Table 1.
Summary of X-ray QPO properties
| Name | PQPO [s] | QPO reference | MBH [M⊙] | log(λEdd) | Mass reference | Type |
|---|---|---|---|---|---|---|
| NGC 1566 | 17 800 | This work | 106.86 | −1.2 | (1) | CL-AGN |
| MCG-6-30-15a | 3670 | (2) | 106.60 | −1.1 | (1) | NLS1 |
| RE J1034+396 | 16 900 | (3) | 106.74 | ∼1.0 | (4) | NLS1 |
| MS 2254.9-3712a | 7200 | (5) | 106.6 | −0.6 | (6) | NLS1 |
| NGC 5506 | 16 000 | (7) | 107.94 | ∼ − 1.3 | (8) | Obscured NLS1 |
| Mrk 766a | 6450 | (9) | 106.82 | −1.25 | (10) | NLS1 |
| 1H 0707-495a | 3800 | (11) | 106.72 | −0.3 | (11) | NLS1 |
| NGC 1365b | 4566 | (12) | 106.85 | −1.5 | (13) | CL-AGN |
| 1ES 1927+654 | 559 | (14) | 106.14 | −0.4 | (15) | CL-AGN/TDE |
| RX J1301.9+2747 | 1500 | (16) | 105.9 | −1.0 | (16) | QPE |
| GSN 069 | 32 000 | (17) | 106 | −0.8 | (17) | QPE/TDE |
| 2XMM J123103.2+110648 | 13 680 | (18) | 105 | −1.0 | (19) | TDE |
| Swift J164449.3+573451 | 200 | (20) | 105.5 | 1.2 | (21) | TDE |
| ASASSN-14li | 131 | (22) | 106.23 | −0.6 | (23) | TDE |
| H1743-322 | 0.006 | (24) | 101.08 | SPL | (25) | XRB |
| GRS 1915+105 | 0.009 | (26) | 101.09 | SPL | (27) | XRB |
| GRO J1655-40 | 0.003 | (28) | 100.8 | SPL | (29) | XRB |
| XTE J1859+226 | 0.005 | (30) | 100.89 | SPL | (31) | XRB |
| XTE J1650-500 | 0.004 | (32) | < 100.86 | SPL | (33) | XRB |
| XTE J1550-564 | 0.005 | (28) | 100.96 | SPL | (34) | XRB |
Notes. The reported QPOs in RX J0437.4-4711, Ton S180, and Sgr A★ are excluded due to the lack of X-ray detections, and the QPOs in AT2020ocn (Pasham et al. 2024) and AT2020afhd (Wang et al. 2025) are excluded due to their extremely low-frequency and likely distinct physical origins. The reported QPOs in XMMU J134736.6+173403 (Sy2; Carpano & Jin 2018), 3XMM J215022.4-055108 (TDE; Zhang et al. 2025b), NGC 5408 X-1 (ultraluminous X-ray sources; ULX; Strohmayer et al. 2007), M82 X-1 (ULX; Pasham et al. 2014), and 4U 1630-47 (XRB; Remillard & McClintock 2006) are not included due to the lack of independent MBH measurements. For XRBs, the QPOs are high-frequency ones. The Eddington ratios for SMBH accreting systems are either obtained from their corresponding QPO references or estimated by this work. For XRBs, high-frequency QPOs are found in the SPL state with high Eddington ratios. (a) The QPO was not detected according to Zhang et al. (2023). (b) The QPO was not detected by Gúrpide & Middleton (2025). References: (1) Koss et al. (2022); (2) Gupta et al. (2018); (3) Xia et al. (2025); (4) Czerny et al. (2016); (5) Alston et al. (2015); (6) Grupe et al. (2010); (7) Zhang et al. (2025a); (8) Papadakis (2004); (9) Zhang et al. (2017); (10) Bentz & Katz (2015); (11) Pan et al. (2016); (12) Yan et al. (2024); (13) Fazeli et al. (2019); (14) Masterson et al. (2025); (15) Li et al. (2022); (16) Song et al. (2020); (17) Miniutti et al. (2023); (18) Lin et al. (2013); (19) Ho et al. (2012); (20) Reis et al. (2012); (21) Mïller & Gültekin (2011); (22) Pasham et al. (2019); (23) Wevers et al. (2017); (24) Homan et al. (2005); (25) Nathan et al. (2024); (26) Remillard (2004); (27) Reid et al. (2014); (28) Remillard et al. (2002); (29) Greene et al. (2001); (30) Cui et al. (2000); (31) Yanes-Rizo et al. (2022); (32) Homan et al. (2003); (33) Orosz et al. (2004); (34) Orosz et al. (2011).
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