Table 6.
Optical properties of the red AGN sample.
| Object | 3XLSS ID | Optical |
|---|---|---|
| 1 | J021835.7−053758 | BL |
| 2 | J022848.4−044426 | BL, flat |
| 3 | J022928.4−051124 | BL |
| 4 | J022809.0−041235 | BL, flat |
| 5 | J020654.9−064552 | NL |
| 6 | J020410.4−063924 | NL |
| 7 | J023315.5−054747 | NL |
| 8 | J021337.9−042814 | BL, blue |
| 9 | J020436.4−042833 | BL |
| 10 | J020543.0−051656 | BL |
| 11 | J020517.3−051024 | BL |
| 12 | J022244.3−030525 | NL, red |
| 13 | J022323.4−031157 | IMD |
| 14 | J022209.6−025023 | NL |
| 15 | J022750.7−052232 | IMD |
| 16 | J022758.4−053306 | NL |
| 17 | J022453.2−054050 | IMD |
| 18 | J022258.8−055757 | IMD |
| 19 | J021844.6−054054 | IMD |
| 20 | J021523.2−044337 | NL |
| 21 | J022321.9−045739 | NL |
| 22 | J022443.6−050905 | IMD |
| 23 | J023418.0−041833 | Noisy |
| 24 | J020543.7−063807 | Noisy |
| 25 | J022932.6−055438 | BL |
| 26 | J021239.2−054816 | Noisy |
| 27 | J021511.4−060805 | NL |
| 28 | J021808.8−055630 | BL |
| 29 | J022538.9−040821 | BL |
| 30 | J020845.1−051354 | – |
| 31 | J020953.9−055102 | BL |
| 32 | J020806.6−055739 | NL, red |
| 33 | J021509.0−054305 | – |
| 34 | J021512.9−060558 | – |
| 35 | J020529.5−051100 | – |
| 36 | J022404.0−035730 | – |
| 37 | J023501.0−055234 | – |
| 38 | J020210.6−041129 | – |
| 39 | J022650.3−025752 | – |
| 40 | J021303.7−040704 | – |
| 41 | J023357.7−054819 | – |
| 42 | J020335.0−064450 | – |
| 43 | J020823.4−040652 | – |
| 44 | J020135.4−050847 | – |
| 45 | J021837.2−060654 | Noisy |
| 46 | J022149.9−045920 | BL |
| 47 | J020311.3−063534 | – |
Notes. Optically unobscured sources (Type 1) are considered to be those with broad emission lines (BL). Whereas obscured sources (Type 2) exhibit only narrow emission lines (NL) or a red continuum. The AGNs are characterised as obscured, unobscured, or intermediate type (IMD) based on visual inspection of their optical spectra. We note that in the optical spectra of sources 13 and 22, while the MgII lines are broad, all other lines are narrow. This is attributed to the wider area from which the MgII originates with respect to the Balmer lines. These sources are characterized as IMD.
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