  The class of meteorites called carbonaceous chondrites are examples of
material from the solar system which have been relatively unchanged from the
time of their initial formation. These meteorites have been classified
according to the temperatures and physical conditions of their parent
planetesimals. We collate available data on amino acid abundance in these
meteorites and plot the concentrations of different amino acids for each
meteorite within various meteorite subclasses. We plot average concentrations
for various amino acids across meteorites separated by subclass and petrologic
type. We see a predominance in the abundance and variety of amino acids in CM2
and CR2 meteorites. The range in temperature corresponding to these subclasses
indicates high degrees of aqueous alteration, suggesting aqueous synthesis of
amino acids. Within the CM2 and CR2 subclasses, we identify trends in relative
frequencies of amino acids to investigate how common amino acids are as a
function of their chemical complexity. These two trends (total abundance and
relative frequencies) can be used to constrain formation parameters of amino
acids within planetesimals. Our organization of the data supports an onion
shell model for the temperature structure of planetesimals. The least altered
meteorites (type 3) and their amino acids originated near cooler surface
regions. The most active amino acid synthesis likely took place at intermediate
depths (type 2). The most altered materials (type 1) originated furthest toward
parent body cores. This region is likely too hot to either favor amino acid
synthesis or for amino acids to be retained after synthesis.
