For , , , and , the same thermal eclipse depth at is
Thus a uncertainty gives
This assumes one independent eclipse measurement with that precision, negligible reflected light in the infrared, no atmosphere, and blackbody emission from the bare surface.
Figure 1.
Blackbody secondary-eclipse spectrum of a 600-kelvin Earth-size planet around the stated M dwarf
. The planet-star ratio is extremely small on the Wien tail at short wavelength and rises toward about 740 parts per million at 17 micrometres.

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