Table 2.
Optical spectral properties of the main SMBHB candidates.
| Name | Telescope | Observation | z | X-ray Luminosity | SMBH mass log(Mbh/M⊙) | |
|---|---|---|---|---|---|---|
| date | (× 1042 erg s−1) | (Hβ) a | (Hα) a | |||
| 1 – eRASSt J0344-3327 | NTT/EFOSC2 | 17/02/2024 | 0.090 | 0.25–8.21 | – | (6.95±2.55) b |
| 2 – eRASSt J0530-4125 | NTT/EFOSC2 | 17/02/2024 | 0.076 | 0.54–7.76 | (7.26±0.48) | (7.41±1.21) |
| 3 – eRASSt J1906-4850 | Magellan/Baade | 26/10/2021 | 0.049 | 1.73–23.80 | 6.63±0.25 c | (6.72±0.50) c |
| 4 – eRASSt J0432-3023 | SAAO | 28/02/2024 | 0.055 | 0.47–9.03 | 7.31±0.19 | (7.08±0.78) |
| 5 – eRASSt J1130-0806 | SAAO | 28/02/2024 | 0.037 | 0.23–1.87 | – | 7.24±0.30 |
| 6 – eRASSt J1522-3722 | SAAO | 19/03/2023 | 0.064 | 1.37–10.85 | 7.35±0.09 | 7.17±0.02 |
| 7 – eRASSt J1141+0635 | NTT/EFOSC2 | 16/02/2024 | 0.101 | 3.28–25.64 | (7.87±0.55) | (7.41±0.48) |
| 8 – eRASSt J0458-2159 | Magellan/Baade | 11/12/2020 | 0.040 | 2.13–17.64 | 6.89±0.05 | 6.85±0.08 |
| 9 – eRASSt J2227-4333 | 6dF | 29/06/2003 | 0.198 | 8.82–59.32 | 7.53±0.22 | 7.46±0.21 |
| 10 – eRASSt J1124-0348 | NTT/EFOSC2 | 18/02/2024 | 0.021 | 0.02–0.77 | (6.14±0.9) | 6.65±0.18 |
| 11 – eRASSt J0036-3125 | SAAO | 06/09/2023 | 0.108 | 1.59–15.76 | 5.93±0.12 | 7.52±0.26 |
| 12 – eRASSt J1003-2607 | LBT/MODS | 02/01/2025 | 0.001 | 0.0007–0.005 | – | – |
| 13 – eRASSt J0818-2252 | SAAO | 02/12/2023 | 0.034 | 1.49–13.64 | 7.49±0.22 | (6.99±0.48) |
| 14 – eRASSt J0600-2939 | SAAO | 22/11/2024 | 0.104 | 1.51–17.11 | – | 7.47±0.11 |
| 15 – eRASSt J0044-3313 | SAAO | 19/10/2022 | 0.107 | 2.09–20.96 | 7.45±0.09 | (6.64±0.47) |
| 16 – eRASSt J0614-3835 | SAAO | 30/11/2023 | 0.054 | 1.14–6.83 | 6.03±0.16 | (6.49±0.58) |
Notes. Table with sources (Column 1) and the corresponding telescopes (Column 2) and date (Column 3) from which the optical spectra were obtained. The spectroscopic redshifts (Column 4) were used to calculate the eROSITA 0.2–2.3 keV luminosities (Column 5) in the faint and bright phases of the candidates. Single-epoch SMBH masses (Columns 6 and 7) were obtained based on the spectral fit of the broad emission lines.
The single-epoch SMBH masses are calculated based on the scaling relations presented in Vestergaard & Peterson (2006) and Mejía-Restrepo et al. (2022) for Hβ and Hα, respectively. We report only statistical uncertainties for the SMBH mass measurements. An additional 0.3 dex should be included to consider the systematic uncertainties.
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