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An Earth-like extra-solar planet emits light which is many orders ofmagnitude fainter than that of the parent star. We propose a method ofidentifying bio-signature spectral lines in light from known extra-solarplanets based on Fourier spectroscopy in the infra-red, using an off-centerpart of a Fourier interferogram only. This results in superior sensitivity tonarrower molecular-type spectral bands, which are expected in the planetspectrum but are absent in the parent star. We support this idea by numericalsimulations which include photon and thermal noise, and show it to be feasibleat a luminosity ratio of 10^-6 for a Sun-like parent star in the infra-red. Wealso carried out a laboratory experiment to illustrate the method. The resultssuggest that this method should be applicable to real planet searches.

Spectroscopic identification of habitable extra-solar planets