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Table 2

Cloud models studied for all planetary candidates listed in Table 1.

Model Shape fsed σ Xmax (ZPl) a (μm) Fe SCC

1 DHS 3 2 yes yes
2 DHS 1 2 yes yes

3 DHS 0.3 2 yes yes/no
4 DHS 0.01 2 yes yes/no

5 DHS 10-2 0.08 no yes
6 DHS 3 × 10-4 0.08 no yes
7 DHS 3 × 10-5 0.08 no yes

8 DHS 3 × 10-4 0.08 yes yes

9 Mie 3 × 10-4 0.08 no yes

Notes. The “shape” column describes whether the grain opacities are described assuming irregular grains (using DHS) or as homogeneous, spherical grains (using Mie theory). fsed is the standard settling parameter from the Ackerman & Marley (2001) cloud model and σ is the width of the log-normal particle size distribution function in this model. Note that the value of σ = 1 formally corresponds to a Dirac delta function. For the parametrized cloud model Xmax describes the maximum cloud mass fraction within the atmosphere, while a denotes the mono-disperse particle size. “Fe” denotes whether iron clouds have been included. The column “SCC” (“self-consistent coupling”) denotes whether the cloud opacities have been coupled to the atmospheric temperature iteration or whether the converged, cloud-free atmospheric temperature structure has been used to obtain spectra including clouds. Note that for GJ 1214b, for example, models 3 and 4 converged with self-consistent coupling.

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