Organic analysis of lunar samples and the Martian surface

In addition to the organogenic elements (H, C, N, O, S, P) which are necessary for the synthesis of organic molecules, the lunar samples from Apollo 11, 12, 14 and 15 contain substantial amounts (approximately equal to 10 to 100 microgram/g) of CO, N2 and CO2, which are released at relatively high temperatures and smaller amounts (approximately equal to 0.1 to 10 microgram/g) of more complex organic compounds (e.g. benzene). Most of these analyses have been performed by mass spectrometry or by combined gas chromatography-mass spectrometry after appropriate volatilization. The release of very small amounts of water has also been observed and is consistent with the findings of goethite (FeO.OH) and with measurements by the suprathermal ion detector. The lunar surface provides one of the less favorable solar system models for the synthesis of organic compounds yet small amounts of these compounds have been detected in the returned samples. It is reasonable to assume that the different physical and developmental features of the planet Mars (increased gravitational field, presence of an atmosphere with CO2, CO and H2O, recent volcanic and tectonic activity, etc.) would favor an increased organic content of the surface of this planet relative to the moon. Therefore the organic molecules present in the Martian soil should be measurable by miniaturized mass spectrometers after fractional distillation or gas chromatographic separation of the volatiles released by moderate heating.