Simulated eclipse spectra of selected planets. The spectrum is calculated from the top-of-the-atmosphere emission, which ultimately depends on the temperatures of both the atmosphere and the surface. In strong SiO spectral features, emission originates from the upper layers of the atmosphere. For an adiabatic T–P profile, this leads to an extremely cold temperature reading and thus the eclipse spectra show deep absorption features. Although clouds do cool the atmosphere slightly, the changes in the eclipse depth are barely visible. Since clouds cool the surface more, the overall blackbody curve of the spectra is lowered and the difference between cloudy and cloudless is seen relatively most clearly on HD20329b and HD213885.