Table 1.
Dual (and triple) AGNs.
| Target | Redshift | RA & Dec | Separation | log(M*) | log(Lbol) | log(LX) | CAGN | ||
|---|---|---|---|---|---|---|---|---|---|
| (degrees) | (″) | (kpc) | (km s−1) | (M⊙) | (erg s−1) | (erg s−1) | |||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
| COS1638-A | 3.5079 | 150.735557 +2.19953 | – | – | – | 10.9 ± 0.4 | 46.7 | 44.5 | 2, 3, 4 |
| COS1638-B | 3.5109 | 150.735847 +2.19962 | 1.1 | 8.2 | 200 | 11.1 ± 0.4 | 46.2 | – | 1, 2, 4 ( ‡ ) |
| GS551-A | 3.7034+ | 53.124385 −27.85169 | – | – | – | 10.9 ± 0.3 | 46.0 | 44.4 | 1, 2, 4 ( * ), 5 |
| GS551-B (⋄) | 3.7022+ | 53.124274 −27.85166 | 0.4 | 2.9 | −25 | – | 44.5 | – | 1 |
| Eastfield (-A) (♮) | 3.7149 | 150.061668 +2.37887 | – | – | – | 9.5 ± 0.2 | 44.8 | – | 1, 2 ( ‡ ) |
| Mr. West (-B) (♮) | 3.7096 | 150.061348 +2.37877 | 1.2 | 8.8 | −340 | 9.4 ± 0.3 | ≲44.3 | – | 1, 2 ( ‡ ) |
| COS1656-A | 3.5101 | 150.271546 +1.61383 | – | – | – | 11.0 ± 0.2 | 45.8 | 44.4 | 1, 2, 4 ( * ) |
| COS1656-B | 3.5084+ | 150.271589 +1.61424 | 1.4 | 10.4 | −60 | 9.7 ± 0.3 | 44.3 | – | 1 |
| GS10578-A | 3.0647+ | 53.165325 −27.81415 | – | – | – | 11.2 ± 0.2 | 44.6 | 44.6 | 1, 2, 4 ( * ), 5 |
| GS10578-B | 3.0644+ | 53.165532 −27.81415 | 0.7 | 4.7 | −30 | – | 44.2 | – | 1 |
| LAE2 | 3.0674 | 53.164688 −27.81489 | 3.6 | 28 | 200 | 8.3 ± 0.4 | ≲44.6 | – | 5 |
Notes. Column (1): target name. Eastfield and Mr West identified the newly discovered companion of Jekyll & Hyde, following Pérez-González et al. (2024). Column (2): Redshift, as measured from the narrower Gaussian component in the UV and optical spectra (typical uncertainty of 0.0002). Column (3): Coordinates RA & Dec. Columns (4), (5) and (6): projected separation and velocity offset of the secondary (and tertiary) AGN from the primary nucleus. Column (7): stellar mass, as inferred from spectral energy distribution analysis (see Sect. 5.7); for COS1638-A and its close companion we provided order of magnitude estimates assuming a conservative Mdust/M* (see Sect. 5.7). Column (8): bolometric luminosity, measured from the NLR Hβ flux using Eq. (3) of Netzer (2019, typical uncertainty of 0.1 dex, not taking into account the bolometric correction scatter), for all but the AGN in LAE2 for which UV continuum is instead used (see Sect. 5.3). Column (9): absorption-corrected X-ray luminosity; see Appendix B. Column (10): flags on specific criteria used to identify AGN: 1 = BPT diagram, 2 = prominent [O III] outflow, 3 = BLR emission, 4 = X-ray emission, 5 = UV line ratios of Nakajima & Maiolino (2022) and Feltre et al. (2016). (⋄)Candidate secondary AGN, as incident ionising flux from the primary AGN could be responsible for the fluxes in this target (see Sect. 5.4). (♮)Candidate AGN, as the presence of highly ionised gas might also be explained by a fading and/or highly obscured AGN in Hyde (Pérez-González et al. 2024), even though no evidence of AGN emission is found in Hyde. ( ‡ )Tentative evidence; see Appendix B. ( * )X-ray emission likely associated with both sources; see Appendix B.
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