Table 1.
Main properties of the targets observed with VLT/MUSE.
| Target | RA | Dec | Redshift | FMP | Gaia Sep. | J | G1 | G2 | Spectrum | Texp | Observation |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (″) | source | (min:s) | date | ||||||||
| J0007+0053 | 00:07:10.02 | +00:53:29.0 | 0.318 | 12 | 0.792 | 15.99 | 17.68 | 19.34 | SDSS (1) | 19:06 | 11/20/22 |
| J0015–2526 ( * ) | 00:15:43.93 | −25:26:17.7 | 0.969 | 62 | – | 15.27 | 16.27 | – | NTT (2) | 19:06 | 12/20/22 |
| J0052–3045 ( * ) | 00:52:37.98 | −30:45:52.2 | 1.462 | 44 | – | 17.63 | 19.78 | – | 2QZ (3) | 26:42 | 12/24/22 |
| J0128–0444 | 01:28:37.44 | −04:44:01.5 | 1.631 | 15 | – | 17.72 | 20.42 | – | SDSS1 | 34:20 | 08/20/22 |
| J0402–3237 | 04:02:15.06 | −32:37:33.4 | 1.280 | 16 | 0.661 | 17.19 | 19.47 | 20.63 | Lemon (4) | 27:12 | 10/19/22 |
| J0525–4153 | 05:25:35.88 | −41:53:46.1 | 2.155 | 26 | – | 16.95 | 18.17 | – | Gaia (5) | 26:42 | 12/29/22 |
| J0545–2236 | 05:45:09.38 | −22:36:33.5 | 2.488 | 21 | 0.554 | 17.31 | 19.51 | 20.11 | Gaia (5) | 26:42 | 01/15/23 |
| J0840–0529 | 08:40:04.14 | −05:29:11.1 | 1.393 | 55 | – | 17.01 | 18.34 | – | Gaia (5) | 26:42 | 01/25/23 |
| J1059+0622( * ) | 10:59:26.44 | +06:22:27.1 | 2.199 | 27 | 0.592 | 15.98 | 17.47 | 17.95 | SDSS (1) | 19:06 | 01/27/23 |
| J2139–4331 | 21:39:57.14 | −43:31:01.7 | 0.485 | 10 | 0.666 | 16.36 | 18.57 | 18.68 | NTT2 | 19:06 | 11/20/22 |
| J2211–0009 | 22:11:11.00 | −00:09:53.4 | 0.667 | 24 | – | 17.17 | 19.26 | – | SDSS (1) | 34:20 | 07/03/22 |
| J2228–3047 | 22:28:49.43 | −30:47:34.5 | 1.948 | 28 | – | 16.87 | 18.19 | – | 2QZ (3) | 34:20 | 08/21/22 |
Notes. Separations (in case of multiple objects), G-band magnitude of the primary component (G1), G-band magnitude of the secondary component (G2, in case of multiple objects), and FMP are extracted from the Gaia catalog; J-band are derived from Gaia Bp and Rp photometry, as is described in the appendix. Redshift is obtained from spatially unresolved spectra whose origin is reported in the table. Texp is the total exposure time of the MUSE observations. ( * )Targets on which we applied the decomposition method described in Sect. 2.1. (1): Lyke et al. (2020); (2): our observations at ESO/NTT (Program ID:109.22W4); (3): Croom et al. (2009); (4): Lemon et al. (2020); (5): Gaia quasars candidate catalog, Gaia Collaboration (2023).
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