Upper: relation between QPO frequency and BH mass. Following Pan et al. (2016), we updated the relation to include more recent QPO detections in NLSy1 MS2254.9−3712 (Alston et al. 2015), Mrk 766 (Zhang et al. 2017), and MCG -6-30-15 (Gupta et al. 2018), TDE ASASSN 14li (Pasham et al. 2019), ultrasoft AGN J1231 (Lin et al. 2013), and J1302 (this work). The two TDEs, ASASSN 14li and Swift J1644+57, have higher QPO frequencies and lower BH masses in comparison to AGNs. As a comparison, we also overplot the frequencies for QPEs (green symbols, Miniutti et al. 2019; Giustini et al. 2020). Lower: relation between BH mass and dimensionless spin parameter assuming that the QPO originates from the 3:2 twin frequency disk resonance (see text for details). Only the case for the prograde orbit is shown. Solid and dashed lines represent cases in which the observed QPO frequency of J1302 corresponds to the radial and vertical epicyclic frequencies, respectively. For comparison, we also show the relation by assuming that the QPO frequency is the Keplerian frequency at ISCO (dotted line). Grey shaded region shows the J1302’s BH mass range ([0.25−2.5]×10⁶ M_⊙, Sun13) and the thick black line represents the best estimate on the BH mass (8 × 10⁵ M_⊙).