Eddington ratio ṁ and black hole mass M_BH parameter space with the five different ṁ regimes marked by dotted lines (note that the vertically logarithmic scale is nonlinear). The two dashed curves mark approximately the lower limit in the ṁ − M_BH space for the existence of UV LD mini-BALs (bottom curve) and BALs (upper curve). The location of various AGN mentioned in this article is marked in the figure. References for the individual measurements of log(M_BH/M_⊙) and ṁ (or L_BOL, assuming η = 0.1 for luminous AGN) are taken from the literature and reported in parentheses, respectively from: Botte et al. (2004) and Kara et al. (2017) for Ark 564 (6.4, 1.1); Vestergaard & Peterson (2006) and Martínez-Paredes et al. (2017) for I Zw 1 (7.4, 1.4); Bentz et al. (2009) and Vasudevan et al. (2010) for Mrk 766 (6.2, 0.4^*); Greenhill et al. (1996) for NGC 1068 (7.2, 0.5); Risaliti et al. (2013) and Vasudevan et al. (2010) for NGC 1365 (6.3, 0.025); Pancoast et al. (2014) and Vasudevan et al. (2010) for NGC 5548 (7.6, 0.025); Grupe et al. (2010) and Middei et al. (2018) for HE 0436−4717 (7.8, 0.09); Dasyra et al. (2007) and Giustini et al. (2011) for PG 1126−041 (8.1, 0.25); Peng et al. (2006) and Chartas et al. (2007) for PG 1115+080 (9.1, 0.2); Saturni et al. (2018) for APM 08279+5255 (10.4, 0.4); Nardini et al. (2015) for PDS 456 (9, 0.8); Jin et al. (2017a) for RX J0439.6−5311 (7.2, 1.8), Czerny et al. (2016) for RE J1034+396 (6, 1); Vasudevan et al. (2010) for NGC 985 (8.4, 0.05); Vasudevan et al. (2010) for NGC 3783 (7.5, 0.05); Devereux et al. (2003) and Ho et al. (1996) for M 81 (7.8, 6 × 10⁻⁴); Gebhardt & Thomas (2009)Prieto et al. (2016) for M 87 (9.8, 10⁻⁶); and Ghez et al. (2008) and Mościbrodzka et al. (2009) for Sgr A* (6.6, < 10⁻⁶). (*) Vasudevan et al. (2010) estimate a lower ṁ for Mrk 766 as they use a larger BH mass than the one used here.