Chemical Modeling for Predicting the Abundances of Certain Aldimines and Amines in Hot Cores

We consider six isomeric groups ({{CH}}₃{{N}}, {{CH}}₅{{N}}, {{{C}}}₂{{{H}}}₅{{N}}, {{{C}}}₂{{{H}}}₇{{N}}, {{{C}}}₃{{{H}}}₇{{N}}, and {{{C}}}₃{{{H}}}₉{{N}}) to review the presence of amines and aldimines within the interstellar medium (ISM). Each of these groups contains at least one aldimine or amine. Methanimine ({{CH}}₂{NH}) from {{CH}}₃{{N}} and methylamine ({{CH}}₃{{NH}}₂) from {{CH}}₅{{N}} isomeric group were detected a few decades ago. Recently, the presence of ethanimine ({{CH}}₃{CHNH}) from {{{C}}}₂{{{H}}}₅{{N}} isomeric group has been discovered in the ISM. This prompted us to investigate the possibility of detecting any aldimine or amine from the very next three isomeric groups in this sequence: {{{C}}}₂{{{H}}}₇{{N}}, {{{C}}}₃{{{H}}}₇{{N}}, and {{{C}}}₃{{{H}}}₉{{N}}. We employ high-level quantum chemical calculations to estimate accurate energies of all the species. According to enthalpies of formation, optimized energies, and expected intensity ratio, we found that ethylamine (precursor of glycine) from {{{C}}}₂{{{H}}}₇{{N}} isomeric group, (1Z)-1-propanimine from {{{C}}}₃{{{H}}}₇{{N}} isomeric group, and trimethylamine from {{{C}}}₃{{{H}}}₉{{N}} isomeric group are the most viable candidates for the future astronomical detection. Based on our quantum chemical calculations and from other approximations (from prevailing similar types of reactions), a complete set of reaction pathways to the synthesis of ethylamine and (1Z)-1-propanimine is prepared. Moreover, a large gas-grain chemical model is employed to study the presence of these species in the ISM. Our modeling results suggest that ethylamine and (1Z)-1-propanimine could efficiently be formed in hot-core regions and could be observed with present astronomical facilities. Radiative transfer modeling is also implemented to additionally aid their discovery in interstellar space.