  Some families of carbonaceous chondrites are rich in prebiotic organics that
may have contributed to the origin of life on Earth and elsewhere. However, the
formation and chemical evolution of complex soluble organic molecules from
interstellar precursors under relevant parent body conditions has not been
thoroughly investigated. In this study, we approach this topic by simulating
meteorite parent body aqueous alteration of interstellar residue analogs. The
distributions of amines and amino acids are qualitatively and quantitatively
investigated and linked to closing the gap between interstellar and meteoritic
prebiotic organic abundances. We find that the abundance trend of methylamine >
ethylamine> glycine > serine > alanine > \b{eta}-alanine does not change from
pre- to post-aqueous alteration, suggesting that certain cloud conditions have
an influential role on the distributions of interstellar-inherited meteoritic
organics. However, the abundances for most of the amines and amino acids
studied here varied by about 2-fold when aqueously processed for 7 days at 125
{\deg}C, and the changes in the {\alpha}- to \b{eta}-alanine ratio were
consistent with those of aqueously altered carbonaceous chondrites, pointing to
an influential role of meteorite parent body processing on the distributions of
interstellar-inherited meteoritic organics. We detected higher abundances of
{\alpha}- over \b{eta}-alanine, which is opposite to what is typically observed
in aqueously altered carbonaceous chondrites; these results may be explained by
at least the lack of minerals and insoluble organic matter-relevant materials
in the experiments. The high abundance of volatile amines in the non-aqueously
altered samples suggests that these types of interstellar volatiles can be
efficiently transferred to asteroids and comets, supporting the idea of the
presence of interstellar organics in solar system objects.
