Relation between black hole mass and host galaxy stellar mass. The galaxy targeted in this work (ALESS073.1) is marked with a star, the star filled in red is by assuming the stellar mass derived from the kinematic fitting by Lelli et al. (2021), while the white filled star considers the stellar mass derived from SED fitting (see Appendix A). The dark gray diamonds and crosses represent z ∼ 0 broad line AGNs presented in Reines & Volonteri (2015) and the massive black holes hosted in ellipticals and spirals at z ∼ 0 by Kormendy & Ho (2013), respectively. In light green diamond, we report the QSO at z ∼ 5.5 studied in Übler et al. (2023). In green, we show the broad line AGNs discovered with JWST at 4 < z < 7 presented in Harikane et al. (2023), Maiolino et al. (2023) and Kocevski et al. (2023) as light blue circles, triangles and pentagons, respectively. The yellow triangle represents the AGN at z ∼ 8.7 identified in Larson et al. (2023). Blue squares are the results obtained by Neeleman et al. (2021) for QSOs at z ∼ 6. Blue triangles are the results for QSOs at z > 2 from Pensabene et al. (2020). Blue crosses are the results for two luminous QSOs at z ∼ 6.8 from Marshall et al. (2023). We note that Pensabene et al. (2020), Neeleman et al. (2021) and Marshall et al. (2023) report the dynamical mass rather than the stellar mass. The black and green solid lines are the best-fit for Reines & Volonteri (2015) and Kormendy & Ho (2013), respectively, and the shaded areas are their 1σ uncertainties. The black dashed line is the relation M_BH = 0.01 × M_⋆.