Notes. Columns 2–5 give the orbital periods P_orb in days, masses of the BH m_BH, masses of the optical companion m_star, and eccentricities e. The given mass ratio q = m_BH/m_star is indicative and provided with no uncertainties (see main text). ⁽¹⁾Gomez & Grindlay (2021). ⁽²⁾Orosz et al. (2007). ⁽³⁾Orosz et al. (2009). ⁽⁴⁾Miller-Jones et al. (2021). ⁽⁵⁾Shenar et al. (2022). For this system we do not have a measurement of the inclination, so there is a large range of possible masses for the BH; we report here the weighted mean, between their spectroscopic and evolutionary mass, i.e. M₁ of their Table 1. ⁽⁶⁾Mahy et al. (2022). Similar to VFTS 243, we have a large range of possible m_BH for HD 130298; we thus use their lower limit on m_BH based on the binary mass function. We also use their evolutionary mass for the optical companion, see their appendix E.1.10. Their eccentricity value is also reported without uncertainty. ⁽⁷⁾Casares et al. (2014). The orbital parameters (provided in their Table 1) have been derived by Casares et al. (2014) by fixing the orbital period to the shown value here, which is thus reported without uncertainty.