SFR and molecular gas mass vs. [CII] luminosity. Left panel:z > 7 quasars with L_[CII] measurements: J1234, J0038, and J0252 (red circles) and J1120, J1342, and J1007 (green circle). Gray dots are the z ≳ 6 quasars from the literature (see Table C.1). The best-fit relation and the relative 68% confidence interval are represented as the solid black line and green-shaded region, respectively. The best-fit parameters of the relation are: slope $1.{15}_{-0.27}^{+0.28}$, normalization $-8.{16}_{-0.06}^{+0.06}$, and intrinsic dispersion $0.{07}_{-0.02}^{+0.03}$ dex. The dotted line is the relation from De Looze et al. (2014) for low-metallicity dwarf galaxies in the local Universe. The dashed line is the best-fit relation from Romano et al. (2022) for galaxies from the ALPINE survey (4 < z < 6), including both detections and stacked non-detections. Right panel:z > 7 quasars with L_[CII] measurements and M_H2 upper limits: J1234, J0038, and J0252 (red circles) and J1342 (green circle); J1007 has both L_[CII] and M_H2 measurements. M_H2 measurements and upper limits for z ≳ 6 quasars from the literature have been homogenized to those presented in this work by assuming a common α_CO of 0.8 M_⊙ pc⁻² (K km s⁻¹)⁻¹ and a CO SLED. The best-fit relation and the relative 68% confidence interval are represented as the solid black line and gray-shaded region, respectively. The best-fit intrinsic dispersion of the relation is ${\delta }_{\mathrm{intr}}=0.{10}_{-0.03}^{+0.06}$ dex. The dashed line is the scaling relation derived by Zanella et al. (2018) for main-sequence (MS) and luminous infrared galaxies, up to z ∼ 6. We also report the scaling relation provided by Madden et al. (2020) for local dwarf galaxies (dotted line).