Table 4.
AGN classification schemes (optical, radio and radio excess selection).
| Radio |
Radio excess |
|||||||
|---|---|---|---|---|---|---|---|---|
| Source ID | z | Morphology | Opt.cl. | M05 | Var. | q24 | q100 | qTIR |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
| J123555+620902* | 1.8750 | 1 | – | – | 0.29 ± 0.04 | 1.01 ± 0.04 | 1.04 ± 0.45 | |
| J123607+620951* | 0.6380 | 2 | SF | Uncl | 0.39 ± 0.03 | 1.62 ± 0.03 | 1.87 ± 0.26 | |
| J123608+621036* | 0.6790 | 1 | HEG | AGN | 0.99 ± 0.03 | 1.45 ± 0.03 | 1.22 ± 0.16 | |
| J123618+621541* | 1.9930 | 1 | – | Uncl | −0.95 ± 0.09 | < 0.73 | ||
| J123620+620844* | 1.0164 | 1 | – | AGN | ✓ | < − 0.78 | < 0.97 | |
| J123621+621708* | 1.9920 | 3* | – | Uncl | −0.92 ± 0.15 | 1.04 ± 0.04 | 1.58 ± 0.21 | |
| J123623+620654* |
 |
4 | – | – | ✓ | −0.48 ± 0.05 | < 0.88 | < 1.07 |
| J123624+621643* | 1.9180 | 1 | – | AGN C | ✓ | −1.06 ± 0.08 | < 0.56 | |
| J123641+621833* | 1.1456 | 3* | A | – | −0.97 ± 0.08 | 0.72 ± 0.04 | 1.36 ± 0.18 | |
| J123642+621331* | 2.0180 | 4 | – | S* | −0.36 ± 0.03 | 0.92 ± 0.03 | 0.89 ± 0.16 | |
| J123644+621133* | 1.0128 | 1 | A | AGN | < − 1.83 | < − 0.06 | ||
| J123646+621405* | 0.9610 | 1 | SF | AGN | −0.12 ± 0.04 | < 0.72 | ||
| J123650+620738* | 1.6095 | 3* | HEG | – | 0.68 ± 0.02 | 1.29 ± 0.03 | 1.05 ± 0.12 | |
| J123653+621444* | 0.3208 | 1 | A | AGN | −0.98 ± 0.13 | < 0.81 | ||
| J123659+621833* |
 |
1 | – | – | −1.2 ± 0.04 | −0.31 ± 0.04 | −0.03 ± 0.01 | |
| J123700+620910* |
 |
3* | – | AGN C | −0.08 ± 0.04 | 0.56 ± 0.04 | 1.29 ± 0.28 | |
| J123709+620838* | 0.9070 | 1 | A | AGN | ✓ | −0.64 ± 0.14 | < 0.91 ± 0.05 | < 1.59 |
| J123714+621826* |
 |
4 | – | – | −1.06 ± 0.06 | −0.03 ± 0.06 | 0.83 ± 0.26 | |
| J123715+620823* | 0.9335 | 1 | – | AGN | −0.99 ± 0.06 | −0.25 ± 0.07 | 0.18 ± 0.04 | |
| J123716+621512* | 0.5605 | 1* | A | AGN C | −0.04 ± 0.05 | < 0.89 | < 1.37 | |
| J123717+621733* | 1.1460 | 2 | SF | AGN C | 0.54 ± 0.03 | 0.80 ± 0.04 | 0.71 ± 0.22 | |
| J123721+621130 (a) |
 |
4 | SF | AGN | – | 0.60 ± 0.05 | 0.92 ± 0.32 | |
| J123726+621129* | 0.9430 | 1 | – | AGN | −2.31 ± 0.14 | < − 0.54 | ||
| J123649+620439 | 0.1130 | 1 | A | – | – | 1.69 ± 0.01 | 1.89 ± 0.20 | |
| J123701+622109* | 0.8001 | 1* | A | – | ✓ | < − 1.49 | 0.51 ± 0.04 | < 1.22 |
| J123739+620505 |
 |
4 | – | – | – | – | – | |
| J123751+621919* |
 |
1 | – | – | ✓ | < − 0.97 | < 1.00 | |
| J123523+622248 |
 |
1 | – | – | – | – | – | |
| J123510+622202 |
 |
4 | – | – | – | – | – | |
| J123656+615659 |
 |
1 | – | – | – | – | – | |
| R | 17% | 82% | 22% | 79% | 92.5% | 100% | ||
| (2/12) | (14/17) | (6/27) | (19/24) | (25/27) | (18/18) | |||
Notes. Check-marks or bold-font corresponds to a positive AGN classification. Entries with a hyphen correspond to sources which are outside the field-of-view of the bands required to classify the object or are not in the redshift range of the classification scheme. Blank entries have multi-wavelength coverage but do no have detections in all bands required. The column headers correspond to: (1) – VLBI source identifier as used in Paper I. (2) – Adopted redshifts from Paper I. Spectroscopic redshifts have no errors whilst errors on photometric redshifts correspond to 68% confidence intervals. (3) – Optical/NIR host galaxy morphologies classified into 1. early-type/bulge dominated, 2. late-type/spiral galaxies, 3. irregular, 4. Unclassified i.e., low surface brightness or unresolved. Potential evidence of interacting systems are marked with a *. (4) – Optical classification from Trouille et al. (2008). Optically normal galaxies (non-AGN) are classified as absorbers (A) or star-formers (SF). AGN are classified into high-excitation galaxies (HEG) or broad line AGN (BL). (5) Radio morphology classification from Muxlow et al. (2005) (AGN C – AGN candidate, S* – starburst + AGN). (6) – Radio variable sources as classified by Radcliffe et al. (2019a). (7) – Radio excess parameter using Spitzer MIPS 24 μm emission. (8) – Radio excess parameter using Herschel PACS 100 μm emission. (9) – Total radio excess parameter using rest-frame bolometric infrared luminosity and rest-frame 1.4 GHz flux density.
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