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The class of meteorites called carbonaceous chondrites are examples ofmaterial from the solar system which have been relatively unchanged from thetime of their initial formation. These meteorites have been classifiedaccording to the temperatures and physical conditions of their parentplanetesimals. We collate available data on amino acid abundance in thesemeteorites and plot the concentrations of different amino acids for eachmeteorite within various meteorite subclasses. We plot average concentrationsfor various amino acids across meteorites separated by subclass and petrologictype. We see a predominance in the abundance and variety of amino acids in CM2and CR2 meteorites. The range in temperature corresponding to these subclassesindicates high degrees of aqueous alteration, suggesting aqueous synthesis ofamino acids. Within the CM2 and CR2 subclasses, we identify trends in relativefrequencies of amino acids to investigate how common amino acids are as afunction of their chemical complexity. These two trends (total abundance andrelative frequencies) can be used to constrain formation parameters of aminoacids within planetesimals. Our organization of the data supports an onionshell model for the temperature structure of planetesimals. The least alteredmeteorites (type 3) and their amino acids originated near cooler surfaceregions. The most active amino acid synthesis likely took place at intermediatedepths (type 2). The most altered materials (type 1) originated furthest towardparent body cores. This region is likely too hot to either favor amino acidsynthesis or for amino acids to be retained after synthesis.

Nature's Starships. I. Observed Abundances and Relative Frequencies of Amino Acids in Meteorites