Table 6.
Known energetic recurring flares.
| ID | z | log MBH | nflare | Δt | E1/L1 | E2/L2 | Emax | r21 | tnext | Ref. |
|---|---|---|---|---|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) |
| ASASSN-14ko | 0.0425 | 7.9 | > 21 | 0.31 | LUV = 1.8 × 1044 | *EUV ∼ 3 × 1050 | ∼1 | – | 1,2,3 | |
| eRASSt J0456 | 0.077 | 7.0 | 5 | ∼0.6 | EX = 1.0 × 1052 | EX = 3.6 × 1051 | EX = 1.0 × 1052 | 0.4 | – | 4,5 |
| LX = 4.6 × 1044 | LX = 1.1 × 1044 | |||||||||
| AT 2022dbl | 0.0284 | 6.4 | 2 | 1.89 | LUV = 7.8 × 1043 | LUV = 3.0 × 1043 | *EUV ∼ 3 × 1050 | 0.4 | 2026/01 | 6 |
| AT 2020vdq | 0.045 | 6.1 | 2 | 2.54 | EUV = 6 × 1049 | EUV = 2 × 1051 | EUV = 2 × 1051 | 30 | 2026/01 | 7 |
| LUV = 6 × 1042 | EUV = 1 × 1044 | |||||||||
| AT 2018fyk | 0.059 | 7.7 | 2 | 3.1 | LUV = 3 × 1044 | LUV = 7 × 1042 | EUV = 9 × 1051 | 0.02 | 2025/03 | 8,9 |
| F01004-2237 | 0.1178 | 7.4 | 2 | 10.3 | EUV = ∼1 − 11 × 1052 | EUV = 0.5 × 1052 | EUV > 1 × 1052 | 0.05–0.5 | 2033 | 10,11 |
| LUV = ∼4 − 11 × 1044 | LUV = 4.4 × 1044 | |||||||||
| IC 3599 | 0.0215 | 6.7 | 2 | 18.8 | LX > 5.6 × 1043 | LX > 1.5 × 1043 | *EX ≳ 4 × 1050 | 0.3? | 2029 | 12,13,14 |
| RX J1331-3243 | 0.0519 | 6.5 | 2 | 27.5 | LX > 1 × 1043 | LX > 6 × 1042 | – | 0.6? | 2050 | 15,16 |
Notes. (1): The identification of the flares (eRASSt J045650.3-203750 and RX J133157.6-324319.7 are listed as short names). (2): Redshift. (3): Black hole mass in a unit of M⊙. For IC 3599, we adopted value from Grupe et al. (2015). (4): Number of flares reported. Note that we did not adopt the three-flares model for IC 3599 proposed by Campana et al. (2015) because the predicted flare in 2019 was not seen (Grupe et al. 2024). (5): The time interval of the observed peaks of the flares in a unit of years in the rest frame. (6)(7): The total energies (if present in the literature) and the peak luminosities of the first and the second flares. We list the energies and luminosities in 0.2–2 keV for those flares detected in the X-ray band, and the values in the UV band from blackbody fit for other flares. For ASASSN-14ko, all flares have similar luminosities, so we list the average for the flares studied in detail. For IC 3599 and RX J1331-3243 with sparse data sampling, we adopted the observed peak luminosities as lower limits. (8): The total energy of the most energetic flare. The values with a ‘*’ label are our own estimates based on literature data, which is not accurate and only used for order of magnitude estimates. Others are taken directly from the literature. The total energy of flares in RX J1331-3243 cannot be estimated due to a lack of observational data. (9): The ratio between the energies of the second and the first flares. If energies are absent in the literature, we calculated the ratio between peak luminosities. Note that the ratios are only for reference for IC 3599 and RX J1331-3243 with only lower limits of luminosities. (10): The predicted peak time of the next flare for those occurring only twice. (11): References are: 1. Payne et al. (2021); 2. Payne et al. (2022); 3. Payne et al. (2023); 4. Liu et al. (2023b); 5. Liu et al. (2024); 6. Lin et al. (2024); 7. Somalwar et al. (2023); 8. Wevers et al. (2019); 9. Wevers et al. (2023); 10. Tadhunter et al. (2017); 11. Dou et al. (2017); 12. Grupe et al. (1995); 13. Grupe et al. (2015); 14. Campana et al. (2015); 15. Hampel et al. (2022); 16. Malyali et al. (2023).
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