Table 1.
Primary SMBHB candidates catalog.
| Name | RA(2000) | Dec(2000) | Radec_err | Separation | Sig. | Factor | Detection | X-ray follow-up |
|---|---|---|---|---|---|---|---|---|
| (°) | (°) | (68%) | (Δ″) | Likelihood | ||||
| 1 – eRASSt J0344-3327 | 56.107460 | –33.45521 | 1.09 | 0.17 | 8.4 | 13.4 | 473.7 | Swift-XRT, NICER |
| 2 – eRASSt J0530-4125 | 82.56909 | –41.42582 | 0.84 | 1.87 | 11.7 | 8.4 | 1106.2 | Swift-XRT, NICER |
| 3 – eRASSt J1906-4850 | 286.53654 | –48.84064 | 0.49 | 1.02 | 10.3 | 7.4 | 3788.3 | Swift-XRT, NICER |
| 4 – eRASSt J0432-3023 | 68.07197 | –30.39961 | 0.63 | 1.23 | 3.0 | 6.8 | 1837.3 | Swift-XRT, NICER |
| 5 – eRASSt J1130-0806 | 172.61730 | –8.10278 | 1.18 | 2.33 | 20.4 | 6.3 | 420.9 | – |
| 6 – eRASSt J1522-3722 | 230.56415 | –37.37989 | 0.85 | 1.24 | 4.0 | 6.2 | 732.1 | NICER |
| 7 – eRASSt J1141+0635 | 175.47668 | 6.58614 | 0.94 | 1.07 | 10.4 | 5.7 | 774.8 | Swift-XRT, NICER, XMM |
| 8 – eRASSt J0458-2159 | 74.66770 | –21.99204 | 0.34 | 0.98 | 3.9 | 5.7 | 8437.1 | NICER |
| 9 – eRASSt J2227-4333 | 336.98212 | –43.56079 | 1.42 | 1.35 | 6.2 | 5.5 | 271.5 | – |
| 10 – eRASSt J1124-0348 | 171.23409 | –3.81142 | 1.17 | 0.93 | 9.9 | 5.4 | 509.8 | NICER |
| 11 – eRASSt J0036-3125 | 9.05142 | –31.41707 | 1.26 | 1.30 | 5.4 | 5.4 | 413.2 | – |
| 12 – eRASSt J1003-2607 | 150.82466 | –26.12018 | 1.08 | 1.62 | 4.9 | 5.3 | 709.1 | Swift-XRT, NICER |
| 13 – eRASSt J0818-2252 | 124.74048 | –22.87709 | 0.52 | 1.36 | 7.7 | 5.3 | 5886.2 | Swift-XRT, NICER |
| 14 – eRASSt J0600-2939 | 90.23452 | –29.65689 | 1.08 | 2.88 | 3.7 | 5.2 | 580.3 | – |
| 15 – eRASSt J0044-3313 | 11.20658 | –33.23234 | 1.11 | 0.60 | 8.5 | 5.2 | 691.3 | Swift-XRT |
| 16 – eRASSt J0614-3835 | 93.71599 | –38.59458 | 0.73 | 1.33 | 7.7 | 5.0 | 1450.6 | – |
Notes. Table with the eROSITA names of the sources (Column 1) and X-ray positions based on the stacked eRASS:4 coordinates (Columns 2 and 3). The “Radec_err” values (Column 4) correspond to the combined positional 1σ 68% error derived from the PSF-fitting performed by the eROSITA source detection pipeline. The separation (Column 5) indicates the distance, in arcseconds, between the eROSITA and Gaia DR3 positions. We include the Significance (Column 6) and Factor (Column 7) parameters used in our SMBHB selection described in Sect. 2.2. We also show the detection likelihood (Column 8) from the eRASS:4 catalog, which corresponds to the negative log-likelihood probability that the source counts are produced by background fluctuations. Larger detection likelihoods correspond to more observed counts relative to the background and, therefore, a smaller likelihood that the observed counts were produced by background fluctuations. Finally, we also report the X-ray missions used to monitor the flux evolution of the candidates (Column 9). Five sources have not been observed. However, they will be targeted by NICER during cycle 7. The candidates are ranked according to their factor F values.
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