Notes. On clouds: Both the ‘Thick’ and ‘Slab’ clouds are based on Burrows et al. (2006), and are vertically extended throughout the atmosphere above a base pressure, with a decaying mass fraction, though the slab clouds account for a greater range of aerosol opacities. The ‘Power law’ clouds parameterise the vertical extent and position using a power law, and fix the base pressure to the location at 2300 K. ‘AM01’ clouds balance the cloud sedimentation and vertical mixing to determine the particle size, and use the sedimentation fraction to determine the vertical extent. ‘ER4’ is the Exo-Rem4 model from Bonnefoy et al. (2016). ‘Mie’ clouds do not use physical optical constants, but directly fit for Mie scattering parameters. The ‘BT-Settl’ cloud model is based on radiation hydrodynamical simulations that solve for the diffusion and mixing of aerosol particles (Allard et al. 2012).^(a) Only T_int, a model parameter, is reported.^(b) W21 used high resolution spectroscopy, and did not infer masses or radii, using masses of 7.2 ± 0.7 M_Jup for the inner three planets and 5.8 ± 0.5 M_Jup for HR 8799 b. A radius of 1.2 ± 0.1 R_Jup was used for all planets. ^(c) R21 uncertainties were limited by the coarseness and boundaries of their model grid. ^(d) Single best retrieval parameters. ^(e) Bayesian model averaged parameters from group A ∩ B.^(f) Unweighted average parameters from group A ∩ B.

References. B11a: Barman et al. (2011); C11: Currie et al. (2011); G11: Galicher et al. (2011); M11: Madhusudhan et al. (2011); M12: Marley et al. (2012); L13: Lee et al. (2013); B15: Barman et al. (2015); B16: Bonnefoy et al. (2016); L17: Lavie et al. (2017); W21: Wang et al. (2021b); R21: Ruffio et al. (2021).