Flux density evolutions during the cooling of a magma ocean with an atmospheric emissivity ϵ = 0.01, computed using brightness temperatures from Lupu et al. (2014, Fig. 7). As for Fig. 5, planets in the β Pictoris (37 pc), TW Hydrae (53 pc), and η Chamaeleontis (94 pc) associations are considered. The subplots indicate different telescope filter wavelengths. Each set of bars consists of flux evolutions for bodies in a given stellar association, orbiting central stars of spectral type (A, G or M). The colors indicate different time intervals after the occurrence of a giant impact (GI). Each vertical bar terminates according to the cooling timescale of the magma ocean Δt_MO (see Fig. 3B). Planetary sizes used for the flux calculations are taken from the data in Fig. 2, based on thespectral type of the host star and the age of the considered stellar association. The black and green horizontal dashed linesmark the sensitivity of the telescope filters for integration times of 5 and 50 h (Table 2), respectively.Magma ocean bodies displaying fluxes greater than these thresholds are detectable.