SFRs as a function of quasar bolometric luminosity. SFRs derived from host [O II] luminosity are shown without dust correction (blue circles) and with constant dust corrections of A_V = 1.0 (dashed line), 1.3 (dashed–dotted line), and 2.2 (blue dotted line) mag, as well as with a bolometric-luminosity-dependent dust correction based on the M_BH–M_⋆ relation (purple dotted line). Horizontal error bars indicate the bin width. For comparison, independent SFR estimates for quasar hosts from far-infrared measurements (z ∼ 0.5–1, orange triangles; S. Serjeant & E. Hatziminaoglou 2009, denoted as S09 in the figure), radio continuum measurements (z ∼ 0.8–1.2, green squares; C. Macfarlane et al. 2021, denoted as M21 in the figure), and CO (J = 5–4) measurements for three luminous quasars at z = 2 (black stars; J. D. Silverman et al. 2026, denoted as S26 in the figure) are also shown.