Wavelength-dependent pressure level, p_gas = p(τ_λ = 1), at which the optical depth due to cloud particles becomes unity, τ = 1, for the grid model planet T_eff,p = 1600 K, log(ɡ) = 3 [cgs], with a G-type host star. The most suitable wavelength region for cloud investigation is λ > 1 µm. The solid black lines show the results based on the original 1D profile extracted from the Baeyens et al. (2022) 3D GCM grid, and the blue lines show the results based on the extrapolated profiles. Only the hollow-spheres opacity are shown to demonstrate the maximum effects of the cloud opacity. The horizontal thin, red line indicates the upper boundary in pressure space of the 3D GCM computational domain. The atmosphere becomes optically thick already at the cloud top at shorter wavelength. The horizontal blue line indicates that the cloud is optically thick at p > 10⁻² bar at the substellar point.