	0.216a	1176	26.29	24.76	24.38	II
J1751+680	17 51 19.629	68 04 43.05	153	8.1	11	.	8e	9	.	0	0.079	978	24.63	23.52	23.40	I
J1754+626	17 54 50.310	62 38 41.96	991	16.2	5	.	0	5	.	6	0.028a	754	24.53	22.23	22.28	I
J1800+717	18 00 42.622	71 44 41.99	144	4.2	1	.	4	0	.	9	--	--	--	--	--	II
J1835+665	18 35 07.338	66 35 00.02	136	4.4	2	.	9	1	.	6	0.354?	1594	25.93	24.26	24.00	II
J1835+620	18 35 10.405	62 04 07.42	800	3.9	2	.	0e	1	.	7	0.518	1688	27.05	24.45	24.38	II
J1844+653	18 44 07.443	65 22 03.07	104	7.5	0	.	8	1	.	9	0.197	1881	25.28	23.16	23.54	II
J1845+818	18 45 15.836	81 49 30.98	596	4.4	5	.	2	6	.	9	0.119	750	25.58	23.52	23.65	II
J1847+707	18 47 34.912	70 44 00.64	226	3.8	31	.	2e	8	.	1e	0.043	265	24.26	23.40	22.82	I
J1850+645	18 50 45.871	64 30 24.68	154	5.6	10	.	6e	4	.	0e	0.080	683	24.64	23.48	23.06	I
J1853+800	18 53 52.077	80 02 50.46	155	5.6	3	.	4e	2	.	1	0.214a	1486	25.53	23.87	23.66	II
J1918+742	19 18 34.885	74 15 05.05	570	6.6	26	.	1	8	.	8	0.194	1636	26.00	24.66	24.19	II
J1951+706	19 51 40.825	70 37 39.99	100	5.2	3	.	4	6	.	0	0.550	2303	26.20	24.74	24.98	II
J2016+608	20 16 18.630	60 53 57.49	332	3.0	2	.	3e	2	.	2	0.121	519	25.35	23.19	23.17	II
J2035+680	20 35 16.549	68 05 41.60	156	11.5	10	.	6	15	.	5	0.133	2143	25.10	23.93	24.10	I
J2042+751c	20 42 37.180	75 08 02.52	1805	10.6	184	.	0	328	.	0	0.104a	1617	25.94	24.95	25.20	II-QSS
J2059+627	20 59 09.560	62 47 44.11	113	4.7	3	.	0	4	.	0	0.267	1444	25.59	24.01	24.14	II?
J2103+649	21 03 13.868	64 56 55.26	123	4.8	9	.	8	7	.	3e	0.215	1279	25.43	24.33	24.20	II
J2111+630	21 11 20.268	63 00 06.17	285	7.0	--		1	0	.	--	--	--	--	--	II
J2114+820	21 14 01.179	82 04 48.28	483	6.0	141	.	1	140	.	9	0.085	772	25.19	24.66	24.66	I
J2128+603	21 28 02.634	60 21 07.96	258	5.9	4	.	5e	6	.	4	0.072?	656	24.77	23.02	23.17	II
J2138+831	21 38 42.266	83 06 49.21	305	5.1	30	.	2	13	.	8	0.135	962	25.41	24.40	24.06	?
J2145+819	21 45 29.887	81 54 54.22	400	18.7	12	.	0	8	.	2	0.146b	3739	25.59	24.07	23.90	II
J2157+664	21 57 02.572	66 26 10.24	1070	5.0	--		34	6	.	0.057?	451	25.19	--	23.70	?
J2204+783	22 04 09.225	78 22 46.92	251	4.0	3	.	4	5	.	4	0.115	663	25.18	23.31	23.51	II
J2209+727	22 09 33.780	72 45 58.36	248	3.7	--		0	4	.	0.201	940	25.67	--	22.88	II
J2242+622	22 42 32.133	62 12 17.53	287	4.2	1	.	6	1	.	9	0.188?	1018	25.68	23.42	23.50	II
J2247+633	22 47 29.714	63 21 15.55	477	4.4	6	.	7e	4	.	2	--	--	--	--	--	I
J2250+729	22 50 43.621	72 56 16.19	653	3.8	--		0	9e	.	--	--	--	--	--	II
J2255+645	22 55 29.943	64 30 06.86	392	4.0	4	.	9	7	.	3	--	--	--	--	--	II
J2307+640	23 07 58.533	64 01 39.22	171	4.6	7	.	3	4	.	3	--	--	--	--	--	II
J2340+621	23 40 56.435	62 10 45.09	185	4.1	2	.	0	2	.	6	--	--	--	--	--	I

$^{\ast}$ I and II stand for FR I and FR II type radio galaxies, respectively.
^a Redshift from the NASA Extragalactic Database.
^b Redshift from Schoenmakers (1999).
^c Core flux densities taken from Pearson et al. (2000).
Label "e'' by the core flux density means extended core (see text).
New giant radio galaxies are written in boldface.

   

Table 3: Map parameters

Name	Observationsa	1.4 GHz			4.9 GHz
		Beam		1st contour	Beam		1st contour
		" $\times$ "	PA	mJy/beam	" $\times$ "	PA	mJy/beam
J0109+731	j,k	5.9 $\times$ 3.7	-39.6	0.86	1.7 $\times$ 1.7		0.39
J0153+712	j,k,l	10.7 $\times$ 9.6	-31.9	1.0	-		N.S.
J0317+769	b,c,d,g,l	22.0 $\times$ 12.1	-68.0	0.7	3.7 $\times$ 2.9	-88.3	0.15
J0318+684	a,b,c	-	N.S.b	-		N.S.
J0342+636	b,f,k	10.6 $\times$ 9.7	68.8	0.45	1.5 $\times$ 1.5		0.16
J0430+773	b,c,f,g	10.6 $\times$ 10.2	82.9	0.6	3.8 $\times$ 3.0	-68.9	0.18
J0455+603	b,c,f	5.9 $\times$ 4.7	46.1	0.14	-		N.S.
J0502+670	b,c,f,k	10.7 $\times$ 9.9	89.2	0.2	3.3 $\times$ 3.1	-64.6	0.1
J0508+609	a,b,c,g	15.0 $\times$ 10.2	-74.5	0.2	3.3 $\times$ 2.8	63.0	0.2
J0519+702	a,b,c,g	13.4 $\times$ 10.4	82.4	0.4	4.4 $\times$ 2.8	-56.1	0.1
J0525+718	a,b,c,g	13.3 $\times$ 10.0	83.1	0.4	-		N.S.
J0531+677	b,c,d,g	25.0 $\times$ 25.0		0.8	1.6 $\times$ 1.6		0.17
J0546+633	a,b,c,g	15.4 $\times$ 10.5	-67.8	0.25	4.2 $\times$ 3.1	72.6	0.1
J0559+607	b,c,f	11.2 $\times$ 9.3	59.5	0.2	-		N.S.
J0607+612	a,b,c,k	15.2 $\times$ 11.5	-68.8	0.4	4.1 $\times$ 3.0	59.0	0.1
J0624+630	b,c,f,g	11.2 $\times$ 9.5	66.0	0.3	3.9 $\times$ 3.3	69.3	0.1
J0633+721	a,b,c,g	13.2 $\times$ 10.9	-82.3	0.3	4.6 $\times$ 2.7	44.0	0.1
J0654+733	a,b,c	16.2 $\times$ 12.5	60.6	0.4	-		N.S.
J0750+656	d,h,k	9.2 $\times$ 4.8	-80.9	0.5	1.7 $\times$ 1.7		0.15
J0757+826	d,h,m	22.0 $\times$ 22.0		5.0	6.1 $\times$ 6.1		0.3
J0803+669	b,c,f	6.7 $\times$ 4.7	58.9	0.35	-		N.S.
J0807+740	a,b,c	13.0 $\times$ 11.3	-30.2	0.3	-		N.S.
J0819+756	a,b,c,g	13.9 $\times$ 12.6	13.2	0.3	7.7 $\times$ 7.7		0.4
J0825+693	a,b,c,g	-		N.S.	-		N.S.
J0828+632	d,h,k	9.8 $\times$ 6.3	-72.1	0.4	1.7	1.7	0.15
J0856+663	b,c,f	13.4 $\times$ 13.4		0.6	-		N.S.
J0926+653	d,h,m	26.0 $\times$ 26.0		1.3	6.1 $\times$ 6.1		0.15
J0926+610	d,k	12.3 $\times$ 4.8	-63.8	0.7	1.7 $\times$ 1.7		0.14
J0939+740	b,c,f	12.0 $\times$ 12.0		0.6	7.0 $\times$ 7.0		0.15
J0949+732	-	-		N.S.	-		N.S.
J1015+683	d,g,h,i	12.2 $\times$ 4.8	-58.0	0.6	4.8 $\times$ 3.6	-11.7	0.13
J1036+677	d,e,h,i	12.4 $\times$ 4.8	-58.1	0.45	5.5 $\times$ 3.2	-59.7	0.1
J1124+749	f,h,m	25.0 $\times$ 25.0		0.5	6.8 $\times$ 6.8		0.15
J1137+613	d,m	9.0 $\times$ 9.0		1.0	7.3 $\times$ 7.3		0.2
J1211+743	f,g,h,i	12.0 $\times$ 12.0		0.4	4.4 $\times$ 3.8	-32.9	0.1
J1216+674	d,m	8.5 $\times$ 8.5		0.5	-		N.S.
J1220+636	d,l,m	8.9 $\times$ 8.9		0.9	7.3 $\times$ 7.3		0.16
J1247+673	d,e,l	26.0 $\times$ 26.0		1.0	-		N.S.
J1251+756	f,h,m	12.6 $\times$ 11.3	39.0	0.3	6.8 $\times$ 6.8		0.1
J1251+787	d,e,h,i	24.0 $\times$ 24.0		0.5	5.4 $\times$ 3.4	-29.6	0.1
J1313+696	d,e	8.0 $\times$ 8.0		0.9	2.5 $\times$ 2.5		0.5
J1410+633	d,m	10.0 $\times$ 10.0		0.6	8.4 $\times$ 8.4		0.3

^a The codes in this column refer to those in Table 1.
^b N.S. stands for not shown sources in Fig. 10.

 

Table 3: continued

Name	Observationsa	1.4 GHz			4.9 GHz
		Beam		1st contour	Beam		1st contour
		" $\times$ "	PA	mJy/beam	" $\times$ "	PA	mJy/beam
J1504+689	d,k	10.0 $\times$ 10.0		0.8	1.8 $\times$ 1.8		0.3
J1523+636	d,e	11.0 $\times$ 11.0		0.8	3.1 $\times$ 3.1		0.22
J1530+824	f,h,m	25.0 $\times$ 25.0		1.0	6.7 $\times$ 6.7		0.15
J1536+843	f,h,m	9.8 $\times$ 5.2	80.6	0.2	6.6 $\times$ 6.6		0.15
J1557+706	d,g,l	10.9 $\times$ 8.9	77.0	1.2	2.0 $\times$ 2.0		0.25
J1632+825	f,g,h,i	13.9 $\times$ 9.5	69.9	1.0	3.3 $\times$ 3.3		0.2
J1650+815	f,h,m	25.0 $\times$ 25.0		0.63	6.6 $\times$ 6.6		0.2
J1732+714	d,e	9.0 $\times$ 4.8	-60.6	0.3	2.8 $\times$ 1.4	-78.0	0.2
J1733+707	d,m	7.9 $\times$ 6.7	-3.1	0.57	6.6 $\times$ 6.6		0.14
J1743+712	d,g,l	7.4 $\times$ 5.0	-66.0	0.4	1.8 $\times$ 1.8		0.16
J1745+712	d,g,l	8.0 $\times$ 5.7	-78.5	0.55	1.8 $\times$ 1.8		0.2
J1751+680	d,k,l	6.9 $\times$ 4.7	-64.2	0.35	1.8 $\times$ 1.4	-23.2	0.12
J1754+626	d,g,l	24.0 $\times$ 24.0		0.8	1.8 $\times$ 1.8		0.15
J1800+717	d,k	7.1 $\times$ 4.7	-61.8	0.45	-		N.S.b
J1835+665	d,m	6.8 $\times$ 4.7	-58.4	0.35	6.8 $\times$ 6.8		0.2
J1835+620	d,e,l,m	-		N.S.	-		N.S.
J1844+653	d,l,m	24.0 $\times$ 24.0		1	7.0 $\times$ 7.0		0.14
J1845+818	f,h,m	13.8 $\times$ 9.4	87.7	0.5	6.3 $\times$ 6.3		0.14
J1847+707	d,e,l	12.2 $\times$ 10.1	-87.6	0.5	2.2 $\times$ 1.4	-60.1	0.15
J1850+645	d,g,l	25.0 $\times$ 25.0		1.0	-		N.S.
J1853+800	f,g,h,i	14.2 $\times$ 9.6	86.7	0.4	5.0 $\times$ 3.4	74.6	0.15
J1918+742	j,k,l	13.0 $\times$ 13.0		0.8	-		N.S.
J1951+706	j,l,m	12.5 $\times$ 12.5		0.35	6.8 $\times$ 6.8		0.2
J2016+608	j,k	6.2 $\times$ 4.9	-50.6	0.4	1.7 $\times$ 1.7		0.15
J2035+680	j,k,l	22.0 $\times$ 22.0		0.65	1.7 $\times$ 1.7		0.15
J2042+751	-	-		N.S.	-		N.S.
J2059+627	j,m	5.5 $\times$ 5.5		0.5	7.0 $\times$ 7.0		0.15
J2103+649	j,l,m	11.7 $\times$ 10.2	84.3	0.3	6.7 $\times$ 6.7		0.16
J2111+630	j,k,l	22.0 $\times$ 22.0		1.0	-		N.S.
J2114+820	a,b,c,g,j,k	12.8 $\times$ 9.7	11.1	0.4	2.9 $\times$ 2.3	-65.5	0.12
J2128+603	j,k	5.4 $\times$ 3.8	-51.5	0.25	1.7 $\times$ 1.7		0.15
J2138+831	a,b,c,g	12.8 $\times$ 9.6	16.7	0.3	6.5 $\times$ 3.4	40.8	0.2
J2145+819	a,b,c	12.7 $\times$ 9.8	19.0	0.4	-		N.S.
J2157+664	j,k,l,m	11.6 $\times$ 10.1	87.5	0.53	4.1 $\times$ 3.2	88.5	0.2
J2204+783	a,b,c,g	13.0 $\times$ 10.2	34.1	0.3	4.1 $\times$ 3.0	45.1	0.14
J2209+727	j,k	7.4 $\times$ 5.2	-57.7	0.3	1.8 $\times$ 1.8		0.22
J2242+622	j,k	5.1 $\times$ 3.8	-36.9	0.25	1.6 $\times$ 1.6		0.14
J2247+633	j,k	6.3 $\times$ 5.0	-45.1	0.4	1.6 $\times$ 1.6		0.1
J2250+729	j,k	7.2 $\times$ 4.9	-51.7	0.4	1.8 $\times$ 1.8		0.2
J2255+645	j,k	6.8 $\times$ 4.8	-60.2	1.0	-		N.S.
J2307+640	j,k	5.7 $\times$ 3.7	-53.9	0.3	-		N.S.
J2340+621	j,k	5.5 $\times$ 3.8	-50.1	0.25	1.6 $\times$ 1.6		0.15

^a The codes in this column refer to those in Table 1.
^b N.S. stands for not shown sources in Fig. 10.

Figure 2: VLA maps of 79 radio galaxies from the sample. A label "L'' or "C'' by the source name indicates the frequency of observation, namely 1.4 or 4.9 GHz, respectively. Dotted lines help to identify equivalent regions in different frequency maps. The core position is marked with an arrow on each map. The angular scale of the 1.4 GHz maps has been kept fixed, except for objects too extended to properly fit in a single page. In those cases, the map size is reduced by a factor of 2 or 3 (marked with "1/2'' or "1/3'', respectively). Map parameters are displayed in Table 3. Contours are separated by factors of $\sqrt {2}$

Figure 2: continued

Figure 2: continued

Figure 2: continued

Figure 2: continued