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Table 1

VLA sample description (Cols. 1 through 6) and observational results (Cols. 7 through 10).

Name ID z S c,1.4 P t,4.9 t obs S abs rms τ int N HI
B1950 (Jy) (W Hz-1) (min) (mJy bm-1) (mJy bm-1) (km s-1) (×1020 cm-2)
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)

0055+30 NGC 315 0.0165 0.464 23.84 27 27.0 1.0 4.5  ±  0.7 8.3  ±  0.3
0104+32 3C 31 0.0169 0.067 24.11 66+47  <1.8 0.6  <2.7  <5.19
0755+37 3C 189 0.0428 0.137 24.62 22  <3.0 1.0  <2.2  <4.23
1322+36 NGC 5141 0.0176 0.054 23.45 57 3.3 0.6 5.5  ±  1.0 10.0  ±  1.8
1346+26 4C 26.42 0.0632 0.135 24.35 139 3.0 0.5 2.2  ±  0.4 4.1  ±  0.7
1350+31 3C 293 0.045 1.652 24.93 20 148.0 1.0 12.8  ±  0.1 23.5  ±  0.2
1626+39 3C 338 0.0303 0.138 23.98 17  <1.8 0.6  <1.3  <2.5
2116+26 NGC 7052 0.0156 0.040 22.80 88  <1.2 0.4  <2.6  <5.1*

Notes.  Clarification of the columns: (1) B2 rado name, (2) ID used in the paper, (3) redshift, (4) core flux at 1.4 GHz, (5) total power at 4.9 GHz, (6) total on-source integration time, (7) peak of the absorbed flux, (8) rms noise, (9) integrated optical depth, and (10) H I column density.

(*)

Upper limit from our VLA observations. Emonts et al. (2010) set NHI < 0.34 × 1020 cm-2.

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