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Table 1

Source and image properties.

Name AGN? P % Alpha Err_alpha 843 843_err 1382 1382_err 2400 2400_err 4800 4800_err 8640 8640_err t (h) rms_4800 rms_8640
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) (15) (16) (17) (18) (19)
ES509 IP 2.7 12 −1.02 0.01 37.00 1.40 22.74 1.16 13.19 0.70 5.94 0.45 3.51 0.39 1.00 0.12 0.14
ES427 IV  <0.2  <1 −1.08 0.01 39.70 1.40 22.30 1.14 12.53 0.65 6.54 0.46 2.83 0.36 0.99 0.11 0.13
ES973 ISPM 0.83 7 −1.15 0.04 14.30 1.10 11.59 1.18 4.08 0.69 1.93 0.29  <0.27 1.96 0.09 0.09
ES798 IM  <0.6  <5 −0.81 0.06 11.80 0.80 11.72 0.90 4.39 0.64 3.07 0.37  <0.33 0.99 0.11 0.13
ES749 I  <0.7 7 −1.08 0.02 15.00 1.00 10.26 0.79 5.12 0.75 2.63 0.29 0.82 0.26 0.86 0.11 0.14
ES775 ISM  <0.2  <6 −1.35 0.02 6.71 0.92 3.34 0.60 2.08 0.43 0.59 0.14  <0.24 1.86 0.08 0.09
ES011 IS?  <0.55  <6 −1.44 0.26 7.17 1.33 9.51 0.68 1.80 0.26  <0.36  <0.39 1.03 0.12 0.13
ES419 IS  <0.2  <5 −1.35 0.11 5.51 1.02 4.42 0.39 1.39 0.24  <0.39  <0.33 1.80 0.13 0.11
ES318  <0.2  <10 −0.78 0.64  <2.40 2.01 0.58 1.30 0.28  <0.30  <0.30 1.84 0.09 0.10
CS703 IP 1.9 7 −0.99 0.01 – – 26.93 1.56 15.52 0.88 8.60 0.82 4.22 0.37 1.31 0.12 0.13
CS114 ISV  <0.2  <3 −1.34 0.03 – – 7.68 0.47 3.19 0.47 2.07 0.36 0.50 0.19 2.26 0.11 0.09
CS194 I?  <0.2  <3 −1.12 0.03 – – 7.00 0.52 2.64 0.34 1.69 0.23 1.19 0.25 2.25 0.09 0.09
CS538  <0.2  <10 −0.88 0.43 – – 1.95 0.29 1.19 0.22  <0.21  <0.27 2.25 0.07 0.09
CS241 S?  <0.2  <12 −1.96 0.81 – – 1.63 0.31 0.54 0.22  <0.24  <0.21 3.81 0.06 0.07
CS415 S?  <0.2  <8 −2.38 0.43 – – 2.64 0.54 0.70 0.08  <0.33  <0.27 2.58 0.11 0.09
CS164  <0.2  <13 −0.92 0.02 – – 1.59 0.29 0.95 0.23 0.76 0.19 0.21 0.11 2.03 0.07 0.09
CS215  <0.2  <13 −0.76 0.02 – – 1.55 0.22 0.73 0.17 0.28 0.15 2.05 0.09 0.10
CS487 M  <0.2  <13 −0.21 0.02 – – 1.54 0.24 1.07 0.23 0.92 0.18 1.28 0.28 2.03 0.07 0.09

Notes. Column (1): source name; Col. (2): evidence for AGN classification: I=S20/S3.6 ratio high (>1000), P=source is polarised at 1.4 GHz, S=steep spectrum, V=VLBI detection, M=morphology; Col. (3): polarised flux density at 1.4 GHz in mJy; Col. (4): percentage of polarised flux density; Cols. (5)–(6): spectral index (Sν ∝ να) and its associated error; Cols. (7)–(16): flux densities and their errors used to construct radio spectra in mJy; Col. (17): integration times at 4.8 GHz and 8.6 GHz; Cols. (18)–(19): 1 σ image sensitivities at 4.8 GHz and 8.6 GHz. Source CS487, at the end of the table, has been de-classified as IFRS because it has been discovered from the high-frequency observations that it is actually associated with an IR object (see Fig. 6).

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