Results for T_eff = 1400 K, log₁₀(ɡ [cms⁻²]) = 3.0 (left), T_eff = 1400 K, log₁₀(ɡ [cms⁻²]) = 5.0 (right), without particle-particle collisions (blue) and with particle-particle collisions (black). Top: pressure level at which the cloud vertical optical depth reaches certain thresholds: p(τ_v = 1) in solid lines and p(τ_v = 0.1). Bottom: number density-weighted surface-averaged radius of the cloud particle population above the pressure level at which cloud optical depth reaches unity (〈〈a〉 _A〉 , solid) and the average observable particle size (〈〈a〉_A〉τ, dashed). The Hubble instrument wavelength ranges (from Wakeford et al. 2020) are shown as the coloured bars at the top left; the wavelengths for the Transiting Exoplanet Survey Satellite (TESS; Ricker et al. 2015), the CHaracterising ExOPlanets Satellite (CHEOPS; Broeg et al. 2013), and the PLAnetary Transits and Oscillations of stars mission (PLATO Rauer et al. 2014) are below. Shown as the ‘ARIEL SW’ bar are the VISPhot (0.5–0.6 µm), FGS₁ (0.6–0.8 µm), and FGS₂ (0.8–1 µm) photometers and the NIRSpec (1.1–1.95 µm) spectrometer wavelengths (Mugnai et al. 2020). The ARIEL Infrared Spectrometer (AIRS) is shown as the bar to the right of this. The JWST wavelength ranges are shown in the group of bars at the bottom.