Table 1: The sample. $P_{\rm 178}$ in Col. (3) is total radio power (W Hz-1sr -1) at rest-frame 178 MHz. Column (4) lists spectral index between 178 and 750 MHz, and Cols. (5) and (6) the radio morphology and emission-line type. Apparent magnitude in rest-frame $R_{\rm C}$-filter and corresponding references are listed in Cols. (7) and (8). Columns (9) and (10) show velocity dispersion measurements from the literature (km s-1) and corresponding references. The last three columns list emission line fluxes in units of 10-15 erg s-1 cm-2, both from the literature and as determined from our wide slit spectrophotometry, and references.
Radio ID Redshift $\log P_{178}$ $\alpha_{178}^{750}$   $m_{R_{\rm C}}$ Ref. $\sigma_{\rm lit}$ Ref. $S_{\rm [OII]}$ $S_{\rm [OIII]}$ Ref.
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
3C 20 0.174 26.49 0.66 FRII HEG 16.80 1     0.634 1.915 W
3C 28 0.1971 26.22 1.06 FRII LEG 18.34 2     5.956 ... W
3C 31 0.0167 23.99 0.57 FRI LEG 11.92 2 249 SHI90 ... 10.349 G
3C 33 0.0595 25.60 0.76 FRII HEG 14.80 3     33.017 147.48 W
3C 35 0.0673 24.99 0.77 FRII LEG 14.94 1     1.0 $\pm $ 0.2 <0.34 A
3C 66B 0.0215 24.35 0.50 FRI LEG 12.55 2     6.782 4.801 W
3C 76.1 0.0324 24.41 0.77 FRI LEG 14.06 2 246 SHI90 <3.0 <2.0 A
3C 83.1B 0.0255 24.53 0.62 FRI LEG <12.11 4          
3C 98 0.0306 24.95 0.78 FRII HEG 14.18 3 175 SHI90 7.936 39.775 W
3C 381 0.1605 26.01 0.81 FRII HEG 18.05 5     1.177 44.31 W
3C 386 0.0170 24.13 0.59 FRI LEG <12.21 4          
3C 388 0.0908 25.64 0.70 FRII LEG 14.12 3 365 H85 1.618 1.901 W
3C 401 0.201 26.32 0.71 FRII LEG 16.68 6     ... 1.192 W
3C 433 0.1016 26.10 0.75 FRII HEG 16.59 5     ... 2.656 W
3C 442A 0.0263 24.35 0.96 FRII LEG 14.07 2 197 SHI90 8.0 $\pm $ 0.8 4.7 $\pm $ 1.0 A
3C 449 0.0171 23.82 0.58 FRI LEG 13.05 2 222 SHI90 <3.0 <2.0 A
3C 452 0.0811 25.88 0.78 FRII HEG 17.16 7     17.149 ... W
3C 465 0.0305 24.87 0.75 FRI LEG 13.14 2 341 FIF95 2.0 $\pm $ 0.4 <4.0 A
4C 11.71 0.0262 24.12 0.75 FRI LEG 14.00 7 249 EFAR99 <5.0 <3.0 A
4C 12.03 0.157 25.77 0.87 FRII LEG 15.91 1     ... 1.394 W
4C 35.40 0.0301 24.29 0.76 FRI LEG 12.83 8$^{{\rm }}$ 204 EFAR99 1.0 $\pm $ 0.2 <1.3 A
References for $m_{R_{\rm C}}$: (1) Converted from $K_{\rm UKIRT}$ (Lilly & Longair 1984) assuming $R_{\rm C}-K=2.5$ (Dunlop et al. 2003); (2) Cao & Rawlings (2004); (3) Owen & Laing (1989); (4) Martel et al. (1999) (upper limit given because of contamination by foreground star); (5) converted from V (Smith & Heckman 1989) assuming $V-R_{\rm C}=0.61$ (Fukugita et al. 1995); (6) converted from K (Lebofsky 1981) assuming $R_{\rm C}-K$=2.5 (Dunlop et al. 2003); (7) converted from V (Sandage 1973) assuming $V-R_{\rm C}=0.61$ (Fukugita et al. 1995); (8) converted from 2MASS $K_{\rm s}$ assuming $R-K_{\rm s}=2.5$ (Dunlop et al. 2003). Emission-line classifications are from Jackson & Rawlings (1997), except for 3C 28 and 4C 12.03 which are from Willott's compilation (http://www-astro.physics.ox.ac.uk/~cjw/3crr/3crr.html), and 3C 442A which we classify as LEG based on our Palomar spectrum. The 1.4 GHz fluxes were taken from NVSS by Condon et al. (1998) and from the surveys of White & Becker (1992) and Laing & Peacock (1980). References for velocity dispersions: SHI90: Smith et al. (1990), H85: Heckman et al. (1985), FIF95: Fisher et al. (1995) and EFAR99: Wegner et al. (1999). References for emission-line fluxes: A: from our data, W and G: from Willott's and Grimes' compilations, respectively (http://www-astro.physics.ox.ac.uk/~cjw/3crr/3crr.html and http://www-astro.physics.ox.ac.uk/~sr/grimes.html).

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