System and global parameters for selected planets in comparison to the 3D GCM model grid parameter space from Baeyens et al. (2022). All model planets are tidally locked such that P_rot=P_orb. Selected planets include hot (WASP-43b, HD 189733b, HD 209458b) and ultra-hot (HAT-P-7b, WASP-18b, WASP-103b, WASP-121b) Jupiters, sub-Neptunes (HD 86226c, TOI-1634b), a Neptune-like planet (TOI-1231b), and a warm Saturn (HATS-6b). We also include the sample of hot and the ultra-hot Jupiters from Table 1 in Baxter et al. (2020) in the T_eff vs T_eq plot (top right) as smaller light grey points and a sample of small M dwarf orbiting planets from exoplanet.eu in the ρ_P vs T_eff plot (bottom left) as grey points with error bars. Potential UV targets (dark golden dots with error bars) are included for comparison (Tables C.1, C.2). The equilibrium temperature given in the literature have been rounded to the next 100 K. References: WASP-103 b: Gillon et al. (2014); WASP-121 b: Delrez et al. (2016); WASP-18 b: Hellier et al. (2009), Sheppard et al. (2017); WASP-43 b: Gillon et al. (2012); HAT-P-7 b: Van Eylen et al. (2012), Pál (2009); HD 209458 b: Torres et al. (2008); HD 189733b: Torres et al. (2008); HD 86226c: Teske et al. (2020); TOI-1634b: Cloutier et al. (2021); HATS-6b: Hartman et al. (2015); TOI-1231b: Burt et al. (2021); The rotational periods for the GCM models are taken from Baeyens et al. (2022).